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CCD UBVRI Photometry of the Galactic open clusters: Be 89, Ru 135, and Be 10

Revista mexicana de …, 2010
By Roberto Vázquez
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© Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México Revista Mexicana de Astronom´ ıa y Astrof´ ısica, 46, 385–430 (2010) CCD UBVRI PHOTOMETRY OF THE GALACTIC OPEN CLUSTERS 1 : BE 89, RU 135, AND BE 10 ˙ Inci Akkaya, 2 William J. Schuster, 3 Ra´ ul Michel, 3 Carlos Chavarr´ ıa-K, 3 Andr´ e Moitinho, 4 Roberto V´ azquez, 3 and Y¨ uksel Karata¸ s 5 Received 2009 May 15; accepted 2010 August 15 RESUMEN Presentamos los par´ ametros fundamentales de enrojecimiento, metalicidad, edad y distancia de los c´ umulos abiertos poco estudiados Be 89, Ru 135 y Be 10, derivados de la fotometr´ ıa CCD UBVRI . Los enrojecimientos interestelares se mi- dieron en el diagrama color-color, y las metalicidades fotom´ etricas se derivaron del exceso de ultravioleta de las estrellas tipo F. Las distancias y edades se obtu- vieron ajustando isocronas a las secuencias observadas en cinco diagramas color- magnitud diferentes. Los promedios ponderados de los m´ odulos de distancia y distancias helioc´ entricas [(V 0 − M V ),d(kpc)] son: (11. m 90 ± 0. m 06, 2.4 ± 0.06) para Be 89, (9. m 58 ± 0. m 07, 0.81 ± 0.03) para Ru 135 y (11. m 16 ± 0. m 06, 1.7 ± 0.05) para Be 10, mientras que los promedios ponderados para las edades [log(A),A(Gyr)] son: (9.58 ± 0.06, 3.8 ± 0.6) para Be 89, (9.58 ± 0.06, 3.8 ± 0.7) para Ru 135 y (9.06 ± 0.05, 1.08 ± 0.08) para Be 10. ABSTRACT The fundamental parameters of reddening, metallicity, age, and distance are presented for the poorly studied open clusters Be 89, Ru 135, and Be 10, de- rived from their CCD UBVRI photometry. The interstellar reddenings, E(B–V ), were measured in the two-color diagram, and the photometric metallicities, [Fe/H], from the ultraviolet excesses of the F-type stars. By fitting isochrones to the ob- served sequences of the clusters in five different color-magnitude diagrams, the weighted averages of distance moduli and heliocentric distances [(V 0 –M V ),d(kpc)] are (11. m 90 ± 0. m 06, 2.4 ± 0.06) for Be 89, (9. m 58 ± 0. m 07, 0.81 ± 0.03) for Ru 135, and (11. m 16 ± 0. m 06, 1.7 ± 0.05) for Be 10, and the weighted averages of the ages [log(A),A(Gyr)] are (9.58 ± 0.06, 3.8 ± 0.6) for Be 89, (9.58 ± 0.06, 3.8 ± 0.7) for Ru 135, and (9.06 ± 0.05, 1.08 ± 0.08) for Be 10. Key Words: open clusters and associations: individual (Be10, Be89, Ru135) — stars: fundamental parameters — stars: Hertzsprung-Russell and C-M diagrams — techniques: photometric 1 Based on observations carried out at the San Pedro M´ artir National Astronomical Observatory (SPM), operated by In- stituto de Astronom´ ıa, Universidad Nacional Aut´ onoma de M´ exico, Ensenada, B. C., Mexico. 2 Department of Astronomy and Space Sciences, Erciyes University, Kayseri, Turkey. 3 Instituto de Astronom´ ıa, Universidad Nacional Aut´ onoma de M´ exico, Ensenada, B. C., Mexico. 4 SIM/IDL, Facultade de Ciencias da Universidade de Lis- boa, Lisboa, Portugal. 5 Istanbul University, Science Faculty, Department of As- tronomy and Space Sciences, Turkey. 1. INTRODUCTION Galactic open clusters, which contain a few tens to a few tens of thousands of stars and are a few parsecs across, are sparsely populated, loosely con- centrated, and gravitationally bound systems. With systematic image searches and follow-up photomet- ric surveys, new open clusters are currently be- ing discovered. By fitting the photometric observa- tions of open clusters to synthetic photometry result- ing from stellar models (i.e., theoretical isochrones), which include the newest input physics, stellar struc- ture, and differing heavy-element abundances, fun- 385
© Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México 386 AKKAYA ET AL. damental parameters such as interstellar reddening, metallicity, distance modulus, and age can be pre- cisely and accurately determined. These parameters have great importance concerning the age-metallicity relation and the metal-abundance gradient in the Galactic disk (e.g., Cameron 1985; Carraro & Chiosi 1994; Friel 1995), as well as the luminosity and mass functions of the open clusters (Piskunov et al. 2008). Open clusters are also very useful for testing the stel- lar evolutionary models, given that their stars were formed at the same time, out of the same cloud, and under similar environmental conditions. Thus, open clusters are ideal entities for the study of stellar evolution since physical properties are tightly con- strained, being mainly distinguished by the stellar mass, so that theoretical models of stellar formation and evolution can be compared with real clusters without excessive complications. For these analy- ses, the fundamental parameters such as interstel- lar reddening, metallicity, distance modulus, and age should be determined as precisely and accurately as possible. In Galactic studies, one of the more severe obser- vational limitations is due to the absence of photo- metric data for nearly half of the approximately 1500 open clusters known. Furthermore, there is a lack of homogeneity in the observations and analyses of the clusters studied. The catalogue of Lyng˚ a (1987), that resulted from a collection of data from many different sources and which includes 422 open clus- ters, constituted the observational basis for a large number of astronomical studies, led to important conclusions about the Galactic disk, and has been very useful for planning subsequent observations by other astronomers. However, this catalogue has been built from parameters obtained by various authors, with diverse observing techniques, distinct calibra- tions, and different criteria for determining the stel- lar ages, rendering it very inhomogeneous and lim- ited for studies requiring precision in the measure- ment of these fundamental parameters. As an ex- ample of the precision and accuracy that one can expect due to the effects of these inhomogeneities, we refer to Janes & Adler (1982), who found that distance moduli of a given cluster obtained by two or more authors have a mean difference of 0. m 55. Within the Sierra San Pedro M´ artir, National As- tronomical Observatory (hereafter SPM) open clus- ter project (cf. Schuster et al. 2007; Michael et al. 2010, in preparation), the aims are the following: 1. A common UBVRI photometric scale for open clusters. 2. An atlas of color-color and color-magnitude di- agrams for these clusters. 3. A homogeneous set of cluster reddenings, dis- tances, ages, and, if possible, metallicities. 4. An increased number of old, significantly red- dened, or distant, open clusters. 5. A selection of interesting clusters for further study. The open clusters for the present study were selected from the large (and most complete) catalogue, “Op- tically visible open Clusters and Candidates” (Dias et al. 2002), which is now also available at the Centre de Donn´ ees Astronomiques de Strasbourg (CDS) 6 . This work aims to provide the fundamental parame- ters of reddening, metallicity, distance modulus and age for the open clusters Be 89, Ru 135, and Be 10. Our final intention is to publish a set of homogeneous photometric UBVRI data for over 300 Galactic clus- ters (Schuster et al. 2007; Tapia et al. 2010). This paper is organized as follows: § 2 describes the observations and reduction techniques. § 3 con- tains the derivation from the UBVRI photometry of reddening and metallicity of the clusters from two- color diagrams, and the inference of distance moduli and ages from color-magnitude diagrams. Their un- certainties are also discussed. Comparisons of these parameters with previous results from the literature are made in § 4, and the conclusions are given in § 5. 2. OBSERVATION AND REDUCTION TECHNIQUES 2.1. The observations This CCD UBVRI project of northern open clus- ters has been undertaken at SPM using always the same instrumental setup (telescope, CCD-detector, and filters), observing procedures, reduction meth- ods, and system of standard stars (Landolt 1983, 1992). A par focal set of UBVRI Johnson-Cousins filters was used for our observations. The 0.84 m f/13 Cassegrain telescope hosted the filter-wheel “Mex- man” provided with the SITE#1 (SI003) CCD cam- era, which has a 1024 × 1024 square pixel array and a 24 µm × 24 µm pixel size; this CCD has non- linearities less than 0.45% over a wide dynamical range, no evidence for fringing even in the I band, and Metachrome II and VISAR coverings to increase sensitivity in the blue and near ultraviolet. The sky- projected pixel size was 0 . ′′ 393, and the field of view 6 http://www.astro.iag.usp.br/~wilton/.
Revista Mexicana de Astronomı́a y Astrofı́sica, 46, 385–430 (2010) CCD UBVRI PHOTOMETRY OF THE GALACTIC OPEN CLUSTERS1 : BE 89, RU 135, AND BE 10 İnci Akkaya,2 William J. Schuster,3 Raúl Michel,3 Carlos Chavarrı́a-K,3 André Moitinho,4 Roberto Vázquez,3 and Yüksel Karataş5 Received 2009 May 15; accepted 2010 August 15 RESUMEN © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México Presentamos los parámetros fundamentales de enrojecimiento, metalicidad, edad y distancia de los cúmulos abiertos poco estudiados Be 89, Ru 135 y Be 10, derivados de la fotometrı́a CCD UBVRI. Los enrojecimientos interestelares se midieron en el diagrama color-color, y las metalicidades fotométricas se derivaron del exceso de ultravioleta de las estrellas tipo F. Las distancias y edades se obtuvieron ajustando isocronas a las secuencias observadas en cinco diagramas colormagnitud diferentes. Los promedios ponderados de los módulos de distancia y distancias heliocéntricas [(V0 − MV ), d(kpc)] son: (11.m 90 ± 0.m 06, 2.4 ± 0.06) para Be 89, (9.m 58 ± 0.m 07, 0.81 ± 0.03) para Ru 135 y (11.m 16 ± 0.m 06, 1.7 ± 0.05) para Be 10, mientras que los promedios ponderados para las edades [log(A), A(Gyr)] son: (9.58 ± 0.06, 3.8 ± 0.6) para Be 89, (9.58 ± 0.06, 3.8 ± 0.7) para Ru 135 y (9.06 ± 0.05, 1.08 ± 0.08) para Be 10. ABSTRACT The fundamental parameters of reddening, metallicity, age, and distance are presented for the poorly studied open clusters Be 89, Ru 135, and Be 10, derived from their CCD UBVRI photometry. The interstellar reddenings, E(B–V ), were measured in the two-color diagram, and the photometric metallicities, [Fe/H], from the ultraviolet excesses of the F-type stars. By fitting isochrones to the observed sequences of the clusters in five different color-magnitude diagrams, the weighted averages of distance moduli and heliocentric distances [(V0 –MV ), d(kpc)] are (11.m 90 ± 0.m 06, 2.4 ± 0.06) for Be 89, (9.m 58 ± 0.m 07, 0.81 ± 0.03) for Ru 135, and (11.m 16 ± 0.m 06, 1.7 ± 0.05) for Be 10, and the weighted averages of the ages [log(A), A(Gyr)] are (9.58 ± 0.06, 3.8 ± 0.6) for Be 89, (9.58 ± 0.06, 3.8 ± 0.7) for Ru 135, and (9.06 ± 0.05, 1.08 ± 0.08) for Be 10. Key Words: open clusters and associations: individual (Be10, Be89, Ru135) — stars: fundamental parameters — stars: Hertzsprung-Russell and C-M diagrams — techniques: photometric 1. INTRODUCTION 1 Based on observations carried out at the San Pedro Mártir National Astronomical Observatory (SPM), operated by Instituto de Astronomı́a, Universidad Nacional Autónoma de México, Ensenada, B. C., Mexico. 2 Department of Astronomy and Space Sciences, Erciyes University, Kayseri, Turkey. 3 Instituto de Astronomı́a, Universidad Nacional Autónoma de México, Ensenada, B. C., Mexico. 4 SIM/IDL, Facultade de Ciencias da Universidade de Lisboa, Lisboa, Portugal. 5 Istanbul University, Science Faculty, Department of Astronomy and Space Sciences, Turkey. Galactic open clusters, which contain a few tens to a few tens of thousands of stars and are a few parsecs across, are sparsely populated, loosely concentrated, and gravitationally bound systems. With systematic image searches and follow-up photometric surveys, new open clusters are currently being discovered. By fitting the photometric observations of open clusters to synthetic photometry resulting from stellar models (i.e., theoretical isochrones), which include the newest input physics, stellar structure, and differing heavy-element abundances, fun385 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México 386 AKKAYA ET AL. damental parameters such as interstellar reddening, metallicity, distance modulus, and age can be precisely and accurately determined. These parameters have great importance concerning the age-metallicity relation and the metal-abundance gradient in the Galactic disk (e.g., Cameron 1985; Carraro & Chiosi 1994; Friel 1995), as well as the luminosity and mass functions of the open clusters (Piskunov et al. 2008). Open clusters are also very useful for testing the stellar evolutionary models, given that their stars were formed at the same time, out of the same cloud, and under similar environmental conditions. Thus, open clusters are ideal entities for the study of stellar evolution since physical properties are tightly constrained, being mainly distinguished by the stellar mass, so that theoretical models of stellar formation and evolution can be compared with real clusters without excessive complications. For these analyses, the fundamental parameters such as interstellar reddening, metallicity, distance modulus, and age should be determined as precisely and accurately as possible. In Galactic studies, one of the more severe observational limitations is due to the absence of photometric data for nearly half of the approximately 1500 open clusters known. Furthermore, there is a lack of homogeneity in the observations and analyses of the clusters studied. The catalogue of Lyngå (1987), that resulted from a collection of data from many different sources and which includes 422 open clusters, constituted the observational basis for a large number of astronomical studies, led to important conclusions about the Galactic disk, and has been very useful for planning subsequent observations by other astronomers. However, this catalogue has been built from parameters obtained by various authors, with diverse observing techniques, distinct calibrations, and different criteria for determining the stellar ages, rendering it very inhomogeneous and limited for studies requiring precision in the measurement of these fundamental parameters. As an example of the precision and accuracy that one can expect due to the effects of these inhomogeneities, we refer to Janes & Adler (1982), who found that distance moduli of a given cluster obtained by two or more authors have a mean difference of 0.m 55. Within the Sierra San Pedro Mártir, National Astronomical Observatory (hereafter SPM) open cluster project (cf. Schuster et al. 2007; Michael et al. 2010, in preparation), the aims are the following: 1. A common UBVRI photometric scale for open clusters. 2. An atlas of color-color and color-magnitude diagrams for these clusters. 3. A homogeneous set of cluster reddenings, distances, ages, and, if possible, metallicities. 4. An increased number of old, significantly reddened, or distant, open clusters. 5. A selection of interesting clusters for further study. The open clusters for the present study were selected from the large (and most complete) catalogue, “Optically visible open Clusters and Candidates” (Dias et al. 2002), which is now also available at the Centre de Données Astronomiques de Strasbourg (CDS)6 . This work aims to provide the fundamental parameters of reddening, metallicity, distance modulus and age for the open clusters Be 89, Ru 135, and Be 10. Our final intention is to publish a set of homogeneous photometric UBVRI data for over 300 Galactic clusters (Schuster et al. 2007; Tapia et al. 2010). This paper is organized as follows: § 2 describes the observations and reduction techniques. § 3 contains the derivation from the UBVRI photometry of reddening and metallicity of the clusters from twocolor diagrams, and the inference of distance moduli and ages from color-magnitude diagrams. Their uncertainties are also discussed. Comparisons of these parameters with previous results from the literature are made in § 4, and the conclusions are given in § 5. 2. OBSERVATION AND REDUCTION TECHNIQUES 2.1. The observations This CCD UBVRI project of northern open clusters has been undertaken at SPM using always the same instrumental setup (telescope, CCD-detector, and filters), observing procedures, reduction methods, and system of standard stars (Landolt 1983, 1992). A par focal set of UBVRI Johnson-Cousins filters was used for our observations. The 0.84 m f/13 Cassegrain telescope hosted the filter-wheel “Mexman” provided with the SITE#1 (SI003) CCD camera, which has a 1024 × 1024 square pixel array and a 24 µm × 24 µm pixel size; this CCD has nonlinearities less than 0.45% over a wide dynamical range, no evidence for fringing even in the I band, and Metachrome II and VISAR coverings to increase sensitivity in the blue and near ultraviolet. The skyprojected pixel size was 0.′′393, and the field of view 6 http://www.astro.iag.usp.br/~wilton/. UBVRI PHOTOMETRY OF OPEN CLUSTERS TABLE 1 LANDOLT’S FIELDS OF STANDARD STARS © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México July 2001 February 2002 Region Nstds Region Nstds PG1528+062 PG1530+057 PG1633+099 PG1657+078 PG2213-006 PG2331+055 MARK A 3 3 5 4 4 3 4 PG0918+029 PG0942-029 PG1047+003 PG1323-086 PG1528+062 SA 95 SA104 SA107 5 5 4 5 3 5 4 4 TOTAL 26 TOTAL 35 of the detector was 6.73×6.73 arcmin2 . Here the results of UBVRI images for the open clusters Be 89, Ru 135, and Be 10 are presented, which were acquired in July 2001 (Be 89 and Ru 135) and February 2002 (Be 10). The exposure times were typically 3×240 seconds for the U filter, 3×180 for B, 3×100 for V , 3 × 100 for R, and 3 × 120 for I. Several standard-star fields from Landolt (1992) were observed nightly to permit the derivation of the photometric transformations to the Johnson-Cousins’ system and the atmospheric extinction coefficients. For the July 2001 observing run, seven Landolt groups were used, containing 26 different standard stars with color ranges, −0.m 25 ≤ (B − V ) ≤ +1.m 14, −1.m 09 ≤ (U −B) ≤ +1.m 14, and −0.m 30 ≤ (V −I) ≤ +1.m 14. Sixteen to twenty-five observations of these Landolt standards were made per night. For the February 2002 run, eight Landolt groups were employed, containing 35 different standard stars with color ranges, −0.m 30 ≤ (B − V ) ≤ +1.m 42, −1.m 18 ≤ (U − B) ≤ +1.m 27, and −0.m 28 ≤ (V − I) ≤ +1.m 77. Fifty-two to seventy-two observations of these Landolt standards were made per night, except one night cut short by clouds, when only 15 observations were managed. The standard-star fields have been observed with exposures of 1 × 240 seconds for the U filter, 1 × 120 for B, 1 × 60 for V , 1 × 60 for R, and 1 × 60 for I. The observed Landolt fields and the number of associated stars in each one are summarized in Table 1. Usually one or more Landolt fields were reobserved nightly with an air-mass range of at least 0.70 in order to measure the coefficients of the atmospheric extinction of the SPM site, which has excel- 387 lent sky conditions. To improve the accuracy, precision, and efficiency of the photometric observations when required, the filters were observed in forward and backward sequences (i.e., UBVRI − IRVBU ), especially for the large air-mass observations. 2.2. Data reduction The usual (night and run) calibrations for CCD photometry were done during each of our observing periods (i.e., bias, twilight-sky flat fields, and darkcurrent determinations) to determine the (night and run) mean correcting frames. Standard data reduction procedures have been used within IRAF,7 the CCDRED and DAOPHOT tasks (aperture and PSF photometry, see Howell 1989, 1990; Stetson 1987, 1990). More details concerning the instrumentation and the observing and reduction procedures of this project will be given in the near future in the succeeding paper of this project (Michel et al. 2010, in preparation, and references therein). To obtain the magnitudes and colors on the standard system for the stars associated with these clusters, we followed Jordi et al. (1995), and Rosselló et al. (1988, and references therein). We proceeded twofold: (i) The natural magnitude of the filter N is defined as: λN n = −2.5·log (ADU ′ s)N , where λN stands for the corresponding filters U, B, V, R, and I, ADU ′ s for the analog-to-digital counts, and the subscript n for the corresponding quantity in the natural photometric system. The atmospheric extinction coefficients for a given filter have been estimated by transforming the nightly λN n ’s to the corresponding magnitudes in the standard system, λN s ’s, with the following equation: ′ λN s − λN n = (zero point)N − κN · XNn ′′ −κN,12 · XN n · (λ1 − λ2 )s , (1) where XN n is the air-mass when measuring λN n . The subscript N, 12 indicates that the color (λ1 − λ2 )s was used to determine the second-order extinction coefficient of filter N . Here we follow the convention that the effective wavelength λ1eff < λ2eff to construct the color (λ1 − λ2 ). Finally, for a proper ′ ′′ determination of κN and κN,12 by a least squares solution, sufficiently large ranges in the air masses and colors of the standard stars (∆XN ≥ 0.7 and ∆(λ1 − λ2 )n ≥ 0.8 for SPM) must be obtained. Note that the standard magnitudes and colors are known to an accuracy of about two percent, reflected in the 7 IRAF is distributed by NOAO (operated by the Association of Universities for Research in Astronomy, Inc.) under cooperative agreement with NSF. 388 AKKAYA ET AL. TABLE 2 ATMOSPHERIC EXTINCTION AND TRANSFORMATION COEFFICIENTS Color λ1 λ2 λ3 ′ ′′ κ1 κ1,12 κ0,12 β12 γ12 rms +1.625 +0.409 +2.375 +0.027 −0.151 0.711 1.016 0.033 0.973 0.923 +0.263 −0.050 −0.008 +0.011 +0.070 0.028 0.010 0.016 0.012 0.010 +1.765 +0.470 +2.455 −0.000 −0.165 0.751 0.979 0.035 1.023 1.038 +0.313 −0.023 −0.054 −0.008 +0.004 0.037 0.018 0.027 0.012 0.014 July 2001 (U − B) (B − V ) V (V − R) (V − I) U B V V V B V R R I V – – – – 0.472 0.243 0.106 0.104* 0.087* −0.056 −0.050 +0.079 +0.030* −0.035* © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México February 2002 (U − B) (B − V ) V (V − R) (V − I) * U B V V V B V R R I V – – – – 0.325 0.212 0.082 0.054* 0.056* −0.056 −0.050 +0.079 +0.030* −0.035* Indicates that extinction coefficients refer to λ2 , otherwise to λ1 . errors of the final transformations of the (bright) standard stars, and that the observed magnitudes and air masses are measured quantities that can have an even better precision. To further simplify the equations, the extra-atmospheric instrumental magnitudes were then introduced using the extinction coefficients of the night: ′ ′′ λN i = λN n −κN ·XN n −κN,12 ·XN n ·(λ1 −λ2 )s . (2) An instrumental color is the subtraction of two instrumental magnitudes with different passbands, (λ1 − λ2 )i = λ1i − λ2i . ′ (ii) Once the atmospheric extinction coefficients κN ′′ and κN,12 have been determined and applied, the nightly transformation coefficients are calculated (i.e., β12 and γ12 ) with the following relations for the colors: (λ1 − λ2 )i = κ0,12 + β12 · (λ1 − λ2 )s + γ12 · (λ1 − λ2 )2s . (3) Due to the Balmer discontinuity that lies in both the U and B passbands, a better transformation for the U − B color has been achieved by substituting the quadratic term on the right side of the above equation with a linear term in the color B − V , obtaining the following expression: (λ1 − λ2 )i = κ0,12 + β12 · (λ1 − λ2 )s + γ12 · (λ2 − λ3 )s , (4) where λ1eff < λ2eff < λ3eff . For the case of the magnitude V , equation (3) has been used as follows: Vi − Vs = κ01 + β12 · (λ1 − λ2 )s + γ12 · (λ1 − λ2 )2s . (5) For equations (3)–(5), κ0,12 and κ01 are the zeropoints of the transformations of the colors (λ1 −λ2 )s , i.e., U − B, B − V , V − R, V − I, etc., and of the V magnitude, respectively. The coefficients β12 and γ12 are the respective first- and second-order transformation coefficients. In general, the second-order atmospheric extinc′′ tion coefficient κV R is expected to be close to zero due to the nearly constant level (ozone-band contribution) of the atmospheric extinction curve at SPM near 5500 Å (Schuster & Parrao 2001). The secondorder extinction and linear-transformation coefficients for correcting to extra-atmospheric standard magnitudes and colors are very similar from night to night, and also from run to run, because, (i) the SPM has excellent sky conditions, and (ii) the same instrumental setup, observing techniques, and data reduction procedures were used for all nights during both observing runs. In Table 2 the mean zero-point corrections, atmospheric extinction, and transformation coefficients are given. In Tables 3, 4, and 5 are given the final transformed CCD UBVRI photometric values for the open clusters, Be 89, Ru 135, and Be 10, respectively. In these tables Columns 1 and 2 give the X and Y (pixels) the position of a star in the CCD field; Columns 3, 5, 7, 9, and 11 the magnitude and color indices V , (B − V ), (U − B), (V − R), and (V − I), respectively (in magnitudes); and