Using the Gaia DR3 data sets, this work gives an analysis of nine open clusters: Dolidze 25, Kron... more Using the Gaia DR3 data sets, this work gives an analysis of nine open clusters: Dolidze 25, Kronberger 13, Kronberger 18, Majaess 99, NGC 7795, Ruprecht 139, Teutsch 55, S1, and FSR 0596, which are close to the Galactic plane of the Milky Way. The number of probable cluster members is found to be 81, 77, 120, 155, 108, 110, 160, and 116 respectively. Radii are determined as 5.40, 5.25, 4.80, 4.20, 4.28, 3.70, 4.30, 4.30, and 3.53 arcmin, respectively. With solar metallicity isochrones log ages of 7.70, 9.00, 8.35, 7.50, 9.00, 8.00, 7.50, 8.50, and 9.5 yr are determined for these clusters. The best fitting of the isochrone produced distances of 2.6, 1.27, 1.16, 1.16, 3.10, 1.64, 2.50, 2.44, and 0.98 kpc that are similar to the distances calculated from inverting median parallaxes. The mass function slopes are in agreement with the Salpeter value. The results of the total masses are found to be 116.07, 79.33, 141.24, 147.34, 145.76, 491.01, 155, 212.46, and 82.79 M☉.
Here, we conducted a photometric and astrometric study of three open stellar clusters Collinder 4... more Here, we conducted a photometric and astrometric study of three open stellar clusters Collinder 467, Dolidze 18, and Ruprecht 70, which have not been photometrically studied before. The most important thing for using Gaia (DR2) database lies in the positions, parallax, and proper motions, which make us split cluster members from the field ones and get precise astrophysical parameters. On studying the radial density profiles of the clusters under study, the actual sizes are estimated and found larger using Gaia. From the color-magnitude diagrams and theoretical isochrones, we simultaneously determined the ages, distance moduli, and reddening of the clusters. However, considering the parallaxes of Gaia (DR2) for the cluster members, we calculated the cluster distance and confirmed what we obtained from the color-magnitude diagram. Then, the Cartesian galactocentric coordinates (X, Y, Z), and the distances from the galactic center (Rg) were also estimated. According to luminosity an...
Revista Mexicana de Astronomía y Astrofísica, 2021
We present a detailed photometric and kinematical analysis of the poorly studied open cluster IC ... more We present a detailed photometric and kinematical analysis of the poorly studied open cluster IC 1434 using CCD VRI, APASS, and Gaia DR2 database for the first time. By determining the membership probability of stars we identify the 238 most probable members with a probability higher than 60%; by using proper motion and parallax data as taken from the Gaia DR2 catalog. The mean proper motion of the cluster is obtained as μx=−3.89±0.19 and μy=−3.34±0.19 mas yr−1 in both the directions of right ascension and declination. The radial distribution of member stars provides the cluster extent as 7.6 arcmin. We estimate the interstellar reddening E(B−V) as 0.34 mag using the transformation equations from the literature. We obtain the values of cluster age and distance as 631±73 Myr and 3.2±0.1 kpc.
Ground-based and Airborne Instrumentation for Astronomy VIII, 2020
The Kottamia Faint Imaging Spectro-Polarimeter (KFISP) has been recently developed, commissioned ... more The Kottamia Faint Imaging Spectro-Polarimeter (KFISP) has been recently developed, commissioned and mounted to the Cassegrain focus of the 1.88m telescope at Kottamia astronomical observatory, Egypt. The KFISP instrument demagnified the Kottamia 1.88m telescope Cassegrain focus from a f/18 with a plate scale 6.09"/mm to f/6.14 with a plate scale of 17.8"/mm. A liquid Nitrogen cooled CCD camera with a 2048×2048 pixels and 13.5-micron square pixel size is fixed to the KFISP through an integrated camera lens. In this paper we describe the camera system, performance, and its software control. As well, KFISP motion control and its software will be introduced. In addition, detailed description of the instrument performance and the results obtained from its operation will be presented.
Revista Mexicana de Astronomía y Astrofísica, 2020
We present a photometric and astrometric analysis of the NGC 2158 cluster using Gaia DR2 and 2MAS... more We present a photometric and astrometric analysis of the NGC 2158 cluster using Gaia DR2 and 2MASS data. The cluster age, color excess, intrinsic distance modulus and distance are calculated to be t = 2.240 ± 0.260 Gyr, E(B − V) = 0.420 ± 0.050 mag, (m − M)⨀ = 12.540 ± 0.130 mag and d⨀ = 3224 ± 200 pc respectively. The photometric analysis and light curve modelling of the proposed eclipsing binary member [NBN2015]78 is performed using the latest version of the Wilson-Devinney (W-D) code. The solutions show that the system is an over-contact binary with a secondary component filling its Roche lobe, with a mass ratio q = 0.262. The primary and the secondary components of the system consist of two late spectral types K1 and K2 respectively. The membership of [NBN2015]78 is discussed using two independent methods, and we find that [NBN2015]78 is an interloper and not a member of NGC 2158.
