Matthew Malkan
University of California, Los Angeles, Physics and Astronomy, Faculty Member
We present the first robust measurement of the high redshift mass–metallicity (MZ) relation at 108 M/M 1010, obtained by stacking spectra of 83 emission-line galaxies with secure redshifts between 1.3 z 2.3. For these redshifts, infrared... more
We present the first robust measurement of the high redshift mass–metallicity (MZ) relation at 108 M/M 1010, obtained by stacking spectra of 83 emission-line galaxies with secure redshifts between 1.3 z 2.3. For these redshifts, infrared grism spectroscopy with the Hubble Space Telescope Wide Field Camera 3 is sensitive to the R23 metallicity diagnostic: ([O ii] λλ3726, 3729 + [O iii] λλ4959, 5007)/Hβ. Using spectra stacked in four mass quartiles, we find a MZ relation that declines significantly with decreasing mass, extending from 12+log(O/H) = 8.8 at M = 109.8 M, to 12+log(O/H) = 8.2 at M = 108.2M. After correcting for systematic offsets between
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Compact starburst galaxies are thought to include many or most of the galaxies from which substantial Lyman continuum emission can escape into the intergalactic medium. Li and Malkan (2018) used SDSS photometry to find a population of... more
Compact starburst galaxies are thought to include many or most of the galaxies from which substantial Lyman continuum emission can escape into the intergalactic medium. Li and Malkan (2018) used SDSS photometry to find a population of such starburst galaxies at z 0.5. They were discovered by their extremely strong [OIII]4959+5007 emission lines, which produce a clearly detectable excess brightness in the i bandpass, compared with surrounding filters. We therefore used the HST/COS spectrograph to observe two of the newly discovered i-band excess galaxies around their Lyman limits. One has strongly detected continuum below its Lyman limit, corresponding to a relative escape fraction of ionizing photons of 20+/-2 imaging, has a 2-sigma upper limit to its Lyman escape fraction of <5 the UV spectroscopy, the existing data could not distinguish these two galaxies. Although a sample of two is hardly sufficient for statistical analysis, it shows the possibility that some fraction of thes...
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We predict luminosity functions and number counts for extragalactic infrared sources at various wavelengths using the framework of our empirically based model. Comparisons of our galaxy count results with existing data indicate that... more
We predict luminosity functions and number counts for extragalactic infrared sources at various wavelengths using the framework of our empirically based model. Comparisons of our galaxy count results with existing data indicate that either galaxy luminosity evolution is not much stronger than Q=3.1, where L is proportional to (1+z)^Q, or that this evolution does not continue beyond a redshift of 2. However, a derivation of the far infrared background from COBE-DIRBE data suggests a stronger evolution for far infrared emission with Q > 4 in the redshift range beteen 0 and 1. We discuss several interpretations of these results and also discuss how future observations can reconcile this apparent conflict. We also make predictions of the redshift distributions of extragalactic infrared sources at selected flux levels which can be tested by planned detectors. Finally, we predict the fluxes at which various future surveys will become confusion limited.
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We determine the global star formation rate density at 0.7<z<1.9 using emission-line selected galaxies identified in Hubble Space Telescope Near Infrared Camera and Multi-Object Spectrograph (HST-NICMOS) grism spectroscopy... more
We determine the global star formation rate density at 0.7<z<1.9 using emission-line selected galaxies identified in Hubble Space Telescope Near Infrared Camera and Multi-Object Spectrograph (HST-NICMOS) grism spectroscopy observations. Observing in pure parallel mode throughout HST Cycles 12 and 13, our survey covers ~104 arcmin2 from which we select 80 galaxies with likely redshifted Ha emission lines. In several cases, a somewhat weaker [OIII] doublet emission is also detected. The Ha luminosity range of the emission-line galaxy sample is 4.4 x 10^41 < L(Ha) < 1.5 x 10^43 erg/s. In this range, the luminosity function is well described by a Schechter function with phi* = (4.24\pm3.55) x 10^-3 Mpc^-3, L* = (2.88\pm1.58) x 10^42 erg/s, and alpha = -1.39\pm0.43. We derive a volume-averaged star formation rate density of 0.138\pm0.058 Msun/yr/Mpc3 at z=1.4 without an extinction correction. Subdividing the redshift range, we find star formation rate densities of 0.088\pm0.0...