Columns 4, 6, 8, 10, and 12 the respective photometric errors, σV , σB−V , σU −B , σV −R , and σV −I (in magnitudes), as provided by IRAF. UBVRI PHOTOMETRY OF OPEN CLUSTERS 389 TABLE 3 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México CCD UBVRI PHOTOMETRY OF BE 89 X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 767.7 466.5 511.7 213 741.7 113.3 678.3 464.6 834.1 701.2 254.5 198 312.4 541.6 334.6 842.2 592.1 560.7 613.3 675.9 360.9 482.7 645.6 268.8 399.4 323 791.4 416.2 219.1 758.7 385.7 797.4 196 365.3 338.1 579.6 738.4 640.5 535.4 521.7 923.2 648.5 620.5 408.6 574.2 697.8 916.7 601.1 53 350.5 112.3 389.8 803 538 925.7 594.4 653.4 299.5 298.7 330 969 328.6 281.7 538.3 496.2 742.6 99.5 403.2 465.7 596.5 338.7 610.2 578.9 280.4 28.1 276.8 770.5 31.2 789.4 526.6 782.1 190.6 887.1 268.5 702.4 248.1 739 206.7 88.8 99.7 595.1 264.4 277.5 51 412.5 157.7 316 499.2 621.2 183 610.8 889.9 859.9 159.1 469.9 76.6 525 818 177.7 274.2 523.6 615 182.5 890.9 609.1 547.1 360.7 533.9 466.9 273.1 235.1 224.4 898.6 823.5 933.5 565.7 11.261 12.118 12.172 12.333 12.911 13.309 13.754 13.761 13.972 13.98 14.089 14.141 14.279 14.368 14.416 14.475 14.528 14.593 14.663 14.669 14.678 14.727 14.744 14.759 14.83 14.851 14.862 14.916 14.92 15.017 15.02 15.033 15.054 15.062 15.082 15.095 15.1 15.128 15.137 15.181 15.185 15.227 15.257 15.258 15.283 15.297 15.308 15.338 15.445 15.466 15.494 15.51 15.534 15.571 15.576 15.658 15.665 15.713 15.766 15.832 15.875 15.876 15.921 0.006 0.011 0.008 0.006 0.005 0.004 0.006 0.006 0.004 0.005 0.004 0.016 0.004 0.01 0.006 0.004 0.006 0.006 0.006 0.005 0.004 0.005 0.006 0.005 0.006 0.006 0.005 0.006 0.004 0.003 0.005 0.004 0.004 0.006 0.029 0.006 0.005 0.006 0.004 0.004 0.007 0.006 0.006 0.006 0.004 0.005 0.004 0.007 0.008 0.006 0.011 0.006 0.005 0.007 0.006 0.007 0.006 0.006 0.006 0.007 0.007 0.008 0.006 0.441 1.362 0.443 0.791 1.193 0.658 1.921 0.706 0.735 0.875 0.819 1.317 1.948 1.818 0.779 2.238 0.79 0.868 1.711 0.846 1.717 1.649 0.691 1.001 0.914 0.726 1.574 0.829 0.83 1.582 1.059 1.676 1.644 0.687 1.49 1.553 0.983 1.618 1.647 1.652 0.816 1.596 0.906 0.705 1.718 1.225 1.523 0.671 1.002 0.911 0.863 0.807 1.337 1.071 0.997 0.873 0.77 1.038 0.979 2.318 1.662 0.839 0.979 0.009 0.018 0.011 0.009 0.007 0.006 0.014 0.01 0.007 0.009 0.007 0.025 0.014 0.059 0.01 0.012 0.011 0.009 0.018 0.009 0.011 0.011 0.009 0.01 0.01 0.009 0.012 0.012 0.008 0.01 0.01 0.012 0.013 0.01 0.048 0.018 0.01 0.015 0.01 0.012 0.015 0.015 0.011 0.012 0.013 0.012 0.012 0.012 0.016 0.011 0.019 0.011 0.012 0.014 0.011 0.013 0.012 0.012 0.011 0.023 0.018 0.015 0.014 0.002 1.191 0.268 0.359 0.855 −0.019 1.75 0.07 0.113 0.333 0.176 0.695 2.029 1.688 0.179 99.999 0.104 0.25 99.999 0.241 1.441 1.23 0.366 0.655 0.308 0.131 1.299 0.256 0.184 1.294 0.974 1.436 1.39 0.347 99.999 1.32 0.543 1.289 1.373 1.448 0.248 1.371 0.312 0.313 1.414 0.75 1.284 0.251 0.516 0.326 0.22 0.09 1.052 0.379 0.578 0.559 0.357 0.406 0.271 99.999 1.08 0.127 0.506 0.007 0.011 0.005 0.007 0.008 0.006 0.024 0.01 0.009 0.011 0.009 0.015 0.041 0.058 0.012 99.999 0.011 0.013 99.999 0.013 0.032 0.029 0.013 0.015 0.015 0.013 0.033 0.015 0.014 0.035 0.022 0.042 0.041 0.013 99.999 0.046 0.024 0.042 0.041 0.042 0.02 0.044 0.018 0.017 0.049 0.027 0.037 0.015 0.026 0.025 0.022 0.016 0.041 0.02 0.026 0.023 0.02 0.026 0.024 99.999 0.063 0.02 0.03 0.315 0.742 0.296 0.378 0.629 0.351 1.058 0.396 0.403 0.508 0.463 0.871 1.023 0.95 0.425 1.33 0.422 0.454 0.907 0.481 0.901 0.895 0.353 0.55 0.518 0.409 0.872 0.443 0.481 0.868 0.612 0.916 0.89 0.363 0.897 0.874 0.495 0.917 0.884 0.909 0.465 0.878 0.508 0.408 0.914 0.643 0.818 0.403 0.527 0.5 0.521 0.456 0.763 0.641 0.537 0.471 0.456 0.609 0.542 1.272 0.982 0.491 0.497 0.009 0.013 0.011 0.012 0.008 0.005 0.009 0.008 0.007 0.01 0.006 0.019 0.006 0.015 0.009 0.006 0.009 0.007 0.01 0.006 0.006 0.007 0.008 0.007 0.007 0.007 0.008 0.008 0.006 0.006 0.007 0.007 0.007 0.007 0.037 0.012 0.006 0.01 0.006 0.007 0.01 0.01 0.007 0.009 0.007 0.007 0.007 0.01 0.011 0.008 0.016 0.008 0.008 0.009 0.007 0.01 0.008 0.008 0.008 0.009 0.01 0.011 0.008 99.999 1.399 0.569 99.999 1.182 0.705 2 0.725 0.777 0.932 0.897 1.663 1.985 1.842 0.853 2.632 0.858 0.902 1.785 0.929 1.683 1.752 0.787 1.024 0.95 0.829 1.696 0.878 0.913 1.68 1.092 1.763 1.715 0.79 1.713 1.684 0.986 1.726 1.718 1.733 0.974 99.999 0.998 0.884 1.785 1.283 1.602 0.884 1.011 1.006 0.961 0.885 1.397 1.239 1.01 1.031 0.952 1.23 1.115 2.36 1.87 0.959 0.976 99.999 0.013 0.017 99.999 0.01 0.006 0.012 0.007 0.006 0.008 0.006 0.017 0.007 0.015 0.008 0.011 0.009 0.007 0.008 0.006 0.006 0.007 0.007 0.007 0.007 0.007 0.007 0.008 0.006 0.005 0.007 0.006 0.006 0.007 0.032 0.013 0.006 0.009 0.006 0.007 0.009 99.999 0.007 0.007 0.007 0.007 0.006 0.01 0.01 0.007 0.024 0.007 0.007 0.008 0.007 0.009 0.008 0.007 0.007 0.007 0.008 0.01 0.009 390 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 337.1 375.5 110.4 713.7 451 369.5 162.3 271.3 471.7 356.9 476.4 181.2 802 22.8 276.6 512.7 234.9 329 489.9 733.2 305.2 437 535.2 918.4 800.1 550.3 32.2 985.1 31.9 172.4 196.1 624 860.7 555.2 659.5 502.4 797.1 89.5 852.3 602.7 910.3 474.6 155.5 667.2 340 612.5 638.7 121.6 148.3 566.6 489.2 190.8 16.9 634.9 366.6 481.7 951.4 809.9 479 540.8 804.6 705.8 126.4 70.3 231.1 623.4 847.5 961 22.8 508.7 170.1 731 105.4 585.8 708 570.8 944.2 593.9 76.8 796 161.5 633.8 471.8 562.9 794.9 840.3 570.1 540.7 181.7 734.7 660.5 883.4 387.1 844.7 134.1 310.2 463.7 116.4 346.8 820.6 82.9 496.5 532.4 148.8 723.9 744.4 116.8 37.2 46.2 851.1 514.7 75.3 104.7 445.5 490.7 177 98.6 777.2 654.1 579.9 654.7 209.9 321.1 327.2 337.6 180.9 675 135.2 281.9 990 15.964 15.993 16.023 16.05 16.078 16.087 16.115 16.162 16.185 16.191 16.2 16.211 16.212 16.24 16.241 16.248 16.28 16.291 16.304 16.312 16.322 16.329 16.358 16.358 16.359 16.378 16.394 16.407 16.409 16.413 16.421 16.428 16.432 16.457 16.457 16.467 16.472 16.492 16.501 16.515 16.523 16.527 16.538 16.554 16.556 16.565 16.576 16.587 16.587 16.594 16.597 16.61 16.621 16.621 16.632 16.632 16.633 16.646 16.669 16.68 16.684 16.7 16.706 16.71 16.711 0.033 0.007 0.012 0.014 0.006 0.006 0.008 0.008 0.006 0.006 0.012 0.009 0.007 0.012 0.007 0.007 0.006 0.011 0.007 0.006 0.005 0.008 0.008 0.008 0.006 0.007 0.015 0.008 0.015 0.008 0.007 0.008 0.007 0.012 0.007 0.007 0.007 0.008 0.01 0.008 0.007 0.007 0.01 0.007 0.008 0.008 0.007 0.01 0.008 0.011 0.007 0.009 0.013 0.009 0.007 0.008 0.012 0.007 0.008 0.013 0.018 0.008 0.008 0.007 0.009 1.211 0.994 0.917 0.946 1.176 1.074 1.018 0.983 1.207 1.081 1.113 1.182 0.882 0.897 2.443 1.015 1.634 1.307 0.927 1.208 1.173 1.223 1.619 1.065 1.084 0.987 0.99 2.525 1.148 1.067 1.047 0.975 1.057 1.537 1.293 1.077 1.024 1.681 0.886 2.703 1.097 1.121 1.145 1.143 1.061 1.09 1.082 2.263 1.048 1.077 1.148 1.016 1.13 1.07 1.145 1.155 1.097 1.114 1.193 1.412 1.015 1.016 1.022 1.154 1.063 0.052 0.015 0.022 0.023 0.016 0.014 0.016 0.016 0.015 0.016 0.024 0.021 0.015 0.022 0.026 0.015 0.019 0.024 0.016 0.016 0.016 0.019 0.022 0.018 0.015 0.016 0.028 0.035 0.028 0.019 0.016 0.016 0.019 0.022 0.019 0.017 0.016 0.023 0.021 0.043 0.018 0.019 0.021 0.016 0.018 0.018 0.019 0.036 0.018 0.025 0.019 0.02 0.027 0.019 0.02 0.021 0.025 0.019 0.021 0.024 0.036 0.019 0.018 0.021 0.023 0.477 0.453 0.315 0.373 0.392 0.431 0.458 0.297 0.464 0.463 0.451 0.455 0.252 0.305 99.999 0.379 1.317 1.078 0.405 0.617 0.614 0.526 1.143 0.713 0.722 0.35 0.285 99.999 0.624 0.538 0.436 0.5 0.44 1.151 0.622 0.407 0.397 99.999 0.361 99.999 0.384 0.381 0.705 99.999 0.213 0.459 0.376 99.999 0.335 0.411 0.428 0.394 0.337 0.304 0.421 0.491 0.623 0.429 0.889 1.014 0.396 0.349 0.358 0.568 0.424 0.035 0.031 0.027 0.035 0.041 0.03 0.031 0.029 0.037 0.029 0.037 0.036 0.029 0.032 99.999 0.035 0.087 0.055 0.031 0.04 0.045 0.04 0.081 0.056 0.042 0.027 0.037 99.999 0.051 0.044 0.037 0.043 0.039 0.074 0.052 0.038 0.035 99.999 0.035 99.999 0.033 0.041 0.05 99.999 0.041 0.04 0.041 99.999 0.036 0.049 0.05 0.043 0.046 0.039 0.043 0.048 0.05 0.042 0.064 0.08 0.063 0.036 0.038 0.055 0.05 0.656 0.542 0.567 0.559 0.679 0.641 0.582 0.551 0.655 0.634 0.639 0.724 0.494 0.57 1.332 0.588 0.901 0.727 0.53 0.717 0.694 0.682 0.92 0.585 0.595 0.531 0.585 1.364 0.631 0.613 0.558 0.533 0.643 0.851 0.739 0.648 0.625 0.924 0.551 1.587 0.679 0.642 0.638 0.569 0.605 0.618 0.626 1.248 0.6 0.656 0.623 0.528 0.646 0.622 0.691 0.649 0.594 0.645 0.626 0.819 0.421 0.609 0.564 0.678 0.65 0.047 0.009 0.018 0.034 0.009 0.008 0.01 0.01 0.01 0.008 0.029 0.016 0.009 0.017 0.009 0.01 0.008 0.019 0.01 0.009 0.008 0.012 0.011 0.012 0.009 0.01 0.02 0.01 0.02 0.011 0.009 0.011 0.012 0.011 0.01 0.01 0.011 0.011 0.014 0.01 0.01 0.01 0.014 0.01 0.011 0.012 0.011 0.013 0.01 0.019 0.01 0.012 0.018 0.013 0.011 0.012 0.02 0.011 0.012 0.013 0.049 0.011 0.012 0.012 0.016 1.349 1.044 1.051 1.207 1.366 1.262 1.158 1.104 1.359 1.33 1.285 1.34 0.956 1.103 2.534 1.206 1.712 1.429 1.098 1.435 1.378 1.393 1.736 1.102 1.122 1.121 99.999 2.644 99.999 1.262 1.102 1.055 1.289 1.67 1.471 1.279 1.275 1.786 1.051 3.138 1.35 1.271 1.212 1.123 1.195 1.301 1.26 2.36 1.217 1.314 1.271 1.074 1.275 1.25 1.383 1.371 1.104 1.276 1.168 1.583 1.112 1.254 1.127 1.367 1.302 0.035 0.009 0.034 0.023 0.009 0.007 0.009 0.01 0.008 0.007 0.026 0.027 0.009 0.015 0.008 0.008 0.007 0.026 0.009 0.008 0.008 0.01 0.01 0.009 0.008 0.009 99.999 0.008 99.999 0.01 0.009 0.012 0.009 0.009 0.009 0.01 0.008 0.009 0.029 0.008 0.009 0.009 0.03 0.009 0.01 0.011 0.01 0.011 0.009 0.014 0.009 0.011 0.017 0.012 0.01 0.01 0.029 0.009 0.011 0.011 0.043 0.011 0.011 0.011 0.014 UBVRI PHOTOMETRY OF OPEN CLUSTERS 391 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 699.6 521.1 535.5 228.4 457.6 341.7 117.5 609.1 285.2 137 283.5 875.4 646 950.4 702.9 791.6 444.9 27.9 346.7 865 528.3 796.7 89 875.6 337.5 363.3 345 397.1 559.6 737.7 64.4 441.6 621.1 548.5 393.8 960.9 474.1 228.6 490.7 507.7 907.1 763.3 199.4 431 465.3 307.3 539 723.5 676.3 960.1 462.5 644.8 938.6 910.1 473 110.2 743.3 139.5 444.2 802.7 262.2 30.5 352.4 588 328.1 149.3 506 304.3 593.8 417.9 150.6 677.4 701.3 586.1 372.4 57.3 230.6 637.8 189.7 955.9 205.4 34.3 886.1 344 505.3 698.1 158.7 808.1 485.8 763 573.6 253.6 845.7 440 258.6 175.6 469.4 540.1 711.8 473.8 931.9 552.7 274.8 545 216 680 911.5 13.4 371.1 114.7 234.8 303.5 743 716.3 844.3 542.5 122.5 483.7 919.8 611.3 642.8 347.4 848.1 599.1 294.5 983.6 544.8 618.3 777.6 375.7 16.725 16.726 16.752 16.755 16.765 16.767 16.768 16.776 16.781 16.781 16.786 16.791 16.793 16.796 16.802 16.805 16.806 16.809 16.846 16.847 16.851 16.856 16.857 16.857 16.858 16.872 16.885 16.891 16.897 16.903 16.906 16.912 16.914 16.916 16.919 16.927 16.932 16.936 16.941 16.978 16.98 16.987 16.989 16.995 17.017 17.022 17.023 17.031 17.037 17.038 17.054 17.064 17.065 17.07 17.076 17.086 17.09 17.095 17.101 17.103 17.11 17.116 17.135 17.138 17.139 0.008 0.007 0.014 0.008 0.008 0.007 0.007 0.008 0.008 0.008 0.008 0.009 0.008 0.009 0.008 0.007 0.011 0.015 0.009 0.007 0.008 0.009 0.012 0.008 0.011 0.009 0.007 0.008 0.008 0.011 0.009 0.008 0.01 0.008 0.015 0.008 0.008 0.01 0.01 0.007 0.008 0.008 0.01 0.009 0.014 0.01 0.017 0.01 0.006 0.011 0.011 0.012 0.009 0.008 0.009 0.01 0.01 0.012 0.008 0.006 0.01 0.009 0.008 0.008 0.011 1.137 1.203 99.999 1.067 1.084 1.055 1.098 0.944 1.19 1.079 1.033 1.686 0.941 1.119 1.073 1.029 1.078 1.125 1.112 1.166 1.096 2.059 2.062 1.21 1.084 0.991 1.132 1.041 1.09 0.866 1.845 1.121 1.047 1.117 1.134 1.093 1.165 0.965 1.693 1.122 1.142 1.076 1.065 2.693 1.188 2.23 99.999 1.928 1.093 1.191 0.865 1.052 1.026 1.079 1.165 1.142 1.134 0.986 1.133 1.031 1.12 1.1 1.107 1.07 1.051 0.02 0.022 99.999 0.018 0.02 0.02 0.021 0.018 0.02 0.021 0.021 0.025 0.018 0.022 0.021 0.018 0.029 0.031 0.021 0.022 0.019 0.037 0.037 0.025 0.025 0.019 0.02 0.02 0.022 0.021 0.032 0.022 0.023 0.024 0.034 0.022 0.023 0.023 0.03 0.023 0.021 0.025 0.025 0.051 0.03 0.043 99.999 0.035 0.02 0.026 0.023 0.031 0.022 0.023 0.026 0.024 0.023 0.025 0.025 0.022 0.025 0.026 0.025 0.024 0.026 0.445 0.423 99.999 0.297 0.501 0.343 0.412 0.242 0.556 0.407 0.301 99.999 0.255 0.444 0.389 0.396 0.605 0.408 0.456 0.525 0.392 99.999 99.999 0.575 0.489 0.256 0.474 0.36 0.364 0.513 99.999 0.537 0.406 0.302 0.38 0.691 0.553 0.636 99.999 0.517 0.464 0.419 0.363 99.999 99.999 99.999 99.999 99.999 0.316 0.519 0.454 0.46 0.48 0.349 0.467 0.466 0.465 0.325 0.35 0.533 0.45 0.282 0.372 0.36 0.389 0.05 0.051 99.999 0.049 0.049 0.05 0.056 0.044 0.058 0.05 0.041 99.999 0.046 0.047 0.051 0.041 0.058 0.055 0.059 0.047 0.05 99.999 99.999 0.055 0.057 0.047 0.047 0.048 0.051 0.05 99.999 0.056 0.055 0.054 0.052 0.061 0.069 0.06 99.999 0.061 0.067 0.05 0.056 99.999 99.999 99.999 99.999 99.999 0.056 0.067 0.054 0.063 0.059 0.065 0.064 0.065 0.058 0.06 0.06 0.068 0.066 0.06 0.07 0.067 0.066 0.629 0.69 0.548 0.643 0.612 0.632 0.699 0.574 0.709 0.629 0.611 0.932 0.579 0.617 0.648 0.571 0.661 0.581 0.63 0.705 0.634 1.138 1.105 0.599 0.571 0.583 0.657 0.628 0.616 0.515 1.05 0.677 0.601 0.642 0.726 0.649 0.649 0.559 0.94 0.646 0.631 0.654 0.597 1.471 0.744 1.252 0.508 1.046 0.613 0.719 0.557 0.596 0.607 0.646 0.676 0.645 0.615 0.594 0.66 0.613 0.61 0.629 0.609 0.618 0.578 0.011 0.012 0.05 0.012 0.011 0.011 0.012 0.012 0.011 0.012 0.011 0.012 0.01 0.014 0.013 0.01 0.019 0.042 0.012 0.012 0.012 0.012 0.017 0.014 0.018 0.012 0.011 0.012 0.013 0.014 0.013 0.013 0.013 0.013 0.045 0.015 0.012 0.013 0.013 0.012 0.011 0.012 0.016 0.012 0.021 0.012 0.06 0.012 0.011 0.015 0.014 0.019 0.012 0.013 0.014 0.014 0.014 0.018 0.012 0.011 0.015 0.015 0.012 0.012 0.015 1.279 1.379 99.999 1.264 1.239 1.209 1.341 1.171 1.379 1.224 1.225 1.824 1.061 1.303 1.277 1.208 1.244 99.999 1.311 1.397 1.291 2.192 2.137 1.234 1.149 1.194 1.347 1.278 1.282 1.087 2.038 1.294 1.146 1.285 1.456 1.345 1.333 1.093 1.866 1.27 1.326 1.322 1.266 2.801 1.357 2.387 99.999 2.081 1.253 1.408 1.073 1.226 1.3 1.281 1.342 1.319 1.292 1.171 1.338 1.164 1.226 1.3 1.285 1.226 1.176 0.01 0.01 99.999 0.012 0.01 0.01 0.009 0.01 0.01 0.011 0.01 0.01 0.01 0.012 0.011 0.009 0.032 99.999 0.012 0.01 0.01 0.009 0.014 0.011 0.016 0.011 0.011 0.01 0.011 0.013 0.011 0.012 0.012 0.011 0.019 0.013 0.012 0.012 0.011 0.011 0.01 0.012 0.015 0.009 0.036 0.011 99.999 0.011 0.01 0.012 0.012 0.014 0.012 0.013 0.012 0.013 0.013 0.015 0.012 0.01 0.013 0.013 0.011 0.011 0.014 392 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 483.7 863.8 433.7 659.9 6.8 798.5 500.4 122.5 105.6 228.4 422.2 370.6 234.2 227.1 465.7 939.4 698.4 577.4 841.5 191.2 433.9 990.5 256.6 72.1 718.7 78.1 18.5 155.1 167 295.3 828.6 225.2 768.4 756.9 441.8 838.2 916 900.7 273.2 537.3 292.2 522.9 520.8 331.5 491.6 496.6 715.5 560.8 649.7 451.4 27.4 91.2 694.9 282.6 729.7 480.3 719.4 863.8 915.3 885.8 368.6 475.2 813.4 421.9 937 613.6 539.9 875.2 385.8 313.8 918.2 607.6 981.5 945.9 154.3 539.7 439 343.7 821.9 248.2 176.1 981.9 617 346.2 676.1 990.1 723.5 669.7 429.1 71.2 850.3 219.1 955.3 21.9 505.3 353.3 114.1 225 386.8 494.7 847.6 358.1 93.4 622.7 569.2 742.1 33.2 847.5 821.6 464.3 132.8 758.5 66.1 229.5 513.5 448.9 632.9 797.3 702.2 314.3 645.2 230.2 60.3 33.9 159.6 506.4 921.3 464.2 770 240.9 17.148 17.151 17.155 17.156 17.16 17.16 17.163 17.164 17.172 17.183 17.183 17.184 17.186 17.192 17.192 17.192 17.203 17.206 17.211 17.226 17.239 17.239 17.24 17.242 17.242 17.252 17.275 17.275 17.281 17.283 17.287 17.3 17.306 17.307 17.311 17.316 17.327 17.331 17.333 17.337 17.348 17.354 17.357 17.364 17.373 17.374 17.381 17.383 17.384 17.391 17.395 17.397 17.397 17.406 17.419 17.432 17.447 17.447 17.455 17.46 17.463 17.465 17.469 17.474 17.488 0.009 0.01 0.009 0.008 0.013 0.009 0.009 0.011 0.012 0.011 0.008 0.009 0.011 0.008 0.009 0.01 0.009 0.017 0.011 0.012 0.007 0.009 0.009 0.01 0.011 0.012 0.01 0.012 0.015 0.011 0.01 0.013 0.01 0.008 0.011 0.009 0.01 0.01 0.007 0.011 0.011 0.01 0.011 0.008 0.01 0.011 0.012 0.012 0.01 0.016 0.01 0.009 0.01 0.011 0.011 0.013 0.014 0.01 0.011 0.009 0.013 0.011 0.01 0.009 0.011 1.14 1.026 1.105 2.042 1.108 1.403 1.122 1.112 1.529 1.112 1.046 1.051 1.187 1.085 1.103 1.276 1.132 1.051 0.902 1.195 1.035 1.11 1.123 1.236 1.323 1.131 1.147 1.127 1.143 1.932 1.08 1.36 1.067 1.145 1.193 1.105 1.089 1.051 1.028 1.088 1.107 1.308 1.113 1.062 1.119 1.092 1.233 1.208 2.199 1.191 1.132 1.184 1.134 1.08 1.022 2.001 1.186 2.317 1.029 1.176 1.159 1.088 1.595 1.131 1.094 0.026 0.025 0.022 0.036 0.028 0.024 0.025 0.03 0.034 0.028 0.026 0.027 0.026 0.023 0.027 0.026 0.023 0.04 0.023 0.026 0.024 0.027 0.024 0.026 0.03 0.032 0.025 0.032 0.035 0.042 0.025 0.038 0.028 0.025 0.026 0.027 0.026 0.029 0.022 0.026 0.025 0.031 0.028 0.025 0.027 0.029 0.03 0.032 0.048 0.036 0.029 0.029 0.028 0.028 0.029 0.045 0.03 0.056 0.03 0.029 0.033 0.026 0.032 0.03 0.027 0.647 0.254 0.388 99.999 0.39 99.999 0.462 0.407 99.999 0.403 0.412 0.351 99.999 0.339 0.514 99.999 0.379 0.388 0.442 0.488 0.315 0.497 0.443 0.365 99.999 0.516 0.244 0.594 99.999 99.999 0.365 99.999 0.302 0.255 0.398 0.333 0.611 0.715 0.578 0.335 0.443 99.999 99.999 0.413 0.275 0.496 99.999 99.999 99.999 99.999 0.41 0.378 0.531 0.427 0.365 99.999 0.51 99.999 0.333 0.371 99.999 99.999 99.999 0.577 0.427 0.083 0.058 0.068 99.999 0.061 99.999 0.061 0.066 99.999 0.062 0.073 0.055 99.999 0.062 0.08 99.999 0.073 0.076 0.052 0.083 0.066 0.071 0.09 0.079 99.999 0.081 0.067 0.094 99.999 99.999 0.065 99.999 0.072 0.07 0.069 0.056 0.096 0.082 0.072 0.074 0.086 99.999 99.999 0.065 0.068 0.105 99.999 99.999 99.999 99.999 0.093 0.088 0.075 0.082 0.078 99.999 0.098 99.999 0.081 0.078 99.999 99.999 99.999 0.098 0.116 0.666 0.562 0.587 1.122 0.616 0.821 0.631 0.646 0.865 0.645 0.636 0.638 0.655 0.65 0.649 0.68 0.675 0.648 0.545 0.723 0.632 0.661 0.653 0.65 0.798 0.644 0.65 0.648 0.647 1.1 0.631 0.828 0.631 0.664 0.7 0.676 0.652 0.687 0.642 0.69 0.686 0.678 0.657 0.648 0.644 0.671 0.667 0.683 1.168 0.661 0.671 0.638 0.656 0.688 0.576 1.109 0.709 1.247 0.667 0.619 0.704 0.629 0.876 0.638 0.673 0.015 0.014 0.012 0.012 0.017 0.012 0.014 0.02 0.018 0.016 0.012 0.014 0.017 0.014 0.014 0.013 0.013 0.026 0.013 0.014 0.013 0.014 0.014 0.016 0.013 0.02 0.018 0.021 0.021 0.014 0.014 0.017 0.016 0.013 0.015 0.013 0.015 0.017 0.012 0.015 0.015 0.014 0.016 0.014 0.016 0.016 0.015 0.016 0.014 0.02 0.014 0.015 0.016 0.013 0.015 0.016 0.016 0.015 0.017 0.014 0.021 0.015 0.014 0.014 0.016 1.34 1.119 1.241 2.142 1.308 1.626 1.316 1.298 1.588 1.287 1.299 1.285 1.367 1.322 1.316 1.285 1.323 1.316 1.135 1.361 1.306 1.364 1.331 1.36 1.492 1.243 1.289 1.242 1.348 2.109 1.299 1.567 1.253 1.308 1.36 1.354 1.349 1.401 1.301 1.322 1.348 1.315 1.275 1.246 1.314 1.317 1.335 1.405 2.263 1.423 1.359 1.274 1.364 1.344 1.232 2.17 1.38 2.393 1.35 1.301 1.269 1.249 1.738 1.316 1.328 0.013 0.012 0.011 0.01 0.016 0.01 0.013 0.017 0.034 0.015 0.012 0.012 0.016 0.012 0.012 0.011 0.012 0.023 0.012 0.012 0.011 0.013 0.012 0.014 0.013 0.017 0.014 0.018 0.018 0.012 0.013 0.015 0.013 0.011 0.014 0.012 0.013 0.012 0.011 0.014 0.016 0.012 0.014 0.013 0.014 0.014 0.014 0.013 0.011 0.018 0.013 0.013 0.016 0.013 0.013 0.014 0.014 0.012 0.014 0.012 0.036 0.013 0.012 0.012 0.014 UBVRI PHOTOMETRY OF OPEN CLUSTERS 393 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 98.1 295 786.1 301 201.2 393.9 550.5 299 252.5 515 298.1 697.3 600.6 264.2 590 343 868.5 420.9 947.8 777.9 355.5 265.5 167.8 693.8 156.8 477.9 150.4 797.1 460.4 332.4 637.3 654.7 270.3 773.2 947.8 848.4 271.4 599.7 396.1 171.3 473.7 352.8 644.7 495.8 612 594.3 894.3 176.1 37 202.8 100.3 349.5 620 697.3 702.2 901.3 40 853.3 395.1 701.8 680.3 18 454.2 808 423.7 961.1 455.6 494.9 57 626.5 344.5 185.3 296.1 767.4 472 519.4 560 109.6 721.5 536.8 560.6 185.7 615.5 483.3 17.2 944.5 580.4 837.6 599.4 336.5 777.1 402.6 769.8 236.6 289.9 500 130.4 570.8 789.6 510.1 634.6 293.9 480.7 530.2 697 619.3 601.4 501.5 754.9 731.4 135 258.4 418.4 537 614.2 831.9 443.3 710.2 808.6 313.4 624.2 988.9 284.8 491.5 917.8 990.6 523.6 604.3 847.1 945.2 17.492 17.506 17.507 17.508 17.51 17.53 17.535 17.553 17.554 17.566 17.569 17.573 17.593 17.612 17.625 17.628 17.632 17.638 17.65 17.662 17.688 17.689 17.694 17.698 17.698 17.701 17.702 17.709 17.71 17.714 17.715 17.717 17.736 17.756 17.757 17.758 17.762 17.762 17.764 17.768 17.771 17.775 17.781 17.782 17.783 17.786 17.786 17.787 17.798 17.816 17.817 17.818 17.823 17.825 17.826 17.829 17.831 17.831 17.841 17.841 17.844 17.853 17.875 17.901 17.902 0.016 0.01 0.011 0.011 0.011 0.01 0.012 0.013 0.012 0.015 0.011 0.011 0.012 0.013 0.011 0.013 0.01 0.015 0.01 0.015 0.013 0.027 0.016 0.01 0.011 0.013 0.014 0.013 0.013 0.01 0.014 0.014 0.011 0.013 0.014 0.013 0.013 0.013 0.014 0.012 0.014 0.015 0.013 0.011 0.015 0.015 0.013 0.012 0.012 0.015 0.018 0.014 0.016 0.012 0.01 0.013 0.017 0.013 0.016 0.014 0.014 0.016 0.014 0.014 0.015 1.336 1.227 1.211 1.831 1.173 1.082 1.089 2.269 1.231 1.214 1.054 0.994 1.082 1.205 1.03 1.189 2.19 1.232 1.645 1.007 1.041 1.214 1.051 1.03 1.012 1.133 1.175 1.872 1.162 1.195 1.079 1.059 1.018 1.221 1.173 1.104 1.327 1.08 1.121 1.24 1.16 2.14 1.382 99.999 1.084 1.1 1.11 1.145 1.108 1.15 1.254 1.244 0.953 1.166 0.929 1.18 1.087 1.142 1.121 1.113 1.105 1.836 1.13 1.144 1.178 0.041 0.027 0.032 0.044 0.028 0.026 0.031 0.062 0.034 0.034 0.031 0.031 0.033 0.036 0.032 0.033 0.063 0.037 0.039 0.037 0.036 0.037 0.036 0.032 0.031 0.035 0.037 0.053 0.032 0.034 0.031 0.031 0.028 0.031 0.039 0.031 0.04 0.035 0.035 0.032 0.037 0.075 0.039 99.999 0.031 0.035 0.033 0.036 0.035 0.037 0.044 0.035 0.032 0.036 0.032 0.037 0.044 0.031 0.037 0.034 0.034 0.056 0.04 0.037 0.039 99.999 99.999 0.568 99.999 99.999 0.392 0.378 99.999 0.417 0.3 99.999 0.284 0.214 99.999 0.499 99.999 99.999 99.999 99.999 0.514 99.999 0.376 99.999 0.395 0.427 99.999 99.999 99.999 99.999 99.999 0.282 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.296 99.999 99.999 99.999 99.999 99.999 0.337 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.098 99.999 99.999 0.082 0.092 99.999 0.095 0.074 99.999 0.079 0.082 99.999 0.108 99.999 99.999 99.999 99.999 0.095 99.999 0.124 99.999 0.097 0.123 99.999 99.999 99.999 99.999 99.999 0.086 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.108 99.999 99.999 99.999 99.999 99.999 0.083 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.827 0.679 0.639 0.982 0.721 0.628 0.645 1.24 0.673 0.692 0.68 0.618 0.586 0.656 0.633 0.655 1.318 0.666 0.95 0.606 0.673 0.738 0.663 0.617 0.652 0.714 0.689 1.037 0.635 0.679 0.667 0.657 0.62 0.629 0.684 0.674 0.748 0.648 0.686 0.697 0.711 1.231 0.856 1.138 0.647 0.658 0.624 0.692 0.65 0.699 0.781 0.722 0.526 0.667 0.635 0.674 0.642 0.652 0.713 0.565 0.66 0.99 0.661 0.671 0.662 0.022 0.014 0.017 0.015 0.016 0.017 0.017 0.017 0.015 0.019 0.016 0.016 0.018 0.017 0.017 0.017 0.014 0.022 0.014 0.021 0.017 0.017 0.023 0.017 0.016 0.018 0.018 0.016 0.016 0.015 0.019 0.018 0.016 0.018 0.018 0.017 0.017 0.018 0.018 0.017 0.018 0.02 0.017 0.015 0.02 0.019 0.017 0.017 0.019 0.021 0.023 0.019 0.021 0.016 0.016 0.017 0.027 0.016 0.022 0.019 0.018 0.021 0.018 0.018 0.019 1.519 1.31 1.222 1.973 1.443 1.285 1.254 2.391 1.299 1.306 1.282 1.299 1.201 1.379 1.281 1.359 2.502 1.389 1.785 1.248 1.31 1.422 1.347 1.289 1.296 1.397 1.349 2.009 1.296 1.28 1.323 1.295 1.215 1.279 1.383 1.372 1.501 1.341 1.344 1.339 1.336 2.34 1.499 2.198 99.999 1.315 1.396 1.318 1.301 1.325 1.535 1.46 1.116 1.332 1.224 1.351 1.285 1.301 1.415 1.197 1.341 2.025 1.306 1.37 1.354 0.02 0.012 0.015 0.012 0.014 0.013 0.016 0.013 0.014 0.018 0.013 0.015 0.015 0.015 0.015 0.015 0.011 0.02 0.012 0.02 0.015 0.016 0.02 0.016 0.015 0.014 0.016 0.014 0.015 0.013 0.018 0.015 0.013 0.015 0.016 0.015 0.014 0.014 0.015 0.014 0.017 0.017 0.015 0.012 99.999 0.018 0.014 0.014 0.017 0.0 2 0.02 0.016 0.019 0.015 0.015 0.015 0.023 0.015 0.019 0.016 0.015 0.018 0.016 0.016 0.017 394 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 934.4 158.7 933.2 212.8 423.1 256.8 768.3 800.6 408.6 819.9 619.3 685 759.6 631.4 103.3 168.4 232 833.2 540.5 732.5 598.9 740.2 802 885.8 532.5 894.3 515.8 795 149.5 920.5 305.1 61.8 365.8 802.9 357.9 227.5 221.6 668.8 675.5 531.4 613.9 224.7 493.7 761.6 163.1 729.5 438.5 619.9 653.4 536.9 447.6 701.6 15.4 598.9 877.5 791.9 388.8 621 641.8 462.2 472.3 905.9 530.1 240.9 959.8 643.1 860.2 454.9 312.1 473.2 290 456.2 29.4 342.1 70.2 600.4 318.2 596.5 957.1 152.3 572.7 672.9 591.5 391.8 883 30.6 383.7 146.5 577.4 462.6 338.5 864.9 576.5 240.8 611.5 181.3 47.7 415.3 423 121.2 614.8 732.1 333 609.9 458.6 660.8 288.7 688.9 179.8 475.8 255.7 375.8 803.7 98.1 405.5 730.4 478.9 93.9 253.9 267.3 189.1 719 585.4 476.2 293.6 832.6 445 781.7 511.2 257.1 17.907 17.909 17.915 17.918 17.923 17.926 17.927 17.937 17.938 17.941 17.942 17.947 17.949 17.954 17.956 17.957 17.957 17.963 17.966 17.971 17.974 17.987 17.987 17.992 18 18.007 18.019 18.019 18.021 18.024 18.027 18.035 18.037 18.046 18.047 18.05 18.058 18.073 18.074 18.077 18.087 18.089 18.093 18.096 18.108 18.112 18.12 18.129 18.137 18.143 18.145 18.146 18.154 18.159 18.166 18.168 18.172 18.177 18.178 18.192 18.197 18.2 18.206 18.21 18.213 0.023 0.014 0.014 0.017 0.014 0.022 0.015 0.014 0.011 0.015 0.015 0.022 0.015 0.015 0.012 0.015 0.014 0.015 0.014 0.014 0.014 0.014 0.017 0.014 0.017 0.015 0.014 0.015 0.016 0.014 0.018 0.015 0.021 0.015 0.014 0.015 0.016 0.016 0.016 0.018 0.015 0.016 