Redshift Evolution of the Galaxy Velocity Dispersion Function

Bezanson, Rachel; Dokkum, Pieter van; Franx, Marijn; Brammer, Gabriel; Brinchmann, Jarle; Kriek, Mariska; Labbé, Ivo; Quadri, Ryan; Rix, Hans─Walter; Sande, Jesse van de; Whitaker, Katherine E.; Williams, R.

doi:10.1088/2041-8205/737/2/l31

Cited by 88 publications

(153 citation statements)

References 48 publications

(57 reference statements)

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“…The dynamical masses were estimated based on a virial relation, the effective radius and the velocity dispersion of each galaxy. The derived effective radius and dynamical mass fit within ≤1σ with the size-mass relation presented by Bezanson et al (2011), predicts values close to those derived here for each galaxy. The calculated distance and dynamical mass are 292.6 Mpc and 1.63 × 10 11 M , respectively.…”

Section: Mfgc 04711supporting

confidence: 85%

A study of the remarkable galaxy system AM 546-324 (the core of Abell S0546)

Faúndez-Abans

Krabbe

Oliveira-Abans

et al. 2012

A&A

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Aims. We report first results of an investigation of the tidally disturbed galaxy system AM 546-324, whose two principal galaxies 2MFGC 04711 and AM 0546-324 (NED02) were previously classified as interacting doubles. This system was selected to study the interaction of ellipticals in a moderately dense environment. We provide spectral characteristics of the system and present an observational study of the interaction effects on the morphology, kinematics, and stellar population of these galaxies. Methods. The study is based on long-slit spectrophotometric data in the range of ∼4500−8000 Å obtained with the Gemini MultiObject Spetrograph at Gemini South (GMOS-S). We have used the stellar population synthesis code STARLIGHT to investigate the star formation history of these galaxies. The Gemini/GMOS-S direct r-G0303 broad band pointing image was used to enhance and study fine morphological structures. The main absorption lines in the spectra were used to determine the radial velocity. Results. Along the whole long-slit signal, the spectra of the Shadowy galaxy (discovered by us), 2MFGC 04711, and AM 0546-324 (NED02) resemble that of an early-type galaxy. We estimated redshifts of z = 0.0696, z = 0.0693 and z = 0.0718, corresponding to heliocentric velocities of 20 141 km s −1 , 20 057 km s −1 , and 20 754 km s −1 for the Shadowy galaxy, 2MFGC 04711 and AM 0546-324 (NED02), respectively. The central regions of 2MFGC 04711 and AM 0546-324 (NED02) are completely dominated by an old stellar population of 2 × 10 9 < t ≤ 13 × 10 9 yr and do not show any spatial variation in the contribution of the stellar-population components. Conclusions. The observed rotation profile distribution of 2MFGC 04711 and AM 0546-324 (NED02) can be adequately interpreted as an ongoing stage of interaction with the Shadowy galaxy as the center of the local gravitational potential-well of the system. The three galaxies are all early-type. The extended and smooth distribution of the material in the Shadowy galaxy is a good laboratory to study direct observational signatures of tidal friction in action.

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Section: Mfgc 04711supporting

confidence: 85%

A study of the remarkable galaxy system AM 546-324 (the core of Abell S0546)

Faúndez-Abans

Krabbe

Oliveira-Abans

et al. 2012

A&A

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“…Velocity dispersion is a measurement of orbital energy and gravitational potential depth. There is evidence from both observations and simulations that velocity dispersion may be a more stable quantity than stellar mass (Loeb & Peebles 2003;Franx et al 2008;van Dokkum et al 2010;Bezanson et al 2011;Oser et al 2012). Additionally, velocity dispersion has been proven to be a better predictor than stellar mass of specific SFR and color (Franx et al 2008;Wake et al 2012b), galaxy clustering properties (Wake et al 2012a; but see also Li et al 2013), and SFR (Bezanson et al 2012) over a wide range of redshift.…”

Section: Ordering Galaxies By Inferred Velocity Dispersionmentioning

confidence: 99%

“…This provides a simple way to link descendant and progenitor populations at different redshifts. This technique has already been used to study the evolution of a number of different galaxy properties: UV luminosity and star formation history (Papovich et al 2011), the stellar velocity dispersion function (Bezanson et al 2011), Hα equivalent width (Fumagalli et al 2012), and mass and structural evolution van Dokkum et al 2010;Brammer et al 2011;Patel et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Tracing Galaxies Through Cosmic Time With Number Density Selection

