3D-HST+CANDELS: THE EVOLUTION OF THE GALAXY SIZE–MASS DISTRIBUTION SINCE z = 3
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Cites background from "3D-HST+CANDELS: THE EVOLUTION OF TH..."
...…for disks (Trujillo et al. 2006, van der Wel et al. 2014); 3) the size distribution at fixed mass is narrower for spheroids than for disks (van der Wel et al. 2014) 4) the evolution of the Tully-Fisher and Faber-Jackson relation has been relatively mild (Cappellari et al. 2009, Cenarro &…...
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...…1) the size-mass relationship is considerably steeper for spheroids than for disks at all redshifts (Bernardi et al. 2010, Shen et al. 2003, van der Wel et al. 2014); 2) since z ∼ 2, the size-mass relation for spheroids has evolved much more rapidly than that for disks (Trujillo et al. 2006, van…...
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...…et al. 2014); 2) since z ∼ 2, the size-mass relation for spheroids has evolved much more rapidly than that for disks (Trujillo et al. 2006, van der Wel et al. 2014); 3) the size distribution at fixed mass is narrower for spheroids than for disks (van der Wel et al. 2014) 4) the evolution of the…...
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...We note that many high redshift studies present the scaling relations for galaxies divided according to whether they are star forming or quiescent, rather than spheroid or disk dominated, but this seems to make little difference to the qualitative results (van der Wel et al. 2014)....
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...A striking recent observation is that, at fixed stellar mass, spheroid-dominated galaxies at z ∼ 2 have much smaller sizes and central densities higher by orders of magnitude compared to today’s (e.g. Barro et al. 2013, Trujillo et al. 2006, van der Wel et al. 2014, van Dokkum et al. 2014, 2008)....
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...In a recent evaluation of star forming disk sizes in CANDELS/3D HST between z=0 and 3 van der Wel et al. (2014) find empirically β= -0.75 (±0.05), which is smaller than β= -0.83 but comes close to it....
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614 citations
Cites background or methods from "3D-HST+CANDELS: THE EVOLUTION OF TH..."
...Step 9 is described in van der Wel et al. (2014), who measured the structural parameters of objects in the J125 and H160 WFC3 bands....
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...These datasets, together with structural parameters and star formation rates presented elsewhere (van der Wel et al. 2014; Whitaker et al. 2014), accomplish an important goal of observational extragalactic astronomy: a census of stars and star formation in reasonably bright galaxies out to z ∼ 2.5....
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...…et al. (2013b) and Patel et al. (2013) describe the evolution of Milky Way like galaxies from z ∼ 2.5 to the present, using number density-matched samples. van der Wel et al. (2014) combine the 3D-HST catalogs with CANDELS photometry to study the evolution of the masssize relation with redshift....
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References
10,384 citations
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"3D-HST+CANDELS: THE EVOLUTION OF TH..." refers methods in this paper
...Finally, we use AB magnitudes and the Chabrier (2003) stellar initial mass function....
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4,288 citations
3,330 citations
"3D-HST+CANDELS: THE EVOLUTION OF TH..." refers background in this paper
...One possibility is that a substantial amount of material flows to the center under the influence of mergers (e.g., Di Matteo et al. 2005) or violently unstable disks and clump formation/migration (Dekel et al. 2009; Ceverino et al. 2010; Dekel & Burkert 2014)....
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2,867 citations
"3D-HST+CANDELS: THE EVOLUTION OF TH..." refers background or methods in this paper
...2005) and the fast evolution of UV-selected galaxies at z > 2 (Giavalisco et al. 1996; Ferguson et al. 2004; Oesch et al. 2010; Mosleh et al. 2012). Our data set allows us to bridge these regimes and probe the origin of this difference. In Figure 12 we show the size evolution of galaxies with stellar mass M∗ ∼ 10(10) M from the present day up to z ∼ 6. Here we have relaxed our magnitude limit to HF160W = 26, which is still within the completeness limit of the CANDELS imaging as can be seen in Figure 2. Size measurements of individual galaxies are no longer reliable at HF160W = 26, but the sample average is still robust to within 15% (van der Wel et al. 2012). For galaxies bluer than U−V = 1, thus selecting a population akin to LBGs we probe the population out to z ∼ 6. The median size evolves quickly with redshift, Reff ∝ (1 + z)−1.1, consistent with recent measurements by Oesch et al. (2010) and Mosleh et al....
