SIZES AND SURFACE BRIGHTNESS PROFILES OF QUIESCENT GALAXIES AT z ∼ 2

By Daniel Szomoru, M. Franx, P. V. van Dokkum. 2011

157 citations recorded by the source corpus.

We use deep Hubble Space Telescope Wide Field Camera 3 near-infrared imaging obtained of the GOODS-South field as part of the CANDELS survey to investigate a stellar mass-limited sample of quiescent galaxies at 1.5 < z < 2.5. We measure surface brightness profiles for these galaxies using a method that properly measures low surface brightness flux at large radii. We find that quiescent galaxies at z ∼ 2 very closely follow Sérsic profiles, with nmedian = 3.7, and have no excess flux at large radii. Their effective radii are a factor of ∼4 smaller than those of low-redshift quiescent galaxies of similar mass. However, there is a significant spread in sizes (), with the largest z ∼ 2 galaxies lying close to the z = 0 mass–size relation. We compare the stellar mass surface density profiles with those of massive elliptical galaxies in the Virgo Cluster and confirm that most of the mass growth which occurs between z ∼ 2 and z = 0 must be due to accretion of material onto the outer regions of the galaxies. Additionally, we investigate the evolution in the size distribution of massive quiescent galaxies. We find that the minimum size growth required for z ∼ 2 quiescent galaxies to fall within the z = 0 size distribution is a factor of ∼2 smaller than the total median size growth between z ∼ 2 and z = 0.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/81564f03507524a17233749973f808796706d78b

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Citations in the corpus

STELLAR KINEMATICS OF z ∼ 2 GALAXIES AND THE INSIDE-OUT GROWTH OF QUIESCENT GALAXIES, (2012, methodology): “…been underestimated, due to an envelope of low surface brightness light, have been addressed with deep Hubble Space Telescope Wide Field Camera 3 (HST WFC3) imaging (Szomoru et al. 2010; 2012), and by stacking results (e.g van der Wel et al. 2008; Cassata et al. 2010; van Dokkum et al. 2008, 2010).”
SUBMILLIMETER GALAXIES AS PROGENITORS OF COMPACT QUIESCENT GALAXIES (2014, background): “…at z ∼ 2 (Daddi et al. 2005; Toft et al. 2005; Trujillo et al. 2006; Toft et al. 2007; Franx et al. 2008; Toft et al. 2009; Williams et al. 2010; van Dokkum et al. 2010; Brammer et al. 2011; Szomoru et al. 2011; Damjanov et al. 2011; Szomoru et al. 2012; Newman et al. 2012; Cassata et al. 2013).”
The Morphologies of Massive Galaxies at 1<z<3 in the CANDELS-UDS Field: Compact Bulges, and the Rise and Fall of Massive Disks (2012, result): “Here, our results for bulges match very well those recently reported by Szomoru et al. (2012), who used the CANDELS imaging in GOODS-South to deduce that quiescent galaxies at 1.5 < z < 2.5 with median Sérsic indices n 3.7 lie a factor of 4 in size below the local size–mass relation.”
Evolution of density profiles in high-z galaxies: compaction and quenching inside-out (2015, unknown): “…Mendel et al. 2013; Cibinel et al. 2013a; Fang et al. 2013; Schawinski et al. 2014; Omand et al. 2014; Bluck et al. 2014; Woo et al. 2015) and at high-z (Wuyts et al. 2011, 2012; Bell et al. 2012; Cheung et al. 2012; Szomoru et al. 2012; Barro et al. 2013; Lang et al. 2014; Tacchella et al. 2015c).”
3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3 (2014, unknown): “This ﬁnding is in general agreement with previous claims based on smaller samples and fewer ﬁelds by Cassata et al. (2011), Newman et al. (2012), Szomoru et al. (2012), Buitrago et al. (2013), and Cassata et al. (2013).”
Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies (2015, background): “SFGs and quiescent galaxies follow well-defined size-mass relations, which are characterized by low-linear relations, log re ∝ a logM (e.g., Law et al. 2012; Mosleh et al. 2012; Szomoru et al. 2012; Newman et al. 2012; van der Wel et al. 2014).”
The star formation history of CALIFA galaxies: Radial structures (2013, methodology): “This number is only slightly smaller than the 25% reported by Szomoru et al. (2012) for a sample of high-redshift galaxies analyzed with multi-band photometry.”
How do minor mergers promote inside-out growth of ellipticals, transforming the size, density profile and dark matter fraction? (2012, background): “…n & 5 (Toft et al. 2005; Trujillo 2006; Toft et al. 2007; van Dokkum et al. 2008; van der Wel et al. 2008, 2009; van Dokkum et al. 2010; van der Wel et al. 2011; Kormendy et al. 2009; Carrasco et al. 2010; Weinzirl et al. 2011; Buitrago et al. 2011; Kormendy & Bender 2012; Szomoru et al. 2012).”