0.014 0.016 0.015 0.018 0.014 0.017 0.018 0.015 0.016 0.017 0.018 0.015 0.016 0.014 0.017 0.015 0.02 0.017 0.015 0.016 0.014 0.016 0.015 1.1 1.164 1.82 1.966 1.285 1.18 1.095 1.333 1.383 1.177 1.16 1.167 1.039 1.155 1.875 1.202 1.076 1.228 2.186 1.174 1.311 1.058 1.962 1.125 1.157 2.014 1.205 1.112 1.349 1.123 1.35 1.319 1.221 1.632 1.069 1.885 1.354 1.1 1.119 1.193 1.106 2.236 1.382 1.225 1.132 2.025 1.361 1.054 1.188 1.175 1.235 1.485 1.272 1.367 1.282 1.401 1.161 1.159 1.327 1.472 1.195 1.039 1.257 1.105 1.313 0.035 0.037 0.054 0.062 0.042 0.053 0.04 0.038 0.041 0.038 0.038 0.045 0.037 0.038 0.057 0.038 0.035 0.041 0.077 0.042 0.043 0.036 0.08 0.039 0.045 0.058 0.045 0.036 0.048 0.037 0.044 0.054 0.049 0.051 0.036 0.061 0.044 0.043 0.041 0.047 0.04 0.074 0.048 0.046 0.043 0.085 0.043 0.042 0.044 0.04 0.049 0.055 0.051 0.045 0.044 0.05 0.049 0.042 0.055 0.051 0.046 0.041 0.042 0.043 0.052 0.362 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.338 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.103 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.145 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.697 0.593 1.113 1.062 0.678 0.746 0.767 0.755 0.851 0.699 0.718 0.653 0.669 0.665 1.035 0.657 0.659 0.677 1.34 0.655 0.739 0.683 1.105 0.768 0.687 1.14 0.741 0.618 0.756 0.71 0.735 0.737 0.707 0.922 0.601 1.044 0.726 0.621 0.69 0.62 0.646 1.198 0.768 0.584 0.694 1.153 0.788 0.69 0.709 0.652 0.675 0.956 0.727 0.74 0.71 0.802 0.669 0.707 0.689 0.753 0.692 0.664 0.708 0.597 0.776 0.018 0.02 0.017 0.022 0.021 0.031 0.019 0.019 0.018 0.02 0.02 0.031 0.02 0.02 0.018 0.02 0.019 0.02 0.018 0.019 0.019 0.018 0.021 0.019 0.021 0.019 0.021 0.021 0.02 0.019 0.023 0.021 0.034 0.019 0.02 0.019 0.02 0.021 0.022 0.023 0.019 0.021 0.019 0.021 0.022 0.023 0.019 0.02 0.024 0.021 0.02 0.021 0.026 0.02 0.022 0.02 0.022 0.021 0.027 0.023 0.021 0.021 0.019 0.02 0.021 1.411 1.298 2.093 2.11 1.334 1.418 1.477 1.517 1.676 1.347 1.414 99.999 1.294 1.334 2.017 1.305 1.312 1.362 2.453 1.271 1.44 1.383 2.155 1.429 1.312 2.213 1.374 1.33 1.502 1.44 1.521 1.495 1.434 1.883 1.27 2.069 1.401 1.31 1.268 1.33 1.327 2.306 1.521 1.25 1.307 2.206 1.495 1.349 1.439 1.362 1.375 1.982 1.413 1.453 1.41 1.445 1.362 1.377 1.43 1.451 1.398 1.325 1.351 1.258 1.546 0.016 0.018 0.014 0.017 0.018 0.026 0.017 0.015 0.013 0.017 0.018 99.999 0.019 0.017 0.013 0.018 0.016 0.018 0.015 0.016 0.018 0.018 0.018 0.017 0.021 0.016 0.022 0.018 0.018 0.017 0.02 0.018 0.027 0.016 0.016 0.016 0.018 0.019 0.043 0.02 0.017 0.017 0.017 0.019 0.019 0.019 0.016 0.019 0.021 0.018 0.019 0.018 0.021 0.017 0.018 0.017 0.019 0.018 0.022 0.019 0.017 0.019 0.019 0.018 0.018 UBVRI PHOTOMETRY OF OPEN CLUSTERS 395 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 237.3 621.9 883.9 205.8 787.6 634.7 558.8 572.2 850.5 516.6 554.8 892.2 17.4 439.4 810.8 463.5 930.3 86.9 907 367 244.2 781 208.4 597.4 891.4 361.8 351.6 546.2 935.6 12.2 625.1 278.9 520 563 332.9 469.5 403.8 411.4 321.3 387 36.1 820.9 951.9 666.2 570.6 803.1 679.4 600.5 720.7 725.9 827.4 15.9 56.8 888.8 981.2 406 406.2 441.8 172.9 173.6 426.2 734.2 888 105.8 634.7 582.9 282.1 455.7 201.7 590.6 113.5 400.5 773.6 399.2 271.4 69.2 366.9 245.4 832.7 114.7 323 154.4 655 828.6 705.1 136.1 975.6 499.8 714.8 673.7 962.8 639.1 74.2 741 735.5 494.4 767.7 986.4 579.2 348.7 563 125.3 552.6 465.6 641 704.7 571 619 213 947.2 989.2 847.1 568.2 449.5 703.4 880.4 411.4 736.7 854.7 553.4 258.3 35.9 798.6 502.5 727.2 354.7 470.6 539.8 106.7 659.3 18.223 18.223 18.224 18.229 18.231 18.232 18.24 18.241 18.255 18.261 18.261 18.263 18.266 18.267 18.271 18.272 18.274 18.281 18.284 18.289 18.29 18.292 18.293 18.304 18.314 18.317 18.324 18.326 18.335 18.349 18.351 18.355 18.365 18.371 18.375 18.393 18.394 18.397 18.414 18.416 18.421 18.421 18.425 18.428 18.43 18.43 18.434 18.438 18.457 18.469 18.475 18.476 18.477 18.479 18.483 18.484 18.485 18.485 18.486 18.486 18.488 18.491 18.496 18.498 18.507 0.014 0.016 0.019 0.018 0.016 0.016 0.016 0.016 0.015 0.018 0.019 0.017 0.017 0.017 0.02 0.015 0.02 0.019 0.017 0.016 0.02 0.023 0.016 0.018 0.015 0.015 0.019 0.019 0.014 0.019 0.018 0.02 0.019 0.018 0.019 0.02 0.02 0.021 0.02 0.017 0.019 0.017 0.017 0.019 0.017 0.015 0.017 0.02 0.02 0.017 0.02 0.022 0.022 0.019 0.018 0.017 0.02 0.02 0.019 0.019 0.019 0.019 0.019 0.019 0.02 2.026 1.277 1.351 1.372 1.22 1.209 1.086 1.268 1.172 1.145 1.212 1.127 1.784 1.143 1.284 1.095 1.912 1.068 0.973 1.188 1.204 1.174 1.255 99.999 1.836 1.698 1.153 1.496 1.212 1.903 1.22 1.338 1.278 1.01 1.35 1.21 99.999 1.344 1.148 1.798 1.391 1.227 1.454 1.053 1.142 1.456 1.176 1.13 1.203 1.391 1.186 1.653 1.117 1.084 1.378 99.999 1.315 1.262 1.209 1.394 1.768 1.138 1.882 1.485 1.102 0.087 0.041 0.054 0.049 0.042 0.048 0.043 0.044 0.05 0.049 0.049 0.048 0.084 0.045 0.054 0.044 0.086 0.049 0.041 0.05 0.046 0.055 0.05 99.999 0.074 0.058 0.053 0.065 0.05 0.078 0.049 0.057 0.051 0.049 0.063 0.051 99.999 0.059 0.046 0.092 0.069 0.058 0.063 0.048 0.058 0.061 0.053 0.053 0.051 0.063 0.055 0.083 0.055 0.052 0.059 99.999 0.059 0.059 0.058 0.065 0.08 0.052 0.097 0.075 0.05 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.101 0.678 0.85 0.748 0.746 0.629 0.621 0.692 0.708 0.648 0.727 0.693 0.979 0.64 0.644 0.692 1.08 0.676 0.632 0.645 0.637 0.759 0.683 1.101 1.029 0.964 0.711 0.798 0.717 1.045 0.739 0.674 0.655 0.689 0.77 0.665 0.786 0.7 0.687 1.077 0.777 0.847 0.869 0.724 0.69 0.852 0.729 0.671 0.648 0.782 0.699 0.955 0.74 0.742 0.669 0.853 0.651 0.635 0.679 0.737 1.056 0.681 1.103 0.969 0.679 0.019 0.022 0.024 0.023 0.022 0.021 0.023 0.021 0.02 0.024 0.024 0.022 0.022 0.022 0.026 0.02 0.025 0.023 0.023 0.022 0.026 0.031 0.022 0.023 0.021 0.02 0.024 0.025 0.02 0.026 0.025 0.027 0.026 0.025 0.026 0.027 0.025 0.027 0.027 0.022 0.025 0.022 0.023 0.025 0.022 0.024 0.021 0.027 0.028 0.022 0.025 0.028 0.028 0.025 0.024 0.024 0.026 0.025 0.024 0.025 0.025 0.024 0.026 0.026 0.027 2.082 1.307 1.542 1.478 1.435 1.333 1.283 1.355 1.416 1.328 1.418 1.381 1.973 1.311 1.307 1.321 2.096 1.321 1.337 1.337 1.301 1.466 1.44 2.184 2.029 1.999 1.358 1.659 1.436 2.07 1.368 1.465 1.351 1.32 1.454 1.433 1.588 1.409 1.394 2.111 1.478 1.556 1.771 1.362 1.348 1.572 1.46 1.408 1.373 1.621 1.394 1.799 1.402 1.398 1.418 1.547 1.365 1.376 1.426 1.377 2.073 1.388 2.092 1.861 1.355 0.016 0.019 0.021 0.021 0.019 0.019 0.019 0.02 0.018 0.021 0.021 0.021 0.019 0.021 0.023 0.018 0.021 0.022 0.02 0.019 0.022 0.058 0.02 0.02 0.016 0.017 0.021 0.021 0.017 0.021 0.022 0.024 0.022 0.021 0.022 0.024 0.022 0.024 0.025 0.019 0.022 0.02 0.019 0.022 0.02 0.022 0.019 0.023 0.023 0.019 0.023 0.024 0.025 0.022 0.021 0.02 0.023 0.022 0.023 0.022 0.02 0.024 0.022 0.022 0.023 396 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 839.3 433.4 775.2 6.7 733.6 162.1 879.8 95.3 297.4 671.1 426 88 561.4 494 220.3 929.4 657.5 658.8 692.9 797.3 225 394.2 186.5 402.9 465.6 272.8 693.1 458.4 93.2 591.8 280.8 935.1 930.1 595 614.2 794.7 721 654.6 907.4 65.7 430.1 275.2 117.1 238.7 608.8 523.2 245.7 726.4 859.9 565.1 277.8 238.2 809.9 55.8 395.8 268.8 591.5 891.8 912.1 198.7 125.7 347.4 942.1 741.3 140.3 690.7 812.5 917 420.3 48.3 236.6 393.4 992.1 334.9 823.1 601.5 649.9 469.1 329.9 609.4 100.7 710.9 425.5 956 787.9 319.2 560.6 176.4 759.5 176.8 725.2 7.2 752.8 893.1 234.8 895.1 711.8 130.4 258.4 792.3 868.4 157.3 611.3 893.5 578.3 567.4 459.6 252.6 332.1 898.4 129.9 564 51.2 211.4 651.9 299.6 140.8 303.2 807.8 103.6 801.9 119.9 212.7 684.9 828.7 224.4 581.8 673.1 946.6 207.4 18.507 18.524 18.527 18.529 18.529 18.53 18.531 18.532 18.546 18.552 18.57 18.573 18.58 18.582 18.592 18.599 18.6 18.601 18.601 18.606 18.609 18.624 18.626 18.633 18.636 18.637 18.64 18.646 18.649 18.655 18.659 18.659 18.66 18.662 18.663 18.668 18.671 18.675 18.676 18.677 18.696 18.699 18.706 18.707 18.709 18.712 18.717 18.719 18.721 18.722 18.725 18.727 18.729 18.73 18.735 18.741 18.743 18.744 18.745 18.75 18.75 18.756 18.757 18.763 18.763 0.021 0.021 0.018 0.02 0.022 0.022 0.021 0.029 0.02 0.014 0.021 0.02 0.019 0.02 0.019 0.019 0.019 0.02 0.021 0.02 0.019 0.023 0.022 0.024 0.021 0.02 0.018 0.022 0.024 0.021 0.02 0.018 0.02 0.023 0.023 0.02 0.021 0.022 0.021 0.02 0.021 0.021 0.022 0.022 0.02 0.022 0.023 0.024 0.024 0.022 0.021 0.02 0.024 0.024 0.023 0.025 0.021 0.019 0.026 0.024 0.026 0.025 0.02 0.021 0.026 1.326 1.128 1.191 1.166 1.287 1.199 1.074 1.219 1.262 1.87 99.999 1.128 1.143 1.125 1.201 1.093 1.262 1.083 1.256 1.412 1.77 1.181 1.727 1.173 1.256 1.18 1.077 1.182 1.155 1.091 1.236 1.458 1.181 1.292 1.322 1.37 99.999 1.265 1.916 1.256 1.289 1.168 1.209 1.273 1.311 1.091 1.195 1.101 1.136 1.177 1.394 1.25 1.082 1.373 1.215 1.145 1.159 1.225 1.251 1.297 1.297 1.258 1.201 99.999 1.45 0.063 0.06 0.054 0.054 0.063 0.063 0.053 0.068 0.069 0.088 99.999 0.059 0.051 0.058 0.059 0.053 0.068 0.066 0.062 0.07 0.088 0.061 0.106 0.064 0.062 0.06 0.054 0.062 0.07 0.058 0.071 0.068 0.063 0.067 0.069 0.066 99.999 0.067 0.089 0.077 0.073 0.063 0.076 0.063 0.068 0.069 0.071 0.066 0.064 0.065 0.087 0.07 0.06 0.081 0.068 0.065 0.07 0.076 0.063 0.075 0.082 0.072 0.076 99.999 0.094 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.729 0.67 0.719 0.681 0.807 0.774 0.756 0.763 0.782 1.144 1.114 0.669 0.789 0.703 0.699 0.664 0.692 0.678 0.746 0.799 1.011 0.727 0.997 0.713 0.695 0.796 0.672 0.718 0.708 0.764 0.705 0.767 0.724 0.708 0.802 0.803 1.159 0.76 1.021 0.863 0.785 0.695 0.789 0.733 0.724 0.694 0.704 0.705 0.705 0.762 0.764 0.833 0.712 0.753 0.762 0.722 0.688 0.692 0.76 0.737 0.807 0.607 0.755 0.716 0.749 0.027 0.027 0.024 0.027 0.029 0.028 0.028 0.043 0.026 0.021 0.028 0.028 0.025 0.026 0.025 0.028 0.026 0.027 0.027 0.028 0.025 0.029 0.028 0.029 0.028 0.026 0.025 0.029 0.033 0.027 0.027 0.024 0.028 0.029 0.03 0.025 0.028 0.027 0.027 0.026 0.029 0.028 0.03 0.028 0.026 0.028 0.029 0.03 0.032 0.029 0.029 0.025 0.031 0.032 0.03 0.03 0.028 0.028 0.032 0.031 0.034 0.031 0.027 0.026 0.034 1.398 1.37 1.444 1.455 1.576 1.415 1.521 1.484 1.46 2.197 2.175 1.364 1.397 1.409 1.389 1.359 1.453 1.41 1.446 1.499 2.037 1.445 2.076 1.385 1.427 1.482 1.38 1.406 1.411 1.435 1.473 1.442 1.447 1.431 1.562 1.627 2.278 1.418 2.031 1.654 1.55 1.415 1.522 1.485 1.422 1.379 1.447 1.403 1.363 1.448 1.512 1.588 1.371 1.572 1.615 1.479 1.442 1.445 1.482 1.449 1.508 1.328 1.421 1.432 1.548 0.024 0.025 0.021 0.023 0.024 0.026 0.024 0.06 0.024 0.016 0.023 0.024 0.024 0.024 0.021 0.023 0.022 0.023 0.025 0.024 0.02 0.026 0.024 0.027 0.024 0.025 0.022 0.025 0.028 0.024 0.023 0.021 0.026 0.027 0.026 0.022 0.022 0.026 0.022 0.023 0.025 0.026 0.025 0.024 0.023 0.026 0.025 0.027 0.03 0.027 0.023 0.024 0.027 0.027 0.026 0.029 0.024 0.023 0.028 0.028 0.029 0.028 0.023 0.025 0.029 UBVRI PHOTOMETRY OF OPEN CLUSTERS 397 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 351.4 150.3 466.5 8.9 50.1 545.7 511.5 702.3 356.5 64.4 540.5 262.6 486.4 335.1 150 277.6 901.4 24.7 2.7 43 857.4 512.6 664.9 948.2 172.3 691.2 751.7 34.1 777.4 239.2 944.3 152.8 860.9 310 632.8 348.4 550.6 387.7 466.4 169.6 614.7 560.2 536.2 545 556.1 181.3 623.1 485.2 975.5 597.1 275.3 412.9 979.6 488.9 171.6 693.7 668.4 184.3 50 576.4 757.6 376.1 349.6 929.2 198.4 347.3 363.3 652.6 594.7 352.3 421.9 47.3 563.3 291.2 558.1 58.1 9 693.1 469.9 217.5 883.6 713.3 696.2 814.9 43.5 830.6 419.2 298.5 586.2 532.8 336.4 942.3 957.5 446.8 294.5 845.7 972.9 341.8 334.4 988.9 561.9 206.7 486.7 687.2 66.9 642.8 617.6 155.9 735.4 395.7 621.1 451.9 430.9 386.4 413.6 424.3 240.8 659.5 460.3 458.6 910.9 472.2 299.9 754.7 740.5 779.7 876.9 294.8 388.7 796.7 18.765 18.767 18.778 18.778 18.779 18.779 18.785 18.786 18.787 18.787 18.787 18.8 18.802 18.806 18.809 18.81 18.811 18.817 18.819 18.827 18.835 18.836 18.842 18.844 18.847 18.848 18.849 18.852 18.853 18.854 18.857 18.863 18.871 18.875 18.877 18.884 18.886 18.891 18.892 18.895 18.897 18.902 18.906 18.907 18.909 18.925 18.927 18.929 18.929 18.935 18.939 18.945 18.946 18.947 18.957 18.96 18.964 18.965 18.968 18.974 18.975 18.976 18.98 18.983 18.998 0.027 0.026 0.023 0.027 0.025 0.023 0.025 0.023 0.026 0.025 0.018 0.025 0.027 0.023 0.023 0.021 0.022 0.027 0.026 0.023 0.023 0.024 0.024 0.023 0.027 0.025 0.023 0.027 0.027 0.025 0.022 0.027 0.027 0.023 0.023 0.024 0.027 0.027 0.025 0.025 0.025 0.024 0.023 0.024 0.021 0.026 0.03 0.029 0.023 0.026 0.024 0.021 0.026 0.025 0.029 0.025 0.027 0.028 0.025 0.026 0.027 0.027 0.027 0.028 0.027 1.316 1.226 1.82 1.061 1.284 1.144 1.352 1.173 1.23 1.204 99.999 1.289 1.422 1.31 1.1 99.999 1.186 99.999 1.34 1.423 1.187 1.339 1.202 1.339 1.233 1.257 1.518 99.999 1.112 1.475 1.698 1.678 1.232 1.18 1.259 1.366 1.425 99.999 1.241 1.265 1.108 1.239 99.999 1.326 1.159 99.999 99.999 1.186 1.439 1.276 99.999 1.414 1.298 1.098 1.238 1.233 1.578 1.151 99.999 1.053 1.537 1.212 1.006 1.214 99.999 0.083 0.074 0.121 0.075 0.071 0.07 0.084 0.074 0.069 0.074 99.999 0.076 0.082 0.08 0.065 99.999 0.072 99.999 0.088 0.076 0.073 0.087 0.073 0.074 0.079 0.076 0.102 99.999 0.072 0.09 0.112 0.128 0.081 0.073 0.076 0.078 0.085 99.999 0.068 0.092 0.075 0.086 99.999 0.079 0.068 99.999 99.999 0.086 0.092 0.085 99.999 0.098 0.08 0.083 0.082 0.085 0.112 0.084 99.999 0.068 0.106 0.075 0.073 0.085 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.734 0.669 1.079 0.738 0.813 0.749 0.81 0.646 0.8 0.64 1.115 0.687 0.813 0.737 0.74 1.061 0.747 1.196 0.887 0.798 0.724 0.725 0.67 0.766 0.734 0.777 0.92 1.154 0.722 0.824 1.066 0.828 0.713 0.766 0.65 0.694 0.775 0.776 0.698 0.831 0.671 0.713 1.01 0.697 0.652 0.949 0.757 0.69 0.841 0.801 0.835 0.897 0.671 0.745 0.721 0.685 1.063 0.721 1.12 0.751 0.785 0.743 0.731 0.774 0.89 0.034 0.034 0.028 0.035 0.03 0.032 0.033 0.032 0.036 0.035 0.025 0.033 0.036 0.029 0.031 0.028 0.029 0.034 0.037 0.033 0.03 0.032 0.032 0.03 0.035 0.032 0.031 0.036 0.034 0.033 0.028 0.034 0.034 0.032 0.029 0.033 0.035 0.038 0.034 0.035 0.033 0.031 0.029 0.03 0.03 0.034 0.038 0.037 0.032 0.036 0.033 0.028 0.034 0.036 0.038 0.033 0.035 0.035 0.034 0.035 0.037 0.034 0.035 0.038 0.033 1.465 1.386 2.077 99.999 1.49 1.417 1.668 1.373 1.585 1.327 2.121 1.436 1.446 1.485 1.425 2.08 1.417 2.237 1.718 1.607 1.417 1.482 1.509 1.627 1.491 1.472 1.642 2.21 1.419 1.601 2.034 1.571 1.414 1.471 1.361 1.428 1.492 1.552 1.474 1.658 1.356 1.356 2.009 1.403 1.387 2.001 1.411 1.424 1.603 1.533 1.705 1.598 1.435 1.487 1.393 1.352 1.967 1.468 2.201 1.385 99.999 1.388 1.503 1.525 1.83 σV −I 0.031 0.029 0.024 99.999 0.029 0.027 0.027 0.029 0.03 0.028 0.019 0.028 0.07 0.028 0.026 0.023 0.026 0.029 0.03 0.027 0.026 0.028 0.026 0.026 0.031 0.029 0.025 0.029 0.03 0.029 0.024 0.033 0.029 0.027 0.028 0.028 0.031 0.032 0.028 0.028 0.029 0.029 0.025 0.028 0.025 0.027 0.035 0.034 0.027 0.03 0.027 0.023 0.028 0.031 0.033 0.031 0.033 0.032 0.027 0.03 99.999 0.03 0.031 0.032 0.029 398 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 861.5 670.2 734.8 579 19.5 17.1 667.3 981 229.2 562.9 173.4 949.5 937.4 698 271.4 317.9 413.3 771 224 233.9 722.2 402.4 232.1 213.3 501.3 276.2 831 570.2 507.6 760.9 534.9 226.9 104.2 429.2 594.5 769.1 558.6 668.6 39.4 558.4 168.9 327.9 201 990.9 900.6 506.9 479.8 296.1 334.8 629.2 135.9 252.3 941.5 11.8 89.6 352.1 871.6 658.1 851.6 781.8 837.6 172.2 25.1 400.3 443.6 155.3 608.5 350.9 230.4 529.3 340.5 366.7 611.8 141.3 592.9 175 891.4 618.2 721.7 750.5 576.3 647.7 820.2 687.2 766.3 846.2 260.7 186.3 389.2 143 643.8 73.2 460.2 642.2 778.7 478.8 6.4 808 419.6 788.4 613.9 731.8 771.5 213.1 911.3 230.6 155 656.9 145.5 979.6 504.6 341.5 587.5 580 158.7 886.4 695.7 249.1 120 298.8 224.3 626.3 13.8 854.6 587.7 23.8 822.1 391.8 121.8 558.8 18.999 19 19 19.007 19.011 19.012 19.013 19.017 19.019 19.023 19.029 19.032 19.033 19.037 19.039 19.052 19.059 19.065 19.071 19.071 19.079 19.086 19.087 19.094 19.098 19.104 19.106 19.108 19.109 19.12 19.126 19.132 19.132 19.134 19.134 19.134 19.145 19.148 19.151 19.161 19.169 19.174 19.182 19.19 19.195 19.215 19.217 19.223 19.229 19.232 19.233 19.244 19.261 19.268 19.273 19.274 19.274 19.275 19.276 19.277 19.279 19.293 19.299 19.307 19.309 0.025 0.03 0.027 0.029 0.03 0.024 0.024 0.025 0.024 0.029 0.026 0.024 0.024 0.025 0.03 0.027 0.026 0.025 0.029 0.024 0.023 0.035 0.027 0.031 0.023 0.026 0.028 0.025 0.028 0.032 0.025 0.033 0.028 0.029 0.03 0.027 0.029 0.034 0.029 0.029 0.027 0.026 0.03 0.04 0.029 0.028 0.033 0.034 0.024 0.028 0.026 0.027 0.027 0.031 0.034 0.025 0.032 0.031 0.028 0.038 0.036 0.035 0.033 0.035 0.035 1.493 1.249 1.318 1.608 1.088 1.449 1.272 1.456 1.331 1.216 1.172 1.401 1.579 1.131 1.18 99.999 1.327 1.461 99.999 99.999 1.334 99.999 99.999 1.402 1.22 1.214 1.2 1.488 1.337 1.369 1.333 1.37 99.999 1.172 1.297 99.999 99.999 1.164 1.171 1.171 99.999 1.198 1.24 1.174 99.999 1.373 1.648 99.999 99.999 0.98 99.999 1.307 1.269 99.999 1.246 99.999 99.999 1.184 1.402 1.023 99.999 99.999 1.18 99.999 99.999 0.093 0.086 0.09 0.127 0.084 0.089 0.079 0.095 0.095 0.079 0.097 0.096 0.102 0.083 0.094 99.999 0.092 0.106 99.999 99.999 0.094 99.999 99.999 0.111 0.084 0.089 0.088 0.102 0.094 0.113 0.113 0.106 99.999 0.089 0.09 99.999 99.999 0.096 0.09 0.098 99.999 0.105 0.1 0.092 99.999 0.121 0.129 99.999 99.999 0.087 99.999 0.122 0.095 99.999 0.133 99.999 99.999 0.125 0.11 0.09 99.999 99.999 0.104 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.986 0.84 0.799 1.03 0.788 0.673 0.735 0.832 0.709 0.77 0.727 1.036 0.961 0.798 0.798 1.027 0.813 1.017 0.996 1.115 0.736 0.653 0.82 0.75 0.76 0.813 0.866 0.769 0.792 0.808 0.818 0.767 0.704 0.663 0.77 1.019 1.156 0.729 0.72 0.749 0.767 0.791 0.777 0.722 1.066 0.739 0.834 0.91 0.73 0.856 1.038 0.86 0.778 0.784 0.778 0.782 0.807 0.72 0.702 0.686 0.929 0.766 0.739 0.778 0.808 0.032 0.04 0.036 0.038 0.038 0.033 0.032 0.033 0.033 0.045 0.034 0.031 0.032 0.032 0.04 0.035 0.034 0.033 0.037 0.032 0.031 0.045 0.036 0.04 0.033 0.035 0.037 0.034 0.037 0.043 0.031 0.041 0.039 0.038 0.038 0.035 0.037 0.044 0.038 0.039 0.037 0.036 0.038 0.048 0.038 0.038 0.042 0.043 0.033 0.037 0.036 0.036 0.037 0.043 0.042 0.037 0.04 0.043 0.038 0.047 0.046 0.045 0.044 0.047 0.045 2.153 1.502 1.665 1.896 1.405 1.466 1.523 1.692 1.439 1.399 1.476 2.1 1.736 1.517 1.538 1.91 1.487 1.909 1.9 2.141 1.433 1.487 1.7 1.547 1.525 1.49 1.63 1.474 1.581 99.999 1.616 1.659 1.455 1.421 1.507 1.987 2.132 1.504 1.532 1.4 1.501 1.43 1.452 1.437 2.435 1.539 1.604 1.79 1.572 1.648 2.093 1.625 1.555 1.513 1.471 1.467 1.532 1.577 1.452 1.484 1.625 1.491 1.511 1.509 1.626 σV −I 0.027 0.042 0.03 0.032 0.035 0.029 0.027 0.029 0.029 0.033 0.03 0.025 0.027 0.028 0.035 0.029 0.03 0.027 0.032 0.027 0.028 0.039 0.03 0.035 0.027 0.032 0.032 0.031 0.031 99.999 0.029 0.036 0.032 0.033 0.034 0.03 0.031 0.038 0.033 0.033 0.032 0.03 0.034 0.044 0.03 0.032 0.038 0.037 0.029 0.032 0.028 0.032 0.032 0.038 0.038 0.032 0.036 0.038 0.034 0.043 0.042 0.039 0.037 0.039 0.039 UBVRI PHOTOMETRY OF OPEN CLUSTERS 399 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 444.7 456.8 728.4 462.2 277.9 56.8 677.5 27 622.8 602.8 938.8 63 825.8 275.4 391.1 637.1 436.3 539.7 464.9 294.7 849.2 666.8 466.8 388.6 735.7 882.1 635.9 668.2 330.7 215.4 560.4 290.7 141 603.6 477.4 119 280 819 475.8 119.9 858 264.9 512.4 666.2 457.7 882 483.8 180.5 929.2 266.8 473 640 561.2 209.9 188.3 517.8 320.9 358 666.5 938.4 408.2 77.9 589 852.4 463.8 621.8 550 917.1 411.7 409.2 911.5 105.9 900.4 122.7 732.5 787 668.3 224.6 629 897.3 836.8 498.3 616 20.1 203 313.5 410.8 965.6 817.6 421.1 491.4 714.2 864.9 54.1 168.8 642.7 346.6 482 656.6 62.9 76 985.5 832.4 228.1 860.2 819.3 442.4 862.4 195.5 270.4 94.6 917.2 491 603.3 795.7 738.9 382.5 888.2 849.7 892.2 221 870.5 176.4 985.4 939 250.5 68.8 948.4 637.8 163.5 19.309 19.309 19.314 19.318 19.319 19.322 19.326 19.329 19.334 19.338 19.339 19.342 19.344 19.345 19.346 19.347 19.349 19.352 19.357 19.359 19.359 19.361 19.366 19.374 19.378 19.378 19.385 19.387 19.388 19.389 19.391 19.396 19.4 19.401 19.402 19.402 19.406 19.407 19.408 19.408 19.417 19.421 19.422 19.422 19.423 19.431 19.433 19.434 19.434 19.441 19.446 19.446 19.448 19.449 19.457 19.462 19.486 19.49 19.495 19.496 19.52 19.522 19.524 19.524 19.53 0.034 0.039 0.025 0.029 0.032 0.032 0.03 0.024 0.032 0.032 0.031 0.035 0.03 0.033 0.025 0.034 0.034 0.036 0.034 0.036 0.031 0.034 0.035 0.031 0.027 0.039 0.046 0.042 0.032 0.034 0.032 0.035 0.038 0.04 0.032 0.036 0.031 0.034 0.034 0.033 0.032 0.032 0.034 0.039 0.036 0.035 0.035 0.031 0.033 0.037 0.04 0.034 0.038 0.038 0.044 0.043 0.039 0.036 0.04 0.032 0.036 0.037 0.037 0.037 0.043 1.228 1.448 99.999 99.999 1.394 99.999 99.999 99.999 99.999 99.999 0.058 99.999 1.391 1.179 99.999 1.119 99.999 0.989 99.999 99.999 99.999 99.999 1.287 99.999 99.999 1.297 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.239 1.075 99.999 99.999 99.999 99.999 99.999 99.999 1.163 1.173 99.999 1.238 99.999 99.999 99.999 1.073 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.103 0.128 99.999 99.999 0.111 99.999 99.999 99.999 99.999 99.999 0.049 99.999 0.128 0.127 99.999 0.105 99.999 0.112 99.999 99.999 99.999 99.999 0.116 99.999 99.999 0.121 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.139 0.103 99.999 99.999 99.999 99.999 99.999 99.999 0.121 0.108 99.999 0.123 99.999 99.999 99.999 0.101 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 −0.805 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.068 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.781 0.735 0.919 0.947 0.763 0.757 1.054 0.744 0.893 0.845 −0.014 0.932 0.923 0.694 0.81 0.795 0.921 0.747 1.036 0.842 0.809 0.856 0.752 0.997 0.789 0.777 0.773 0.798 0.757 0.647 0.851 0.905 0.794 0.641 0.887 0.741 0.661 0.802 0.794 0.897 0.891 0.712 0.923 0.661 0.959 0.73 0.729 0.755 0.708 0.876 0.744 0.864 0.778 0.862 0.768 0.717 0.874 0.887 0.724 0.802 0.803 0.736 0.729 0.835 0.707 0.042 0.053 0.033 0.039 0.043 0.044 0.04 0.035 0.04 0.042 0.051 0.045 0.039 0.042 0.034 0.045 0.044 0.046 0.042 0.046 0.041 0.043 0.046 0.04 0.038 0.049 0.057 0.054 0.043 0.047 0.042 0.046 0.047 0.05 0.043 0.047 0.043 0.042 0.044 0.044 0.042 0.044 0.045 0.051 0.044 0.045 0.046 0.044 0.046 0.046 0.051 0.045 0.049 0.049 0.056 0.054 0.05 0.049 0.051 0.045 0.051 0.052 0.049 0.047 0.054 1.514 1.484 1.728 1.675 1.523 1.532 2.148 1.549 1.6 1.981 99.999 1.785 1.644 1.487 1.552 1.547 1.863 1.48 2.132 1.649 1.512 1.542 1.431 1.83 1.559 1.575 1.455 1.537 1.49 1.336 1.644 1.718 1.655 1.385 1.788 1.436 1.476 1.491 1.474 1.647 1.776 1.467 1.66 1.418 1.946 1.481 1.489 1.516 1.439 1.742 1.498 1.681 1.55 1.65 1.594 1.517 1.501 1.506 1.451 1.625 1.662 1.391 1.413 1.611 1.526 σV −I 0.039 0.05 0.03 0.034 0.034 0.038 0.031 0.031 0.037 0.039 99.999 0.039 0.036 0.037 0.03 0.039 0.038 0.041 0.036 0.039 0.035 0.038 0.04 0.037 0.034 0.043 0.052 0.048 0.036 0.04 0.036 0.038 0.041 0.044 0.036 0.042 0.039 0.038 0.041 0.038 0.035 0.036 0.042 0.045 0.038 0.04 0.041 0.037 0.039 0.042 0.045 0.039 0.043 0.041 0.048 0.049 0.045 0.042 0.045 0.035 0.042 0.043 0.042 0.043 0.047 400 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 75.8 908.5 103 77.8 121 259.3 925.9 131.7 767.5 302.2 95.2 899.7 486.9 649.4 916.2 498 194.4 844 737.2 581.6 229.5 469.2 46.7 592.9 178.3 503.6 712.3 961 299.2 752.7 180.5 436.2 750.6 173.4 411.3 792.5 161.2 991.4 467.9 128 14.1 865 392.3 365.9 588.6 579.9 558.7 354.3 593.7 552.9 892.1 554 761.4 714.2 765.7 226.7 746.9 709.1 569.3 591.2 880.7 367.8 950.8 934.6 764.4 40 71 212.9 159.4 789.5 467.2 666.9 412.9 963.8 521.8 29.1 502.3 320.5 871.7 643.2 253.8 621.4 421.1 608.8 705.3 337.6 856.7 803 612.6 404.1 544.1 14.6 523.3 702.9 202.8 340.6 340.9 306.8 566.1 299.1 268.9 795.5 267.2 142.5 626 894.9 526.6 593.1 301.3 395.2 668.7 713.5 350.4 641.3 428.6 376.9 864.7 639.3 712.7 728.1 516.2 729.5 884.1 542.4 654.5 884.8 97.3 985.3 609.6 625.4 19.53 19.532 19.533 19.539 19.557 19.559 19.575 19.58 19.594 19.614 19.614 19.631 19.638 19.639 19.64 19.654 19.66 19.66 19.688 19.693 19.697 19.7 19.714 19.716 19.721 19.729 19.732 19.732 19.736 19.736 19.737 19.738 19.739 19.75 19.753 19.765 19.767 19.77 19.782 19.803 19.814 19.817 19.849 19.911 19.94 19.969 19.985 19.988 19.992 20 20.015 20.018 20.019 20.025 20.037 20.043 20.045 20.051 20.07 20.073 20.073 20.092 20.096 20.102 20.103 0.048 0.034 0.038 0.037 0.038 0.042 0.041 0.031 0.032 0.045 0.036 0.035 0.042 0.039 0.041 0.045 0.047 0.043 0.04 0.041 0.046 0.05 0.045 0.043 0.043 0.046 0.045 0.045 0.041 0.046 0.048 0.042 0.036 0.048 0.041 0.036 0.054 0.036 0.049 0.044 0.051 0.046 0.051 0.047 0.049 0.048 0.053 0.058 0.057 0.062 0.049 0.05 0.053 0.056 0.06 0.053 0.051 0.06 0.054 0.04 0.064 0.049 0.062 0.062 0.061 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.055 99.999 99.999 1.345 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.991 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.111 99.999 99.999 0.184 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.154 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.659 0.783 0.821 0.745 0.818 0.8 0.746 1.095 0.717 0.999 0.718 0.998 0.709 0.946 1.102 0.997 0.891 0.928 0.894 0.659 0.924 1.015 0.774 0.834 0.788 0.819 0.794 0.903 0.807 0.796 0.872 0.61 0.737 0.803 0.809 0.826 0.793 0.628 0.799 0.748 0.889 0.823 0.767 1.17 0.713 1.129 1.096 1.099 1.104 0.999 0.983 0.999 0.965 0.95 1.167 0.954 1.082 0.939 0.836 0.869 0.873 0.823 0.843 0.85 0.842 0.064 0.044 0.051 0.05 0.05 0.054 0.055 0.041 0.044 