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We measure the evolution of the correlation between black hole mass and host spheroid velocity dispersion over the last 6 billion years, by studying three carefully selected samples of active galaxies at z=0.57, z=0.36 and z<0.1. For... more
We measure the evolution of the correlation between black hole mass and host spheroid velocity dispersion over the last 6 billion years, by studying three carefully selected samples of active galaxies at z=0.57, z=0.36 and z<0.1. For all three samples, virial black hole masses are consistently estimated using the line dispersion of Hβ and the continuum luminosity at 5100A or Halpha line luminosity, based on our cross calibration of the broad line region size-luminosity relation. For the z=0.57 sample, new stellar velocity dispersions are measured from high signal-to-noise ratio spectra obtained at the Keck Telescope, while for the two lower redshift samples they are compiled from previous works. Extending our previous result at z=0.36, we find an offset from the local relation, suggesting that for fixed M_BH, distant spheroids have on average smaller velocity dispersions than local ones. The measured offset at z=0.57 is d log sigma_*=0.12 ± 0.05± 0.06 (or d log M_BH=0.50 ± 0.22± ...
Research Interests: Physics, Organic Chemistry, Astrophysical Plasma, Black Holes, Accretion Disks, and 15 moreCosmology, Galaxy evolution, Dispersion Relation, Optical Properties, Accretion, Black Hole, Seyfert galaxies, Active Galaxies, Fundamental plane, Broad Line Region, Signal to Noise Ratio, Hubble Space Telescope Images, Physical Properties, present day, and Selective Sampling
An observation of Mrk 478 using the Chandra Low Energy Transmission Grating Spectrometer is presented. The source exhibited 30-40% flux variations on timescales of order 10000 s together with a slow decline in the spectral softness over... more
An observation of Mrk 478 using the Chandra Low Energy Transmission Grating Spectrometer is presented. The source exhibited 30-40% flux variations on timescales of order 10000 s together with a slow decline in the spectral softness over the full 80 ks observation. The 0.15--3.0 keV spectrum is well fitted by a single power law with photon index of Gamma = 2.91 +/- 0.03. Combined with high energy data from BeppoSAX, the spectrum from 0.15 to 10 keV is well fit as the sum of two power laws with Gamma = 3.03 +/- 0.04, which dominates below 2 keV and 1.4 +/- 0.2, which dominates above 2 keV (quoting 90% confidence uncertainties). No significant emission or absorption features are detected in the high resolution spectrum, supporting our previous findings using the Extreme Ultraviolet Explorer but contradicting the claims of emission lines by Hwang & Bowyer (1997). There is no evidence of a warm absorber, as found in the high resolution spectra of many Sy 1 galaxies including others class...
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A sample of 102 local (0.02 < z < 0.1) Seyfert galaxies with black hole masses MBH > 10^7 M_sun was selected from the Sloan Digital Sky Survey (SDSS) and observed using the Keck 10-m telescope to study the scaling relations... more
A sample of 102 local (0.02 < z < 0.1) Seyfert galaxies with black hole masses MBH > 10^7 M_sun was selected from the Sloan Digital Sky Survey (SDSS) and observed using the Keck 10-m telescope to study the scaling relations between MBH and host galaxy properties. We study profile changes of the broad Hbeta emission line within the 3-9 year time-frame between the two sets of spectra. The variability of the broad Hbeta emission line is of particular interest, not only since it is used to estimate MBH, but also since its strength and width is used to classify Seyfert galaxies into different types. At least some form of broad-line variability (in either width or flux) is observed in the majority ( 66 change for 38 obscuration. The broad Hbeta line virtually disappears in 3/102 ( 3 cases. We discuss potential causes for these changing-look AGNs. While similar dramatic transitions have previously been reported in the literature, either on a case-by-case basis or in larger samples...
