The Sloan Lens Acs Survey. Ix. Colors, Lensing, and Stellar Masses of Early-Type Galaxies

Auger, Matthew W.; Treu, Tommaso; Bolton, A.; Gavazzi, R.; Koopmans, L. V. E.; Marshall, Phil; Bundy, Kevin; Moustakas, Leonidas A.

doi:10.1088/0004-637x/705/2/1099

Cited by 292 publications

(490 citation statements)

References 42 publications

(41 reference statements)

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“…According to these results, if we normalize in our sample the stellar mass estimates obtained by adopting a Chabrier IMF to a Salpeter IMF, we measure a median value of the dark over total matter fraction of approximately 0.4 within R e . This result is consistent, given the errors, with the average values of 0.3 (see Koopmans et al 2006;Grillo et al 2009;Auger et al 2009) and 0.4 (see Bolton et al 2008b) for the two-dimensional dark over total mass fractions determined, respectively, inside disks with apertures equal to the average Einstein (0.6 times the effective radius) and effective radii of the SLACS lens galaxies. Furthermore, in six of these galaxies Barnabè et al (2009) have combined integral field spectroscopy with lensing data and measured values between 15% and 30% for the three-dimensional dark over total mass fractions within R e .…”

Section: Resultssupporting

confidence: 85%

“…In fact, these quantities, which are measured from the SDSS multicolor photometry, agree very well (especially at the high mass end considered here) with the values determined by fitting different spectral indices in the galaxy spectra. 2 Moreover, in a recent study Auger et al (2009) have compared in a subsample of approximately 50 massive lens galaxies the photometric stellar masses estimated by modeling in different ways (as done by the MPA/JHU collaboration and by Grillo et al 2009) the public SDSS photometry and their new Hubble Space Telescope (HST) photometry. Despite some minor differences, the authors conclude that, overall, there is consistency between all the independently measured stellar masses.…”

Section: The Samplementioning

confidence: 99%

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Projected Central Dark Matter Fractions and Densities in Massive Early-Type Galaxies From the Sloan Digital Sky Survey

Grillo

2010

ApJ

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We investigate in massive early-type galaxies the variation of their two-dimensional central fraction of dark over total mass and dark matter density as a function of stellar mass, central stellar velocity dispersion, effective radius, and central surface stellar mass density. We use a sample of approximately 1.7 × 10 5 galaxies from the Sloan Digital Sky Survey Data Release Seven (SDSS DR7) at redshift smaller than 0.33. We apply conservative photometric and spectroscopic cuts on the SDSS DR7 and the MPA/JHU value-added galaxy catalogs, to select galaxies with physical properties similar to those of the lenses studied in the Sloan Lens ACS Survey. The values of the galaxy stellar and total mass projected inside a cylinder of radius equal to the effective radius are obtained, respectively, by fitting the SDSS multicolor photometry with stellar population synthesis models, under the assumption of a Chabrier stellar initial mass function (IMF), and adopting a one-component isothermal total mass model with effective velocity dispersion approximated by the central stellar velocity dispersion. The plausibility of an isothermal model to represent the galaxy total mass distribution is supported by independent gravitational lensing and stellar-dynamical analyses performed in the lens subsample, which is found here to represent nicely the entire galaxy sample. We find that within the effective radius the stellar mass estimates differ from the total ones by only a relatively constant proportionality factor. In detail, we observe that the values of the projected fraction of dark over total mass and the logarithmic values of the central surface dark matter density (measured in M kpc −2 ) have almost Gaussian probability distribution functions, with median values of 0.64 +0.08 −0.11 and 9.1 +0.2 −0.2 , respectively. We discuss the observed correlations between these quantities and other galaxy global parameters and show that our results disfavor an interpretation of the tilt of the fundamental plane in terms of differences in the galaxy dark matter content and give useful information on the possible variations of the galaxy stellar IMF and dark matter density profile. Finally, we provide some observational evidence on the likely significant contribution of dry minor mergers, feedback from active galactic nuclei, and/or coalescence of binary black holes on the formation and evolution of massive early-type galaxies.