0.061 0.05 0.046 0.056 0.049 0.053 0.059 0.061 0.055 0.052 0.053 0.059 0.063 0.057 0.056 0.057 0.058 0.063 0.058 0.054 0.062 0.065 0.057 0.049 0.064 0.054 0.05 0.067 0.049 0.063 0.058 0.068 0.059 0.068 0.063 0.068 0.06 0.068 0.074 0.073 0.078 0.066 0.064 0.07 0.071 0.075 0.069 0.065 0.075 0.071 0.054 0.081 0.067 0.08 0.079 0.079 1.378 1.484 1.507 1.469 1.575 1.578 1.606 2.149 1.519 2.143 1.589 1.983 1.443 1.839 2.141 1.877 1.646 1.806 1.663 1.452 1.842 1.862 1.553 1.589 1.674 1.774 1.554 1.805 1.557 1.516 1.657 1.383 1.497 1.464 1.547 1.767 1.646 1.346 1.71 1.63 1.702 1.599 1.598 2.019 1.476 2.104 2.086 2.062 2.013 1.859 1.759 1.977 1.771 1.773 2.653 1.796 2.086 1.743 1.621 1.614 1.621 1.563 1.656 1.701 1.731 0.06 0.041 0.045 0.044 0.043 0.048 0.049 0.033 0.037 0.046 0.045 0.039 0.05 0.043 0.043 0.052 0.051 0.047 0.046 0.047 0.049 0.054 0.05 0.049 0.049 0.05 0.055 0.049 0.047 0.053 0.055 0.049 0.041 0.056 0.047 0.042 0.057 0.043 0.052 0.049 0.058 0.053 0.057 0.052 0.056 0.052 0.058 0.063 0.063 0.068 0.058 0.055 0.058 0.061 0.061 0.06 0.055 0.066 0.062 0.049 0.073 0.058 0.069 0.068 0.068 UBVRI PHOTOMETRY OF OPEN CLUSTERS 401 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 3 (CONTINUED) X Y V σV (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 417.5 88.7 964.3 473.2 583 849.2 635 686.7 831.9 285.4 506.3 503.3 788 645.4 158 252.2 969.6 322.6 909.1 853.6 512.3 981.4 605.7 147.8 805.1 754.5 475.5 419.7 880 253 825.6 533.3 870 584.9 971.2 568.3 901.7 990.6 784.3 404.5 809.9 109.2 726.7 833.3 993.4 961.8 605.6 666.7 795.7 960.8 941.4 943.9 871.2 889.1 606.2 218.9 573.6 194.1 382.4 379.1 940.4 683.9 646.6 651.2 96.9 66.5 964.5 246.9 973.6 173.2 787 273.4 825.9 870.4 959.5 830.4 802.5 36.3 580.8 669.4 909.6 443.1 609.3 326.8 170.9 339.4 500.4 192.3 751.6 349.6 359.6 900.1 313.4 437.1 364 811.1 527.1 99.4 120.9 453.6 444.3 244.7 741.3 224.1 103.9 45.4 654.6 251.2 833.8 427.6 20.105 20.105 20.109 20.111 20.113 20.113 20.117 20.118 20.122 20.127 20.128 20.132 20.132 20.144 20.15 20.154 20.161 20.165 20.172 20.174 20.185 20.196 20.21 20.217 20.219 20.221 20.225 20.226 20.227 20.236 20.239 20.24 20.24 20.244 20.246 20.252 20.253 20.254 20.266 20.27 20.283 20.284 20.286 20.29 20.302 20.321 20.342 20.364 20.365 20.395 20.398 20.409 20.423 20.445 20.516 0.058 0.056 0.052 0.05 0.058 0.058 0.055 0.062 0.053 0.058 0.078 0.063 0.063 0.061 0.063 0.054 0.056 0.064 0.053 0.056 0.068 0.049 0.055 0.074 0.063 0.066 0.066 0.062 0.081 0.064 0.08 0.053 0.074 0.073 0.064 0.074 0.055 0.059 0.062 0.069 0.071 0.091 0.066 0.075 0.067 0.068 0.074 0.064 0.074 0.082 0.074 0.072 0.072 0.099 0.091 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.879 0.838 0.865 0.936 0.89 0.874 0.834 0.834 0.99 0.826 0.871 0.841 1.038 0.765 0.85 0.763 0.731 1.02 0.764 0.913 0.781 1.012 0.826 0.757 0.787 1.162 1.036 1.068 0.744 0.642 0.861 0.827 1.169 0.869 0.994 0.787 0.945 0.836 0.913 0.76 1.089 0.771 0.689 0.811 0.825 0.888 0.794 0.884 0.871 0.832 0.766 0.899 0.918 1.046 1.033 0.075 0.072 0.067 0.067 0.077 0.079 0.071 0.081 0.068 0.078 0.097 0.081 0.08 0.081 0.081 0.075 0.078 0.084 0.072 0.071 0.088 0.064 0.074 0.094 0.082 0.082 0.083 0.079 0.1 0.089 0.102 0.075 0.095 0.093 0.083 0.096 0.075 0.079 0.08 0.089 0.089 0.115 0.085 0.098 0.084 0.089 0.096 0.082 0.097 0.105 0.1 0.094 0.095 0.126 0.117 1.816 1.649 1.622 1.724 1.741 1.723 1.764 1.697 2.078 1.626 1.794 1.593 1.841 1.65 1.721 1.564 1.694 99.999 1.539 1.708 1.463 2.157 1.676 1.442 1.687 1.901 1.813 1.914 1.675 1.399 1.667 1.543 2.122 1.801 1.929 1.691 1.747 1.78 1.661 1.6 2.181 1.674 1.695 1.545 1.805 1.768 1.636 1.768 1.794 1.804 1.65 1.637 1.676 1.884 2.15 0.063 0.063 0.061 0.057 0.066 0.065 0.061 0.069 0.057 0.067 0.083 0.071 0.07 0.069 0.075 0.062 0.062 99.999 0.061 0.064 0.077 0.053 0.065 0.085 0.07 0.073 0.073 0.071 0.088 0.077 0.088 0.063 0.081 0.079 0.069 0.081 0.061 0.064 0.072 0.078 0.075 0.097 0.073 0.082 0.071 0.073 0.082 0.072 0.08 0.087 0.084 0.082 0.082 0.112 0.096 2.3. The data inspection tools elipse and safe Since the stellar density of a cluster increases towards its center with respect to the field stars, an awk macro (elipse, Moitinho 2003, private communication) was used to extract the data of the central region of a given cluster, as defined by visual inspec- tion in a visual (V ) or red (R) image, thus increasing the contrast of the cluster with respect to the surrounding field stars. An ellipse was fitted visually to the image in order to extract the photometric data of the central region of the cluster. To further support the analyses of the clusters, a Java-based computer program (safe, McFarland 2010) was developed and 402 AKKAYA ET AL. TABLE 4 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México CCD UBVRI PHOTOMETRY OF RU 135 X Y V σV 862.7 237.1 294 753.2 219.7 251.1 914.4 905.1 244 765.1 754.6 312 929 311.8 240.7 375.8 170 900.7 59.6 469.5 853.8 809.4 811.6 655.4 900.3 153.8 989.5 472.4 61.3 501.1 183.2 818.7 351.3 379.3 343.8 68.5 706.7 150.3 313.6 375.9 799.1 903.7 864.3 521.4 892.6 461.7 76.8 695.9 463 203.7 360.7 470.2 247.4 548 140.3 188.1 209.3 328.2 88 211 627.1 358.2 333.6 444 231.5 325.4 387.3 283.1 343 263.2 595.1 237 620.7 218 654.7 509.4 857.1 534.8 741.6 871.1 549.7 200.3 527.3 207.9 605.3 224 155.8 41.7 424.6 339.4 613.4 387.8 781.1 703.7 500.2 932 365.8 444 97.8 51 842.4 825.4 726.9 803.3 572.3 670.2 948.6 250.4 117 756.4 106.8 568.1 662.2 486 317 605.9 882.8 109.8 606.1 270.2 281.9 15.2 309.4 583.4 302.6 286.1 329.6 138.8 11.132 11.689 11.871 12.258 12.337 12.691 12.697 12.769 12.8 12.809 13.162 13.221 13.228 13.467 14.015 14.124 14.153 14.153 14.168 14.189 14.221 14.231 14.256 14.441 14.467 14.601 14.68 14.741 14.918 14.956 14.976 14.986 14.994 15.06 15.111 15.134 15.192 15.197 15.205 15.224 15.23 15.288 15.3 15.316 15.322 15.425 15.463 15.488 15.506 15.517 15.546 15.559 15.6 15.611 15.616 15.655 15.658 15.663 15.683 15.74 15.745 15.779 15.836 15.841 0.003 0.003 0.008 0.002 0.004 0.005 0.005 0.004 0.004 0.005 0.002 0.002 0.002 0.002 0.003 0.003 0.003 0.005 0.003 0.003 0.004 0.003 0.003 0.005 0.003 0.003 0.004 0.004 0.005 0.005 0.004 0.003 0.004 0.003 0.004 0.006 0.004 0.004 0.004 0.003 0.004 0.005 0.004 0.005 0.004 0.005 0.006 0.006 0.005 0.007 0.005 0.004 0.004 0.004 0.005 0.005 0.005 0.006 0.005 0.004 0.005 0.004 0.008 0.005 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 0.597 0.71 0.742 0.742 0.789 0.734 0.729 0.768 0.755 0.686 2.372 0.995 1.885 1.023 0.818 1.035 0.835 1.018 0.831 0.859 1.196 1.853 1.446 0.948 2.276 1.895 1.226 0.969 1.098 1.036 0.99 2.001 0.999 2.422 1.031 1.088 1.84 1.112 2.212 2.564 2.175 0.988 1.032 1.04 1.195 1.084 1.174 1.072 1.279 2.078 1.068 1.315 2.152 1.321 1.837 1.176 1.184 1.1 1.884 1.191 1.194 1.274 1.821 1.097 0.004 0.003 0.003 0.004 0.003 0.004 0.004 0.003 0.003 0.005 0.006 0.011 0.009 0.005 0.005 0.006 0.005 0.01 0.006 0.006 0.008 0.011 0.008 0.009 0.011 0.013 0.008 0.008 0.01 0.009 0.008 0.012 0.009 0.017 0.009 0.014 0.014 0.01 0.017 0.018 0.017 0.01 0.011 0.01 0.011 0.011 0.015 0.014 0.011 0.021 0.012 0.012 0.019 0.012 0.016 0.013 0.014 0.014 0.018 0.013 0.013 0.014 0.024 0.014 0.212 0.364 0.405 0.405 0.409 0.418 0.383 0.401 0.378 0.426 2.415 0.399 1.897 0.446 0.444 0.31 0.345 0.422 0.403 0.494 0.529 1.838 1.047 0.543 2.269 1.697 0.502 0.442 0.407 0.428 0.385 1.942 0.384 99.999 0.352 0.459 1.504 0.388 99.999 99.999 99.999 0.556 0.343 0.404 0.554 0.441 0.552 0.396 0.749 99.999 0.374 0.62 99.999 0.62 1.35 0.437 0.464 0.398 1.365 0.571 0.591 0.588 99.999 0.394 0.002 0.003 0.004 0.005 0.005 0.005 0.004 0.006 0.006 0.005 0.033 0.007 0.024 0.008 0.01 0.012 0.01 0.013 0.012 0.011 0.014 0.038 0.02 0.013 0.088 0.049 0.021 0.017 0.02 0.019 0.019 0.079 0.017 99.999 0.02 0.025 0.079 0.023 99.999 99.999 99.999 0.022 0.023 0.023 0.031 0.025 0.029 0.025 0.034 99.999 0.028 0.035 99.999 0.033 0.085 0.029 0.031 0.029 0.119 0.033 0.034 0.037 99.999 0.031 0.36 0.387 0.45 0.45 0.47 0.431 0.433 0.447 0.439 0.414 1.276 0.549 1.003 0.579 0.462 0.63 0.483 0.592 0.462 0.494 0.693 0.993 0.811 0.552 1.236 1.004 0.715 0.556 0.654 0.627 0.602 1.115 0.585 1.301 0.571 0.632 1.03 0.657 1.223 1.531 1.197 0.573 0.632 0.609 0.706 0.609 0.651 0.65 0.735 1.127 0.643 0.747 1.191 0.743 1.014 0.689 0.693 0.659 1.005 0.699 0.717 0.737 0.987 0.614 0.01 0.014 0.038 0.002 0.015 0.014 0.014 0.01 0.01 0.012 0.002 0.003 0.003 0.002 0.02 0.003 0.017 0.008 0.024 0.004 0.005 0.003 0.003 0.005 0.003 0.004 0.005 0.004 0.006 0.005 0.004 0.004 0.004 0.004 0.005 0.009 0.005 0.006 0.005 0.004 0.005 0.006 0.006 0.006 0.006 0.006 0.008 0.009 0.006 0.008 0.007 0.006 0.005 0.006 0.006 0.007 0.006 0.008 0.006 0.006 0.006 0.007 0.012 0.006 99.999 0.86 0.895 99.999 0.97 0.886 0.915 0.956 0.867 0.861 2.387 1.099 1.88 1.125 0.976 1.266 1.001 99.999 0.995 1.025 1.353 1.896 1.556 1.138 2.373 1.915 1.464 1.137 1.297 1.253 1.212 2.156 1.193 2.513 1.177 1.309 1.986 1.316 2.286 3.096 2.282 1.197 1.293 1.242 1.405 1.244 1.321 1.255 1.424 2.196 1.261 1.489 2.26 1.479 1.982 1.392 1.377 1.325 1.983 1.372 1.432 1.462 1.85 1.263 99.999 0.011 0.014 99.999 0.01 0.003 0.003 0.003 0.003 0.003 0.01 0.007 0.01 0.003 0.003 0.003 0.004 99.999 0.004 0.004 0.005 0.004 0.003 0.005 0.003 0.005 0.004 0.005 0.006 0.005 0.004 0.004 0.005 0.004 0.005 0.008 0.004 0.005 0.004 0.003 0.005 0.005 0.005 0.005 0.005 0.005 0.007 0.027 0.006 0.006 0.007 0.005 0.004 0.005 0.005 0.006 0.006 0.007 0.005 0.005 0.006 0.006 0.027 0.006 UBVRI PHOTOMETRY OF OPEN CLUSTERS 403 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 184.3 290.3 185.1 752.2 882.7 752.8 366.3 768.8 338.2 824.9 886.1 306.2 191.6 92 415.8 413.4 95.5 24.3 815.3 813.1 515.2 610.2 282.9 630.8 344.2 79.3 572.8 129.5 737.2 264.5 934.5 760.6 61.3 746.1 137 490.8 409.1 95.7 354.4 812.7 505.7 863.5 972.6 2.1 391.1 873.1 586.2 290 725.5 555 854 461.8 905.1 456.4 99.2 927.5 680.8 213.2 406.4 419 586.2 794.2 678.4 849.3 365.7 156.4 820 303.8 234.9 402 333.3 733.8 480.5 543 90.7 64.7 231.2 824.7 669.5 678 968.1 213.4 889.5 299.1 887.9 638.1 188.3 294 830.9 635.4 162.9 270.1 213.6 127 811.1 777.8 237.7 550.9 553.6 114.2 235.2 408.2 283.6 22.9 941.2 355.6 194.2 537.6 730.3 118.5 830.6 206.6 658.1 63.5 100.3 250.4 771.5 176.8 15.1 781.6 770.3 475 105.6 622.9 861.7 210.8 482.6 705.6 942 61.4 892.8 570 15.872 15.937 16.002 16.035 16.039 16.051 16.091 16.107 16.112 16.124 16.133 16.141 16.186 16.2 16.235 16.237 16.243 16.3 16.324 16.356 16.388 16.405 16.434 16.465 16.467 16.506 16.526 16.538 16.557 16.594 16.614 16.634 16.652 16.664 16.673 16.687 16.709 16.717 16.733 16.742 16.752 16.767 16.781 16.789 16.817 16.842 16.85 16.873 16.877 16.887 16.893 16.913 16.923 16.941 16.949 16.953 16.967 16.969 16.987 16.995 17.031 17.04 17.043 17.07 17.073 17.083 0.006 0.005 0.006 0.005 0.006 0.004 0.006 0.006 0.006 0.006 0.006 0.006 0.005 0.006 0.006 0.007 0.006 0.006 0.006 0.006 0.007 0.006 0.006 0.007 0.007 0.008 0.021 0.006 0.013 0.007 0.009 0.008 0.007 0.008 0.007 0.008 0.008 0.01 0.007 0.007 0.009 0.008 0.009 0.009 0.009 0.01 0.008 0.009 0.008 0.008 0.013 0.008 0.011 0.007 0.01 0.009 0.008 0.009 0.009 0.011 0.01 0.009 0.012 0.01 0.01 0.008 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 2.283 1.284 2.123 1.217 1.919 1.208 2.366 2.45 1.23 2.435 1.304 1.819 1.206 1.869 1.435 2.121 1.18 1.182 1.194 1.982 1.684 1.342 1.129 1.319 1.347 1.229 1.805 1.239 1.498 2.012 2.107 1.309 1.884 2.049 1.193 1.758 1.326 1.954 1.144 1.902 1.286 1.727 1.918 2.02 1.322 1.587 1.634 2.045 1.24 1.771 1.408 1.371 1.366 2.022 99.999 1.58 1.871 1.477 1.7 1.88 1.26 1.926 2.349 1.88 1.297 1.268 0.023 0.016 0.027 0.016 0.021 0.015 0.027 0.028 0.017 0.032 0.019 0.02 0.016 0.025 0.019 0.028 0.017 0.018 0.02 0.024 0.025 0.022 0.018 0.021 0.021 0.021 0.034 0.021 0.023 0.031 0.038 0.022 0.03 0.033 0.022 0.029 0.023 0.034 0.023 0.031 0.025 0.03 0.033 0.04 0.026 0.032 0.031 0.036 0.025 0.034 0.027 0.028 0.029 0.036 99.999 0.03 0.036 0.03 0.035 0.043 0.025 0.043 0.061 0.04 0.03 0.026 99.999 0.499 99.999 0.546 99.999 0.579 99.999 99.999 0.653 99.999 99.999 99.999 0.543 99.999 0.716 99.999 0.262 0.353 0.593 99.999 99.999 0.947 0.392 0.568 0.765 99.999 99.999 0.392 0.822 99.999 99.999 0.639 99.999 99.999 0.559 99.999 0.727 99.999 0.481 99.999 0.652 99.999 99.999 99.999 0.71 99.999 99.999 99.999 0.451 99.999 0.58 99.999 0.665 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.761 99.999 99.999 99.999 99.999 99.999 99.999 0.038 99.999 0.043 99.999 0.042 99.999 99.999 0.05 99.999 99.999 99.999 0.044 99.999 0.063 99.999 0.04 0.047 0.054 99.999 99.999 0.081 0.045 0.059 0.07 99.999 99.999 0.059 0.107 99.999 99.999 0.071 99.999 99.999 0.074 99.999 0.077 99.999 0.064 99.999 0.098 99.999 99.999 99.999 0.095 99.999 99.999 99.999 0.082 99.999 0.111 99.999 0.088 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.103 99.999 99.999 99.999 99.999 99.999 1.231 0.723 1.139 0.715 1.051 0.727 1.308 1.312 0.762 1.381 0.718 0.921 0.708 0.999 0.793 1.122 0.649 0.701 0.76 1.103 0.941 0.769 0.709 0.785 0.768 0.74 1.028 0.714 0.862 1.095 1.144 0.777 1.057 1.109 0.743 1.029 0.763 1.103 0.698 1.057 0.752 1.082 1.026 1.077 0.76 0.878 0.874 1.175 0.718 0.988 0.796 0.773 0.772 1.123 1.036 0.939 1.029 0.851 0.979 1.037 0.741 1.098 1.293 1.07 0.828 0.764 0.007 0.007 0.007 0.008 0.007 0.006 0.007 0.008 0.009 0.008 0.008 0.008 0.008 0.008 0.008 0.008 0.009 0.01 0.009 0.008 0.008 0.009 0.008 0.01 0.009 0.01 0.067 0.01 0.01 0.008 0.012 0.009 0.009 0.01 0.01 0.01 0.011 0.012 0.01 0.009 0.012 0.01 0.011 0.012 0.011 0.012 0.01 0.011 0.011 0.011 0.012 0.011 0.013 0.009 0.013 0.011 0.01 0.012 0.011 0.014 0.012 0.011 0.016 0.012 0.013 0.011 2.301 1.418 2.165 1.418 2.013 1.435 2.527 2.477 1.471 2.598 1.438 1.676 1.429 1.928 1.576 2.164 1.354 1.439 1.495 2.116 1.798 1.516 1.405 1.499 1.506 1.461 99.999 1.408 1.671 2.074 2.187 1.533 2.061 2.11 1.437 2.007 1.498 2.117 1.407 2.031 1.481 2.244 2.028 2.098 1.488 1.721 1.742 2.249 1.433 1.947 1.58 1.49 1.539 2.116 2.123 1.806 2.015 1.668 1.894 2.012 1.467 2.084 2.421 2.077 1.58 1.493 σV −I 0.006 0.007 0.006 0.007 0.006 0.006 0.006 0.006 0.008 0.006 0.007 0.006 0.007 0.006 0.007 0.007 0.008 0.008 0.008 0.007 0.007 0.008 0.008 0.009 0.008 0.008 99.999 0.009 0.009 0.007 0.01 0.009 0.008 0.008 0.009 0.008 0.01 0.011 0.01 0.008 0.011 0.008 0.009 0.01 0.01 0.011 0.009 0.009 0.01 0.009 0.011 0.01 0.011 0.008 0.039 0.01 0.009 0.01 0.009 0.014 0.01 0.009 0.013 0.01 0.011 0.009 404 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 368.6 445.4 218.5 476.3 822 906.3 482.2 237.5 527.7 906.9 201.5 925.6 466 446.9 745.3 751.7 607.5 753.5 319.2 810 110.2 357.8 328.3 818.2 611.8 508 971.1 919.6 547.2 824.3 7.8 869.9 974.9 792.6 31.4 518.1 334.7 87.4 87.5 469.8 655.5 528.4 137.2 111.4 201.9 7.3 164.5 229.5 167.3 608.8 72.4 434.2 734.2 659.9 468.6 690.6 795.7 205.9 879.8 873.3 714.3 601.7 24.5 331.1 768.7 282.8 275.1 296.3 564.4 271.1 108.5 510.2 595.9 120.7 735.7 842.3 732.9 149.5 902.1 492.6 579.2 152.2 572.6 233.6 878.6 904 933.7 451.6 762.8 740.1 964.6 75.8 836.7 70.5 231.7 986.5 319.3 635.1 118.1 311.8 739.7 429.3 347.9 480.8 256.5 867.5 726.6 217.8 585.6 515.9 138.1 466.3 186.9 520.9 429.6 72.8 217.1 710.5 460.8 85.5 705.9 801.2 485.1 514 929.6 723.2 66.9 607.3 766.4 211.7 25.7 367.4 17.086 17.104 17.138 17.139 17.151 17.165 17.168 17.173 17.181 17.183 17.184 17.197 17.217 17.218 17.219 17.219 17.223 17.224 17.236 17.241 17.245 17.249 17.26 17.263 17.306 17.31 17.322 17.327 17.357 17.382 17.389 17.397 17.418 17.424 17.429 17.43 17.448 17.453 17.459 17.461 17.461 17.463 17.469 17.476 17.485 17.487 17.489 17.505 17.511 17.522 17.532 17.534 17.542 17.547 17.551 17.57 17.582 17.583 17.584 17.587 17.594 17.623 17.627 17.632 17.642 17.643 0.009 0.011 0.009 0.01 0.01 0.01 0.009 0.009 0.009 0.011 0.009 0.015 0.009 0.014 0.011 0.011 0.011 0.011 0.01 0.011 0.011 0.01 0.01 0.01 0.011 0.012 0.011 0.012 0.011 0.011 0.013 0.01 0.009 0.015 0.013 0.012 0.013 0.011 0.012 0.012 0.011 0.012 0.011 0.014 0.012 0.011 0.013 0.011 0.012 0.012 0.013 0.012 0.012 0.013 0.012 0.012 0.014 0.014 0.012 0.011 0.013 0.012 0.015 0.014 0.012 0.014 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 2.122 1.301 1.362 1.332 2.077 1.756 1.926 2.32 1.942 1.385 1.217 99.999 1.854 99.999 1.391 1.897 1.342 1.803 1.311 1.403 1.413 1.513 1.815 1.784 1.419 1.431 1.909 1.279 1.756 1.823 2.027 1.69 2.62 1.873 2.082 1.284 1.36 2.005 2.073 1.473 1.536 2.028 1.984 1.968 2.028 1.361 1.42 1.33 1.653 1.609 1.351 1.447 1.702 2.064 1.368 1.328 99.999 2.232 1.381 1.898 1.376 2.037 1.367 1.393 2.137 99.999 0.051 0.029 0.033 0.028 0.049 0.039 0.045 0.052 0.045 0.034 0.031 99.999 0.043 99.999 0.034 0.053 0.033 0.038 0.031 0.035 0.035 0.034 0.041 0.041 0.035 0.035 0.05 0.038 0.048 0.052 0.051 0.046 0.081 0.055 0.063 0.037 0.036 0.058 0.068 0.041 0.039 0.067 0.051 0.058 0.063 0.035 0.037 0.042 0.053 0.046 0.043 0.054 0.047 0.052 0.038 0.04 99.999 0.07 0.044 0.05 0.044 0.073 0.045 0.045 0.077 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.196 0.746 0.757 0.758 1.21 0.991 1.131 1.267 1.052 0.8 0.8 0.83 0.993 1.086 0.881 1.078 0.786 1.094 0.75 0.861 0.787 0.825 1.021 1.012 0.804 0.81 1.064 0.767 1.025 1.022 1.085 1.029 1.382 1.034 1.137 0.757 0.796 1.093 1.098 0.854 0.858 1.127 1.097 1.092 1.17 0.78 0.789 0.812 1.014 0.846 0.77 0.914 0.974 1.102 0.812 0.828 1.103 1.212 0.803 1.123 0.8 1.104 0.758 0.835 1.201 1.004 0.011 0.014 0.012 0.013 0.013 0.013 0.012 0.012 0.011 0.014 0.012 0.022 0.011 0.019 0.014 0.015 0.014 0.014 0.013 0.015 0.015 0.013 0.013 0.013 0.015 0.014 0.014 0.015 0.014 0.014 0.016 0.013 0.012 0.019 0.016 0.016 0.016 0.014 0.015 0.015 0.014 0.016 0.014 0.019 0.016 0.016 0.017 0.015 0.015 0.015 0.017 0.015 0.015 0.017 0.015 0.017 0.018 0.018 0.015 0.014 0.017 0.015 0.018 0.018 0.016 0.018 2.257 1.485 1.519 1.494 2.301 1.952 2.12 2.38 1.994 1.585 1.525 1.654 1.949 99.999 1.718 2.063 1.55 2.079 1.474 1.66 1.558 1.591 1.969 1.956 1.572 1.613 2.097 1.542 1.975 1.953 2.095 1.973 2.67 1.989 2.149 1.542 1.521 2.092 2.116 1.673 1.66 2.086 2.082 2.107 2.187 1.54 1.548 1.523 1.966 1.679 1.537 1.728 1.843 2.127 1.61 1.662 2.119 2.285 1.618 2.092 1.574 2.101 1.545 1.554 2.278 1.968 σV −I 0.009 0.012 0.01 0.011 0.011 0.01 0.01 0.01 0.009 0.012 0.011 0.019 0.009 99.999 0.012 0.012 0.012 0.012 0.011 0.013 0.013 0.011 0.011 0.011 0.014 0.013 0.012 0.013 0.012 0.012 0.013 0.011 0.01 0.016 0.013 0.014 0.014 0.012 0.012 0.013 0.012 0.013 0.012 0.015 0.013 0.012 0.015 0.013 0.013 0.013 0.015 0.014 0.013 0.014 0.013 0.014 0.015 0.015 0.013 0.012 0.015 0.013 0.016 0.016 0.013 0.016 UBVRI PHOTOMETRY OF OPEN CLUSTERS 405 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 271 410.2 174.1 451.2 310.9 654.1 789.2 775.5 348.7 210.8 544.3 323.4 902.9 296.1 356 779.3 363.4 547.8 780.8 203 92.1 702.2 662.5 725.8 877.3 985.6 218.7 951.4 275.4 555.7 246 850.1 129.8 768.6 226.9 848.3 624.2 656.1 924.3 485.3 776.4 626.6 169.6 475.8 615.9 668.5 981.7 88.4 473.4 695.6 125.4 71.7 781.7 19.2 384.2 71.3 293.6 234.5 794.2 686.7 381.4 262.2 240.9 732.9 452.9 564.3 201.8 815.2 880.8 656.3 206.9 576.7 702.1 886.6 659.8 480.9 696.3 401.1 681.7 529.6 482.3 599.5 109.5 846.7 604.5 36.2 990.2 601.4 917.2 623 477.7 318.6 812.3 441 536.2 140.9 723.6 803.5 227.8 616.3 302.7 122.4 13.8 636.9 881 54.3 547.5 918.6 332.3 951.5 635.6 725.7 950.3 816.2 164.6 330.1 340 473.4 480.8 716.9 612.5 314.4 642.1 252.3 761 183.9 217.1 294.3 236.3 758.2 189.2 495.4 17.667 17.667 17.669 17.669 17.67 17.672 17.683 17.685 17.694 17.701 17.701 17.708 17.715 17.717 17.728 17.733 17.74 17.756 17.761 17.767 17.767 17.768 17.769 17.775 17.777 17.784 17.789 17.796 17.799 17.803 17.818 17.819 17.822 17.826 17.83 17.842 17.843 17.859 17.873 17.878 17.878 17.891 17.892 17.894 17.927 17.93 17.934 17.936 17.939 17.943 17.946 17.949 17.958 17.964 17.968 17.97 17.974 17.978 17.983 17.991 17.995 17.997 17.999 18.004 18.011 18.017 0.013 0.015 0.014 0.015 0.012 0.013 0.014 0.014 0.013 0.013 0.015 0.014 0.012 0.014 0.013 0.015 0.014 0.015 0.016 0.015 0.017 0.014 0.014 0.013 0.013 0.016 0.014 0.013 0.015 0.012 0.014 0.014 0.015 0.015 0.015 0.019 0.015 0.016 0.015 0.015 0.016 0.015 0.018 0.014 0.016 0.016 0.017 0.014 0.015 0.019 0.016 0.015 0.016 0.015 0.014 0.019 0.017 0.017 0.02 0.015 0.016 0.018 0.017 0.015 0.018 0.016 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 99.999 2.004 1.98 1.413 1.611 2.396 1.487 1.056 1.294 2.119 1.373 2.048 2.119 1.454 1.282 1.307 1.812 1.413 1.361 1.781 1.47 1.339 1.962 1.525 2.019 1.468 1.235 1.41 1.899 1.857 1.866 1.613 1.398 1.358 2.57 99.999 1.392 1.834 2.234 1.752 1.894 1.644 1.62 1.815 1.859 1.474 1.544 1.761 1.801 1.944 1.876 2.197 1.83 1.341 1.563 1.929 1.661 1.8 2.19 1.378 2.145 2.129 99.999 1.675 1.444 1.859 99.999 0.065 0.065 0.045 0.051 0.086 0.048 0.037 0.041 0.077 0.045 0.074 0.066 0.05 0.045 0.062 0.06 0.049 0.063 0.067 0.049 0.041 0.062 0.05 0.067 0.054 0.043 0.05 0.074 0.064 0.078 0.051 0.049 0.049 0.116 99.999 0.049 0.074 0.144 0.07 0.074 0.061 0.066 0.075 0.074 0.055 0.055 0.074 0.072 0.083 0.073 0.096 0.074 0.055 0.058 0.075 0.071 0.074 0.101 0.06 0.103 0.102 99.999 0.065 0.065 0.069 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.113 1.171 1.109 0.727 0.882 1.263 0.826 0.658 0.753 1.122 0.831 1.048 1.185 0.817 0.818 0.778 1 0.831 0.879 1.064 0.797 0.828 1.058 0.897 1.091 0.825 0.789 0.79 1.156 1.158 1.13 0.868 0.868 0.833 1.193 1.086 0.844 1.18 1.974 0.986 1.086 0.991 0.904 1.039 1.086 0.858 0.887 1.037 1.124 1.13 1.089 1.098 0.997 0.781 0.882 1.103 0.979 0.975 1.16 0.862 1.202 1.164 1.041 0.916 0.852 1.2 0.018 0.02 0.019 0.019 0.016 0.017 0.019 0.019 0.018 0.017 0.019 0.018 0.016 0.019 0.017 0.02 0.018 0.019 0.024 0.019 0.024 0.018 0.018 0.017 0.017 0.023 0.018 0.017 0.019 0.016 0.018 0.018 0.018 0.02 0.019 0.024 0.02 0.02 0.02 0.019 0.02 0.019 0.023 0.018 0.021 0.02 0.023 0.019 0.019 0.026 0.02 0.02 0.021 0.019 0.019 0.023 0.022 0.021 0.026 0.02 0.02 0.022 0.022 0.02 0.023 0.02 2.15 2.15 2.12 1.478 1.75 2.388 1.652 1.364 1.529 2.14 1.64 1.956 2.209 1.569 1.611 1.535 1.911 1.632 1.686 2.072 1.56 1.609 2.044 1.742 2.078 1.595 1.573 1.571 2.143 2.171 2.125 1.65 1.63 1.656 2.303 2.079 1.607 2.467 4.023 1.968 2.068 1.87 1.844 2.036 2.107 1.685 1.728 1.989 2.07 99.999 2.093 2.188 1.972 1.552 1.744 2.052 1.907 1.939 2.207 1.676 2.232 2.223 1.954 1.793 1.645 2.208 σV −I 0.014 0.016 0.016 0.016 0.014 0.014 0.016 0.017 0.015 0.014 0.016 0.015 0.013 0.016 0.014 0.017 0.016 0.017 0.02 0.016 0.02 0.016 0.015 0.014 0.014 0.019 0.016 0.015 0.016 0.013 0.015 0.016 0.017 0.02 0.015 0.02 0.018 0.016 0.016 0.017 0.017 0.016 0.02 0.015 0.018 0.018 0.02 0.016 0.016 99.999 0.017 0.016 0.017 0.016 0.015 0.02 0.019 0.018 0.021 0.018 0.017 0.018 0.018 0.016 0.021 0.017 406 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 784.2 86 559.1 621.8 89.1 565.2 770 936 64.9 561.6 339.2 29.4 639.4 942.9 660 538.7 534 104.2 702.1 634.1 18.8 301.3 154.6 180.2 384.4 367.9 321.6 617 396.5 243.6 708.6 424.6 253.4 112.5 389.1 298.2 423.5 922.1 361 111 398.2 405.6 363.4 472.3 508.4 532.6 440.5 320.9 986.6 450 316.1 372.5 783.9 829.5 705.8 464.5 813.9 19.2 512.9 222.8 600.4 540.9 636.8 21.3 889.9 21.5 128.7 981.2 342.8 401.8 656.5 744.2 383.1 416.7 663.2 865.9 141.5 688.4 780.1 270 510.9 10.3 206.9 768.2 852.9 309.7 612.5 286.2 58.7 599.2 351.1 577.9 180.6 889.7 755.3 499.2 913 215.9 805.6 255.6 792.5 225.2 27.7 394.6 686.7 342.2 318.1 308 868 304.8 17.4 313.5 448.8 42.3 232.2 290 846.9 958.6 820.6 860.4 462.1 233.2 651.7 121.5 118.8 499.6 429 912.4 506.6 444.2 539.7 597.5 18.022 18.029 18.031 18.038 18.039 18.053 18.055 18.057 18.068 18.07 18.074 18.1 18.101 18.101 18.104 18.109 18.114 18.117 18.118 18.123 18.126 18.13 18.143 18.148 18.155 18.17 18.174 18.182 18.187 18.188 18.197 18.198 18.204 18.207 18.211 18.214 18.215 18.22 18.225 18.225 18.237 18.237 18.238 18.245 18.246 18.246 18.253 18.257 18.258 18.265 18.267 18.267 18.271 18.278 18.284 18.285 18.287 18.293 18.315 18.32 18.32 18.325 18.335 18.338 18.343 18.346 0.015 0.016 0.016 0.017 0.022 0.017 0.022 0.015 0.017 0.016 0.017 0.019 0.019 0.018 0.023 0.017 0.019 0.023 0.018 0.018 0.018 0.018 0.018 0.018 0.02 0.019 0.02 0.018 0.018 0.017 0.02 0.022 0.02 0.022 0.017 0.021 0.021 0.022 0.022 0.019 0.019 0.017 0.02 0.019 0.019 0.02 0.021 0.019 0.019 0.021 0.023 0.02 0.016 0.024 0.02 0.023 0.016 0.019 0.021 0.021 0.02 0.019 0.019 0.021 0.02 0.022 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 2.148 1.98 1.299 1.493 99.999 1.386 1.488 1.618 1.828 1.428 1.326 99.999 2.005 1.596 1.76 1.532 1.979 99.999 1.589 1.809 1.946 99.999 1.457 1.716 1.228 1.586 1.019 1.43 99.999 1.309 1.445 1.574 0.938 1.442 1.574 1.365 99.999 1.356 99.999 1.185 1.697 1.904 1.409 1.863 1.405 1.317 1.903 1.64 1.978 1.365 99.999 1.298 1.419 1.401 1.89 1.72 1.365 1.905 1.412 1.965 1.612 1.841 1.504 1.371 1.877 1.346 0.088 0.088 0.06 0.064 99.999 0.057 0.072 0.061 0.09 0.06 0.058 99.999 0.086 0.071 0.09 0.074 0.087 99.999 0.074 0.081 0.082 99.999 0.065 0.076 0.061 0.071 0.054 0.065 99.999 0.065 0.066 0.076 0.049 0.067 0.071 0.073 99.999 0.078 99.999 0.062 0.089 0.102 0.074 0.099 0.064 0.069 0.098 0.078 0.104 0.064 99.999 0.069 0.073 0.077 0.088 0.107 0.068 0.102 0.071 0.102 0.087 0.106 0.075 0.066 0.088 0.072 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.192 1.055 0.839 0.887 0.807 