Extremely compact massive galaxies at z ~ 1.4

By Ignacio Trujillo, G. Feulner, Y. Goranova, U. Hopp, M. Longhetti, P. Saracco, R. Bender, V. Braito, R. Ceca, N. Drory and 2 more. 2006

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The optical rest-frame sizes of 10 of the most massive (∼5 × 10 11 h −2 M� ) galaxies found in the near-infrared MUNICS survey at 1.2 < z < 1.7 are analysed. Sizes are estimated in both the J and Kfilters. These massive galaxies are at least a factor of 4 +1.9 (±1σ ) smaller in the rest-frame V-band than local counterparts of the same stellar mass. Consequently, the stellar mass density of these objects is (at least) 60 times larger than that of massive ellipticals today. Although the stellar populations of these objects are passively fading, their structural properties are rapidly changing since that redshift. This observational fact disagrees with a scenario where the more massive and passive galaxies are fully assembled at z ∼ 1.4 (i.e. a monolithic scenario) and points towards a dry merger scenario as the responsible mechanism for the subsequent evolution of these galaxies.

Subfields: Astronomy and Astrophysics, Instrumentation

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The ATLAS3D project – I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria (2010, result): “…2008; Trujillo et al. 2009; Taylor et al. 2010), we find no massive and superdense (LK >∼ 10 11 L⊙,K and Re <∼ 2 kpc) ETGs in our parent sample, contrary to what is found from photometry of ETGs at redshiftz >∼ 1.5 (e.g. Daddi et al. 2005; Trujillo et al. 2006; Cimatti et al. 2008; van Dokkum etal.”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “Recent work has demonstrated that massive, passive galaxies already exist at z ∼ 2 (e.g., Trujillo et al. 2006; Kriek et al. 2009) and that these systems are much more compact than local massive galaxies (Trujillo et al. 2006; Longhetti et al. 2007; van Dokkum 2008), suggesting that they must grow…”
THE EVOLVING RELATIONS BETWEEN SIZE, MASS, SURFACE DENSITY, AND STAR FORMATION IN 3 × 104 GALAXIES SINCE z = 2 (2009, methodology): “It is nonetheless instructive to investigate whether the specific characteristics of the UDS data and our fitting techniques have introduced systematic biases; we thus performed simulations analogous to Trujillo et al. (2006b) to test our effective radius measurements.”
Compact high-redshift galaxies are the cores of the most massive present-day spheroids (2009, methodology): “…that high-redshift spheroids may have significantly smaller effective radii than low-redshift analogues of the same mass (e.g. Daddi et al. 2005; Trujillo et al. 2006a, 2007; Toft et al. 2007; van Dokkum et al. 2008; Franx et al. 2008; van der Wel et al. 2008; Cimatti et al. 2008; Buitrago et…”
SIZES AND SURFACE BRIGHTNESS PROFILES OF QUIESCENT GALAXIES AT z ∼ 2 (2011, background): “…discussion, focusing in particular on their extremely compact nature compared to low redshift galaxies of similar mass (e.g., Daddi et al. 2005; Trujillo et al. 2006; Toft et al. 2007; van der Wel et al. 2008; van Dokkum et al. 2008; Damjanov et al. 2009; Hopkins et al. 2009; Saracco et al.…”
Size Evolution of the Most Massive Galaxies at 1.7 < z < 3 from GOODS NICMOS Survey Imaging (2008, methodology): “In previous papers we conduct many simulations in order to check the importance of surface brightness dimming at different observational conditions (NIR ground-based; Trujillo et al. 2004; 2006a,b; and using ACS data Trujillo et al. 2007).”
Dynamical Properties of z ~ 2 Star-forming Galaxies and a Universal Star Formation Relation (2007, result): “Such high surface/ matter densities are higher than local spheroid densities (Bender et al. 1992) and similar to that of z 1:5 spheroids, which are also smaller and denser than local spheroids (Trujillo et al. 2006; Longhetti et al. 2007).”
The VIMOS VLT deep survey: the assembly history of the stellar mass in galaxies: from the young to the old universe (2007, unknown): “High-z massive galaxies have been observed in previous surveys (Fontana et al. 2004; Saracco et al. 2005; Cimatti et al. 2004; Glazebrook et al. 2004; Fontana et al. 2006; Trujillo et al. 2006).”