Leja

Dokkum

Franx

2013

ApJ

Self Cite

104

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A central challenge in observational studies of galaxy formation is how to associate progenitor galaxies with their descendants at lower redshifts. One promising approach is to link galaxies at fixed number density rather than fixed luminosity or mass. This method is effective if stellar mass rank order is broadly conserved through cosmic time. In this paper, we use the Guo et al. semi-analytical model to analyze under what circumstances this assumption is valid in the context of a cosmological simulation. Specifically, we select progenitor galaxies at a constant number density and compare the stellar mass evolution of their descendants to the evolution at a constant number density. The median stellar mass of the descendants increases by a factor of four (0.6 dex) from z = 3 to z = 0. Constant number density selection reproduces this to within 40% (0.15 dex) over a wide range of number densities. We show that the discrepancy primarily results from scatter in the stellar mass growth rates and merging. After applying simple, observationally based corrections for these processes, the discrepancy is reduced to 12% (0.05 dex). We conclude that number density selection can be used to predict the median descendant mass of high-redshift progenitor galaxies. The main uncertainty in this study is that semi-analytical models do not reproduce the observed mass evolution of galaxies, which makes the quantitative aggregate effects of star formation, merging, and quenching on the rank order of galaxies somewhat uncertain.

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“…To calculate σ mod consistently, we therefore scaled the stellar mass with the ratio of the model flux to the Sérsic model flux. Bezanson et al (2011) find that the model and the observed velocity dispersion correlate very well in the range 60 km s −1 < σ < 300 km s −1 , for galaxies in the redshift range 0.05 < z < 0.07, and for a few galaxies with redshifts 1 < z < 2.5. The SDSS spectroscopic sample extends to z ∼ 0.5, and therefore contains many more massive galaxies.…”

Section: Lensesmentioning

confidence: 63%

“…The physical region where the velocity dispersion is averaged is therefore different for a sample of galaxies with different sizes and redshifts. To account for this, we followed Bezanson et al (2011) and scaled the observed spectroscopic velocity dispersion to a fixed size of R e /8 using σ spec = σ ap spec (8.0r ap /R e ) 0.066 , with r ap = 1.5 the radius of the SDSS spectroscopic fiber, R e the effective radius in the r-band, and σ ap spec the observed velocity dispersion. This correction is based on the best-fit relation determined using 40 galaxies in the SAURON sample (Cappellari et al 2006).…”

Section: Lensesmentioning

confidence: 99%

Stellar mass versus velocity dispersion as tracers of the lensing signal around bulge-dominated galaxies

Uitert

Hoekstra

Franx

et al. 2012

A&A

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We present the results of a weak gravitational lensing analysis to determine whether the stellar mass or else the velocity dispersion is more closely related to the amplitude of the lensing signal around galaxies, hence to the projected distribution of dark matter. The lensing signal on smaller scales than the virial radius corresponds most closely to the lensing velocity dispersion in the case of a singular isothermal profile, but is also sensitive on larger scales to the clustering of the haloes. We have selected over 4000 lens galaxies at a redshift z < 0.2 with concentrated (or bulge-dominated) surface brightness profiles from the ∼300 square degree overlap between the Red-sequence Cluster Survey 2 (RCS2) and the data release 7 (DR7) of the Sloan Digital Sky Survey (SDSS). We consider both the spectroscopic velocity dispersion and a model velocity dispersion (a combination of the stellar mass, the size, and the Sérsic index of a galaxy). Comparing the model and spectroscopic velocity dispersion we find that they correlate well for galaxies with concentrated brightness profiles. We find that the stellar mass and the spectroscopic velocity dispersion trace the amplitude of the lensing signal on small scales equally well. The model velocity dispersion, however, does significantly worse. A possible explanation is that the halo properties that determine the small-scale lensing signal -mainly the total mass -also depend on the structural parameters of galaxies, such as the effective radius and Sérsic index, but we lack data for a definitive conclusion.

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Redshift Evolution of the Galaxy Velocity Dispersion Function

Cited by 88 publications

References 48 publications

A study of the remarkable galaxy system AM 546-324 (the core of Abell S0546)

A study of the remarkable galaxy system AM 546-324 (the core of Abell S0546)

Tracing Galaxies Through Cosmic Time With Number Density Selection

Stellar mass versus velocity dispersion as tracers of the lensing signal around bulge-dominated galaxies

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