0.855 0.853 0.909 1.04 0.836 0.741 1.057 1.115 0.899 1.015 0.813 1.072 0.851 0.917 0.98 1.028 0.833 0.845 0.924 0.854 0.804 0.532 0.894 1.183 0.848 0.877 0.844 0.491 0.795 0.838 0.802 1.157 0.835 1.07 0.773 1.03 1.024 0.799 1.07 0.88 0.785 1.11 0.884 0.952 0.834 0.861 0.757 0.872 0.818 1.043 0.866 0.826 1.126 0.875 1.152 1.006 0.941 0.853 0.874 1.076 0.774 0.02 0.021 0.022 0.022 0.031 0.022 0.031 0.02 0.022 0.021 0.023 0.024 0.024 0.024 0.03 0.022 0.024 0.031 0.024 0.023 0.023 0.025 0.023 0.022 0.028 0.024 0.026 0.023 0.023 0.022 0.027 0.029 0.027 0.029 0.024 0.027 0.027 0.031 0.028 0.025 0.025 0.022 0.027 0.025 0.024 0.025 0.027 0.024 0.025 0.028 0.032 0.025 0.022 0.034 0.025 0.031 0.023 0.026 0.026 0.027 0.025 0.025 0.025 0.028 0.026 0.028 2.261 2.044 1.645 1.685 1.608 1.639 1.702 1.789 2.018 1.62 1.488 2.019 2.153 1.693 99.999 1.646 2.005 99.999 1.785 1.95 2.036 1.548 1.665 1.912 1.574 1.66 1.198 1.689 2.231 1.596 1.683 1.611 1.119 1.616 1.67 1.571 2.236 1.643 1.994 1.57 2.009 1.998 1.622 2.073 1.716 1.582 2.102 1.748 1.912 1.655 1.686 1.512 1.663 1.638 2.021 1.69 1.684 2.129 1.69 2.143 1.89 1.843 1.648 1.735 2.048 1.577 0.015 0.017 0.019 0.019 0.028 0.019 0.026 0.017 0.018 0.018 0.02 0.02 0.019 0.02 99.999 0.019 0.02 99.999 0.02 0.019 0.019 0.02 0.019 0.019 0.024 0.021 0.024 0.02 0.019 0.02 0.024 0.036 0.023 0.024 0.022 0.025 0.022 0.028 0.024 0.021 0.022 0.019 0.024 0.02 0.02 0.021 0.023 0.021 0.02 0.023 0.029 0.022 0.018 0.029 0.021 0.027 0.018 0.021 0.023 0.023 0.021 0.021 0.022 0.024 0.022 0.025 UBVRI PHOTOMETRY OF OPEN CLUSTERS 407 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 639.9 122.9 127.3 540.9 978.6 659 104 770.3 899.1 180.3 345 980.7 406.1 303.4 515.2 396.6 823.8 432.4 52 215.9 375.3 260 267.9 154.6 206.2 221.3 814.4 785.2 376.4 60.1 173.3 757.7 130.9 508.9 14.3 839.1 143.1 777.5 980.3 667.4 262.9 484.1 367.6 823 303.9 516.4 799.6 855.3 197.1 403.5 818.2 704.8 28.5 165.3 22.7 185.4 621.6 330.4 315.5 53.7 439.8 5.5 980.2 680.5 541.5 512.2 912.8 438.9 48.8 740.8 104 782.1 207.9 966.7 688.8 472.9 502.8 395.9 164.1 159.3 91.2 620.2 537.1 593.6 700.1 235.4 600.2 848.6 915.8 810.4 388.7 943.6 882.2 358.9 573 85.2 748.6 317 109.1 918.3 826.2 774.3 282.5 523.5 451 220.8 39.2 551 877.7 324.7 589.4 894.4 652.7 665 930 623.1 83.4 960.7 126.4 308.2 787.2 44.3 79.5 36.6 662.9 504.4 228.9 523.6 401.1 293.2 879.7 846.2 18.351 18.356 18.363 18.372 18.374 18.377 18.382 18.389 18.391 18.395 18.395 18.404 18.405 18.409 18.409 18.411 18.411 18.415 18.424 18.429 18.433 18.439 18.443 18.445 18.451 18.458 18.472 18.485 18.486 18.488 18.492 18.494 18.496 18.501 18.505 18.515 18.52 18.521 18.522 18.526 18.527 18.53 18.541 18.549 18.551 18.557 18.561 18.564 18.566 18.566 18.57 18.576 18.578 18.585 18.589 18.598 18.607 18.61 18.627 18.634 18.634 18.636 18.638 18.643 18.646 18.648 0.02 0.019 0.021 0.021 0.02 0.019 0.023 0.021 0.02 0.021 0.022 0.024 0.021 0.023 0.022 0.021 0.021 0.021 0.024 0.021 0.022 0.022 0.022 0.022 0.02 0.024 0.031 0.023 0.025 0.026 0.024 0.023 0.023 0.023 0.02 0.028 0.025 0.023 0.021 0.023 0.025 0.021 0.025 0.022 0.023 0.024 0.023 0.025 0.023 0.025 0.025 0.022 0.027 0.027 0.024 0.026 0.028 0.026 0.024 0.027 0.023 0.023 0.033 0.024 0.027 0.026 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 99.999 2.021 1.369 1.293 1.343 1.354 1.993 1.532 1.712 1.473 1.844 99.999 1.656 1.512 1.413 1.497 1.484 1.636 1.852 99.999 1.477 1.408 1.594 1.359 1.383 2.053 99.999 99.999 1.586 1.612 99.999 1.46 1.187 1.763 1.176 1.266 1.335 1.276 1.768 1.723 1.252 99.999 1.708 1.38 1.505 99.999 1.459 1.465 99.999 1.69 1.54 1.553 99.999 1.856 1.583 1.487 1.828 1.31 1.479 99.999 1.46 1.511 99.999 1.658 99.999 99.999 99.999 0.128 0.075 0.079 0.078 0.066 0.102 0.085 0.09 0.081 0.108 99.999 0.103 0.083 0.091 0.084 0.088 0.095 0.122 99.999 0.081 0.083 0.093 0.083 0.081 0.139 99.999 99.999 0.094 0.107 99.999 0.088 0.075 0.114 0.071 0.076 0.09 0.076 0.124 0.102 0.075 99.999 0.118 0.079 0.087 99.999 0.089 0.102 99.999 0.105 0.098 0.083 99.999 0.136 0.122 0.102 0.145 0.092 0.098 99.999 0.084 0.105 99.999 0.116 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.076 1 0.876 0.876 0.858 0.858 1.042 0.95 0.834 0.985 0.988 1.021 0.986 0.835 0.943 0.958 0.87 0.937 1.044 1.16 0.993 0.955 1.07 0.827 0.923 1.143 0.913 1.052 1.068 0.917 1.101 0.794 0.861 0.975 0.799 0.899 0.843 0.872 0.952 1.005 0.896 0.968 0.853 0.899 0.856 0.88 0.834 0.853 1.085 1.072 0.942 0.872 1.05 1.183 0.921 0.992 1.004 0.876 0.808 0.998 0.796 0.871 1.007 0.973 0.996 1.068 0.026 0.025 0.028 0.028 0.027 0.026 0.029 0.026 0.028 0.029 0.03 0.031 0.027 0.029 0.028 0.027 0.027 0.027 0.032 0.027 0.028 0.028 0.029 0.029 0.025 0.03 0.041 0.029 0.031 0.033 0.03 0.03 0.03 0.029 0.027 0.036 0.035 0.03 0.027 0.031 0.033 0.028 0.035 0.029 0.03 0.031 0.031 0.032 0.03 0.032 0.033 0.028 0.034 0.035 0.032 0.033 0.035 0.035 0.032 0.034 0.032 0.03 0.044 0.033 0.035 0.033 2.029 2.035 1.682 1.654 1.618 1.646 2.059 1.793 1.676 1.814 1.964 1.913 1.937 1.619 1.806 1.759 1.662 1.814 2.025 2.277 1.941 1.775 2.051 1.625 1.776 2.151 1.728 2.032 2.026 1.739 2.03 1.602 1.633 1.954 1.56 1.744 1.668 1.668 1.888 1.975 1.68 1.913 1.63 1.813 1.702 1.712 1.653 1.697 2.083 2.093 1.782 1.689 2.069 2.167 1.721 1.901 2.002 1.657 1.629 1.951 1.656 1.685 1.948 1.796 2.026 2.021 0.022 0.02 0.024 0.025 0.024 0.021 0.024 0.022 0.024 0.025 0.024 0.026 0.023 0.025 0.025 0.023 0.024 0.023 0.026 0.022 0.023 0.025 0.024 0.025 0.022 0.025 0.034 0.025 0.026 0.028 0.026 0.025 0.025 0.024 0.023 0.032 0.03 0.026 0.023 0.025 0.028 0.023 0.031 0.024 0.026 0.026 0.026 0.027 0.025 0.026 0.031 0.025 0.029 0.029 0.028 0.028 0.03 0.031 0.028 0.028 0.03 0.026 0.038 0.028 0.029 0.028 408 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 843.5 551.7 563.2 153.6 677.8 673.5 447 171.2 111.4 897.7 438.2 728.5 526.3 493.5 971.6 953.2 956.6 573.8 335.5 668.1 708.8 885.7 406.5 481.8 616 62.7 727.2 231.5 891.7 407.4 228.8 453.3 388 630 195.9 204.1 323.9 698.5 121.7 603.2 414.9 624.4 674.2 809.2 111.2 641.6 706.7 162.7 33 786.1 426.4 439.5 71.7 567.8 709.3 20.2 207.7 488.5 386.1 961.5 254.6 879 13.3 295 849.6 168.7 66.1 960.8 503.2 563.6 429.4 800 635.2 179.8 715.1 829.8 606 738.8 242.4 172.3 311.4 469.3 93.3 722.6 821.2 847.1 372.7 830.7 489 464.8 294.4 607.4 225.2 800.9 47.4 719.7 163.8 952.2 228.9 728.3 842.3 638.4 106.6 703.8 623.8 270.6 714.9 101.3 204.7 752.9 882.9 926.8 788.2 433.5 905.9 2.5 625.7 710.4 287.8 948.9 427.2 423.8 655.7 348.6 88.4 305.3 839.7 274.3 125.9 239.5 504.2 806.8 18.651 18.656 18.666 18.674 18.675 18.676 18.68 18.682 18.688 18.689 18.694 18.694 18.7 18.71 18.713 18.715 18.717 18.722 18.725 18.727 18.727 18.738 18.739 18.74 18.741 18.742 18.743 18.756 18.758 18.76 18.763 18.765 18.767 18.768 18.772 18.775 18.778 18.779 18.781 18.783 18.79 18.791 18.791 18.803 18.81 18.827 18.834 18.835 18.841 18.847 18.849 18.849 18.849 18.855 18.855 18.862 18.873 18.873 18.885 18.901 18.904 18.904 18.904 18.906 18.906 18.917 0.025 0.026 0.026 0.03 0.026 0.025 0.023 0.027 0.025 0.028 0.022 0.023 0.032 0.03 0.023 0.023 0.025 0.027 0.028 0.024 0.03 0.026 0.028 0.026 0.031 0.026 0.028 0.025 0.031 0.024 0.028 0.03 0.03 0.026 0.031 0.028 0.028 0.029 0.027 0.028 0.028 0.028 0.029 0.026 0.03 0.029 0.025 0.031 0.031 0.032 0.029 0.031 0.028 0.03 0.028 0.029 0.03 0.027 0.029 0.028 0.03 0.033 0.032 0.026 0.033 0.029 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 99.999 1.477 1.485 99.999 99.999 1.295 99.999 1.598 99.999 1.507 99.999 1.754 99.999 1.57 99.999 1.178 1.625 99.999 1.439 1.679 99.999 1.609 99.999 1.557 99.999 1.334 99.999 1.347 99.999 1.447 1.479 99.999 1.289 99.999 99.999 1.74 99.999 99.999 1.666 1.429 99.999 1.47 1.497 1.589 99.999 99.999 1.265 99.999 99.999 1.372 0.984 99.999 99.999 99.999 99.999 99.999 1.327 1.502 99.999 1.321 1.582 99.999 1.273 99.999 99.999 99.999 99.999 0.101 0.096 99.999 99.999 0.081 99.999 0.117 99.999 0.123 99.999 0.122 99.999 0.114 99.999 0.076 0.129 99.999 0.1 0.134 99.999 0.108 99.999 0.097 99.999 0.095 99.999 0.11 99.999 0.089 0.116 99.999 0.093 99.999 99.999 0.146 99.999 99.999 0.128 0.095 99.999 0.135 0.108 0.117 99.999 99.999 0.101 99.999 99.999 0.131 0.09 99.999 99.999 99.999 99.999 99.999 0.096 0.116 99.999 0.11 0.133 99.999 0.126 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.124 0.911 0.844 0.914 1.028 0.854 1.093 0.988 1.106 0.825 1.154 0.985 0.879 1.146 1.165 0.831 1.071 1.178 0.748 0.917 1.073 1.009 1.123 0.899 1.123 0.781 0.975 0.956 1.105 0.872 1.011 0.998 0.883 1.048 1.055 0.999 0.803 1.076 0.991 0.896 1.095 1.07 0.918 0.921 0.981 1.019 0.813 0.866 1.079 0.977 0.704 0.84 0.971 0.93 1.011 0.888 0.859 0.87 0.988 0.772 1.062 0.866 0.88 1.079 0.955 1.066 0.032 0.035 0.032 0.041 0.033 0.032 0.029 0.035 0.032 0.035 0.029 0.029 0.041 0.039 0.029 0.03 0.032 0.035 0.036 0.032 0.038 0.035 0.036 0.033 0.039 0.033 0.036 0.034 0.04 0.033 0.036 0.037 0.04 0.033 0.043 0.037 0.036 0.038 0.036 0.036 0.037 0.036 0.039 0.036 0.038 0.036 0.034 0.042 0.039 0.04 0.038 0.041 0.037 0.038 0.037 0.038 0.04 0.036 0.039 0.036 0.04 0.042 0.04 0.035 0.041 0.039 2.155 1.761 1.699 1.751 1.99 1.717 1.996 1.847 2.015 1.728 2.162 1.828 1.758 2.108 2.188 1.629 2.083 2.152 1.537 1.763 2.178 1.961 2.148 1.728 2.12 1.621 1.983 1.771 2.104 1.685 1.865 1.977 1.665 2.059 1.995 1.905 1.586 2.062 1.895 1.646 2.058 2.058 1.723 1.763 1.802 1.981 1.643 1.667 2.028 1.836 1.467 1.577 1.853 1.76 1.898 1.73 1.688 1.696 1.954 1.62 2.02 1.709 1.704 2.038 1.862 2.091 0.028 0.03 0.028 0.034 0.028 0.027 0.026 0.03 0.027 0.031 0.024 0.025 0.035 0.032 0.025 0.026 0.027 0.029 0.031 0.027 0.031 0.028 0.031 0.029 0.033 0.029 0.03 0.028 0.033 0.027 0.031 0.032 0.036 0.027 0.035 0.031 0.03 0.031 0.03 0.032 0.031 0.03 0.032 0.03 0.033 0.031 0.028 0.037 0.033 0.035 0.033 0.038 0.031 0.033 0.031 0.033 0.033 0.031 0.032 0.031 0.033 0.037 0.036 0.029 0.035 0.031 UBVRI PHOTOMETRY OF OPEN CLUSTERS 409 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 832.4 446.1 37.5 808.3 591.6 890.1 256.4 599.7 529.8 467.2 534.2 970.9 3.7 349.1 557.9 186.3 586.5 785.8 444.9 59.1 364.8 401.7 534.8 986.6 488.6 514.2 175.8 841.3 247.6 850.1 263.3 138.2 141.4 214.2 69.6 420.3 915.2 410.9 316.2 403.4 593.6 676.9 285.4 286.7 233.6 512.6 242.3 926 722.6 34.2 651 836.3 43.8 73.1 983.4 494.7 320.2 325.6 161.5 449.4 880.9 336.7 928.6 76.9 34.9 943.4 227.2 669.5 479.3 302.7 730.9 733.4 755 249.7 978.5 562.9 423 901.3 773.8 285.4 39.3 279 607.7 525.9 392.6 848.2 400.4 374.8 32.3 77.2 556.3 836.6 646.1 28.8 412.4 365.6 603.1 688.8 365.1 363.3 857.8 632.8 778.7 352.7 29.8 251.8 279.8 240.2 736.2 960 276.2 742.4 279.1 569.8 206.6 928.4 25.9 636.9 36.4 861.1 742.3 53.5 656.5 344 370.8 759.5 593.5 768.1 885.5 119.6 210.5 779.2 18.917 18.919 18.92 18.92 18.926 18.932 18.938 18.946 18.95 18.951 18.951 18.952 18.959 18.961 18.965 18.969 18.973 18.98 18.982 18.984 18.995 18.997 18.997 19.001 19.008 19.015 19.019 19.019 19.02 19.028 19.031 19.037 19.039 19.043 19.043 19.044 19.044 19.045 19.048 19.05 19.05 19.056 19.057 19.057 19.058 19.062 19.069 19.069 19.077 19.084 19.084 19.084 19.085 19.085 19.085 19.09 19.098 19.101 19.103 19.105 19.107 19.118 19.121 19.133 19.139 19.14 0.034 0.031 0.033 0.032 0.034 0.035 0.029 0.033 0.032 0.034 0.031 0.031 0.031 0.03 0.037 0.035 0.034 0.029 0.033 0.034 0.032 0.029 0.033 0.033 0.034 0.041 0.033 0.04 0.031 0.029 0.047 0.036 0.033 0.036 0.037 0.03 0.034 0.036 0.04 0.035 0.035 0.033 0.037 0.033 0.035 0.035 0.042 0.032 0.034 0.041 0.032 0.04 0.037 0.041 0.037 0.037 0.036 0.037 0.038 0.036 0.034 0.034 0.038 0.039 0.034 0.04 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 99.999 99.999 99.999 99.999 99.999 1.506 1.337 1.331 1.47 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.471 99.999 99.999 1.293 99.999 99.999 99.999 99.999 99.999 99.999 1.58 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.435 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.149 0.141 0.104 0.124 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.151 99.999 99.999 0.142 99.999 99.999 99.999 99.999 99.999 99.999 0.158 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.172 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.13 1.101 0.871 0.826 0.971 0.821 0.834 0.883 0.912 0.946 0.821 0.999 0.989 0.868 1.045 1.031 0.898 1.059 1.231 0.887 1.143 0.923 1.202 0.964 1.172 0.704 0.873 1.047 0.922 0.935 1.062 0.994 0.921 1.058 0.992 1.027 0.74 0.869 1.112 1.015 0.966 0.983 0.863 0.966 1.032 0.921 0.719 1.189 1.005 1.018 0.944 0.974 0.971 1.031 0.861 0.966 0.885 0.959 0.94 1.045 0.996 0.849 1.093 1.02 1.047 0.876 0.043 0.041 0.042 0.042 0.044 0.045 0.039 0.042 0.042 0.043 0.04 0.039 0.04 0.038 0.046 0.045 0.044 0.038 0.043 0.044 0.041 0.04 0.043 0.043 0.044 0.053 0.043 0.056 0.039 0.039 0.062 0.046 0.044 0.047 0.047 0.039 0.045 0.046 0.05 0.045 0.046 0.043 0.048 0.041 0.047 0.044 0.057 0.041 0.044 0.055 0.042 0.05 0.049 0.053 0.048 0.047 0.047 0.048 0.05 0.047 0.045 0.045 0.049 0.049 0.044 0.053 2.156 1.936 1.787 1.61 1.788 1.69 1.652 1.747 1.734 1.884 1.681 1.955 1.947 1.734 1.992 1.951 1.765 1.987 2.186 1.723 2.128 1.765 2.196 1.821 2.098 1.486 1.701 1.925 1.768 1.816 2.053 1.891 1.784 2.001 1.921 1.861 1.495 1.784 2.124 1.91 1.784 1.85 1.815 1.86 2.015 1.742 1.553 2.15 2.004 2.027 1.788 1.909 1.842 2.106 1.718 1.921 1.73 1.798 1.783 1.886 1.839 1.713 99.999 1.982 2.03 1.764 σV −I 0.037 0.035 0.037 0.036 0.038 0.038 0.035 0.036 0.036 0.037 0.035 0.034 0.033 0.034 0.04 0.038 0.038 0.031 0.036 0.038 0.034 0.034 0.035 0.036 0.036 0.046 0.036 0.043 0.036 0.032 0.051 0.039 0.037 0.04 0.04 0.034 0.04 0.039 0.043 0.039 0.039 0.036 0.039 0.036 0.038 0.038 0.048 0.034 0.037 0.045 0.036 0.042 0.041 0.044 0.041 0.04 0.041 0.042 0.042 0.04 0.037 0.039 99.999 0.041 0.036 0.044 410 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 531.2 573.9 167.8 742.1 131.4 254.2 325.1 123.8 712 138.6 308 413.7 694.2 791.7 92.9 746.4 806.8 188.5 342.8 150 431.9 79.9 74.2 195.8 313.9 122.9 447.3 786.7 49.7 462.2 816.8 335.6 529.1 127.2 373.5 545.3 869.2 946 817.1 433 169 627.9 407.8 190.4 521.2 955.9 308 811.5 662.4 567.6 275.9 320.2 547.3 583.3 869.8 257.1 696.3 561.9 837.7 440 714.5 856.5 965.3 429 616.2 105.3 900.2 235.7 394.8 70.2 559.3 283.7 500.9 717.4 860.4 125.4 749.5 652.5 164.3 876.4 368.4 31.5 851.7 851.8 414.4 833.7 777.5 764.1 879 326.2 624.6 640 274.1 978.3 856 742.5 116.7 798.7 938.4 668.9 717.6 746.5 36.7 704.9 251.3 989.5 221.6 410.5 195.7 612.7 511.6 461.1 175.1 848.3 949.2 126 620.7 922.2 323.5 393.4 64.6 148.2 493.3 187.3 366.4 614.4 256.1 310.3 600.1 162.8 504.1 984.4 19.146 19.152 19.153 19.154 19.156 19.161 19.161 19.167 19.169 19.172 19.173 19.178 19.179 19.18 19.187 19.19 19.194 19.204 19.206 19.214 19.214 19.219 19.22 19.222 19.225 19.227 19.228 19.229 19.233 19.233 19.234 19.239 19.25 19.25 19.256 19.258 19.258 19.259 19.265 19.266 19.272 19.272 19.274 19.275 19.276 19.277 19.282 19.285 19.289 19.29 19.292 19.292 19.294 19.294 19.299 19.304 19.304 19.308 19.308 19.309 19.319 19.32 19.323 19.324 19.327 19.328 0.035 0.039 0.043 0.035 0.039 0.047 0.042 0.035 0.036 0.035 0.039 0.04 0.034 0.036 0.034 0.039 0.04 0.041 0.038 0.046 0.034 0.033 0.036 0.044 0.042 0.04 0.038 0.037 0.043 0.042 0.043 0.035 0.034 0.035 0.043 0.036 0.045 0.042 0.044 0.046 0.04 0.045 0.039 0.041 0.039 0.043 0.036 0.038 0.036 0.041 0.04 0.046 0.038 0.05 0.046 0.043 0.041 0.038 0.041 0.042 0.043 0.045 0.042 0.043 0.042 0.044 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.933 0.957 0.721 1.082 0.93 0.986 0.853 1.078 0.955 0.916 0.839 0.776 1.148 0.943 0.936 1.141 0.904 0.953 0.949 0.971 1.122 0.775 1.032 0.993 0.988 0.908 1.149 0.881 0.823 1.042 0.919 0.881 0.839 0.869 0.904 0.985 0.746 0.913 1.169 0.883 1.081 1.076 0.969 0.979 1.096 0.787 0.964 1.021 0.951 1.019 0.962 0.852 0.912 0.741 0.953 0.924 0.87 0.714 0.975 0.908 0.926 0.938 0.918 0.993 1.033 0.877 0.046 0.049 0.056 0.044 0.05 0.06 0.058 0.045 0.046 0.045 0.05 0.052 0.044 0.049 0.045 0.049 0.052 0.053 0.048 0.059 0.046 0.047 0.046 0.058 0.053 0.054 0.053 0.048 0.056 0.053 0.057 0.047 0.046 0.046 0.056 0.048 0.057 0.053 0.056 0.059 0.051 0.058 0.053 0.054 0.049 0.055 0.046 0.049 0.048 0.055 0.052 0.061 0.05 0.062 0.059 0.054 0.054 0.051 0.055 0.055 0.056 0.058 0.054 0.057 0.053 0.057 1.736 1.839 1.646 2.094 1.817 1.986 1.738 2.006 1.834 1.796 1.674 1.618 2.102 1.83 1.797 2.147 1.744 1.758 1.786 1.846 2.029 1.618 2.034 1.984 1.887 1.713 2.101 1.723 1.624 2.05 1.797 1.678 1.695 1.749 1.726 1.863 1.591 1.826 2.164 1.641 2 2.036 99.999 1.796 2.113 1.58 1.81 1.972 1.808 1.891 1.768 1.663 1.726 1.518 1.822 1.754 1.695 1.496 1.77 1.891 1.76 1.788 1.789 1.875 2.053 1.755 σV −I 0.04 0.042 0.047 0.038 0.043 0.051 0.046 0.038 0.04 0.038 0.045 0.045 0.037 0.041 0.039 0.042 0.044 0.045 0.042 0.051 0.038 0.039 0.038 0.047 0.046 0.047 0.043 0.042 0.048 0.045 0.049 0.042 0.038 0.039 0.047 0.041 0.049 0.045 0.047 0.052 0.045 0.048 99.999 0.046 0.042 0.049 0.043 0.041 0.041 0.045 0.045 0.053 0.042 0.056 0.051 0.048 0.047 0.047 0.047 0.045 0.049 0.049 0.046 0.05 0.045 0.048 UBVRI PHOTOMETRY OF OPEN CLUSTERS 411 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 522 854.9 91.4 80.9 609.4 535.1 142 234.7 576.9 265.2 484.4 863 952.6 423.5 875.3 725 101.1 458.5 209.6 22 740.2 213.7 804 581.8 771.5 636.8 878.9 471.6 691.4 351.3 691.6 418.6 674.6 283.6 876.5 489.4 821.5 844.3 924 823.5 457.9 673 783.8 254.4 586.7 317.8 436.8 604.8 693.5 818.4 891.9 648.6 355.5 198.1 6.3 970.5 561.3 461.6 700.3 277.2 107.9 868.5 162.4 216.5 588.3 485.5 825.8 956.3 319.3 819.9 303.9 329.2 157.2 697.3 548.7 901.1 851.3 798.4 283 221.9 527.4 383.6 109.3 264.4 859.9 191.8 583.8 176.1 958.7 575.3 105.9 551.3 86.3 39.2 295.5 551.2 260.6 797.3 861.3 326.6 381.7 954.1 201.3 771 43.5 190.9 304.7 123.3 80.5 396.2 798.9 648.7 981.3 709.5 953.8 496.8 457 812 988.2 413.6 591.5 498.7 532.2 339.1 262.3 208.1 142.1 871.5 718.3 495.2 340.1 581.3 19.33 19.331 19.332 19.334 19.34 19.344 19.352 19.352 19.352 19.355 19.362 19.367 19.369 19.371 19.374 19.375 19.381 19.382 19.385 19.386 19.388 19.389 19.393 19.397 19.398 19.402 19.402 19.408 19.41 19.415 19.417 19.418 19.418 19.42 19.428 19.429 19.433 19.434 19.435 19.436 19.44 19.441 19.444 19.445 19.445 19.446 19.447 19.447 19.447 19.448 19.448 19.451 19.452 19.453 19.453 19.454 19.457 19.459 19.461 19.464 19.474 19.477 19.479 19.48 19.48 19.482 0.047 0.043 0.046 0.046 0.041 0.039 0.041 0.045 0.042 0.045 0.041 0.046 0.041 0.048 0.042 0.038 0.049 0.041 0.043 0.049 0.042 0.045 0.042 0.039 0.043 0.048 0.045 0.043 0.052 0.043 0.054 0.043 0.049 0.05 0.048 0.042 0.052 0.042 0.043 0.049 0.044 0.048 0.044 0.056 0.054 0.05 0.046 0.044 0.044 0.046 0.052 0.043 0.046 0.05 0.041 0.049 0.039 0.051 0.048 0.05 0.048 0.047 0.06 0.049 0.05 0.048 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.049 0.987 0.94 0.839 1.101 0.957 0.979 1.004 0.927 0.972 1.076 1.187 0.885 0.875 0.978 0.86 0.784 0.99 0.859 0.883 0.915 1.037 1.018 1.01 0.902 0.997 1.071 0.824 0.991 0.898 0.992 1.03 0.969 0.97 0.907 0.917 0.957 0.848 1.099 0.868 1.021 0.844 0.974 1.024 0.874 1.044 0.83 1.068 0.881 0.965 0.843 0.995 0.751 0.904 0.862 0.868 0.955 0.956 0.958 0.933 0.833 0.815 0.951 1.033 0.96 0.896 0.06 0.055 0.059 0.058 0.055 0.052 0.055 0.056 0.055 0.059 0.052 0.059 0.053 0.064 0.054 0.051 0.066 0.054 0.055 0.063 0.056 0.058 0.053 0.052 0.057 0.061 0.06 0.058 0.066 0.057 0.068 0.056 0.062 0.063 0.062 0.055 0.068 0.056 0.057 0.067 0.06 0.062 0.058 0.071 0.07 0.064 0.059 0.057 0.058 0.058 0.066 0.056 0.059 0.068 0.055 0.064 0.052 0.069 0.061 0.063 0.061 0.061 0.079 0.066 0.064 0.063 1.921 1.853 1.942 1.667 2.041 1.934 1.869 1.963 1.784 1.942 2.053 2.081 1.827 1.673 1.745 1.695 1.49 1.942 1.651 1.815 1.752 1.973 1.744 1.891 1.716 1.819 2.068 1.693 1.879 1.819 1.836 2.015 1.889 1.946 1.724 1.69 1.826 1.764 2.106 1.654 1.885 1.715 1.951 2.03 1.746 2.039 1.718 2.055 1.648 1.907 1.699 2.095 1.502 1.767 1.805 1.694 1.828 1.788 1.9 1.714 1.788 1.739 1.847 99.999 1.785 1.758 σV −I 0.051 0.046 0.049 0.051 0.044 0.043 0.046 0.049 0.046 0.049 0.045 0.05 0.046 0.062 0.048 0.044 0.061 0.046 0.048 0.053 0.048 0.049 0.048 0.042 0.049 0.053 0.05 0.046 0.058 0.049 0.059 0.046 0.053 0.053 0.053 0.049 0.058 0.047 0.047 0.058 0.049 0.053 0.048 0.06 0.061 0.054 0.05 0.048 0.05 0.05 0.057 0.049 0.053 0.057 0.045 0.054 0.044 0.06 0.053 0.056 0.053 0.052 0.067 99.999 0.055 0.054 412 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 4 (CONTINUED) X Y V σV 733.2 188.1 241.6 336.6 123.8 271.4 272.9 479.4 40.7 521.9 445.2 404.4 706.5 479.3 274.8 681.5 42.7 743.6 364.5 801.8 147 699.5 770.9 12.4 102.6 255.3 288.1 781.3 512.4 536 608.4 236.3 963.2 353.3 415.2 421.8 337.1 942.6 357.5 305.1 124.5 634.3 305.6 758 302.2 614 98.1 382.1 489.2 552 382.4 897 666.9 958.8 46.7 696.3 68.7 796.6 334.2 675.3 811.8 677.6 573.2 797.7 767.1 835.3 569.2 485.6 688.4 377.8 395.6 932.5 244.8 657.8 360.4 412.5 721.5 737.3 866.7 422.6 72.2 622.5 624.1 552.8 247.1 438.3 841.7 777.6 417.9 771.4 673.6 237.2 883.8 764 975.4 781.1 384.8 576.3 622.5 783.6 735.8 291 394.4 810.2 975.8 429.6 192.3 741.7 710.2 974.2 372.2 807.5 941.8 613.9 571.6 258.5 519.8 668.3 355.7 933.4 698.1 679.1 19.6 61.9 19.483 19.49 19.49 19.492 19.493 19.496 19.5 19.501 19.506 19.513 19.519 19.523 19.524 19.532 19.533 19.533 19.535 19.54 19.545 19.545 19.547 19.55 19.551 19.555 19.557 19.559 19.56 19.561 19.564 19.568 19.568 19.572 19.582 19.586 19.59 19.593 19.596 19.599 19.6 19.604 19.61 19.613 19.616 19.62 19.629 19.637 19.646 19.675 19.681 19.683 19.693 19.707 19.711 19.72 19.735 19.737 19.746 19.796 19.804 19.819 19.819 19.857 0.054 0.044 0.072 0.046 0.048 0.05 0.049 0.055 0.046 0.043 0.05 0.054 0.045 0.055 0.051 0.056 0.054 0.046 0.05 0.054 0.048 0.059 0.048 0.048 0.05 0.047 0.044 0.052 0.058 0.062 0.065 0.054 0.054 0.056 0.049 0.054 0.046 0.055 0.058 0.05 0.061 0.059 0.057 0.056 0.052 0.061 0.055 0.05 0.064 0.052 0.059 0.054 0.065 0.068 0.067 0.069 0.06 0.073 0.056 0.063 0.06 0.066 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.944 1.041 1.021 1.05 0.858 1.046 0.916 0.839 0.926 0.955 0.862 0.929 0.861 0.992 1.014 0.973 0.984 0.836 0.935 0.942 0.89 0.952 0.882 0.702 1.002 0.993 0.905 0.893 0.783 0.936 0.865 0.913 1.102 0.975 0.91 0.875 0.941 0.945 0.848 0.879 0.703 0.839 0.993 0.875 0.839 0.925 0.868 0.824 0.796 0.765 0.672 0.811 1.076 0.823 0.921 1.204 1.169 1.062 1.069 1.033 0.978 0.903 0.068 0.057 0.091 0.059 0.062 0.063 0.064 0.072 0.06 0.058 0.063 0.07 0.061 0.078 0.065 0.071 0.07 0.06 0.064 0.068 0.063 0.076 0.065 0.064 0.065 0.063 0.059 0.068 0.073 0.077 0.082 0.069 0.07 0.073 0.065 0.07 0.062 0.073 0.075 0.069 0.077 0.076 0.075 0.072 0.068 0.079 0.072 0.066 0.081 0.069 0.077 0.074 0.082 0.085 0.086 0.089 0.077 0.092 0.072 0.081 0.076 0.09 1.815 1.99 1.979 1.884 1.746 1.924 1.731 1.665 1.796 1.777 1.726 1.776 1.766 1.753 1.944 1.792 1.839 1.651 1.769 1.757 1.712 1.714 1.673 1.608 1.8 1.81 1.741 1.77 1.765 99.999 1.697 1.728 1.999 1.731 1.821 1.671 1.661 1.789 1.715 1.627 1.571 1.718 1.891 1.725 1.73 1.762 1.799 1.602 1.629 1.598 1.541 1.623 1.893 1.605 1.911 2.166 2.212 2.041 2.015 1.913 2.086 1.797 σV −I 0.058 0.048 0.077 0.051 0.055 0.054 0.055 0.061 0.051 0.048 0.056 0.061 0.05 0.063 0.055 0.063 0.059 0.054 0.055 0.059 0.054 0.064 0.055 0.053 0.056 0.054 0.052 0.057 0.062 99.999 0.071 0.06 0.059 0.064 0.055 0.062 0.056 0.06 0.064 0.058 0.068 0.065 0.064 0.064 0.061 0.068 0.06 0.06 0.07 0.059 0.066 0.064 0.071 0.078 0.072 0.075 0.064 0.079 0.062 0.07 0.064 0.072 UBVRI PHOTOMETRY OF OPEN CLUSTERS © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 5 X Y V σV 374.5 528.6 804.6 102.5 85.1 400.8 491.8 213.6 206.6 517.1 508.4 444.3 908.6 407.5 633.4 741.7 31.6 589.3 863.5 519.3 567.4 450.5 706.6 639.9 622.6 586.6 595.8 209.6 751.6 616.3 177.9 567.3 116.4 541.2 841 483.6 603.6 104.1 371.1 468.5 379.1 688.2 100.7 607.3 432.8 752.4 176.1 761.4 334.6 483.1 852.3 470.5 103.4 743.2 423.8 214.1 650.9 310.3 578.3 299.7 390 459.5 530.2 173.2 644.8 637.7 153.4 217.9 881.2 174.5 74.1 856.8 510.5 723.9 867.4 851.9 866.6 880.9 351.2 366.4 848 698.6 851.7 431.3 657.2 148.1 597.2 539.8 23.4 578.8 800.4 361.2 449.5 597 369 399.1 451.3 534.7 346 770.4 133 451.3 643.9 201.2 561.6 477 857.6 56.5 7.4 180.7 785.3 40.7 445.9 451.7 223.5 963.5 189.3 507.4 84.9 35.5 387.4 792.8 521.1 345.1 415.5 814.6 775.1 58.4 848.3 655 610.1 392.2 11.244 12.352 12.746 13.562 13.573 13.729 13.945 14.418 14.437 14.542 14.555 14.646 14.664 14.681 14.681 14.689 14.741 14.783 14.814 14.868 14.908 14.955 14.967 15.018 15.028 15.161 15.205 15.27 15.352 15.353 15.365 15.391 15.472 15.507 15.568 15.593 15.598 15.609 15.696 15.712 15.732 15.734 15.771 15.78 15.8 15.804 15.804 15.818 15.869 15.918 15.93 15.934 15.943 15.994 16.024 16.045 16.106 16.106 16.194 16.248 16.254 16.259 16.284 16.373 16.383 16.4 0.004 0.002 0.003 0.002 0.003 0.002 0.003 0.003 0.003 0.003 0.003 0.004 0.005 0.005 0.004 0.005 0.004 0.004 0.004 0.004 0.005 0.004 0.005 0.004 0.004 0.005 0.005 0.004 0.005 0.004 0.007 0.005 0.007 0.005 0.006 0.005 0.005 0.006 0.005 0.006 0.005 0.006 0.007 0.007 0.006 0.006 0.009 0.005 0.006 0.006 0.009 0.006 0.009 0.007 0.007 0.006 0.007 0.007 0.007 0.01 0.007 0.007 0.008 0.008 0.007 0.008 413 CCD UBVRI PHOTOMETRY OF BE 10 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 