Resolved Galaxies in the Hubble Ultra Deep Field: Star Formation in Disks at High Redshift

By D. Elmegreen, Bruce G. Elmegreen, S. Ravindranath, D. Coe. 2007

271 citations recorded by the source corpus.

The photometric redshift distributions, spectral types, Sérsic indices, and sizes of all resolved galaxies in the Hubble Space Telescope Ultra Deep Field (UDF) are studied in order to understand the environment and nature of star formation in the early universe. Clumpy disk galaxies that are bright at short wavelengths (rest-frame λ < 5000 Å) dominate the UDF out to z ~ 5.5. Their uniformity in V/Vmax and comoving volume density suggest that they go even further, spanning a total time more than an order of magnitude larger than their instantaneous star formation times. They precede as well as accompany the formation epoch of distant red galaxies and extreme red objects. Those preceding could be the premerger objects that combined to make red spheroidal types at z ~ 2-3. Clumpy disks that do not undergo mergers are likely to evolve into spirals. The morphology of clumpy disks, the size and separation of the clumps, and the prevalence of this type of structure in the early universe suggests that most star formation occurs by self-gravitational collapse of disk gas.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/517fc61b4a3f183711f7e5efbd878ef6a15b1fed

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. A. Dekel
4. R. Dav'e
5. R. Somerville
6. P. V. van Dokkum
7. T. Naab
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In Instrumentation

1. L. Hernquist
2. P. Hopkins
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6. R. Dav'e
7. C. Conroy
8. R. Somerville