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We have found a sample of extreme emission-line galaxies (EELGs) with strong [OIII]λ5007 emission at z ∼ 0.5. Using broadband photometric selection and requiring small uncertainties in photometry, we searched the 14th Data Release (DR14)... more
We have found a sample of extreme emission-line galaxies (EELGs) with strong [OIII]λ5007 emission at z ∼ 0.5. Using broadband photometric selection and requiring small uncertainties in photometry, we searched the 14th Data Release (DR14) of the Sloan Digital Sky Survey (SDSS) and found 2658 candidates with strong i-band excess (i - z ≤ r - i - 0.7). We further obtained 649 SDSS spectra of these objects, and visually identified 22 [OIII] emitters lying at 0.40 < z < 0.63. Having constructed their UV-IR spectral energy distributions (SED) we found that they have fairly blue r-W2 and red W1-W4 colors, indicative of strong warm dust emission. Their rest-frame [OIII]λ5007 equivalent widths are mostly 200-600 Å, and their high [OIII]λ5007/Hβ ratios put them at the boundary of star-forming galaxies and AGNs on line ratio classification diagrams. The typical E(B-V) and electron temperature of [OIII] emitters are ∼ 0.1-0.3 mag and ∼ 10^4 K, respectively. The lowest metallicity of our [...
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From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Object Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear... more
From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Object Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear luminosity, total host-galaxy luminosity and spheroid luminosity. Keck spectroscopy is used to estimate black hole mass (M_BH). We study the cosmic evolution of the M_BH-spheroid luminosity (L_sph) relation. In combination with our previous work, totaling 40 Seyfert-1 galaxies, the covered range in BH mass is substantially increased, allowing us to determine for the first time intrinsic scatter and correct evolutionary trends for selection effects. We re-analyze archival HST images of 19 local reverberation-mapped active galaxies to match the procedure adopted at intermediate redshift. Correcting spheroid luminosity for passive luminosity evolution and taking into account selection effects, we determine that at fixed present-day V-band spheroid luminosity,...
Research Interests: Physics, Organic Chemistry, Astrophysical Plasma, Black Holes, Accretion Disks, and 15 moreCosmology, Galaxy evolution, Dispersion Relation, Optical Properties, Accretion, Black Hole, Seyfert galaxies, Active Galaxies, Fundamental plane, Broad Line Region, Signal to Noise Ratio, Hubble Space Telescope Images, Physical Properties, present day, and Selective Sampling
We investigate the cosmic evolution of the black hole (BH) mass -- bulge luminosity relation using a sample of 52 active galaxies at z ∼ 0.36 and z ∼ 0.57 in the BH mass range of 10^7.4-9.1 M_. By consistently applying multi-component... more
We investigate the cosmic evolution of the black hole (BH) mass -- bulge luminosity relation using a sample of 52 active galaxies at z ∼ 0.36 and z ∼ 0.57 in the BH mass range of 10^7.4-9.1 M_. By consistently applying multi-component spectral and structural decomposition to high-quality Keck spectra and high-resolution HST images, BH masses (M_ BH) are estimated using the Hβ broad emission line combined with the 5100 Ånuclear luminosity, and bulge luminosities (L_ bul) are derived from surface photometry. Comparing the resulting M_ BH-L_ bul relation to local active galaxies and taking into account selection effects, we find evolution of the form M_ BH / L_ bul∝ (1+z)^γ with γ=1.8±0.7, consistent with BH growth preceding that of the host galaxies. Including an additional sample of 27 active galaxies with 0.5<z<1.9 taken from the literature and measured in a consistent way, we obtain γ=0.9±0.7 for the M_ BH-L_ bul relation and γ=0.4±0.5 for the M_ BH--total host galaxy luminos...
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The recent updates of the North Ecliptic Pole deep (0.5 deg 2 , NEP-Deep) multi-wavelength survey covering from X-ray to radio-wave is presented. The NEP-Deep provides us with several thousands of 15 µm or 18 µm selected sample of... more
The recent updates of the North Ecliptic Pole deep (0.5 deg 2 , NEP-Deep) multi-wavelength survey covering from X-ray to radio-wave is presented. The NEP-Deep provides us with several thousands of 15 µm or 18 µm selected sample of galaxies, which is the largest sample ever made at this wavelengths. A continuous filter coverage in the mid-infrared wavelength (7, 9, 11, 15, 18, and 24 µm) is unique and vital to diagnose the contributions from starbursts and AGNs in the galaxies out to z=2. The new goal of the project is to resolve the nature of the cosmic star formation history at the violent epoch (e.g. z=1-2), and to find a clue to understand its decline from z=1 to present universe by utilizing the unique power of the multiwavelength survey. The progress in this context is briefly mentioned.