0.433 1.483 0.738 0.771 0.794 0.823 1.083 0.861 1.655 1.759 0.95 1.57 1.603 1.387 0.876 1.573 0.975 1.062 0.925 1.009 0.907 1.024 0.99 1.656 0.907 1.029 0.964 0.846 1.04 1.037 0.988 0.948 1.739 0.894 1.184 1.022 1.042 1.105 0.952 1.048 1.139 0.99 2.373 1.302 1.125 0.955 1.002 0.987 1.027 0.987 1.355 1.941 1.465 1.005 1.058 0.904 0.969 1.112 1.084 1.415 0.972 1.014 1.025 0.949 1.153 1.081 0.004 0.004 0.014 0.012 0.009 0.004 0.006 0.006 0.009 0.009 0.006 0.009 0.009 0.008 0.007 0.009 0.007 0.009 0.008 0.008 0.01 0.009 0.01 0.011 0.008 0.01 0.01 0.009 0.011 0.01 0.014 0.011 0.015 0.01 0.012 0.012 0.011 0.012 0.012 0.012 0.012 0.013 0.022 0.015 0.012 0.012 0.02 0.012 0.013 0.012 0.015 0.019 0.016 0.017 0.016 0.013 0.015 0.016 0.015 0.018 0.015 0.017 0.017 0.017 0.018 0.018 0.246 1.346 0.231 0.174 0.213 0.227 1.061 0.496 0.976 1.117 0.52 0.914 0.96 0.694 0.567 1.054 0.547 0.579 0.572 0.572 0.476 0.557 0.642 1.017 0.535 0.61 0.523 0.512 0.567 0.552 99.999 0.545 1.021 0.568 0.646 0.542 0.518 0.655 0.478 0.583 0.41 0.576 99.999 1.238 0.44 0.708 99.999 0.53 0.597 0.511 1.184 99.999 0.72 0.68 0.558 0.538 0.555 0.539 0.575 0.792 0.5 0.63 0.572 0.514 0.455 0.596 0.002 0.009 0.004 0.008 0.008 0.007 0.013 0.012 0.029 0.039 0.014 0.029 0.032 0.02 0.018 0.034 0.013 0.018 0.016 0.017 0.019 0.018 0.019 0.043 0.018 0.021 0.02 0.021 0.027 0.026 99.999 0.026 0.07 0.025 0.034 0.027 0.026 0.032 0.028 0.027 0.029 0.026 99.999 0.059 0.033 0.037 99.999 0.03 0.032 0.033 0.056 99.999 0.053 0.04 0.037 0.033 0.035 0.041 0.041 0.063 0.042 0.046 0.047 0.041 0.05 0.05 0.22 0.851 0.44 0.499 0.493 0.548 0.631 0.568 0.93 0.991 0.584 0.973 0.953 0.834 0.578 0.982 0.599 0.677 0.598 0.65 0.605 0.618 0.632 0.994 0.557 0.658 0.594 0.534 0.668 0.649 0.606 0.577 1.084 0.581 0.715 0.62 0.635 0.707 0.51 0.602 0.697 0.614 1.413 0.82 0.732 0.643 0.621 0.597 0.622 0.608 0.929 1.128 0.88 0.594 0.612 0.598 0.579 0.665 0.649 0.881 0.552 0.645 0.629 0.599 0.708 0.653 0.005 0.003 0.014 0.006 0.01 0.003 0.005 0.004 0.004 0.004 0.004 0.004 0.005 0.005 0.005 0.004 0.005 0.005 0.005 0.005 0.007 0.006 0.007 0.005 0.005 0.006 0.006 0.005 0.006 0.006 0.008 0.006 0.005 0.006 0.007 0.007 0.007 0.007 0.007 0.007 0.006 0.007 0.009 0.007 0.006 0.007 0.01 0.007 0.007 0.007 0.007 0.007 0.007 0.008 0.008 0.007 0.008 0.008 0.009 0.008 0.008 0.008 0.009 0.01 0.008 0.009 0.5 1.631 0.873 0.971 0.994 1.047 1.185 1.152 1.859 1.963 1.217 1.898 1.87 1.638 1.191 1.911 1.275 1.376 1.217 1.353 1.248 1.289 1.313 1.986 1.161 1.357 1.256 1.113 1.397 1.337 1.262 1.264 2.128 1.198 1.381 1.29 1.345 1.358 1.169 1.329 1.421 1.293 2.839 1.523 1.487 1.324 1.271 1.253 1.392 1.281 1.81 2.184 1.831 1.265 1.298 1.216 1.209 1.41 1.363 1.775 1.22 1.339 1.317 1.235 1.467 1.351 0.004 0.003 0.005 0.003 0.005 0.002 0.004 0.003 0.004 0.004 0.003 0.003 0.004 0.004 0.004 0.004 0.004 0.004 0.004 0.004 0.006 0.005 0.006 0.004 0.004 0.005 0.006 0.005 0.005 0.005 0.007 0.006 0.004 0.005 0.006 0.006 0.006 0.006 0.006 0.006 0.005 0.006 0.007 0.006 0.005 0.006 0.01 0.006 0.006 0.006 0.006 0.006 0.006 0.008 0.007 0.006 0.007 0.007 0.008 0.007 0.008 0.008 0.008 0.008 0.007 0.008 414 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 5 (CONTINUED) X Y V σV 884.7 208.4 503 341.8 848.8 56.6 511.8 461.4 890.3 127.6 830.3 706.8 857.7 313 407.9 213.7 898.4 889.5 365.8 715.2 357.7 784.3 181.3 522.8 455.4 536.7 572.6 574.3 855.7 96.4 440.9 292.2 149.1 371.1 349.9 607 423.8 441.5 36.8 715.7 144.7 802.6 774.7 191.5 514.3 99 893.2 12.1 39.7 474.5 409 243.4 887.8 327.7 513.6 260.1 523.4 114.3 866.3 290.3 14.3 564.4 730.8 261.7 706.4 802 48.6 805.8 790.6 333.4 423.3 322.6 242.7 238.9 254.8 688.2 571.3 653.2 686.4 474.9 892.1 569.5 763.7 213.6 56.9 204.4 727 880.8 413 437.4 6.7 965.8 539.7 574 929.1 221.9 474.2 905.7 325.6 428.8 730.6 409.2 676.4 467.7 252.1 474.9 66.3 738.1 680.8 383.9 656.5 636.6 772 285.9 492.9 639 384.8 985.8 66 808.9 755.5 268.5 410 942.4 423.4 127.4 632 466.8 894.1 687.5 601.3 334 16.466 16.475 16.51 16.511 16.524 16.606 16.662 16.689 16.715 16.715 16.725 16.785 16.872 16.925 16.949 16.953 17.005 17.022 17.048 17.055 17.073 17.087 17.117 17.118 17.126 17.159 17.166 17.175 17.194 17.246 17.249 17.372 17.39 17.396 17.412 17.414 17.521 17.548 17.565 17.578 17.578 17.587 17.64 17.646 17.666 17.676 17.676 17.685 17.708 17.72 17.738 17.772 17.774 17.787 17.796 17.802 17.822 17.856 17.867 17.882 17.885 17.917 17.936 17.968 17.993 18.008 0.008 0.008 0.008 0.008 0.008 0.01 0.011 0.009 0.009 0.009 0.01 0.01 0.011 0.012 0.012 0.013 0.011 0.011 0.016 0.013 0.011 0.012 0.012 0.012 0.012 0.012 0.013 0.011 0.013 0.012 0.013 0.014 0.016 0.017 0.017 0.014 0.014 0.018 0.016 0.015 0.016 0.014 0.016 0.017 0.015 0.016 0.017 0.017 0.018 0.018 0.018 0.02 0.018 0.017 0.018 0.015 0.02 0.019 0.019 0.018 0.018 0.02 0.022 0.019 0.02 0.021 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) 1.086 1.024 1.006 1.129 1.026 1.935 1.341 1.125 1.14 1.047 1.637 1.056 1.904 1.122 1.302 1.287 1.021 1.114 1.443 1.254 1.263 1.403 1.17 1.295 1.307 1.075 1.082 1.081 1.31 1.057 1.181 0.91 1.512 1.202 1.324 1.71 1.159 1.225 1.302 1.21 1.36 1.354 1.149 1.286 1.21 1.118 1.512 2.008 1.833 1.213 1.276 1.189 1.255 1.19 1.189 1.352 1.218 1.384 1.156 1.424 1.144 1.354 1.58 1.199 1.141 1.223 0.02 0.018 0.019 0.02 0.017 0.029 0.025 0.022 0.023 0.022 0.028 0.023 0.035 0.025 0.028 0.028 0.025 0.029 0.031 0.028 0.028 0.035 0.029 0.03 0.028 0.028 0.029 0.026 0.031 0.029 0.032 0.03 0.042 0.035 0.044 0.048 0.037 0.042 0.042 0.04 0.042 0.042 0.038 0.042 0.039 0.039 0.047 0.066 0.061 0.045 0.047 0.05 0.047 0.047 0.047 0.05 0.049 0.051 0.052 0.055 0.045 0.054 0.064 0.047 0.054 0.053 0.582 0.511 0.488 0.472 0.602 99.999 0.556 0.507 0.518 0.381 99.999 0.478 99.999 0.556 0.395 99.999 0.351 0.542 0.552 0.469 99.999 99.999 0.525 0.428 0.36 0.559 99.999 0.412 99.999 0.576 99.999 0.391 99.999 0.396 99.999 99.999 99.999 0.274 99.999 99.999 99.999 99.999 0.329 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.055 0.047 0.046 0.055 0.052 99.999 0.072 0.053 0.063 0.087 99.999 0.059 99.999 0.076 0.079 99.999 0.064 0.081 0.113 0.093 99.999 99.999 0.095 0.099 0.099 0.088 99.999 0.076 99.999 0.089 99.999 0.082 99.999 0.105 99.999 99.999 99.999 0.119 99.999 99.999 99.999 99.999 0.115 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.682 0.643 0.611 0.625 0.665 1.089 0.801 0.705 0.672 0.643 1.015 0.659 1.129 0.74 0.792 0.719 0.677 0.686 0.878 0.821 0.83 0.875 0.737 0.75 0.759 0.685 0.733 0.688 0.855 0.629 0.733 0.518 0.98 0.785 0.801 1.005 0.74 0.766 0.791 0.723 0.811 0.812 0.762 0.797 0.705 0.783 0.942 1.197 1.07 0.778 0.802 0.769 0.771 0.798 0.753 0.797 0.765 0.872 0.716 0.944 0.675 0.742 1.026 0.668 0.783 0.781 0.01 0.009 0.009 0.009 0.009 0.01 0.01 0.01 0.011 0.011 0.011 0.012 0.011 0.013 0.012 0.016 0.013 0.012 0.014 0.012 0.012 0.014 0.013 0.013 0.013 0.014 0.015 0.013 0.015 0.014 0.016 0.018 0.016 0.017 0.027 0.015 0.015 0.02 0.018 0.017 0.017 0.015 0.017 0.018 0.018 0.018 0.018 0.018 0.018 0.02 0.02 0.022 0.021 0.02 0.021 0.018 0.022 0.02 0.021 0.019 0.021 0.023 0.022 0.022 0.022 0.023 1.432 1.329 1.271 1.327 1.333 2.228 1.702 1.466 1.401 1.34 2.004 1.354 2.153 1.505 1.595 1.445 1.353 1.397 1.739 1.633 1.682 1.728 1.513 1.565 1.594 1.419 1.476 1.421 1.567 1.387 1.521 1.134 1.856 1.635 99.999 2.008 1.539 1.565 1.631 1.521 1.647 1.655 1.505 1.64 1.437 1.49 1.802 2.364 2.129 1.545 1.637 1.614 1.636 1.576 1.546 1.668 1.563 1.692 1.514 1.89 1.487 1.599 1.892 1.44 1.586 1.527 σV −I 0.009 0.008 0.008 0.008 0.008 0.008 0.009 0.009 0.009 0.009 0.009 0.01 0.009 0.011 0.01 0.014 0.011 0.011 0.012 0.011 0.011 0.012 0.011 0.011 0.011 0.012 0.013 0.011 0.013 0.012 0.014 0.015 0.014 0.014 99.999 0.012 0.014 0.017 0.015 0.015 0.016 0.014 0.015 0.016 0.015 0.015 0.015 0.015 0.015 0.017 0.018 0.019 0.017 0.017 0.017 0.015 0.019 0.018 0.019 0.016 0.018 0.019 0.019 0.018 0.019 0.021 UBVRI PHOTOMETRY OF OPEN CLUSTERS 415 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 5 (CONTINUED) X Y V σV 535.4 1.8 131.7 299.4 849.6 689.8 534.8 292.6 282.5 714.4 858.6 839.7 648.3 171.7 841 166.7 451.1 405.4 545 263.3 628 836.7 212.6 183.9 412 394.7 474 418.6 867.5 533.3 833.6 785 147.5 923.2 751.8 318.5 396.5 468.1 896.9 396.9 348.2 113.9 123.9 188.5 459.8 916.2 497 368.5 776.1 170.7 148.2 189.2 378.7 263.5 104.9 24.9 422.7 306.5 277.9 186 533.3 253.5 715.4 712.4 448.1 609.2 613.7 843.6 267.7 501.5 729.5 859.2 528.8 554.1 893.1 700.2 508 656.6 735.1 905.5 620.1 606.4 430 637.9 575.8 242.9 293.8 425.5 459.4 340.2 648 881.8 96.9 440.8 598 252 631.9 971.5 315.8 618.1 244 481.2 260.3 232.5 706.3 404.3 679.7 727 544.8 861 343.8 835.9 118.9 578.8 687.7 934.1 394.9 460.1 407.8 664.5 695 681.5 449.4 767.3 498.6 556.3 407.9 678.5 275.5 485.8 839.3 585.4 18.015 18.024 18.042 18.047 18.062 18.094 18.117 18.124 18.183 18.208 18.238 18.259 18.272 18.286 18.289 18.324 18.348 18.352 18.401 18.407 18.446 18.459 18.459 18.474 18.491 18.494 18.5 18.501 18.507 18.551 18.578 18.581 18.593 18.603 18.632 18.654 18.673 18.694 18.702 18.707 18.707 18.714 18.716 18.72 18.732 18.735 18.745 18.757 18.758 18.838 18.877 18.887 18.897 18.899 18.934 18.938 18.968 18.971 18.973 18.978 18.983 19.008 19.048 19.074 19.079 19.098 0.019 0.026 0.021 0.019 0.024 0.023 0.02 0.024 0.023 0.023 0.025 0.025 0.024 0.023 0.025 0.023 0.026 0.028 0.03 0.027 0.028 0.029 0.029 0.029 0.028 0.028 0.029 0.031 0.031 0.033 0.031 0.032 0.032 0.03 0.033 0.039 0.033 0.031 0.034 0.033 0.032 0.035 0.036 0.03 0.036 0.036 0.03 0.036 0.033 0.036 0.036 0.047 0.037 0.039 0.042 0.038 0.037 0.042 0.043 0.045 0.044 0.04 0.04 0.046 0.043 0.052 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 1.177 99.999 1.376 1.43 1.465 1.259 1.365 1.263 1.156 1.247 1.095 1.207 1.333 1.402 99.999 1.254 1.444 1.482 1.26 1.567 1.358 1.248 1.188 1.357 1.274 1.647 1.768 1.587 99.999 99.999 1.44 99.999 1.31 1.326 1.431 1.68 1.371 99.999 99.999 99.999 1.097 1.267 1.283 1.243 1.533 1.225 99.999 1.458 1.258 99.999 99.999 99.999 99.999 99.999 1.154 1.184 99.999 99.999 99.999 1.271 99.999 1.121 99.999 99.999 99.999 99.999 0.052 99.999 0.058 0.063 0.073 0.069 0.068 0.063 0.061 0.066 0.063 0.065 0.087 0.07 99.999 0.077 0.08 0.08 0.08 0.091 0.088 0.081 0.076 0.085 0.077 0.103 0.109 0.092 99.999 99.999 0.097 99.999 0.09 0.091 0.098 0.14 0.101 99.999 99.999 99.999 0.089 0.105 0.1 0.101 0.136 0.1 99.999 0.126 0.101 99.999 99.999 99.999 99.999 99.999 0.116 0.113 99.999 99.999 99.999 0.133 99.999 0.103 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.788 0.806 0.868 0.826 0.929 0.719 0.8 0.682 0.77 0.868 0.785 0.754 0.811 0.868 0.782 0.723 0.854 0.829 0.82 1.028 0.842 0.762 0.814 0.844 0.961 0.942 0.954 0.877 1.092 0.875 0.827 0.907 0.876 0.934 1.016 0.96 0.732 0.83 0.731 0.918 0.824 0.865 0.822 0.822 0.796 0.833 0.813 0.905 0.745 1.064 0.93 1.111 0.891 0.788 0.819 0.763 0.884 0.797 0.826 0.804 0.866 0.69 0.815 0.977 0.803 1.169 0.022 0.028 0.023 0.021 0.025 0.026 0.023 0.026 0.026 0.026 0.027 0.028 0.026 0.025 0.028 0.027 0.027 0.031 0.032 0.028 0.03 0.031 0.031 0.031 0.03 0.029 0.03 0.033 0.03 0.035 0.035 0.033 0.034 0.031 0.034 0.04 0.036 0.034 0.037 0.035 0.035 0.037 0.04 0.034 0.04 0.039 0.033 0.037 0.038 0.036 0.039 0.045 0.039 0.042 0.045 0.042 0.039 0.045 0.047 0.049 0.045 0.045 0.042 0.048 0.046 0.049 1.584 1.643 1.751 1.707 1.84 1.5 1.617 1.553 1.535 1.672 1.553 1.515 1.597 1.748 1.521 1.533 1.735 1.693 1.674 1.917 1.735 1.58 1.606 1.728 1.855 1.849 1.854 1.756 2.078 1.784 1.644 1.75 1.779 1.832 1.964 1.868 1.642 1.744 1.609 1.794 1.644 1.666 1.598 1.635 1.679 1.65 1.769 1.844 1.586 2.07 1.791 2.138 1.749 1.58 1.632 1.529 1.783 1.645 1.69 1.638 1.76 1.423 1.766 1.808 1.624 2.38 0.019 0.025 0.02 0.018 0.021 0.022 0.019 0.023 0.022 0.022 0.024 0.024 0.023 0.022 0.024 0.023 0.025 0.026 0.028 0.024 0.026 0.028 0.028 0.028 0.025 0.026 0.026 0.028 0.027 0.031 0.029 0.03 0.03 0.028 0.029 0.035 0.032 0.03 0.033 0.031 0.031 0.032 0.034 0.03 0.034 0.034 0.029 0.033 0.032 0.032 0.033 0.04 0.034 0.037 0.039 0.037 0.035 0.04 0.04 0.043 0.04 0.041 0.038 0.041 0.041 0.043 416 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México TABLE 5 (CONTINUED) X Y V σV 167 660.7 840.5 747.2 791.4 884.2 799.2 315.9 325.3 425 151.9 568.2 75.1 660.3 277.2 636.9 854.3 170.4 740 305.6 861.4 780.4 891.1 384.8 637.2 680.1 50 215.8 10.3 537.4 255.4 49 847.1 550.9 576.3 680 751.4 429.8 394.7 249.1 295.1 340.6 863.5 376.6 732.4 673.3 136.6 892.5 284.6 466.8 669.1 187.3 595.7 630.9 340.1 915.1 607.4 512.5 500.5 645.4 280.7 636.5 64.8 111.6 819.8 65.4 666.8 542.1 711 514.5 338.5 936 629.2 924 790.9 25.3 459 3.8 753.4 809 874.9 698.1 293.3 418.7 805.2 336.1 623.4 105.5 150.2 755.5 613.8 860.1 455.1 223.9 605.8 942.8 599.4 671.7 541.9 454.9 687.7 429 450.8 251.6 367 983.9 657 456.9 383.3 539.7 168.4 587.1 393.6 688.9 219.6 246.1 739.3 543.2 889.6 198.8 373 27.4 290.5 302.7 973.7 154.5 123.8 933 500.9 32.8 718.2 714.9 19.103 19.15 19.152 19.16 19.163 19.165 19.181 19.202 19.204 19.212 19.217 19.221 19.235 19.244 19.248 19.254 19.257 19.273 19.313 19.324 19.326 19.33 19.334 19.344 19.358 19.359 19.363 19.368 19.382 19.389 19.402 19.409 19.419 19.421 19.428 19.428 19.432 19.437 19.449 19.45 19.451 19.502 19.553 19.579 19.58 19.593 19.593 19.595 19.607 19.614 19.63 19.651 19.668 19.671 19.671 19.683 19.686 19.723 19.725 19.733 19.778 19.805 19.82 19.867 19.902 19.921 0.045 0.054 0.043 0.045 0.047 0.051 0.052 0.05 0.052 0.044 0.047 0.054 0.048 0.052 0.057 0.045 0.055 0.055 0.051 0.057 0.058 0.055 0.055 0.055 0.055 0.059 0.055 0.058 0.057 0.064 0.059 0.064 0.062 0.057 0.055 0.067 0.055 0.061 0.07 0.074 0.058 0.06 0.066 0.066 0.067 0.073 0.067 0.067 0.067 0.067 0.066 0.074 0.077 0.075 0.067 0.075 0.073 0.087 0.077 0.08 0.08 0.095 0.096 0.104 0.083 0.083 (B − V ) σB−V (U − B) σU −B (V − R) σV −R (V − I) σV −I 99.999 99.999 99.999 99.999 1.091 99.999 0.898 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 1.12 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.134 99.999 0.122 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.15 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 99.999 0.722 0.909 0.855 0.911 1.029 0.982 0.858 0.923 0.875 0.935 0.799 0.835 0.765 0.846 0.866 0.738 0.83 0.856 0.914 0.888 0.985 0.838 0.772 0.848 0.871 0.798 0.807 0.845 0.799 0.841 0.946 1.089 0.748 0.939 0.747 0.844 0.942 0.739 0.955 1.107 1.154 0.86 0.812 0.706 0.877 1.04 0.855 0.782 0.787 0.828 0.834 0.59 0.868 0.842 0.813 1.065 0.876 1.044 0.659 0.884 0.997 0.729 1.05 1.086 0.717 0.707 0.049 0.055 0.046 0.047 0.048 0.051 0.054 0.052 0.055 0.046 0.05 0.056 0.051 0.054 0.058 0.05 0.057 0.058 0.053 0.062 0.059 0.058 0.062 0.058 0.058 0.061 0.058 0.06 0.061 0.066 0.059 0.062 0.066 0.058 0.063 0.068 0.057 0.066 0.071 0.071 0.057 0.064 0.071 0.074 0.068 0.072 0.069 0.072 0.074 0.071 0.072 0.081 0.079 0.08 0.074 0.074 0.074 0.083 0.085 0.08 0.08 0.098 0.092 0.102 0.092 0.094 1.51 1.812 1.658 1.802 1.882 1.883 1.651 1.83 1.748 1.814 1.651 1.794 1.586 1.677 1.697 1.543 1.646 1.768 1.897 1.794 2.026 1.746 1.6 1.678 1.628 1.688 1.878 1.786 1.702 1.734 1.764 2.069 1.66 1.903 1.659 1.673 1.76 1.616 1.734 2.083 2.063 1.765 1.646 1.493 1.819 1.947 1.816 1.72 1.794 1.802 1.711 1.558 1.744 1.804 1.711 2.101 1.854 2.022 1.552 1.757 1.972 1.584 2.009 2.178 1.592 1.598 0.043 0.049 0.041 0.042 0.043 0.046 0.049 0.046 0.048 0.041 0.046 0.05 0.047 0.049 0.053 0.043 0.052 0.051 0.046 0.053 0.051 0.051 0.053 0.051 0.052 0.056 0.051 0.053 0.055 0.059 0.054 0.055 0.059 0.051 0.054 0.063 0.052 0.058 0.064 0.063 0.05 0.055 0.062 0.065 0.062 0.064 0.061 0.064 0.063 0.063 0.062 0.074 0.073 0.069 0.063 0.066 0.067 0.076 0.076 0.073 0.071 0.088 0.082 0.088 0.08 0.082 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México UBVRI PHOTOMETRY OF OPEN CLUSTERS 417 used to help us in the visualization and analysis of the photometric data (e.g., Schuster et al. 2007). These programs facilitate the elimination of field and apparent non-member stars of a given cluster from the diagnostic diagrams used to enhance the apperception of cluster features. Once a satisfactory first estimate of the parameters was obtained, a full-frame solution was also consulted and refined. safe is capable of displaying simultaneously in different color-color (CC) and color-magnitude (CM) diagrams the cluster’s data and has an interactive way to identify a (group of) star(s) in one particular diagram and to see where it falls in the other diagrams. This program is capable of displaying up to 16 different diagrams for a given cluster and is very useful for the determination of a cluster’s physical parameters. Figure 1a-c presents the DSS redfilter images of Be 89 (Panel a), Ru 135 (Panel b) and Be 10 (Panel c), with the regions analyzed in this work enclosed by ellipses. The central (X, Y ) pixel coordinates of the nearly circular regions in Figure 1a-c, which are considered for the photometric analyses are the following: (584, 488) pixels for Be 89, (542, 504) for Ru 135, and (517, 493) for Be 10. The diameters in arcminutes (∆X, ∆Y ) of nearly circular regions in Figure 1a-c are the following: (2.27, 2.65) for Be 89, (2.62, 2.67) for Ru 135, and (3.12, 2.34) for Be 10. 3. ANALYSES OF THE OPEN CLUSTERS BE 89, RU 135, AND BE 10 The (U − B, B − V ), two-color or CC, diagram, and five CM diagrams have been used together with the zero-age-main-sequence (ZAMS) intrinsic-color calibrations of Schmidt-Kaler (1982, hereafter SK82) and with the Padova isochrones (Girardi et al. 2000, hereafter GBBC; Bertelli et al. 2008; Marigo et al. 2008, hereafter MGBG) to obtain reddenings, metallicities, distance moduli, and ages for these clusters. Our analysis technique for our program clusters places particular emphasis upon the fit of the ZAMS intrinsic colors and Padova isochrones to the observational data of the clusters, and this depends in turn upon important characteristics of the CM and CC diagrams for open clusters (e.g., Paunzen & Netopil 2006, their § 3), which are summarized as follows: 1. A procedure for eliminating non-members. 2. A determination of the interstellar reddening as accurately as possible. 3. Visibility of the turn-off. Fig. 1. DSS red-filter images of the Galactic open clusters Be 89 (Panel a), Ru 135 (Panel b), and Be 10 (Panel c). The regions analyzed with the elipse inspection tool, to derive first estimates for the fundamental parameters, are enclosed by ellipses. Orientation as usual: north is up, and east to the left. 418 AKKAYA ET AL. 4. Compensation for binary stars which tend to widen the main-sequence distribution. 5. Consideration of the red-clump stars (if present) to improve the isochrone fit. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México 6. An appropriate choice of the isochrone which corresponds to the correct heavy-element abundance (Z). Regarding the locus of the main sequence in a CM diagram, and independent of any cosmic dispersion, the main-sequence strips or bands in the CM diagrams are affected by the contamination of binary and multiple stars; particularly, the mid-points are shifted to brighter magnitudes and the colors to redder values due to this contamination, and also sometimes due to variable intercluster extinction. For this reason, the SK82 ZAMS and the MGBG isochrones have been fitted to the blue- and faint-most concentrations within the observed broad main-sequence bands whenever possible, assuming that these concentrations reflect the single-star distribution (e.g., Carney 2001), and that most stars observed red- and bright-ward of these are in fact binary, or multiple, systems. In the absence of proper-motion/radial-velocity measurements to insure cluster membership, and to minimize the effects of field-star contamination, we have concentrated more on the central regions of the clusters rather than using the full-frame CCD images; this has been accomplished by using the elipse or safe programs, described above. These have been used to select an elliptical, or polygonal area (with as many as 10 sides), centered on the open cluster as seen in a V or R image, excluding stars outside this area from further analyses. (See Figure 1). These interactive analyses greatly increase the contrast of cluster members with respect to the field stars, and thus the scatter in the CM and CC diagrams is significantly reduced. Also, the observational errors, e.g., σ(U −B) , of these three clusters have been considered as a criterion in selecting the more reliable data for further analyses. The values of σ(U −B) are almost always larger than the ones of σ(B−V ) due to the smaller sensitivity of the CCD in the ultraviolet, and the errors σ(R−I) , σ(V −I) , and σ(V −R) are among the smallest. The observational errors, such as σ(U −B) , σ(B−V ) , and σ(B−R) , have been selected to be less m than ≈ 0.m 10 (and sometimes < ∼ 0. 05) in some of the diagnostic diagrams presented in the analyses to follow, such as the (U − B, B − V ), (V, B − V ), and (V, B − R) diagrams. Interstellar reddenings of the program clusters have been estimated from shifts of the intrinsic-color sequences of SK82 in the (U − B, B − V ) diagram, until the best fit to the data of the clusters was achieved: along the U − B axis by 0.72 E(B − V ) + 0.05 E(B − V )2 and along the (B − V ) axis by E(B − V ). For this, F-type stars have been fitted above the main sequence of SK82 [i.e., blue-ward in (U − B)], and simultaneously the red-clump stars above the red-giant colors of SK82 with consistent ultraviolet excesses according to the normalizations of Sandage (1969). The two-color sequence of SK82 has been constructed from the intrinsic colors of SK82 m for zero-age dwarfs [(B − V )0 < ∼ 0. 75] and for giants m > [(B − V )0 ∼ 0. 75]. Once the two-color sequence of SK82 has been fixed as indicated above, to determine the photometric metal abundance, [Fe/H], one first locates the F-type stars in the (U −B, B −V ) diagram and compares their location with that of their counterparts of known metallicity (e.g., the SK82’s ZAMS calibration). Deviations between the two are due mainly to their differences in metal content, an ultraviolet excess, δ(U − B), being caused by differences in line blanketing. The metal-deficient F-type cluster stars, if present, lie blue-ward of the “hump region” of the ZAMS sequence, where an eyeball-fitted osculating curve similar to “the hump” has been fitted to the data points of the F-stars (i.e., the thick line above the hump of the F-star region in Figures 2, 5, and 8) and, simultaneously, to the red-clump stars (if present), since they also will lie blue-ward of the redgiant colors of SK82 with a corresponding ultraviolet excess. This ultraviolet excess is correlated with the photometric metallicity of the cluster. Then, a metallicity value, [Fe/H], for a cluster can be derived from the empirical calibration, [Fe/H]-δ(U − B)0.6 , of Karataş & Schuster (2006), allowing the determination of [Fe/H] independently of the isochrones to be fitted to the data, thus reducing from three to two the free parameters to be derived from the CM diagrams. Heavy-element abundances (Z) of the three clusters have been obtained from the photometric metal abundances [Fe/H] with the expression Z = Z⊙ · 10[Fe/H] , Z⊙ = +0.019 . (6) Finally, the appropriate isochrones of MGBG were computed online in terms of the resulting heavyelement abundance for further analyses of the clusters (distances and ages). To estimate the the age of a cluster (A) and the true distance modulus (DM = V0 − MV ) in a CM diagram, for example the (V, B − V ) dia- UBVRI PHOTOMETRY OF OPEN CLUSTERS 419 TABLE 6 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México ADOPTED INTERSTELLAR EXTINCTION LAW E(V −I) E(B−V ) E(R−I) E(B−V ) E(V −R) E(B−V ) E(B−R) E(B−V ) 1.25 0.69 0.56 1.56 gram, the absolute magnitudes, MV , of the MGBG isochrones have been shifted by DM + 3.1 E(B − V ) along the magnitude axis and their corresponding colors, (B −V )0 , reddened by adding the color excess E(B − V ) until some DM value provides a good fit of the appropriate isochrone to the faint/blue concentration of the observed lower main sequence of the cluster and, if present, of the red-clump stars. One has to take into account when determining the DM that metal-poor stars are sub-luminous as compared with their solar-like counterparts by determining a reliable value for Z from the CC diagram. To infer the age of the cluster, the (logarithm of the) age of the isochrones, log A, has been varied until a good match with the observed sequences, i.e., the upper main-sequence (MS), the turn-off (TO) stars, and, if present, the red-clump (RC) stars, has been achieved. A fine tuning of the DM has been made if necessary. The uncertainties of E(B − V ), Z, DM , and log A are discussed in § 3.4. Following a similar procedure to that outlined above, the distance moduli and cluster ages have also been derived from analyses of four other CM diagrams for each of the clusters. The corresponding color excesses applied in the diagrams were iterated starting with the previously derived color excess estimates, E(B − V ), and the results were intercompared by means of the standard interstellar extinction law adopted (see Table 6; also cf. Dean, Warren, & Cousins 1978; Mathis 1990; Straiz̧ys 1995) until satisfactory solutions were obtained for all the CM diagrams. The derived extinction laws do not differ significantly from that of Table 6. 