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Section: Resultssupporting

confidence: 85%

Section: The Samplementioning

confidence: 99%

Projected Central Dark Matter Fractions and Densities in Massive Early-Type Galaxies From the Sloan Digital Sky Survey

Grillo

2010

ApJ

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“…Random errors in stellar mass estimates are small with good photometry (typically ∼0.1 dex in this work; see also Auger et al 2009), but systematic errors are not well understood.…”

Section: Appendix B Measurement Errors In Stellar Masses and Radiimentioning

confidence: 68%

Can Minor Merging Account for the Size Growth of Quiescent Galaxies? New Results From the Candels Survey

Newman

Ellis

Bundy

et al. 2012

ApJ

444

101

608

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The presence of extremely compact galaxies at z ∼ 2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 galaxies selected with 0.4 < z < 2.5 and stellar masses M * > 10 10.7 M in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and the mean size of these systems at fixed stellar mass grows by a factor of 3.5 ± 0.3 over this redshift interval. The data are sufficiently deep to identify companions to these hosts whose stellar masses are ten times smaller. By searching for these around 404 quiescent hosts within a physical annulus 10 h −1 kpc < R < 30 h −1 kpc, we estimate the minor merger rate over 0.4 < z < 2. We find that 13%-18% of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6% ± 2% per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers may explain most of the size evolution observed at z 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes.

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“…This is about 8 times less than in SLACS, where the discovery rate is 0.005 (e.g., Auger et al 2009). However, our selection function is very different from SLACS, because of (i) the contrast between the QSO SDSS J0013+1523 G2 G1 5 arcsec Fig.…”

Section: Spectroscopic Search In Sdssmentioning

confidence: 75%

First case of strong gravitational lensing by a QSO: SDSS J0013+1523 atz= 0.120

Courbin¹,

Tewes²,

Djorgovski

et al. 2010

A&A

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We present the first case of strong gravitational lensing by a QSO: SDSS J0013+1523 at z = 0.120. The discovery is the result of a systematic search for emission lines redshifted behind QSOs, among 22 298 spectra of the SDSS data release 7. Apart from the z = 0.120 spectral features of the foreground QSO, the spectrum of SDSS J0013+1523 also displays the [O ii] and Hβ emission lines and the [O iii] doublet, all at the same redshift, z = 0.640. Using sharp Keck adaptive optics K-band images obtained using laser guide stars, we unveil two objects within a radius of 2 from the QSO. Deep Keck optical spectroscopy clearly confirms one of these objects at z = 0.640 and shows traces of the [O iii] emission line of the second object, also at z = 0.640. Lens modeling suggests that they represent two images of the same z = 0.640 emission-line galaxy. Our Keck spectra also allow us to measure the redshift of an intervening galaxy at z = 0.394, located 3.2 away from the line of sight to the QSO. If the z = 0.120 QSO host galaxy is modeled as a singular isothermal sphere, its mass within the Einstein radius is M E (r < 1 h −1 kpc) = 2.16 × 10 10 h −1 M and its velocity dispersion is σ SIS = 169 km s −1 . This is about 1-σ away from the velocity dispersion estimated from the width of the QSO Hβ emission line, σ * (M BH ) = 124 ± 47 km s −1 . Deep optical HST imaging will be necessary to constrain the total radial mass profile of the QSO host galaxy using the detailed shape of the lensed source. This first case of a QSO acting as a strong lens on a more distant object opens new directions in the study of QSO host galaxies.

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The Sloan Lens Acs Survey. Ix. Colors, Lensing, and Stellar Masses of Early-Type Galaxies

Cited by 292 publications

References 42 publications

Projected Central Dark Matter Fractions and Densities in Massive Early-Type Galaxies From the Sloan Digital Sky Survey

Projected Central Dark Matter Fractions and Densities in Massive Early-Type Galaxies From the Sloan Digital Sky Survey

Can Minor Merging Account for the Size Growth of Quiescent Galaxies? New Results From the Candels Survey

First case of strong gravitational lensing by a QSO: SDSS J0013+1523 atz= 0.120

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