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Compact starburst galaxies are thought to include many or most of the galaxies from which substantial Lyman continuum emission can escape into the intergalactic medium. Li and Malkan (2018) used SDSS photometry to find a population of... more
Compact starburst galaxies are thought to include many or most of the galaxies from which substantial Lyman continuum emission can escape into the intergalactic medium. Li and Malkan (2018) used SDSS photometry to find a population of such starburst galaxies at z~0.5. They were discovered by their extremely strong [OIII]4959+5007 emission lines, which produce a clearly detectable excess brightness in the i bandpass, compared with surrounding filters. We therefore used the HST/COS spectrograph to observe two of the newly discovered i-band excess galaxies around their Lyman limits. One has very strongly detected continuum below its Lyman limit, corresponding to an escape fraction of ionizing photons of 20+/-2%. The other, which is less compact in UV imaging, has a 3-sigma upper limit to its Lyman escape fraction of <5%. Before the UV spectroscopy, the existing data could hardly distinguish these two galaxies. This suggests that roughly ~half of the strong [OIII] emitters as a class...
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Until recently, it was assumed that the diffuse extragalactic background light (EBL) in the FUV has a sharp and complete cut-off at energies above the Lyman limit. However, newly discovered extreme emission line starburst galaxies (EELGs)... more
Until recently, it was assumed that the diffuse extragalactic background light (EBL) in the FUV has a sharp and complete cut-off at energies above the Lyman limit. However, newly discovered extreme emission line starburst galaxies (EELGs) and other galaxies with substantial escape fractions of EUV photons in the Lyman continuum (LyC) region are increasingly common at high redshifts. The recent observations indicate that many more LyC photons at high redshifts escape from such galaxies into intergalactic space than was previously suspected. They are probably the major cause of reionization of the intergalactic medium. In this paper we estimate the contribution of these hitherto unconsidered EUV photons from EELGs at all redshifts to the (EBL), and their subsequent effect on the absorption of extragalactic high energy $\gamma$-rays. For the more distant $\gamma$-ray sources, particularly at $z \ge 3$, the intergalactic opacity above a few GeV is significantly higher than previously es...
Research Interests: Physics and Astrophysics
The two major functions in galaxy evolution that we would like to measure are the stellar populations in galaxies, and their time-derivative, the star formation rate. Especially at redshifts above 1, both of these measures are benefiting... more
The two major functions in galaxy evolution that we would like to measure are the stellar populations in galaxies, and their time-derivative, the star formation rate. Especially at redshifts above 1, both of these measures are benefiting greatly from wide-area infrared observations. Several space-based and ground-based examples will be discussed. 1 Understanding Galaxy Evolution with Deep Fields Since this is a conference talk rather than a journal paper, I’ll start on a philosophical note. Let’s reflect on some of the good fortune observational cosmologists enjoy. The task of understanding the contents of the universe, (let alone their evolution), is so audacious, that it is remarkable we can even start doing the job. One reason we can is that gravity helpfully imposes some clear organization on how matter is arranged. Luminous mass appears (at most wavelengths) to be strikingly organized into stars and galaxies. Biologists rely heavily on their crucial organizing concepts of cell,...
We test the evolution of the correlation between black hole mass and bulge properties, using a carefully selected sample of 20 Seyfert 1 galaxies at z=0.36 ±0.01. We estimate black hole mass from the Hβ line width and the optical... more
We test the evolution of the correlation between black hole mass and bulge properties, using a carefully selected sample of 20 Seyfert 1 galaxies at z=0.36 ±0.01. We estimate black hole mass from the Hβ line width and the optical luminosity at 5100 Å, based on the empirically calibrated photo-ionization method. Velocity dispersion are measured from stellar absorption lines around Mgb (5175 Å) and Fe (5270 Å) using high S/N Keck spectra, and bulge properties (luminosity and effective radius) are measured from HST images by fitting surface brightness. We find a significant offset from the local relations, in the sense that bulge sizes were smaller for given black hole masses at z=0.36 than locally. The measured offset is Δ M•=0.62 ± 0.10, 0.45 ±0.13, 0.59 ±0.19, respectively for M•–σ, M•–Lbulge, and M•–Mbulge relations. At face value, this result implies a substantial growth of bulges in the last 4 Gyr, assuming that the local M•–bulge property relation is the universal evolutionary e...