3.1. Be 89 The (U − B, B − V ) diagram of Be 89 is shown in Figure 2. An interstellar reddening of (B − V ) = 0.m 60 ± 0.m 09 has been derived by shifting the intrinsic two-color stellar sequence of SK82 along the reddening vector as described in the previous section. (Another possibility, to fit the stars by E(B − V ) ≃ 0.m 73 to the blue (B-star) branch of the ZAMS curve, would leave many stars far from a good fit). Six stars apparently in the cluster are noticed with (B − V ) ≈ 1.m 6 and (U − B) ≈ 1.m 4 Fig. 2. The (U − B, B − V ) diagram of Be 89. The “S” curves (upper parts, ZAMS, and lower parts, red giants) have been taken from the two-color relations of SK82 and are displayed for the interstellar reddening values E(B − V ) = 0.m 00 and 0.m 60 (the bluer and redder versions, respectively). A reddening vector is also shown as an arrow, and big open circles mark the six RC candidates, and open squares, the blue-straggler ones. A heavy solid curve represents our best fit to the data; this has been adjusted to the main-sequence F-type stars above (i.e., blue-ward of) the ZAMS colors of SK82 and, simultaneously, to the RC stars above the red-giant colors of SK82. This fit has been used to estimate the heavy-element abundance of the cluster, which is shown in Table 7. (big open circles in Figure 2) lying near, but above (i.e., blue-ward of) the giant sequence of SK82, the expected location of the RC stars; their subsequent locations in the CM diagrams confirm this classification (see Figures 3 and 4). A seventh candidate falls further from the expected RC locus in four of the five CM diagrams. The F-type and RC stars of Be 89 (cf. Figure 2, (B − V ) ≈ 1.m 0 and ≈ 1.m 6, respectively) lie above the (reddened) ZAMS two-color calibration of SK82 by δ(U − B) ≃ 0.m 1. Our best eyeball fit to the data is shown as the heavy solid curve in Figure 2. In the dereddened two-color diagram, the heavy line gives a value of (U − B)0 = −0.m 10 ± 0.m 02 at (B − V )0 = 0.m 44, and at this same color index, the highest point of the SK82 hump has (U − B)0 = −0.m 02. The resulting ultraviolet excess, δ(U −B) = +0.m 08±0.m 02, has been converted to δ(0.6) = +0.m 10 ± 0.m 02 at © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México 420 AKKAYA ET AL. Fig. 3. CM diagrams, (V, B − V ) and (V, R − I), for Be 89. Solid lines show the interpolated Z = +0.008 isochrones of MGBG (cf. Table 7 for the inferred metallicity). Big open circles denote the RC candidates, and open squares, the blue-straggler ones. See the text and Table 8 for the inferred values of the distance modulus and age. (B−V ) = +0.m 60 with the normalization ratios given by Sandage (1969, his Table 1A). These values have been listed in Table 7, together with the corresponding photometric metallicity [Fe/H]= −0.35±0.02 dex derived with help of the calibration [Fe/H]-δ(0.6) of Fig. 4. CM diagrams, (V, V − I), (V, V − R), and (V, B −R), (top, center and bottom panels, respectively) for Be 89. The isochrone curves and the symbols have the same meaning as in Figure 3. See the text and Table 7 for the inferred values of reddening and metallicity, and Table 8 for the distance modulus and age. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México UBVRI PHOTOMETRY OF OPEN CLUSTERS 421 been computed from E(B − V ) with help of Table 6, and then the isochrone ages have been varied until a satisfactory fit to the data has been obtained through the observed upper-MS, TO, and RC sequences of the cluster (cf. Figures 3–4). The resulting inferred mean age of Be 89 is log(A) = 9.58 ± 0.06 dex (A = 3.8 ± 0.6 Gyr). For all of these CM diagrams of Be 89, two isochrones have been plotted to provide a means for appreciating the uncertainties of the derived distances and ages. In Table 8 the range in ages provided by these isochrone pairs, the final values for the distances and ages from each CM diagram, and the mean values for each cluster are given. Error estimates of (V0 − MV ) and log(A) are discussed in § 3.4 below, and the mean results given in Table 8 have been calculated with equations (8) and (9) inserting the corresponding parameters summarized in the table. Fig. 5. The CC diagram of Ru135. The SK82 curves and the symbols have the same meaning as in Figure 2. See the text and Table 7 for the inferred values of the reddening and metallicity. Karataş & Schuster (2006). Note that the δ(0.6) in the notation of the latter authors corresponds to delta(0.6) in the notation of Sandage (1969). Applying the above relation between [Fe/H] and Z, where [Fe/H] has been estimated as −0.35 ± 0.02 dex, gives Z = +0.008 ± 0.0003. The online isochrones of MGBG have been iterated using this metal abundance when further analyzing Be 89. In Figures 3 and 4, the isochrones of MGBG for Z = +0.008 have been over-plotted in five CM diagrams: (V, B − V ), (V, R − I), (V, V − I), (V, V − R), and (V, B − R) after reddening the isochrones along the color axis with a color excess corresponding to E(B − V ) = 0.m 60, converted with help of Table 6, and adding a visual extinction of AV = 3.1 · E(B − V ) = 1.m 86 to the absolute magnitudes of the isochrones. The isochrones have then been shifted vertically to obtain the best fit to the observed lower-MS and and RC sequences. This vertical shift is the (true) distance modulus, DM = (V0 − MV ). The best fit for Be 89 is DM = 11.m 90 ± 0.m 06 (d = 2.4 ± 0.06 kpc, cf. Table 8). To derive an age estimate for Be 89, the isochrones of MGBG for Z = +0.008 have been shifted in the CM planes as above, i.e., MV + 3.1E(B −V )+DM and C0 (λ1 −λ2 )+E[C(λ1 −λ2 )], respectively, where the latter color excesses have 3.2. Ru 135 The same procedures outlined in § 3, and § 3.1 for Be 89, have also been used for the clusters Ru 135 and Be 10. A reddening of E(B − V ) = 0.m 63 ± 0.m 12 has been derived for Ru 135 (cf. Figure 5). However, a clump of A-type stars at (B − V ) ≃ 0.m 8 and (U − B) ≃ 0.m 4 seems to be present, with a horizontal-like distribution which does not fit satisfactorily the reddened two-color ZAMS curve of SK82. These stars (Sp ≈ A-types) are probably less reddened than Ru 135 by ≃ 0.m 3 in E(B −V ), nearer, and most probably not cluster members (cf. the open squares in the CC and CM diagrams of Figures 5, 6, and 7), or they could be blue stragglers belonging to the cluster. For this latter case, they would be peculiar because of an ultraviolet-flux excess present in their spectral energy distributions (SEDs), and only a spectroscopic study with good signal-to-noise ratios would reveal more about their true nature. Ru 135 contains a considerable number of F- and later-type stars, and appears to have its blue-most turn-off limit at (B −V ) ≈ +1.m 0 and (U −B) ≈ 0.m 4, corresponding to a dereddened (B − V ) ≈ +0.m 43 (i.e., Sp ≈ F5V). The best fit to the observed Fhump sequence in the (U − B, B − V ) diagram is the solid curve shifted blue-ward with respect to the two-color SK82 curve (cf. Figure 5). From the ultraviolet excess of these cluster F stars and following the procedure outlined at the beginning of § 3, [Fe/H]= −0.71 ± 0.02 dex (Z = +0.004 ± 0.0002) has been derived. The isochrones of MGBG with this metallicity have been computed on line and used in the following analyses. 422 AKKAYA ET AL. TABLE 7 NORMALIZED (U-B) EXCESSES AND DERIVED METALLICITIES Cluster (U − B)SK82 [mag] (U − B)0,fit [mag] δ(U − B) [mag] δ(0.6) [mag] [Fe/H] [dex] Z Be 89 Ru 135 Be 10 −0.02 −0.02 −0.02 −0.10 −0.16 −0.09 0.08 0.14 0.07 0.10 0.14 0.11 −0.35 −0.71 −0.49 0.008 0.004 0.006 ≤ ±0.01 ±0.02 ±0.02 ±0.02 ±0.02 ≤ ±0.001 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México error TABLE 8 DISTANCE AND AGE ESTIMATES OF THE CLUSTERS Color (V0 − MV ) [mag] d [kpc] log(A) range log(A) A [Gyr] Be 89: E(B − V ) = 0.60 ± 0.09 & Z = +0.008 ± 0.001 (B − V ) (R − I) (V − I) (V − R) (B − R) 11.90 ± 0.10 11.90 ± 0.20 11.90 ± 0.15 11.90 ± 0.10 11.90 ± 0.20 2.4 ± 0.1 2.4 ± 0.2 2.4 ± 0.2 2.4 ± 0.1 2.4 ± 0.2 Mean 11.90 ± 0.06 2.4 ± 0.06 9.45–9.55 9.50–9.60 9.50–9.60 9.50–9.60 9.45–9.55 9.55 ± 0.15 9.60 ± 0.20 9.60 ± 0.20 9.60 ± 0.15 9.55 ± 0.10 3.6 ± 1.4 4.0 ± 2.3 4.0 ± 2.3 4.0 ± 1.6 3.6 ± 0.9 9.58 ± 0.06 3.8 ± 0.6 Ru 135: E(B − V ) = 0.63 ± 0.12 & Z = +0.004 ± 0.001 (B − V ) (R − I) (V − I) (V − R) (B − R) 9.50 ± 0.15 9.70 ± 0.15 9.60 ± 0.20 9.60 ± 0.15 9.50 ± 0.20 0.75 ± 0.05 0.87 ± 0.06 0.83 ± 0.08 0.83 ± 0.06 0.75 ± 0.07 Mean 9.58 ± 0.07 0.81 ± 0.03 9.60–9.70 9.55–9.65 9.55–9.65 9.55–9.65 9.60–9.70 9.60 ± 0.15 9.55 ± 0.15 9.55 ± 0.15 9.60 ± 0.15 9.60 ± 0.15 4.0 ± 1.6 3.6 ± 1.5 3.6 ± 1.5 4.0 ± 1.5 4.0 ± 1.6 9.58 ± 0.06 3.8 ± 0.7 Be 10: E(B − V ) = 0.75 ± 0.09 & Z = +0.006 ± 0.001 (B − V ) (R − I) (V − I) (V − R) (B − R) 11.20 ± 0.11 11.10 ± 0.20 11.15 ± 0.15 11.15 ± 0.20 11.20 ± 0.10 1.7 ± 0.1 1.7 ± 0.2 1.7 ± 0.1 1.7 ± 0.2 1.7 ± 0.1 Mean 11.16 ± 0.06 1.70 ± 0.05 The five CM diagrams, (V, B − V ) through (V, B − R), of Ru 135 are displayed in Figures 6 and 7 together with the reddened isochrones that best fit the data for the derived color excess and metallicity, E(B − V ) = 0.m 63 and Z = +0.004. The distance moduli, (V0 − MV ), and ages, A, found from these five CM diagrams and their respective isochrone fittings are given in Table 8. In these CM diagrams a significant number of stars are seen extending to brighter magnitudes and red-ward from the fainter and redder observational limits of the main sequences, i.e., the stars extending 9.05–9.15 9.10–9.20 9.05–9.15 9.05–9.15 9.05–9.15 9.05 ± 0.10 9.10 ± 0.10 9.05 ± 0.15 9.05 ± 0.10 9.05 ± 0.05 1.1 ± 0.3 1.3 ± 0.3 1.1 ± 0.3 1.1 ± 0.3 1.1 ± 0.1 9.06 ± 0.05 1.08 ± 0.08 red-ward and upward from (V, B −V ) ≈ (18.m 5, 1.m 5) or (V, R − I) ≈ (18.m 5, 0.m 9) (cf. Figure 6). These are probably field red-giant stars contributed by the Galactic bulge, as suggested by the Galactic longitude and latitude of Ru 135, ℓ ≃ 16.4◦ and b ≃ +6.2◦ (see Binney & Merrifield 1998; Stanek et al. 1996, Figures 3.5 and 2, respectively). The fact that Ru 135 lies near the direction of the Galactic central region also explains the significant number of brighter and bluer foreground stars seen in its CC and CM diagrams. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México UBVRI PHOTOMETRY OF OPEN CLUSTERS 423 Fig. 6. The (V, B − V ) and (V, R − I) diagrams for Ru 135. Solid lines show the isochrones of MGBG interpolated to Z = +0.004. See the text, and Tables 7 and 8, for the inferred values of reddening, metallicity, distance modulus, and age. Stars shown with open-square symbols are most likely field, or blue-straggler, stars. 3.3. Be 10 In Figure 8 the loci of stars observed in the direction of Be 10 are shown in the (U − B, B − V ) diagram, together with the standard interstellar reddening vector and the two-color curve of SK82, shifted along this vector to procure the best fit to the data. From the fits along the (B − V ) and (U − B) axes, E(B − V ) = 0.m 75 ± 0.m 09 and ([Fe/H], Fig. 7. The (V, V − I), (V, V − R) and (V, B − R) diagrams for Ru 135. The symbols are the same as in Figure 6. See the text, and Tables 7 and 8, for the inferred values of reddening, metallicity, distance modulus, and age. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México 424 AKKAYA ET AL. Fig. 8. The (U − B, B − V ) plot of Be 10. The symbols and the curves are the same as in Figure 2. Z) = (−0.49 ± 0.02 dex, +0.006 ± 0.0003) are found, following the procedures described in § 3 and § 3.1 (see Table 8 for partial and mean results). Again, the appropriate isochrones of MGBG have been computed online with this corresponding metallicity and are used below for further analyses of Be 10. For Be 10, DM = (V − 3.1 · E(B − V ) − MV ) = 11.m 16 ± 0.m 06, the distance, d = 1.7 ± 0.05 kpc, the metallicity, Z = +0.006 ± 0.0003, log(A) = 9.06 ± 0.05, and the age, A = 1.08 ± 0.08 Gyr have been measured. Our results are listed in Tables 7 and 8. The resulting (best) isochrone fitting to the corresponding Be 10 data in the (V, B − V ), (V, R − I), (V, V − I), (V, V − R) and (V, B − R) diagrams are displayed in Figures 9 and 10, where one can see that the isochrones reproduce well the observed lower and upper MS, the TO, and RC sequences of this cluster. 3.4. Estimated errors and weighted averages In Table 7, the ultraviolet excesses and the metallicities are given for Be 89, Ru 135, and Be 10, and in Table 8, the mean values for the distance moduli, heliocentric distances, logarithmic ages, and ages, together with the corresponding estimates of precision. The errors were calculated in a straightforward manner (cf. Bevington & Robinson 2003, and references therein). In the following the details of this error analysis are presented. Fig. 9. The (V, B−V ) and (V, R−I) diagrams for Be 10. Solid lines show the isochrones of MGBG interpolated to Z = +0.006. The larger open circles identify the RC candidates. See the text, and Tables 7 and 8, for the inferred values for reddening, metallicity, distance modulus, and age. 3.4.1. Errors in E(B − V ) and Z The random errors in the color excess E(B − V ) and photometric metallicity [Fe/H] were estimated as follows: (i) By moving the two-color curve of SK82 backward and forward along the standard reddening UBVRI PHOTOMETRY OF OPEN CLUSTERS 425 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México vector in the (U − B, B − V ) diagram until a good fit with the observed GK-type, RC, and F-hump sequences was achieved. (No BA-type sequences were present for these clusters.) The precision of the determinations also depends on the scatter of the data points (cf. Figure 5 of Ru 135 and Figure 8 of Be 10 for good and fair cases, respectively). The uncertainties given in Tables 7 and 8 reflect this. Following this procedure, a typical error in E(B − V ) for the quality of the reduced data of our clusters is (conservatively) ≈ 0.m 04. The systematic error in E(B − V ) depends on the color calibration used. In the case of SK82, the uncertainty can be safely assumed to be, at the most, of the order of the difference between two adjacent spectral subclasses. (ii) The random photometric-metallicity uncertainty has then been estimated from the parabolic (eyeball) fit to the data of the maximum characterizing the ultraviolet flux excess of the stars at the dereddened color (B − V )0 ≃ 0.m 44 (Sp ≃ F5) and then following Sandage’s (1969) normalization procedure. The uncertainty of the metal content Z was determined from the relation (e.g., Bevington & Robinson 2003): σZ = ln 10 × Z × σ[Fe/H] . (7) σ[Fe/H] has been estimated from the uncertainty in the ultraviolet excess δ(U − B) at the F hump between the observed and the SK82 twocolor curves and is typically ±0.m 02. Assuming hZi = 0.006 (the mean of the three clusters) | σZ | ≤ 0.0003 is obtained with equation (7) above. Assuming an error of about 0.001 for Z is, in our case, a quite conservative estimate. Fig. 10. The (V, V − I), (V, V − R) and (V, B − R) diagrams for Be 10. The symbols are the same as in Figure 9. See the text, and Tables 7 and 8, for the inferred values for reddening, metallicity, distance modulus, and age. (iii) On the other hand, the deviation of the assumed reddening vector from the “true” one depends on the quotient E(U − B)/E(B − V ), which can strongly deviate locally from its canonical value of 0.72 (see Chavarrı́a, de Lara, & Hasse 1987; Johnson 1977). This uncertainty may produce errors larger than the precision quoted above. For a crude estimate, using the extremes of the cited values of E(U − B)/E(B − V ) and a typical color excess of E(B − V ) = 0.m 50, the uncertainty in δ(U − B) could be as large as 0.m 150.m 20. However, since our displacements of the SK82 curve in the CM-diagrams are consistent with the canonical value for the interstellar ex- 426 AKKAYA ET AL. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México tinction law, we assume that this error contribution is negligible statistically. (iv) Another systematic uncertainty results from the two-color calibration of SK82: from the uncertainty of (U − B) or (B − V ) in the two-color calibration curve of SK82, which is expected to be of the order of the difference between two m typical spectral subclasses (in our case < ∼ 0. 05) for the (U-B) index; and from the fit of the whole curve to √ a cluster data set, of the orm der < 0. 05/ N , where there are N pivotal ∼ points considered when adjusting the SK2 twocolor curve (the BA-type, the F-hump, the GKtype, and the RC sequences; i.e., N > ∼ 3). Summarizing, the systematic uncertainty in δ(U −B) should be less than roughly three times that given by the precision of the flux measurements. 3.4.2. Errors in the distance moduli and ages (i) The uncertainties σDMi for the moduli given in Table 8 that result from fitting the appropriate isochrones to the data in the CM diagrams depend on the photometric uncertainties (flux measurement and standard-transformation errors), the absolute magnitude and intrinsic color calibration errors (see for example, SK82), the color excess uncertainty of a given color [which depends on E(B−V )], and on the reddening law adopted. We assume that the isochrones only contain the errors of the absolute magnitude and intrinsic-color calibrations and that the photometric and transformation errors are small (≈ 0.m 03) when compared to the other sources of error. In our case, the largest contribution to the distance modulus uncertainty is due to the uncertainty in the absolute-magnitude scale, followed by the uncertainty in the slope of the reddening vector, and the color-excess error, about 0.m 3, 0.m 15 and 0.m 12, respectively, which combine to give an expected total uncertainty as large as σDMi ∼ = 0.m 25. The moduli resulting from the CM diagrams of each object and the mean moduli for the three clusters are given in Table 8, and the mean of the moduli has been derived from the five moduli, weighted with their respective (usually unequal) precisions, with the following expression: DM = 2 Σ(DM )i /σDM  i ; (i = 1, ..., 5),  2 Σ 1/σDM i (8) and the associated mean uncertainty is estimated from the individual uncertainties of the five CM-diagrams of a given cluster by the relation: X 1 1 = (9) 2 (σmean ) (σDM )2i The combined error is the square root of the sum of the squared uncertainties and is expected to be about 0.m 15, or even less. (ii) The uncertainty in the log(A) has a random error due to the (eyeball) fit of the isochrone with the appropriate metallicity to a given CM diagram of a cluster in question, and a quantitative estimate is obtained by jiggling brightward and faint-ward the isochrone curve until a good fit of the lower main sequence produces the DM . Then the age of the isochrone is varied until a good fit to the upper main sequence, the TO, and the RC sequences is achieved. The two isochrones shown in the CM diagrams of the program clusters give a quantitative estimate of this last error. Several different authors have computed isochrones as function of the metallicity, and the physics behind seems to be well understood. One does not expect a large variation in the log(A) error due to any uncertainty in the physics, and the uncertainties of E(B − V ) and (V0 −MV ) play a secondary role because the age errors depend more on the form of the isochrone curve and how it embraces the data (i.e., the the upper main-sequence and TO regions and the RC sequence) and, less significantly, on the reddening law (except perhaps the blue and nearultraviolet filters). More problematic is the case when the TO region is not well defined (i.e., isolated from field stars) and/or the RC sequence is not present. In our case, the errors for the different colors of Table 8 reflect these uncertainties. 4. COMPARISON OF FUNDAMENTAL PARAMETERS OF THE THREE CLUSTERS The reddening values of our three clusters have been compared to ones derived from the dust maps of Schlegel, Finkbeiner & Davis (1998; hereafter, SFD); these are based on the COBE/DIRBE and IRAS/ISSA maps, and take into account the dust absorption all the way to infinity. E(B − V )(ℓ, b)∞ values of our three clusters have been taken from SFD maps using the web pages of NED8 . These E(B − V )(ℓ, b)∞ values are 0.m 99 for Be 89, and 1.m 06 for both Ru 135 and Be 10. However, Arce & 8 http://nedwww.ipac.caltech.edu/forms/calculator. html. UBVRI PHOTOMETRY OF OPEN CLUSTERS 427 TABLE 9 FUNDAMENTAL PARAMETERS OF BE 89, RU 135, AND BE 10 (l◦ , b◦ ) E(B − V ) [mag] [Fe/H] [dex] Z (V0 − MV ) [mag] d [kpc] log(A) Isochrone RGC [kpc] Reference Be 89 83.16, +4.82 0.60 1.03 1.05 −0.35 − − +0.008 solar solar 11.90 12.40 11.54 2.40 3.00 2.04 9.58 8.93 9.02 m8† b4 g0 8.55 − − this work Tadross 2008a Subramaniam et al. 2010 Ru 135 16.42, +6.23 0.63 1.10 −0.71 − +0.004 solar 9.58 11.33 0.81 1.85 9.58 8.70 m8 b4 7.72 − this work Tadross 2008b 138.62, +8.88 0.75 0.87 0.71 −0.49 − − +0.006 +0.008 solar 11.16 11.80 11.26 1.70 2.30 1.79 9.06 8.80 9.00 m8 g2 B4 9.84 − − this work Lata et al. 2004 MN07 Cluster Be 10 © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México † Isochrone sources: B4 = Bertelli et al. (1994); b4 = Bonatto et al. (2004); g0 = GBBC; g2 = Girardi et al. (2002); m8 = MGBG. Goodman (1999) caution that SFD reddening maps overestimate the reddening values when the color excess E(B − V ) is more than ≈ 0.m 15. For the revision of SFD reddening estimates, the equations of Bonifacio, Monai & Beers (2000) and Schuster et al. (2004) have been adopted. Then the final reddening, E(B − V )A , for a given star is reduced compared to the total reddening E(B − V )(ℓ, b)∞ by a factor {1 − exp[−d sin |b|/H]}, where b, d, and H are the Galactic latitude (Column 2 of Table 9), the distance from the observer to the object (Column 7 of Table 9), and the scale height of the dust layer in the Galaxy, respectively; here we have assumed H = 125 pc (Bonifacio et al. 2000). Note that Galactic latitudes of our three clusters are less than 10◦ . These reduced final reddenings are E(B − V )A = 0.m 54 for Be 89, 0.m 36 for Ru 135, and 0.m 64 for Be 10. For Be 89, our reddening value of 0.m 60 is in good agreement with the value of 0.m 54 obtained from the dust maps of SFD. For Be 10 our reddening value of E(B − V ) = 0.m 75 is within about 1σ of the value 0.m 64 derived from the SFD dust maps, and for Ru 135, our reddening value of 0.m 63 differs by about 2σ from the value of 0.m 36 obtained from these SFD maps. These reddening values derived by different methods are in reasonable agreement with each other, giving confidence to our results. As can be seen from the summarized results given in Table 9, the reddening value 0.m 60 found here for Be 89 is smaller than the E(B − V ) = 1.m 03 of Tadross (2008a; hereafter T08a), and than the E(B − V ) = 1.m 05 of Subramaniam, Carraro, & Janes (2010, hereafter S10). Our derived distance modulus and distance for Be 89, [(V0 − MV ), d(kpc)] = (11.m 90±0.m 06, 2.4±0.06), are smaller than the values of (12.m 39, 3.00) of T08a and larger than the (11.m 54, 2.04) of S10. Our inferred age [log(A), A(Gyr)] = (9.58, 3.8 Gyr) for this cluster is considerably older than (8.93, 0.85 Gyr) given by T08a and larger than the estimate (9.02, 1.06 Gyr) by S10. For the analysis of Be 89, T08a used JHK photometry and the isochrones of Bonatto, Bica, & Girardi (2004) with a solar metallicity. This is, partially, the origin of the disagreement between the two age estimates, since our lower metallicity for Be 89 will necessarily lead to a larger age for a given TO. Also, most probably, the differences are partially due to the different procedural approaches for estimating the fundamental parameters; we derive in a straightforward manner the estimates for the interstellar extinction and metallicity: by fitting SK82’s ZAMS to the data in the (U − B, B − V ) diagram, by then measuring the ultraviolet excess of the F-type stars to derive a cluster metallicity, and finally using the appropriate isochrones in CM diagrams to estimate the true distance modulus and age of Be 89. Two parameters (reddening and metallicity) are estimated in a CC diagram separately from the other two parameters (distance and age) from the CM diagrams. S10 have also assumed a solar metallicity (Z⊙ ) for their isochrones (from GBBC) and have used only CM diagrams to estimate the reddening, distance, and age of Be 89. Previous results in the literature for Ru 135 are found in the work by Tadross (2008b; hereafter T08b), and for Be 10 in the papers by Lata et al. (2004; L04) and Maciejewski & Niedzielski (2007; MN07). Our reddening value E(B − V ) = 0.m 63 ± 0.m 12 for Ru 135 is significantly smaller compared to the reddening value of 1.m 10 given by T08b. Also, our derived distance modulus and distance, [(V0 − MV ), d(kpc)] = (9.m 58, 0.81), for Ru 135 are significantly smaller than (11.m 33, 1.85), and our inferred age [log(A), A] = (9.58, 3.80 Gyr) is considerably older than (8.70, 0.50 Gyr), values by T08b. