Technology

Elsner, Ann E.; Clark, Christopher A.

doi:10.1002/9781119011804.ch12

Cited by 5 publications

(7 citation statements)

References 101 publications

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“…The mass function of galaxies has been studied extensively over the past few years out to z ∼ 4 − 5, for both the star forming and quiescent galaxies (Dickinson et al 2003;Fontana et al 2006;Rudnick et al 2006;Elsner et al 2008;Pérez-González et al 2008;Ilbert et al 2013;Muzzin et al 2013). Using a Spitzer IRAC selected sample Pérez-González et al 2008 estimated the stellar mass function of galaxies and calculated the global stellar mass density of ∼ 2.7 × 10 7 M /M pc 3 at 3.0 < z < 3.5.…”

Section: Discussionmentioning

confidence: 99%

A Study of Massive and Evolved Galaxies at High Redshift

Nayyeri

Mobasher

Hemmati

et al. 2014

ApJ

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We use data taken as part of HST/WFC3 observations of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) to identify massive and evolved galaxies at 3 < z < 4.5. This is performed using the strength of the Balmer break feature at rest-frame 3648Å, which is a diagnostic of the age of the stellar population in galaxies. Using WFC3 H-band selected catalog for the CANDELS GOODS-S field and deep multi-waveband photometry from optical (HST) to midinfrared (Spitzer) wavelengths, we identify a population of old and evolved post-starburst galaxies based on the strength of their Balmer breaks (Balmer Break Galaxies-BBGs). The galaxies are also selected to be bright in rest-frame near-IR wavelengths and hence, massive. We identify a total of 16 BBGs. Fitting the spectral energy distribution (SED) of the BBGs show that the candidate galaxies have average estimated ages of ∼ 800 Myr and average stellar masses of ∼ 5×10 10 M , consistent with being old and massive systems. Two of our BBG candidates are also identified by the criteria that is sensitive to star forming galaxies (LBG selection). We find a number density of ∼ 3.2 × 10 −5 M pc −3 for the BBGs corresponding to a mass density of ∼ 2.0 × 10 6 M /M pc 3 in the redshift range covering the survey. Given the old age and the passive evolution, it is argued that some of these objects formed the bulk of their mass only a few hundred million years after the Big Bang.

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Section: Discussionmentioning

confidence: 99%

A Study of Massive and Evolved Galaxies at High Redshift

Nayyeri

Mobasher

Hemmati

et al. 2014

ApJ

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“…The top right panel shows a comparison between the integral of the star-formation rate density from field galaxies (black line) and that from GRBs (blue line) with the stellar mass density inferred from rest-frame visible light observations, assuming a standard Salpeter IMF. z < 4 stellar mass densities are estimates from Marchesini et al (2011) andElsner et al (2008) and at z ∼ 6 from Chary (2008). The bottom left panel illustrates the Thomson scattering cross section derived for CMB photons from Planck and that inferred from the SFRs displayed in panel 1, assuming an escape fraction of ionizing photons of 10-20% and assuming the higher Lyman-continuum production rate inferred in Shim et al (2011).…”

Section: Metallicity Constraints On Grb-derived Sfrmentioning

confidence: 97%

Gamma-Ray Bursts and the Early Star-Formation History

et al. 2016

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We review the uncertainties in high-z star-formation rate (SFR) measures and the constraints that one obtains from high-z gamma-ray burst (GRB) rates on them. We show that at the present time, the GRB rates per unit star-formation at z > 3 are higher than at lower redshift. There could be a multitude of reasons for this: a stellar metallicity bias for GRB production, a top-heavy initial mass function (IMF) and/or missing a significant fraction of star-formation in field galaxy surveys due to incompleteness, surface brightness limitations and cosmic variance. We also compare metallicity predictions made using a hierarchical model of cosmic chemical evolution based on two recently proposed SFRs, one based on the observed galaxy luminosity function at high redshift and one based on the GRB rate and find that within the considerable scatter in metal abundance measures, they both are consistent with the data. Analyzing the ensemble of different measurements together, we conclude that despite metallicity biases, GRBs may be a less biased probe of star-formation at z > 3 than at z < 2. There is likely to be a common origin to the high GRB rate per unit star-formation and the high observed Lyman-continuum production rate in high redshift galaxies and that this may be due to a relative overabundance of stars with mass >25 M ⊙ which are likely GRB progenitors. We also find that to reconcile these measurements with the Thomson scattering

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“…Stellar masses (M * ) of galaxies are usually calculated from multi-wavelength observations (for example Bundy et al 2006;Mortlock et al 2011). Stellar mass functions and stellar mass co-moving volume densities have now been studied in detail, indicating a clear history of stellar mass growth, whereby around half of all stellar mass is in place by z ∼ 1 (e.g., Drory et al 2005;Conselice et al 2007;Elsner et al 2008, Pérez-González et al 2008Mortlock et al 2011;Muzzin et al 2013;Ilbert et al 2013;Duncan et al 2014;Mortlock et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The Halo Masses of Galaxies to z ∼ 3: A Hybrid Observational and Theoretical Approach

Conselice

Twite

Palamara

et al. 2018

ApJ

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We use a hybrid observational/theoretical approach to study the relation between galaxy kinematics and the derived stellar and halo masses of galaxies up to z = 3 as a function of stellar mass, redshift and morphology. Our observational sample consists of a concatenation of 1125 galaxies with kinematic measurements at 0.4 < z < 3 from long-slit and integral-field studies. We investigate several ways to measure halo masses from observations based on results from semi-analytical models, showing that galaxy halo masses can be retrieved with a scatter of ∼ 0.4 dex by using only stellar masses. We discover a third parameter, relating to the time of the formation of the halo, which reduces the scatter in the relation between the stellar and halo masses, such that systems forming earlier have a higher stellar mass to halo mass ratio, which we also find observationally. We find that this scatter correlates with morphology, such that early-type, or older stellar systems, have higher M * /M halo ratios. We furthermore show using this approach, and through weak lensing and abundance matching, that the ratio of stellar to halo mass does not significantly evolve with redshift at 1 < z < 3. This is evidence for the regulated hierarchical assembly of galaxies such that the ratio of stellar to dark matter mass remains approximately constant since z = 2. We use these results to show that the dark matter accretion rate evolves from dM halo /dt ∼ 4000 M year −1 at z ∼ 2.5, to a few 100 M year −1 by z ∼ 0.5.

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Technology

Cited by 5 publications

References 101 publications

A Study of Massive and Evolved Galaxies at High Redshift

A Study of Massive and Evolved Galaxies at High Redshift

Gamma-Ray Bursts and the Early Star-Formation History

The Halo Masses of Galaxies to z ∼ 3: A Hybrid Observational and Theoretical Approach

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