GMASS ultradeep spectroscopy of galaxies at $z$ ~ 2 - II. Superdense passive galaxies: how did they form and evolve? (2008, methodology): “As discussed in the next sections and found in other works (e.g. Daddi et al. 2005a, Trujillo et al. 2006), the sizes derived Table 4.”
Compaction and quenching of high-z galaxies in cosmological simulations: blue and red nuggets (2014, background): “…= 2 − 3 are compact ellipticals with suppressed star formation rates (SFR), for which we adopt the nickname “red nuggets”1 (Daddi et al. 2005; Trujillo et al. 2006a,b; van Dokkum et al. 2008; Damjanov et al. ⋆ E-mail: zolotov.1@osu.edu † E-mail: dekel@huji.ac.il 1 The term “nugget” does…”
Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift (2007, background): “…during mergers by the scattering of disk stars (Toomre 1977; Barnes & Hernquist 1992; Schweizer 1996); they also grew during mergers of other spheroids (e.g., Khochfar & Burkert 2003; Bundy et al. 2004; Graham 2004; van Dokkum 2005; Bell et al. 2006; Robertson et al. 2006; Trujillo et al. 2006b).”
TWO BRIGHT SUBMILLIMETER GALAXIES IN A z = 4.05 PROTOCLUSTER IN GOODS-NORTH, AND ACCURATE RADIO-INFRARED PHOTOMETRIC REDSHIFTS (2008, background): “…ongoing mergers (Tacconi et al. 2006; 2008), have very compact sizes reminiscent of massive, evolved galaxies atz∼ 1.5−3 (Daddi et al. 2005a; Trujillo et al. 2006; Zirm et al. 2007; Tacconi et al. 2006; 2008; Cimatti et al. 2008) and have high star formation efficiencies compared to…”
SUPERDENSE MASSIVE GALAXIES IN THE NEARBY UNIVERSE (2009, background): “The discovery (Daddi et al. 2005; Trujillo et al. 2006) that the most massive galaxies (M⋆&10 11M⊙), independently of their star formation rate (Pérez-González et al. 2008), were much more compact in the past (a factor of ∼4 at z&1.5 than their equally massive local counteparts; Trujillo et al.…”
Strong size evolution of the most massive galaxies since z~2 (2007, methodology): “At even higher z (i.e. z∼2.5) there has been also recent claims of very compacts (re.1 kpc) massive galaxies (Trujillo et al. 2006a; Zirm et al. 2007; Toft et al. 2007).”
Size evolution of normal and compact galaxies in the EAGLE simulation (2015, background): “Observational studies have detected massive compact red galaxies at high redshifts (e.g. Cimatti et al. 2004; Daddi et al. 2005; Trujillo et al. 2006; van Dokkum et al. 2008; Damjanov et al. 2009).”
Mass, metal, and energy feedback in cosmological simulations (2007, result): “Such a scenario is supported by the observations by Trujillo et al. (2006) and Trujillo et al. (2007) showing a trend of galaxies becoming smaller from z = 0 → 2, in general agreement with Mo et al. (1998).”
CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY—THE HUBBLE SPACE TELESCOPE OBSERVATIONS, IMAGING DATA PRODUCTS, AND MOSAICS (2011, background): “Finally, the evolution of galaxies with very low specific SFRs (passive galaxies) is also of interest, with sources having been found out to at least z= 2.5 (e.g., Daddi et al. 2005; Trujillo et al. 2006; Cimatti et al. 2008; van Dokkum et al. 2008).”
Hubble Space Telescope and Spitzer Imaging of Red and Blue Galaxies at z ~ 2.5: A Correlation between Size and Star Formation Activity from Compact Quiescent Galaxies to Extended Star-forming Galaxies (2007, methodology): “…mass-size relationship is consistent with the evolution of the mass-size relation derived from the FIRES survey for galaxies at z 2:5, which were found to be a factor of 2 0:5 smaller than galaxies of similar mass in the SDSS (based on sizes derived from ground-based data; Trujillo et al. 2006a).”
Submillimeter Galaxies at z ~ 2: Evidence for Major Mergers and Constraints on Lifetimes, IMF, and CO-H2 Conversion Factor (2008, background): “…that most of the apparentlymassive (K 20Y21) passively evolving (= ‘‘quiescent,’’ ‘‘passively’’ evolving, or ‘‘red-sequence’’) galaxies in the same redshift range as the SMGs are remarkably compact (Daddi et al. 2004a, 2004b, 2005; Trujillo et al. 2006, 2007; Zirm et al. 2007; Toft et al. 2007).”