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México 428 AKKAYA ET AL. In defense of the present results, our value for E(B − V ) (0.m 63) falls between the value derived from SFD (0.m 36) and the value of T08b (1.m 10); our value is in much better agreement with SFD. T08b used the solar-metallicity isochrones of Bonatto et al. (2004), and his results are based on the comparison of isochrones to observed data in the J, (J − H) and K, (J −K) planes of infrared photometry. These differences between our values and those of T08b are probably due mainly to the largely different values for the interstellar reddening, but also to the difference in the assumed metallicities, to the use of different stellar models and isochrone sets, which make use of differing input physics and colour-temperature transformations, and to distinct photometric data sets. For the Be 10 open cluster, our reddening value E(B − V ) = 0.m 75 is in reasonable agreement with the value of E(B − V ) = 0.m 87 given by L04, and in good agreement with E(B − V ) = 0.m 71 by MN07. For the metallicity of the Be 10 cluster, L04 adopt the Z = +0.008 isochrones of Girardi et al. (2002), and MN07 adopt the solar isochrones of Bertelli et al. (1994). From our two-color diagram, Z = +0.006 has been derived (see § 3.3), which is in agreement, within the error bars, with the value of L04. Our distance modulus and distance for Be 10, [(V0 − MV ), d(kpc)]= (11.m 16, 1.70) differ from the values (11.m 8, 2.3) of L04, but very little from the values of MN07, (11.m 26, 1.79). Our inferred age [log(A), A] = (9.06, 1.08 Gyr) for this cluster disagrees by almost a factor of two (0.5 Gyr) with L04, but is in good agreement with MN07, (9.00, 1.00 Gyr). Again, our interstellar reddening for Be 10, E(B − V ) = 0.m 75 falls between the value derived from SFD (0.m 64) and the value 0.m 87 by L04. The age values in Table 9 have been compared to ages estimated with the (age, ∆V ) calibration given by Carraro & Chiosi (1994; their equation 3). Note that this last calibration does not consider the metal abundance of the cluster. Here, ∆V means the magnitude difference between the RC and TO, which is well known as an age indicator. Both open clusters Be 89 and Be 10 have RC candidates (see the CM plots for these two clusters, Figures 3–4, and Figures 9–10, respectively). TO values occur at V ≈ 16.m 5 for Be 89 and V ≈ 14.m 8 for Be 10, whereas the RCs occur at V ≈ 15.m 3 and V ≈ 14.m 7, respectively. From this age-∆V calibration of Carraro & Chiosi (1994), ages have been estimated as log(A) = 9.1 (1.3 Gyr) for Be 89 and log(A) = 8.6 (0.4 Gyr) for the Be 10. The average age values given by us, log(A) = 9.58 (3.8 Gyr) for Be 89 and log(A) = 9.06 (1.08 Gyr) for Be 10 are somewhat older than the ones estimated from this relation of Carraro & Chiosi (1994). However, these age differences are at least partially explained by the sub-solar metallicities of these two clusters ([Fe/H]= −0.35 dex for Be 89 and −0.49 dex for Be 10; see § 3.1, § 3.3, and Table 9). Lower metallicities require larger ages for the same TO. In Table 9 our results are summarized for Be 89, Ru 135, and Be 10: Columns 1 and 2 contain the cluster name and Galactic coordinates, respectively. The resulting reddening, E(B − V ), is given in Column 3. The metallicity and heavy-element abundances, [Fe/H] and (Z), are given in Columns 4 and 5, respectively. True distance modulus values, (V0 − MV ), and their corresponding heliocentric distances to the observer are given in Columns 6 and 7, respectively. Column 8 gives the average age (i.e., log(A); where A is in years), as derived from the five CM diagrams. Different isochrones used by us and by other authors are referenced in Column 9. Average Galactocentric distances are listed in Column 10. The corresponding references from the literature are listed in Column 11. 5. CONCLUSIONS CCD UBVRI photometry of three poorly studied Galactic open clusters, Be 89, Ru 135, and Be 10, has been analyzed, based on new SPM observations. The fundamental parameters of reddening, metallicity, age, and distance of these open clusters have been inferred and presented in Tables 7–9. The interstellar reddenings and metallicities of these three clusters have been determined from twocolor, (U − B, B − V ), diagrams prior to the use of the CM diagrams. Heavy element abundances, Z, of the three clusters have been found from the ultraviolet excess, δ(U − B), of the F-stars by comparison with the two-color curve of SK82 (ZSK82 = Z⊙ ), by using the normalizations of Sandage (1969), and by applying the calibration, [Fe/H]-δ(0.6), of Karataş & Schuster (2006), with the advantage of reducing by two the number of free parameters of the isochrones when fitting to the data in the CM diagrams. When necessary, we have iterated slightly afterwards for a better, more consistent, solution for the four cluster parameters (reddening, metallicity, distance, and age). Deeper U frames would improve our determinations employing this method, which allows us to estimate the reddening and metallicity independently using a CC diagram, in contrast to the exclusive fitting of isochrones to CM diagrams and the use UBVRI PHOTOMETRY OF OPEN CLUSTERS of the solar metallicity, which are the more common techniques used in the literature. © Copyright 2010: Instituto de Astronomía, Universidad Nacional Autónoma de México The present adjustments of the SK82, CC relations to the MS and RC stars, and of the MGBG isochrones to MS, TO, and RC stars in the CM diagrams show good consistency and appropriate fits for all three open clusters, in the one CC diagram and all five CM diagrams. Good consistency is seen in the Figures 2–4 for Be 89, Figures 5–7 for Ru 135, and Figures 8–10 for Be 10. The CC and CM diagrams of Be 89 and Ru 135 suggest that they are metal-poor and old for their location in the Galaxy, compared to other open clusters. For Be 89, stars with V < 16.m 2 and (B − V ) ≤ 0. 9 are most likely foreground or blue-straggler stars. The blue-straggler and RC candidates in the field of Be 89 need spectroscopic and/or astrometric observations to test their cluster membership and to elucidate their nature. m Similar candidates for blue-straggler or bright foreground stars are seen in the CC and CM diagrams of Ru 135 and Be 10, Figures 5–7 and 8–10, respectively. In the case of Ru 135 and for stars with V fainter than about 14.m 2, the onset of the cluster sequence in the CM diagrams is clearly seen. Objects brighter than this limit and with (B − V ) ≤ 0.m 9 are probably blue stragglers or bright foreground stars. Despite its similar age to Be 89, no RC stars are noticeable in the CM diagrams of Ru 135. On the other hand, the CC and CM diagrams of Be 10 show clear evidence for an RC grouping, although it is somewhat younger than the other two clusters. The lack of any RC stars in the CM diagrams of Ru 135, contrasting with Be 89 and Be 10, may result either from relative differences in mass segregation and our emphasis on the inner regions of these clusters, or from the poorness of these cluster fields and smallnumber statistics. Ru 135, being closer to the Galactic center, may be more perturbed and less dynamically relaxed than the other two clusters. Also, Be 89 and Be 10 each show only eight, or fewer, RC candidate stars, and it is not clear that all of these are in fact cluster members. For the typical accuracy of photometric observations (and we are no exception), the final error estimates are fixed by the accuracy of the cluster parameters as given by the systematic uncertainties in the absolute-magnitude, intrinsic-color, and reddeningvector calibrations, for example, the adequacies, or not, of the SK82 colors, the MGBG isochrones, and the standard interstellar-reddening curve. 429 Finally, further radial velocity and proper motion information for these clusters will allow us to clean with more assurance most non-members from the CC and CM diagrams in order to obtain better determinations of their physical parameters and to better understand the nature of the blue-straggler and red-clump candidates in these three open clusters. Deeper photometric observations, especially in the U and B bands, will provide clearer, cleaner, and more precise solutions from the CC diagram. This work was supported by the Conacyt projects 33940, 45014, 49434 and PAPIIT-Universidad Nacional Autónoma de México IN111500 (Mexico). İA acknowledges a grant from the Mexican Government (Secretarı́a de Relaciones Exteriores). YK acknowledges financial support of the Scientific and Technical Research Council of Turkey (TUBITAK, BIDEB2219). This research made use of the WEBDA open cluster database of J.-C. Mermilliod. We also thank an anonymous referee for valuable suggestions and comments that helped improve this work substantially. REFERENCES Arce, H. G., & Goodman, A. A. 1999, ApJ, 512, L135 Bertelli, G., Bressan, A., Chiosi, C., Fagotto, F., & Nasi, E. 1994, A&AS, 106, 275 Bertelli, G., Girardi, L., Marigo, P., & Nasi, E. 2008, A&A, 484, 815 Bevington, P. R., & Robinson, D. K. 2003, Data Reduction and Error Analysis for the Physical Sciences (3th ed.; Boston: McGraw-Hill) Binney, J., & Merrifield, M. 1998, Galactic Astronomy (Princeton: Princeton Univ. 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Ibraheem L A D I Amosa
تمهید إنَّ الـحَمْدَ لِلّهِ نَـحْمَدُهُ وَنَسْتَعِيْنُهُ وَنَسْتَغْفِرُهُ، وَنَعُوذُ بِاللهِ مِنْ شُرُورِ أَنْفُسِنَا وَمِنْ سَيِّئَاتِ أَعْمَالِنَا، مَنْ يَهْدِهِ اللهُ فَلَا مُضِلَّ لَهُ، وَمَنْ يُضْلِلْ فَلَا هَادِيَ لَهُ، وَأَشْهَدُ أَن لاَّ إِلَهَ إِلاَّ الله وَحْدَهُ لَا شَرِيْكَ لَهُ وَأَشْهَدُ أَنَّ مُـحَمَّداً عَبْدُهُ وَرَسُولُه. o يَا أَيُّهَا الَّذِينَ آمَنُوا اتَّقُوا اللَّهَ حَقَّ تُقَاتِهِ وَلَا تَمُوتُنَّ إِلَّا وَأَنْتُمْ مُسْلِمُونَ o يَا أَيُّهَا النَّاسُ اتَّقُوا رَبَّكُمُ الَّذِي خَلَقَكُمْ مِنْ نَفْسٍ وَاحِدَةٍ وَخَلَقَ مِنْهَا زَوْجَهَا وَبَثَّ مِنْهُمَا رِجَالًا كَثِيرًا وَنِسَاءً وَاتَّقُوا اللَّهَ الَّذِي تَسَاءَلُونَ بِهِ وَالْأَرْحَامَ إِنَّ اللَّهَ كَانَ عَلَيْكُمْ رَقِيبًا o يَا أَيُّهَا الَّذِينَ آمَنُوا اتَّقُوا اللَّهَ وَقُولُوا قَوْلًا سَدِيدًا يُصْلِحْ لَكُمْ أَعْمَالَكُمْ وَيَغْفِرْ لَكُمْ ذُنُوبَكُمْ وَمَنْ يُطِعِ اللَّهَ وَرَسُولَهُ فَقَدْ فَازَ فَوْزًا عَظِيمًا إِنَّ أَصْدَقَ الْحَدِيثِ كِتَابُ اللَّهِ وَأَحْسَنَ الْهَدْىِ هَدْىُ مُحَمَّدٍ ﷺ وَشَرَّ الأُمُورِ مُحْدَثَاتُهَا وَكُلَّ مُحْدَثَةٍ بِدْعَةٌ وَكُلَّ بِدْعَةٍ ضَلاَلَةٌ وَكُلَّ ضَلاَلَةٍ فِي النَّارِ أَمَّا بَعْدُ، تُقَدِّمُ هَذِهِ الْجَلْسَةُ شَرْحًا لِلنُّصُوصِ الدِّينِيَّةِ لِطَالِبِي الْعِلْمِ. قَدْ لَا يُلَاحِظُ الْمَرْءُ الْعَمَلَ الشَّاقَّ الَّذِي قَامَ بِهِ الْعُلَمَاءُ مُنْذُ قُرُونٍ لِضَمَانِ بَقَاءِ تَعَالِيمِ الْإِسْلَامِ أَصِيلَةً وَأَصِيلَةً. وَمِنْ هَؤُلَاءِ الْعُلَمَاءِ الَّذِينَ وَرَّثُوا النَّبِيَّ: عُلَمَاءَ الْحَدِيثِ .عُلَمَاءُ الْحَدِيثِ مِنْ أَعْلَامِ أُمَّتِنَا، تَفَرَّغُوا لِثَانِي أَشْرَفِ عِلْمِ بَعْدَ الْقُرْآنِ الْكَرِيمِ، وَهُوَ سُنَّةُ النَّبِيِّ الْكَرِيمِ بِالدِّرَاسَةِ وَالشَّرْحِ، مِمَّا سَهَّلَ عَلَى الْمُسْلِمِينَ مَعْرِفَتَهُمْ بِرَبِّهِمْ وَسَاعَدَهُمْ عَلَى الْعَمَلِ بِالْإِسْلَامِ. حَصَرَ عُلَمَاءُ الْحَدِيثِ مِنْ لَدُنِ الصَّحَابَةِ إِلَى زَمَانِنَا هَذَا وَعَدَّهُمْ شَيْءٌ لَا قِبَلَ لِأَحَدٍ بِهِ، وَلَكِنْ يُمْكِنُنَا الْإِشَارَةُ إِلَى أَبْرَزِ عُلَمَاءِ الْحَدِيثِ عَلَى مَرِّ الْعُصُورِ : فَمِمَّنْ كَانَتْ لَهُ عِنَايَةٌ ظَاهِرَةٌ بِالْحَدِيثِ وَرِوَايَتُهُ مِنْ الصَّحَابَةِ الْخُلَفَاءِ الرَّاشِدُونَ الْأَرْبَعَةُ ، ثُمَّ أَبُو هُرَيْرَةَ سَيِّدُ الْحُفَّاظِ ، وَعَبْدُ اللَّهِ بْنُ عَمْرِو بْنِ الْعَاصِ ، وَمُعَاذُ بْنُ جَبَلٍ أَعْلَمُ الْأُمَّةِ بِالْحَلَالِ وَالْحَرَامِ ، وَأُبَيُّ بْنُ كَعْبٍ ، وَأَبُو عُبَيْدَةَ بْنُ الْجَرَّاحِ، وَعَبْدُ اللَّهِ بْنُ مَسْعُودٍ ، وَعَبْدُ اللَّهِ بْنُ عُمَرَ ، وَعَبْدُ اللَّهِ بْنُ عَبَّاسٍ ، وَأَبُو سَعِيدٍ الْخُدْرِيُّ ، وَأَنَسُ بْنُ مَالِكٍ ، وَجَابِرُ بْنُ وَجَابِرِ بْنِ عَبْدِ اللَّهِ ، وَعَائِشَةُ ، وَأُمُّ سَلَمَةَ وَغَيْرُهُمْ رَضِيَ اللَّهُ عَنْهُمْ . ثُمَّ مِنْ طَبَقَةِ التَّابِعِينَ سَعِيدُ بْنُ الْمُسَيِّبِ ، وَالْحَسَنُ الْبَصْرِيُّ ، وَمُحَمَّدُ بْنُ سِيرِينَ ، وَعِكْرِمَةُ ، وَنَافِعٌ ، وَأَبُو سَلَمَةَ بْنُ عَبْدِ الرَّحْمَنِ ، وَسَالِمُ بْنُ عَبْدِ اللَّهِ بْنِ عُمَرَ ، وَخَارِجَةُ بْنُ زَيْدٍ ، وَالْقَاسِمُ بْنُ مُحَمَّدٍ ، وَعُرْوَةُ بْنُ الزُّبَيْرِ ، وَبَكْرُ بْنُ عَبْدِ اللَّهِ الْمُزَنِيّ ، وَسُلَيْمَانُ بْنُ يَسَارٍ ، وَطَاوُوسٌ ، وَعَبْدُ اللَّهِ بْنُ شَقِيقٍ ، وَالزُّهْرِيُّ ، وَإِبْرَاهِيمُ النَّخَعِيُّ ، وَعُمَرُ بْنُ عَبْدِ الْعَزِيزِ . ثُمَّ عُلَمَاءُ الْحَدِيثِ مِنْ أَتْبَاعِ التَّابِعِينَ الَّذِينَ كَانَ لَهُمْ بَصَرٌ بِهِ وَهُمْ فِي الْجُمْلَةِ أَوَّلُ مَنْ نَظَرَ فِي الْإِسْنَادِ وَتَكَلَّمَ عَنْ أَحْوَالِ الرُّوَاةِ ، فَمِنْهُمْ مَالِكُ بْنُ أَنَسٍ ، وَشُعْبَةُ بْنُ الْحَجَّاجِ ، وَأَبُو إِسْحَاقَ الْفَزَارِيُّ ، وَالْأَوْزَاعِيُّ ، وَالْأَعْمَشُ ، وَمَعْمَرُ بْنُ رَاشِدٍ ، وَعَبْدُ اللَّهِ بْنُ الْمُبَارَكِ ، وَغَيْرُهُمْ . وَجَابِرُ بْنُ وَجَابِرِ بْنِ عَبْدِ اللَّهِ ، وَعَائِشَةُ ، وَأُمُّ سَلَمَةَ وَغَيْرُهُمْ رَضِيَ اللَّهُ عَنْهُمْ . ثُمَّ مِنْ طَبَقَةِ التَّابِعِينَ سَعِيدُ بْنُ الْمُسَيِّبِ ، وَالْحَسَنُ الْبَصْرِيُّ ، وَمُحَمَّدُ بْنُ سِيرِينَ ، وَعِكْرِمَةُ ، وَنَافِعٌ ، وَأَبُو سَلَمَةَ بْنُ عَبْدِ الرَّحْمَنِ ، وَسَالِمُ بْنُ عَبْدِ اللَّهِ بْنِ عُمَرَ ، وَخَارِجَةُ بْنُ زَيْدٍ ، وَالْقَاسِمُ بْنُ مُحَمَّدٍ ، وَعُرْوَةُ بْنُ الزُّبَيْرِ ، وَبَكْرُ بْنُ عَبْدِ اللَّهِ الْمُزَنِيّ ، وَسُلَيْمَانُ بْنُ يَسَارٍ ، وَطَاوُوسٌ ، وَعَبْدُ اللَّهِ بْنُ شَقِيقٍ ، وَالزُّهْرِيُّ ، وَإِبْرَاهِيمُ النَّخَعِيُّ ، وَعُمَرُ بْنُ عَبْدِ الْعَزِيزِ . ثُمَّ عُلَمَاءُ الْحَدِيثِ مِنْ أَتْبَاعِ التَّابِعِينَ الَّذِينَ كَانَ لَهُمْ بَصَرٌ بِهِ وَهُمْ فِي الْجُمْلَةِ أَوَّلُ مَنْ نَظَرَ فِي الْإِسْنَادِ وَتَكَلَّمَ عَنْ أَحْوَالِ الرُّوَاةِ ، فَمِنْهُمْ مَالِكُ بْنُ أَنَسٍ ، وَشُعْبَةُ بْنُ الْحَجَّاجِ ، وَأَبُو إِسْحَاقَ الْفَزَارِيُّ ، وَالْأَوْزَاعِيُّ ، وَالْأَعْمَشُ ، وَمَعْمَرُ بْنُ رَاشِدٍ ، وَعَبْدُ اللَّهِ بْنُ الْمُبَارَكِ ، وَغَيْرُهُمْ . ثُمَّ مَنْ أَخَذَ عَنْ هَؤُلَاءِ مِنْ أَئِمَّةِ الْحَدِيثِ وَعُلَمَاءِ الْجَرْحِ وَالتَّعْدِيلِ كَيَحْيَى بْنِ سَعِيدٍ ، وَعَبْدِ الرَّحْمَنِ بْنِ مَهْدِيٍّ ، وَالشَّافِعِيِّ ، وَأَحْمَدَ بْنِ حَنْبَلٍ. وَعَلِيُّ بْنُ الْمَدِينِيِّ ، وَيَحْيَى بْنُ مَعِينٍ ، وَإِسْحَاقُ بْنُ رَاهْوَيْهِ ، وَأَبُو عُبَيْدٍ ، وَنُعَيْمُ بْنُ حَمَّادٍ ، وَهَنَّادُ بْنُ السَّرِيِّ ، وَعَمْرُو بْنُ عَلِيٍّ الْفَلَّاسُ . ثُمَّ الْبُخَارِيُّ ، وَمُسْلِمٌ ، وَأَبُو دَاوُد ، وَالنَّسَائِيُّ ، وَالتِّرْمِذِيُّ ، وَابْنُ مَاجَةَ ، وَالذُّهْلِيُّ ، وَالدَّارِمِيُّ ، وَأَحْمَدُ بْنُ سِنَانٍ الْقَطَّانُ ، وَأَحْمَدُ بْنُ مَنْصُورٍ الرَّمَادِيُّ ، وَحَجَّاجُ بْنُ الشَّاعِرِ ، وَإِبْرَاهِيمُ الْحَرْبِيُّ وَعَبَّاسُ الدُّورِيُّ ، وَابْنُ أَبِي خَيْثَمَةَ ، وَزَكَرِيَّا بْنُ يَحْيَى السَّاجِيُّ ، وَأَبُو حَاتِمٍ الرَّازِيّ ، وَأَبُو زُرْعَةَ الرَّازِيّ .ثُمَّ ابْنُ خُزَيْمَةَ ، وَابْنُ حِبَّانَ ، وَالْعُقَيْلِيُّ ، وَالطَّبَرَانِيُّ ، وَأَبُو سَعِيدِ بْنُ يُونُسَ ، وَابْنُ النَّجَّادِ ، وَابْنُ الْأَخْرَمِ النَّيْسَابُورِيُّ ، وَحَمْزَةُ الْكِنَانِيُّ ، وَأَبُو بَكْرٍ الْجِعَابِيُّ ، وَأَبُو بَكْرٍ الشَّافِعِيُّ ، وَأَبُو بَكْرِ بْنُ السُّنِّيِّ ، وَأَبُو أَحْمَدَ بْنُ عَدِيٍّ . ثُمَّ أَبُو الْفَتْحِ الْأَزْدِيُّ ، وَأَبُو إِسْحَاقَ الْمُسْتَمْلِي ، وَأَبُو زَيْدٍ الْمَرْوَزِيُّ ، وَأَبُو أَحْمَدَ الْجُرْجَانِيُّ ، وَأَبُو أَحْمَدَ الْحَاكِمُ ، وَأَبُو سَعِيدٍ الرَّازِيُّ ، وَأَبُو حَفْصِ بْنُ شَاهِينَ ، وَأَبُو الْحَسَنِ الدَّارَقُطْنِيُّ ، وَالْخَطِيبُ الْبَغْدَادِيُّ ، وَالْمُعَافَى بْنُ زَكَرِيَّا ، وَأَبُو عَبْدِ اللَّهِ بْنُ مَنْدَهْ .ثُمَّ أَبُو عَبْدِ اللَّهِ الْحَاكِمُ النَّيْسَابُورِيُّ ، وَأَبُو حَامِدٍ الْإِسْفَرَائِينِيُّ ، وَعَبْدُ الْغَنِيِّ الْأَزْدِيُّ ، وَأَبُو سَعْدٍ الْمَالِينِيُّ ، وَأَبُو بَكْرِ بْنُ مَرْدَويَّةَ ، وَأَبُو نُعَيْمٍ الْأَصْبَهَانِيُّ . ثُمَّ أَبُو بَكْرٍ الْبَيْهَقِيُّ ، وَأَبُو يَعْلَى الْخَلِيلِيُّ ، وَأَبُو الْفَتْحِ الرَّازِيّ ، وَأَبُو حَفْصٍ النَّيْسَابُورِيُّ ، وَأَبُو مَسْعُودٍ الْبَجَلِيُّ .ثُمَّ أَبُو طَاهِرٍ الثَّقَفِيُّ ، وَأَبُو يَعْلَى الصَّابُونِيُّ ، وَأَبُو مُحَمَّدٍ الْبَلْخِيّ ، وَابْنُ حَزْمٍ الْقُرْطُبِيُّ ، وَأَبُو نَصْرٍ الْمَوْصِلِيُّ . ثُمَّ أَبُو الْفَضْلِ النَّيْسَابُورِيُّ ، وَأَبُو إسْمَاعِيلَ الْهَرَوِيُّ ، وَأَبُو عَمْرٍو الْمُزَكَّى ، وَأَبُو إِسْحَاقَ الْحِبَّالُ وَأَبُو الْفَتْحِ الْأَصْبَهَانِيُّ ، وَأَبُو الْفَرَجِ الشِّيرَازِيُّ ، وَأَبُو الْمُظَفَّرِ السَّمْعَانِيُّ . ثُمَّ أَبُو الْحَسَنِ الْهَرَّاسِيُّ ، وَشُجَاعُ بْنُ فَارِسٍ الزُّهْرِيُّ ، وَأَبُو الْفَضْلِ الْمَقْدِسِيُّ ، وَأَبُو طَاهِرٍ الْحِنَّائِيُّ الدِّمَشْقِيُّ ، وَأَبُو يَعْلَى بْنُ الْفَرَّاءِ الْحَنْبَلِيُّ. ثُمَّ أَبُو مُحَمَّدٍ هِبَةُ اللَّهِ بْنُ سَهْلٍ النَّيْسَابُورِيُّ ، وَأَبُو مُحَمَّدٍ إسْمَاعِيلُ بْنُ عَبْدِ الرَّحْمَنِ النَّيْسَابُورِيُّ الْقَارِىءُ ، وَأَبُو الْقَاسِمِ تَمِيمُ بْنُ أَبِي سَعِيدٍ الْجُرْجَانِيُّ ، وَأَبُو مُحَمَّدٍ طَاهِرُ بْنُ سَهْلٍ الِاسْفِرَائِينِيُّ ، وَأَبُو جَعْفَرٍ مُحَمَّدُ بْنُ أَبِي عَلِيٍّ الْهَمَذَانِيُّ ، وَأَبُو مُحَمَّدٍ عَبْدُ الْحَقِّ الْغِرْنَاطِيُّ . ثُمَّ أَبُو مَسْعُودٍ الْأَصْبَهَانِيُّ ، وَأَبُو الْفُتُوحِ الْهَمَذَانِيُّ ، وَأَبُو الْمُظَفَّرِ التُّرِيكِيُّ الْعَبَّاسِيُّ ، وَأَبُو الْعَلَاءِ الْعَطَّارُ. ثُمَّ ابْنُ بَشْكُوَالَ الْقُرْطُبِيُّ ، وَأَبُو الْفَضْلِ الطُّوسِيُّ ، وَقُطْبُ الدِّينِ النَّيْسَابُورِيُّ ، وَأَبُو مُحَمَّدٍ الْأَزْدِيُّ .ثُمَّ مُوَفَّقُ الدِّينِ بْنُ قُدَامَةَ ، وَأَبُو الْبَرَكَاتِ السَّعْدِيُّ ، وَأَبُو الطَّاهِرِ الْأَنْمَاطِيُّ ، وَأَبُو طَالِبٍ الْوَاسِطِيُّ وَابْنُ الصَّلَاحِ ، وَالنَّوَوِيُّ .ثُمَّ ابْنُ تَيْمِيَّةَ ، وَابْنُ الْقَيِّمِ ، وَالْمِزِّيُّ ، وَابْنُ عَبْدِ الْهَادِي ، وَابْنُ كَثِيرٍ. ثُمَّ الْعِرَاقِيُّ ، وَالْهَيْثَمِيُّ ، وَابْنُ حَجَرٍ الْعَسْقَلَانِيُّ ، وَالسَّخَاوِيُّ ، وَالسُّيُوطِيُّ . ثُمَّ حَصَلَتْ نُدْرَةٌ وَاضِحَةٌ فِي عُلَمَاءِ الْحَدِيثِ خَاصَّةً ، وَكَانَ مِنْ أَبْرَزِهِمْ فِي الْعُصُورِ الْمُتَأَخِّرَةِ الْمُبَارَكِفُورِيُّ ، وَالسِّنْدِيُّ ، وَجَمَالُ الدِّينِ الْقَاسِمِيُّ ، وَإِسْمَاعِيلُ بْنُ مُحَمَّدٍ الْعَجْلُونِي . ثُمَّ أَحْمَدُ شَاكِرٍ ، وَالْأَلْبَانِيُّ ، وَعَبْدُ الْعَزِيزِ بْنُ بَازٍ ، وَمُقْبِلُ بْنُ هَادِي الْوَادِعِيُّ . هَذِهِ الْجَلْسَةُ هِيَ رِحْلَةٌ لِلْمُسْلِمِينَ فِي تَقْدِيرِ وَفَهْمِ هَذَا الْجَانِبِ الثَّرِيِّ وَالْفَرِيدِ مِنْ الْعَقِيدَةِ الْإِسْلَامِيَّةِ. وَأَيْضًا ، تَمَّ شَرْحُ كُلِّ حَدِيثٍ فِي هَذَا الْمُجَلَّدِ وَسُرِدَتْ سِيرَةٌ مُخْتَصَرَةٌ لِرُوَاةِ قَبْلَ الْأَسْئِلَةِ وَالْأَجْوِبَةِ فِي كُلِّ صَبَاحٍ أَحَدٍ فِي كِنْكِيرِي، وَيْلَارِي، كُمْبُوتْسُو، كَنُو نَيْجِيرِيَا. وَتَشْمَلُ الْمَوَادُّ الْمُسْتَخْدَمَةُ كُتُبًا لِلشَّيْخِ مُحَمَّدِ نَاصِرِ الدِّينِ الْأَلْبَانِيِّ وَشُرُوحًا مَأْخُوذَةً مِنْ مَوْقِعِ الدُّرَرِ السُّنِّيَّةِ وَأُخْرَى مَعَ تَعْدِيلَاتٍ. وَأَسْأَلُ اللَّهَ أَنْ يَجْعَلَنَا مِنَ الّمُتَمَسِّكِينَ بِالسُّنَّةِ الْعَامِلِينَ بِهَا، وَ أَنْ يُلْهَمَنَا الْهُدَى وَالرُّشْدَ، وَالتَّوْفِيقَ والسَّدَادَ. وَأَنْ يَغْفِرَلَنَا وَلِوَالِدَيْنَا وَلِلْمُسْلِمِينَ، وَصَلَّى اللَّهُ عَلَى نَبِيِّنَا مُحَمَّدِ وَعَلَى آلِهِ وَصَحْبِهِ أَجْمَعِينَ جَمْعُ وَإِعْدَادُ: إبراهيم أبوبكر أمسا المعلمي
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Comunicación y salud, un campo emergente en Latinoamérica
Revista Comunicación UPB, 2021
Revista Comunicación UPB
Reseña crítica del libro Comunicación y salud en América Latina: contribuciones al campo, editado por Mónica Petracci y Janet García.
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Cognitive Science of Religion
Encyclopedia of Psychology and Religion, 2016
Dimitris Xygalatas
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I CAMPI FLEGREI E LA LEGGENDA DEL MONTE BARBARO
ArcheoMedia. L'archeologia on line, 2023
giuseppe pipino
THE PHLEGRAEAN FIELDS AND THE MEDIEVAL LEGEND OF MONTE BARBARO Monte Barbaro is the highest (331 m) of the Campi Flegrei volcanic hills, and corresponds to the Mons Gaurus celebrated by Latin authors. It is the residual southern part of a volcanic cone, having other slightly less elevated parts, which overall today is referred to as the Gauro crater or volcano. A widespread medieval legend indicates Monte Barbaro as the entrance to the center of the earth, visited by Virgil, and rich in treasures. Throughout the area there are ancient excavations and tunnels, used in Roman times as communication routes, for aqueducts or for the research and collection of underground thermal sources, which may have contributed to the legend, also taking into account that within the crater remains of Roman buildings have been recognized.
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Inteligencia de Negocios
Darwin Ocasal Jara
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Modelling strain localization in Ti–6Al–4V at high loading rate: a phenomenological approach
Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences, 2019
Vadim Silberschmidt
A phenomenological approach, based on a combination of a damage mechanism and a crystal plasticity model, is proposed to model a process of strain localization in Ti–6AI–4V at a high strain rate of 10 3  s −1 . The proposed model is first calibrated employing a three-dimensional representative volume element model. The calibrated parameters are then employed to investigate the process of onset of strain localization in the studied material. A suitable mesh size is chosen for the proposed model by implementing a mesh-sensitivity study. The influence of boundary conditions on the initiation of the strain localization is also studied. A variation of crystallographic orientation in the studied material after the deformation process is characterized, based on results for different boundary conditions. The study reveals that the boundary conditions significantly influence the formation of shear bands as well as the variation of crystallographic orientation in the studied material. Results...
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Stand up comedy
Febrian Wardoyo
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V. Gasparini, "'I will not be thirsty. My lips will not be dry'. Individual strategies of re-constructing the afterlife in the Isiac cults", in K. Waldner, R.L. Gordon, W. Spickermann (eds.), Burial rituals, ideas of afterlife, and the individual […] (PAwB LVII), Stuttgart 2016, pp. 125-150.
Valentino Gasparini
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What Is the Minimum Clinically Important Change in Negative Symptoms of Schizophrenia? PANSS Based Post-hoc Analyses of a Phase III Clinical Trial
Frontiers in Psychiatry
György Németh
IntroductionMinimum clinically important difference (MCID) is a measure that defines the minimum amount of change in an objective score of a clinical test that must be reached for that change to be clinically noticeable. We aimed to find the MCID for patients with predominantly negative symptoms of schizophrenia at its earliest occurrence.MethodsData of a 26-week long, double-blind study with 454 patients [Positive and Negative Symptom Scale Negative Factor Score (PANSS-FSNS) ≥24, Positive and Negative Symptom Scale Positive Factor Score (PANSS-FSPS) ≤ 19] treated with cariprazine 4.5 mg/d or risperidone 4 mg/d were analyzed. The Clinical Global Impression—Improvement scale was used to quantify minimum improvement (CGI-I = 3) and no clinical change (CGI-I = 4) on the PANSS-FSNS, and the MCID was estimated with the following methods: as the mean PANSS-FSNS changes corresponding to the first instance of minimal improvement across all visits (MCID1); as the difference between the PANSS...
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A comparison of the gene expression profiles of CRL-1807 colonocytes exposed to endogenous AAPH-generated peroxides and exogenous peroxides from heated oil
Redox Report, 2007
Joseph Lunec
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如何办理加拿大Queen’s毕业证 | 一比一原版Queen’s录取通知书
一比一原版(NYU毕业证书 NYU毕业证如何办理
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Real-time monitoring of water level and storage dynamics of irrigation tank using IoT
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Krishnaveni Muthiah
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Molecular characterization and identification of SNPs in ATP1A1 isoform of sodium-phosphate adenosine triphosphatase across diverse breeds of riverine buffaloes (Bubalus bubalis) and Indian native cattle (Bos indicus): A plausible candidate gene for heat tolerance
The Indian Journal of Animal Sciences
Monika Sodhi
In the present study, efforts were made to sequence characterize the selected exonic region (18–21) of ATP1A1 gene to identify variations/SNPs in different breeds of Indian riverine buffaloes and native cattle. The sequence characterization of selected intronic/exonic region (17–21) of ATP1A1 gene was carried out in a total of 120 samples which included 6 animals each of 8 buffalo breeds and 72 animals of 12 cattle breeds. Genomic DNA was extracted from the whole blood by enzymatic digestion using proteinase K using phenol:chloroform method.. Three sets of primers were designed using Primer3 software to amplify genomic region from intron 17 to intron 21 of ATP1A1 gene in both cattle and buffaloes. The amplified products were purified by enzymatic method and purified PCR products were sequenced using forward primers in an ABI 3100 Automated DNA Sequencer. The chromatogram of each sequence obtained was checked manually. Base calling was performed with Phred and contig assembly was...
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