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In the present-day universe, the global properties of bulges and early-type galaxies correlate with the mass of their central black holes, indicating a connection between galaxy evolution and nuclear activity. Understanding the origin of... more
In the present-day universe, the global properties of bulges and early-type galaxies correlate with the mass of their central black holes, indicating a connection between galaxy evolution and nuclear activity. Understanding the origin of this relation is a major challenge for cosmological models. Using Keck spectra and HST images, we present direct measurements of the correlations between black hole mass and host spheroid luminosity and velocity dispersion at z=0.36, showing that the relations evolved significantly in the past 4 billion years. It appears that black holes of a few 108 M⊙ completed their growth before their host galaxies, and that the current scaling relations are only the final point of the co-evolution of galaxies and black holes.
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Research Interests: Physics, Organic Chemistry, Astrophysical Plasma, Star Formation, Luminous Infrared Galaxies, and 13 moreBackground Subtraction, Polycyclic Aromatic Hydrocarbon, Electron Density, High Resolution, Energy Production, Infrared, Seyfert galaxies, Luminosity function, Active Galaxies, Boolean Satisfiability, Starburst Galaxies, Polarized Light Microscopy, and new combination
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The two major functions in galaxy evolution that we would like to measure are the stellar populations in galaxies, and their time-derivative, the star formation rate. Especially at redshifts above 1, both of these measures are benefiting... more
The two major functions in galaxy evolution that we would like to measure are the stellar populations in galaxies, and their time-derivative, the star formation rate. Especially at redshifts above 1, both of these measures are benefiting greatly from wide-area infrared observations. Several space-based and ground-based examples will be discussed. 1 Understanding Galaxy Evolution with Deep Fields Since this is a conference talk rather than a journal paper, I’ll start on a philosophical note. Let’s reflect on some of the good fortune observational cosmologists enjoy. The task of understanding the contents of the universe, (let alone their evolution), is so audacious, that it is remarkable we can even start doing the job. One reason we can is that gravity helpfully imposes some clear organization on how matter is arranged. Luminous mass appears (at most wavelengths) to be strikingly organized into stars and galaxies. Biologists rely heavily on their crucial organizing concepts of cell,...
We investigate the cosmic evolution of the black hole (BH) mass – bulge luminosity relation using a sample of 52 active galaxies at z ∼ 0.36 and z ∼ 0.57 in the BH mass range of 107.4−9.1M. By consistently applying multi-component... more
We investigate the cosmic evolution of the black hole (BH) mass – bulge luminosity relation using a sample of 52 active galaxies at z ∼ 0.36 and z ∼ 0.57 in the BH mass range of 107.4−9.1M. By consistently applying multi-component spectral and structural decomposition to high-quality Keck spectra and high-resolution HST images, BH masses (MBH) are estimated using the Hβ broad emission line combined with the 5100 Å nuclear luminosity, and bulge luminosities (Lbul) are derived from surface photometry. Comparing the resulting MBH − Lbul relation to local active galaxies and taking into account selection effects, we find evolution of the form MBH/Lbul ∝ (1+z)γ with γ = 1.8±0.7, consistent with BH growth preceding that of the host galaxies. Including an additional sample of 27 active galaxies with 0.5 < z < 1.9 taken from the literature and measured in a consistent way, we obtain γ = 0.9 ± 0.7 for the MBH − Lbul relation and γ = 0.4 ± 0.5 for the MBH–total host galaxy luminosity (L...
From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Object Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear... more
From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Object Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear luminosity, total host-galaxy luminosity and spheroid luminosity. Keck spectroscopy is used to estimate black hole mass (MBH). We study the cosmic evolution of the MBH-spheroid luminosity (Lsph) relation. In combination with our previous work, totaling 40 Seyfert-1 galaxies, the covered range in BH mass is substantially increased, allowing us to determine for the first time intrinsic scatter and correct evolutionary trends for selection effects. We re-analyze archival HST images of 19 local reverberation-mapped active galaxies to match the procedure adopted at intermediate redshift. Correcting spheroid luminosity for passive luminosity evolution and taking into account selection effects, we determine that at fixed present-day V-band spheroid luminosity, MB...