Using the Gaia DR3 data sets, this work gives an analysis of nine open clusters: Dolidze 25, Kron... more Using the Gaia DR3 data sets, this work gives an analysis of nine open clusters: Dolidze 25, Kronberger 13, Kronberger 18, Majaess 99, NGC 7795, Ruprecht 139, Teutsch 55, S1, and FSR 0596, which are close to the Galactic plane of the Milky Way. The number of probable cluster members is found to be 81, 77, 120, 155, 108, 110, 160, and 116 respectively. Radii are determined as 5.40, 5.25, 4.80, 4.20, 4.28, 3.70, 4.30, 4.30, and 3.53 arcmin, respectively. With solar metallicity isochrones log ages of 7.70, 9.00, 8.35, 7.50, 9.00, 8.00, 7.50, 8.50, and 9.5 yr are determined for these clusters. The best fitting of the isochrone produced distances of 2.6, 1.27, 1.16, 1.16, 3.10, 1.64, 2.50, 2.44, and 0.98 kpc that are similar to the distances calculated from inverting median parallaxes. The mass function slopes are in agreement with the Salpeter value. The results of the total masses are found to be 116.07, 79.33, 141.24, 147.34, 145.76, 491.01, 155, 212.46, and 82.79 M☉.
Here, we conducted a photometric and astrometric study of three open stellar clusters Collinder 4... more Here, we conducted a photometric and astrometric study of three open stellar clusters Collinder 467, Dolidze 18, and Ruprecht 70, which have not been photometrically studied before. The most important thing for using Gaia (DR2) database lies in the positions, parallax, and proper motions, which make us split cluster members from the field ones and get precise astrophysical parameters. On studying the radial density profiles of the clusters under study, the actual sizes are estimated and found larger using Gaia. From the color-magnitude diagrams and theoretical isochrones, we simultaneously determined the ages, distance moduli, and reddening of the clusters. However, considering the parallaxes of Gaia (DR2) for the cluster members, we calculated the cluster distance and confirmed what we obtained from the color-magnitude diagram. Then, the Cartesian galactocentric coordinates (X, Y, Z), and the distances from the galactic center (Rg) were also estimated. According to luminosity an...
Revista Mexicana de Astronomía y Astrofísica, 2021
We present a detailed photometric and kinematical analysis of the poorly studied open cluster IC ... more We present a detailed photometric and kinematical analysis of the poorly studied open cluster IC 1434 using CCD VRI, APASS, and Gaia DR2 database for the first time. By determining the membership probability of stars we identify the 238 most probable members with a probability higher than 60%; by using proper motion and parallax data as taken from the Gaia DR2 catalog. The mean proper motion of the cluster is obtained as μx=−3.89±0.19 and μy=−3.34±0.19 mas yr−1 in both the directions of right ascension and declination. The radial distribution of member stars provides the cluster extent as 7.6 arcmin. We estimate the interstellar reddening E(B−V) as 0.34 mag using the transformation equations from the literature. We obtain the values of cluster age and distance as 631±73 Myr and 3.2±0.1 kpc.
Ground-based and Airborne Instrumentation for Astronomy VIII, 2020
The Kottamia Faint Imaging Spectro-Polarimeter (KFISP) has been recently developed, commissioned ... more The Kottamia Faint Imaging Spectro-Polarimeter (KFISP) has been recently developed, commissioned and mounted to the Cassegrain focus of the 1.88m telescope at Kottamia astronomical observatory, Egypt. The KFISP instrument demagnified the Kottamia 1.88m telescope Cassegrain focus from a f/18 with a plate scale 6.09"/mm to f/6.14 with a plate scale of 17.8"/mm. A liquid Nitrogen cooled CCD camera with a 2048×2048 pixels and 13.5-micron square pixel size is fixed to the KFISP through an integrated camera lens. In this paper we describe the camera system, performance, and its software control. As well, KFISP motion control and its software will be introduced. In addition, detailed description of the instrument performance and the results obtained from its operation will be presented.
Revista Mexicana de Astronomía y Astrofísica, 2020
We present a photometric and astrometric analysis of the NGC 2158 cluster using Gaia DR2 and 2MAS... more We present a photometric and astrometric analysis of the NGC 2158 cluster using Gaia DR2 and 2MASS data. The cluster age, color excess, intrinsic distance modulus and distance are calculated to be t = 2.240 ± 0.260 Gyr, E(B − V) = 0.420 ± 0.050 mag, (m − M)⨀ = 12.540 ± 0.130 mag and d⨀ = 3224 ± 200 pc respectively. The photometric analysis and light curve modelling of the proposed eclipsing binary member [NBN2015]78 is performed using the latest version of the Wilson-Devinney (W-D) code. The solutions show that the system is an over-contact binary with a secondary component filling its Roche lobe, with a mass ratio q = 0.262. The primary and the secondary components of the system consist of two late spectral types K1 and K2 respectively. The membership of [NBN2015]78 is discussed using two independent methods, and we find that [NBN2015]78 is an interloper and not a member of NGC 2158.
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Papers by Y.H.M. Hendy