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...2005) and the fast evolution of UV-selected galaxies at z > 2 (Giavalisco et al. 1996; Ferguson et al. 2004; Oesch et al. 2010; Mosleh et al. 2012). Our data set allows us to bridge these regimes and probe the origin of this difference. In Figure 12 we show the size evolution of galaxies with stellar mass M∗ ∼ 10(10) M from the present day up to z ∼ 6. Here we have relaxed our magnitude limit to HF160W = 26, which is still within the completeness limit of the CANDELS imaging as can be seen in Figure 2. Size measurements of individual galaxies are no longer reliable at HF160W = 26, but the sample average is still robust to within 15% (van der Wel et al. 2012). For galaxies bluer than U−V = 1, thus selecting a population akin to LBGs we probe the population out to z ∼ 6. The median size evolves quickly with redshift, Reff ∝ (1 + z)−1.1, consistent with recent measurements by Oesch et al. (2010) and Mosleh et al. (2012). Once we include all late-type galaxies, regardless of color, the evolution matches that of the U−V < 1 galaxies at z 2....
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...The zero-th order expectation is that disk scale lengths evolve fast, approximately as the inverse of the Hubble parameter (Mo, Mao & White 1998), and early and recent work on the average sizes of Lyman Break Galaxies (LBGs) at high redshifts (z ∼ 2 − 6) roughly agree with this expectation for a ΛCDM cosmology: Giavalisco et al. (1996), Ferguson et al. (2004), Oesch et al....
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...The zero-th order expectation is that disk scale lengths evolve fast, approximately as the inverse of the Hubble parameter (Mo, Mao & White 1998), and early and recent work on the average sizes of Lyman Break Galaxies (LBGs) at high redshifts (z ∼ 2 − 6) roughly agree with this expectation for a ΛCDM cosmology: Giavalisco et al. (1996), Ferguson et al. (2004), Oesch et al. (2010), and Mosleh et al....
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...The zero-th order expectation is that disk scale lengths evolve fast, approximately as the inverse of the Hubble parameter (Mo, Mao & White 1998), and early and recent work on the average sizes of Lyman Break Galaxies (LBGs) at high redshifts (z ∼ 2 − 6) roughly agree with this expectation for a ΛCDM cosmology: Giavalisco et al. (1996), Ferguson et al. (2004), Oesch et al. (2010), and Mosleh et al. (2012) all find rapid size evolution with redshift: Reff ∝ (1 + z)β=−1.1. In contrast, the average size at a given stellar mass of the population of disk-dominated galaxies evolves slowly at late times (z 1) has been reported to evolve slowly as measured at fixed galaxy mass (β = −0.2) or not at all (Lilly et al. 1998; Ravindranath et al. 2004; Barden et al. 2005). The implication would be that the evolution of the disk galaxy population is decoupled from the evolution of the dark matter halo population. One fundamental difference between the results on LBGs and lower-redshift disk galaxies is the rest-frame wavelength at which the sizes are measured: the rest-frame UV light seen for LBGs originates from young stars that may be, and are generally expected to be, distributed differently than bulk of baryonic and stellar mass, not to mention the consequences of extinction. The advent of ground-based near-infrared imaging surveys helped to bridge the z < 1 and z > 2 regimes by enabling size measurements in a consistent manner at a fixed rest-frame wavelength. Early results suggested slow evolution for late-type galaxies up to z ∼ 3 (Trujillo et al. 2006a), but the uncertainties at z > 1 were such that evolution in that regime was not strongly constrained. Later ground-based work pointed at faster evolution at a fixed galaxy mass: Franx et al. (2008) found β = −0....
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