We present the results of ROSAT All–Sky Survey observations of Seyfert and IR–luminous galaxies from the Extended 12 μm Galaxy Sample and the optically–selected CfA Sample. Detections are available for 80% (44/55) of the Seyfert 1s and... more
We present the results of ROSAT All–Sky Survey observations of Seyfert and IR–luminous galaxies from the Extended 12 μm Galaxy Sample and the optically–selected CfA Sample. Detections are available for 80% (44/55) of the Seyfert 1s and 34% (23/67) of the Seyfert 2s in the 12 μm sample, and for 76% (26/34) of the Seyfert 1s and 38% (6/16) of the Seyfert 2s in the CfA sample. Roughly half of the Seyferts (mostly Seyfert 1s) have been fitted to an absorbed power–law model, yielding an average photon index of Γ=2.26±0.11 for 43 Seyfert 1s and Γ=2.45±0.18 for 10 Seyfert 2s, with both types having a median value of 2.3. The soft X–ray luminosity correlates with the 12 μm luminosity, with Seyfert 1s having relatively more soft X–ray emission than Seyfert 2s of similar mid–infrared luminosities, by a factor of 1.6 ± 0.3. Several physical interpretations of these results are discussed, including the standard unified model for Seyfert galaxies. Infrared–luminous non–Seyferts are shown to have...
We analyze the fluctuations in the X-ray flux of 20 AGN (mainly Seyfert 1 galaxies) monitored by RXTE and XMM-Newton with a sampling frequency ranging from hours to years, using structure function (SF) analysis. We derive SFs over four... more
We analyze the fluctuations in the X-ray flux of 20 AGN (mainly Seyfert 1 galaxies) monitored by RXTE and XMM-Newton with a sampling frequency ranging from hours to years, using structure function (SF) analysis. We derive SFs over four orders of magnitude in the time domain (0.03-300 days). Most objects show a characteristic time scale, where the SF flattens or changes slope. For 10 objects with published power-spectral density (PSD) the break time scales in the SF and PSD are similar and show a good correlation. We also find a significant correlation between the SF timescale and the mass of the central black hole, determined for most objects by reverberation mapping.
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From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Ob ject Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear... more
From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Ob ject Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear luminosity, total host-galaxy luminosity and spheroid luminosity. Keck spectroscopy is used to estimate black hole mass (MBH). We study the cosmic evolution of the MBH-spheroid luminosity (Lsph) relation. In combination with our previous work, totaling 40 Seyfert-1 galaxies, the covered range in BH mass is substantially increased, allowing us to determine for the first time intrinsic scatter and correct evolutionary trends for selection effects. We re-analyze archival HST images of 19 local reverberation-mapped active galaxies to match the procedure adopted at intermediate redshift. Correcting spheroid luminosity for passive luminosity evolution and taking into account selection effects, we determine that at fixed present-day V-band spheroid luminosity, M...
The Spitzer high resolution spectra of 72 Seyfert galaxies f rom the 12μm Galaxy Sample are presented and discussed. The presence of starbur t components in these galaxies can be quantified by powerful mid-IR diagnostics tools (i.e.... more
The Spitzer high resolution spectra of 72 Seyfert galaxies f rom the 12μm Galaxy Sample are presented and discussed. The presence of starbur t components in these galaxies can be quantified by powerful mid-IR diagnostics tools (i.e. 11.25μm PAH feature equivalent width and the H2 emission line intensity), as well as the AGN dominance can be measured by specific fine structure line ratios (e.g. [NeV] /[NeII], [NeV] /[SiII], etc.). The two types of Seyfert galaxies do not show any statistical di fference in our diagnostic tools. However, the Seyfert 2’s showing hidden Broad Line Regions i n pectro-polarimetric observations have on average an higher AGN dominance, a weaker st r formation component and a warmer [60 25] spectral index than those without broad emission lines.
We report on the analysis of the first complete far-infrared spectrum (43-197μm) of the Seyfert 2 galaxy NGC 1068 as observed with the Long Wavelength Spectrometer (LWS) onboard the Infrared Space Observatory (ISO). In addition to the 7... more
We report on the analysis of the first complete far-infrared spectrum (43-197μm) of the Seyfert 2 galaxy NGC 1068 as observed with the Long Wavelength Spectrometer (LWS) onboard the Infrared Space Observatory (ISO). In addition to the 7 expected ionic fine structure emission lines, the OH rotational lines at 79, 119 and 163μm were all detected in emission, which is unique among galaxies with full LWS spectra, where the 119μm line, when detected, is always in absorption. The observed line intensities were modelled together with ISO Short Wavelength Spectrometer (SWS) and optical and ultraviolet line intensities from the literature, considering two independent emission components: the AGN component and the starburst component in the circumnuclear ring of ∼ 3 kpc in size. Using the UV to mid-IR emission line spectrum to constrain the nuclear ionizing continuum, we have confirmed previous results: a canonical power-law ionizing spectrum is a poorer fit than one with a deep absorption tr...
We combine Hubble Space Telescope images from the Great Observatories Origins Deep Survey with archival Very Large Telescope and Keck spectra of a sample of 11 X-ray selected broad-line active galactic nuclei in the redshift range 1 <... more
We combine Hubble Space Telescope images from the Great Observatories Origins Deep Survey with archival Very Large Telescope and Keck spectra of a sample of 11 X-ray selected broad-line active galactic nuclei in the redshift range 1 < z < 2 to study the black hole mass stellar mass relation out to a lookback time of 10 Gyrs. Stellar masses of the spheroidal component (Msph,⋆) are derived from multi-filter surface photometry. Black hole masses (MBH) are estimated from the width of the broad MgII emission line and the 3000Å nuclear luminosity. Comparing with a uniformly measured local sample and taking into account selection effects, we find evolution in the form MBH/Msph,⋆∝ (1+z), in agreement with our earlier studies based on spheroid luminosity. However, this result is more accurate because it does not require a correction for luminosity evolution and therefore avoids the related and dominant systematic uncertainty. We also measure total stellar masses (Mhost,⋆). Combining ou...
From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Ob ject Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear... more
From high-resolution images of 23 Seyfert-1 galaxies at z=0.36 and z=0.57 obtained with the Near Infrared Camera and Multi-Ob ject Spectrometer on board the Hubble Space Telescope (HST), we determine host-galaxy morphology, nuclear luminosity, total host-galaxy luminosity and spheroid luminosity. Keck spectroscopy is used to estimate black hole mass (MBH). We study the cosmic evolution of the MBH-spheroid luminosity (Lsph ) relation. In combination with our previous work, totaling 40 Seyfert-1 galaxies, the covered range in BH mass is substantially increased, allowing us to determine for the first time intrinsic scatter and correct evolutionary trends for selection effects. We re-analyze archival HST images of 19 local reverberation-mapped active galaxies to match the procedure adopted at intermediate redshift. Correcting spheroid luminosity for passive luminosity evolution and taking into account selection effects, we determine that at fixed present-day V-band spheroid luminosity, ...
Infrared photometry and later infrared spectroscopy provided powerful diagnostics to distinguish between the main emission mechanisms in galaxies: AGN and Starburst. After the pioneering work on infrared photometry with IRAS in the far-IR... more
Infrared photometry and later infrared spectroscopy provided powerful diagnostics to distinguish between the main emission mechanisms in galaxies: AGN and Starburst. After the pioneering work on infrared photometry with IRAS in the far-IR and the San Pedro Martir and ESO ground-based work in the near-IR, ISO photometry extended up to 200 μm the coverage of the galaxies energy distributions. Then Spitzer collected accurate mid-infrared spectroscopy on different samples of galaxies. We will review the work done on the 12 μm galaxy sample since the times of IRAS photometry to the new Spitzer spectroscopy. The main results on the multifrequency data of 12 μm selected Seyfert galaxies are presented and discussed in the light of unification and evolution models. The spectroscopic work of Spitzer will soon be complemented at longer wavelengths by the Herschel spectrometers and in the future by SPICA at higher redshift. © 2010: Instituto de Astronomia, UNAM.
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We image 19 quasars with 22 damped Lyman α (DLA) systems using the F160W filter and the Near-Infrared Camera and Multiobject Spectrograph aboard the Hubble Space Telescope, in both direct and coronagraphic modes. We reach 5σ detection... more
We image 19 quasars with 22 damped Lyman α (DLA) systems using the F160W filter and the Near-Infrared Camera and Multiobject Spectrograph aboard the Hubble Space Telescope, in both direct and coronagraphic modes. We reach 5σ detection limits of ∼H=22 in the majority of our images. We compare our observations to the observed Lyman-break population of high-redshift galaxies, as well as Bruzual & Charlot evolutionary models of present-day galaxies redshifted to the distances of the absorption systems. We predict H magnitudes for our DLAs, assuming they are producing stars like an L∗ Lyman-break galaxy (LBG) at their redshift. Comparing these predictions to our sensitivity, we find that we should be able to detect a galaxy around 0.5-1.0 L∗(LBG) for most of our observations. We find only one new possible candidate, that near LBQS00100012. This scarcity of candidates leads us to the conclusion that most damped Lyman α systems are not drawn from a normal LBG luminosity function nor a loca...
We provide an updated calibration of C IV λ1549 broad emission line-based single-epoch (SE) black hole (BH) mass estimators for active galactic nuclei (AGNs) using new data for six reverberation-mapped AGNs at redshift z = 0.005 − 0.028... more
We provide an updated calibration of C IV λ1549 broad emission line-based single-epoch (SE) black hole (BH) mass estimators for active galactic nuclei (AGNs) using new data for six reverberation-mapped AGNs at redshift z = 0.005 − 0.028 with BH masses (bolometric luminosities) in the range 106.5–107.5 M (1041.7– 1043.8 erg s−1). New rest-frame UV-to-optical spectra covering 1150–5700 Å for the six AGNs were obtained with the Hubble Space Telescope (HST). Multi-component spectral decompositions of the HST spectra were used to measure SE emission-line widths for the C IV, Mg II, and Hβ lines as well as continuum luminosities in the spectral region around each line. We combine the new data with similar measurements for a previous archival sample of 25 AGNs to derive the most consistent and accurate calibrations of the C IV-based SE BH mass estimators against the Hβ reverberation-based masses, using three different measures of broad-line width: full-width at half maximum (FWHM), line di...
The Spitzer high resolution spectra of 72 Seyfert galaxies f rom the 12μm Galaxy Sample are presented and discussed. The presence of starbur t components in these galaxies can be quantified by powerful mid-IR diagnostics tools (i.e.... more
The Spitzer high resolution spectra of 72 Seyfert galaxies f rom the 12μm Galaxy Sample are presented and discussed. The presence of starbur t components in these galaxies can be quantified by powerful mid-IR diagnostics tools (i.e. 11.25μm PAH feature equivalent width and the H2 emission line intensity), as well as the AGN dominance can be measured by specific fine structure line ratios (e.g. [NeV] /[NeII], [NeV] /[SiII], etc.). The two types of Seyfert galaxies do not show any statistical di fference in our diagnostic tools. However, the Seyfert 2’s showing hidden Broad Line Regions i n pectro-polarimetric observations have on average an higher AGN dominance, a weaker st r formation component and a warmer [60 25] spectral index than those without broad emission lines.
Compact starburst galaxies are thought to include many or most of the galaxies from which substantial Lyman continuum emission can escape into the intergalactic medium. Li & Malkan used Sloan Digital Sky Survey photometry to find a... more
Compact starburst galaxies are thought to include many or most of the galaxies from which substantial Lyman continuum emission can escape into the intergalactic medium. Li & Malkan used Sloan Digital Sky Survey photometry to find a population of such starburst galaxies at z ∼ 0.5. They were discovered by their extremely strong [O iii] λλ4959+5007 emission lines, which produce a clearly detectable excess brightness in the i bandpass, compared with surrounding filters. We therefore used the Hubble Space Telescope (HST)/COS spectrograph to observe two of the newly discovered i-band excess galaxies around their Lyman limits. One has strongly detected continuum below its Lyman limit, corresponding to a relative escape fraction of ionizing photons of 20% ± 2%. The other, which is less compact in UV imaging, has a 2σ upper limit to its Lyman escape fraction of <5%. Before the UV spectroscopy, the existing data could not distinguish these two galaxies. Although a sample of two is hardly ...