Citations in the corpus

• A physical model for z∼ 2 dust-obscured galaxies (2009, background): “Both observations (e.g. Elmegreen et al. 2007; Daddi et al. 2008; Genzel et al. 2006; Elmegreen et al. 2009; Förster Schreiber et al. 2009) and models (e.g. Bournaud et al. 2008; Dekel et al. 2009; Elmegreen 2009; Ceverino, Dekel & Bournaud 2010; Elmegreen & Burkert 2010) suggest that disc…”
• SMOOTH(ER) STELLAR MASS MAPS IN CANDELS: CONSTRAINTS ON THE LONGEVITY OF CLUMPS IN HIGH-REDSHIFT STAR-FORMING GALAXIES (2012, background): “…Steward Observatory, 933 N. Cherry Street, University of Arizona, Tucson, AZ 85721, USA 11 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany (ACS), the statistics on irregular galaxy number counts have since increased significantly (e.g., Elmegreen et al. 2007).”
• Rotational support of giant clumps in high-z disc galaxies (2011, background): “First dubbed “clump-cluster” and “chain” galaxies, based on their face-on or edge-on images (Cowie et al. 1995; van den Bergh 1996; Elmegreen et al. 2004, 2005, 2007), a significant fraction of these galaxies (> 50% for the more massive ones) are confirmed by spectroscopic measurements to be…”
• The ATLAS3D project – XX. Mass–size and mass–σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function (2012, background): “They are characterized by giant gas clumps (Elmegreen et al. 2007; Genzel et al. 2011), have high gas fractions (Daddi et al. 2010; Tacconi et al. 2010), possess large velocity dispersion and are dominated by turbulent motions (Förster Schreiber et al. 2006, 2009; Genzel et al. 2006, 2008; Law et…”
• Multiple minor mergers: formation of elliptical galaxies and constraints for the growth of spiral disks (2007, background): “At redshift 1, stellar disks had on average smaller truncation radii (Trujillo & Pohlen 2005) and smaller exponential scalelengths (e.g., Elmegreen et al. 2007b).”
• On the origin of the galaxy star‐formation‐rate sequence: evolution and scatter (2009, background): “…by guest on 30 July 2018 recent observational and theoretical evidence for clumpy disks at high redshifts (e.g. Elmegreen et al. 2007, 2009; Agertz, Teyssier & Moore 2009; Ceverino, Dekel & Bournaud 2009; Dekel, Sari & Ceverino 2009).”
• Compaction and quenching of high-z galaxies in cosmological simulations: blue and red nuggets (2014, background): “While the massive starforming discs of stellar mass∼ 1011M⊙ extend to effective radii of several kpc (Elmegreen et al. 2007; Genzel et al. 2006, 2008), the quenched spheroids of a similar mass have effective radii of order 1 kpc (Carollo et al. 2013; van der Wel et al. 2014).”
• CONSTRAINTS ON THE ASSEMBLY AND DYNAMICS OF GALAXIES. I. DETAILED REST-FRAME OPTICAL MORPHOLOGIES ON KILOPARSEC SCALE OF z ∼ 2 STAR-FORMING GALAXIES (2010, background): “…and disk-like types at higher redshift compared to the local galaxy population (e.g., Lotz, Primack, & Madau 2004; Lotz et al. 2006; Law et al. 2007a; Scarlata et al. 2007a,b; Elmegreen et al. 2007; Pannella et al. 2009), hinting at the diversity of processes driving early galaxy evolution.”
• High-redshift clumpy discs and bulges in cosmological simulations (2009, background): “The large fraction of clumpy massive galaxies at z ∼ 2 (e.g. Elmegreen et al. 2007; Tacconi et al. 2008) suggests that the clumpy phase should last for a few gigayears.”
• MOST SUBMILLIMETER GALAXIES ARE MAJOR MERGERS (2010, background): “…mergers (Lotz et al. 2006; Conselice et al. 2008), or the consequence of clumpy star formation in a kinematically more coherent structure such as an underlying rotating disk (Förster-Schreiber et al. 2006, 2009; Genzel et al. 2006; Elmegreen et al. 2007), or strong and structured extinction.”
• The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, background): “…important central stellar bulge-like component at higher galaxy masses and clumpier appearances towards shorter wavelengths (e.g., Wuyts et al. 2011b, 2012, 2013; Nelson et al. 2013, 2016b; Lang et al. 2014, see also Elmegreen et al. 2007, 2009; Law et al. 2012a; Tacchella et al. 2015b, 2018).”
• On the frequency, intensity, and duration of starburst episodes triggered by galaxy interactions and mergers (2008, background): “In each panel, the black arrows indicate, respectively, the first pericenter passage between the two galaxies and the merger epoch. star formation (see for example Elmegreen et al. 2007), via fragmentation of the gas disk and clump formation (Bournaud et al. 2007a).”
• A DIVERSITY OF PROGENITORS AND HISTORIES FOR ISOLATED SPIRAL GALAXIES (2012, background): “These gas-rich and unstable disks fragment and are observed as having a clumpy morphology in high-redshift galaxy surveys (Elmegreen et al. 2004, 2007).”
• The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies (2015, background): “The stellar components formed at earlier epochs likely evolved into elliptical galaxies and bulges through mergers of the primordial star-forming disks (Elmegreen et al. 2007; Article number, page 1 of 42 ar X iv :1 50 6.”
• Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “…al. 2010), have large velocity dispersion, are turbulent compared to their local counterparts (Förster Schreiber et al. 2006, 2009; Genzel et al. 2006, 2008; Law et al. 2012; Kassin et al. 2012; Stott et al. 2016) and appear unstable to clump formation (Elmegreen et al. 2007; Genzel et al. 2011).”
• From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z ~ 2 from Integral Field Spectroscopy in the SINS Survey (2008, background): “Elmegreen et al. (2007) emphasize that a fairly large fraction of their clumpy HUDF galaxies have radial brightness distributions flatter than those of exponential disks (Sersic indices<1), again similar to that of BX 482 (Fig.”
• Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, background): “We find diverse morphologies, which represent all the main morphological types observed in the UDF, namely discs, spheroids, clump clusters, chain galaxies, tadpoles, mergers, and other irregular types (Elmegreen et al. 2005, 2007).”
• THE THICK DISKS OF SPIRAL GALAXIES AS RELICS FROM GAS-RICH, TURBULENT, CLUMPY DISKS AT HIGH REDSHIFT (2009, background): “The clumps in these galaxies have masses up to a few 108 M⊙, sizes of around a kpc, and likely formed internally by gravitational instabilities (Elmegreen et al. 2007).”
• THE HIDDEN “AGN MAIN SEQUENCE”: EVIDENCE FOR A UNIVERSAL BLACK HOLE ACCRETION TO STAR FORMATION RATE RATIO SINCE z ∼ 2 PRODUCING AN MBH–M* RELATION (2012, background): “Morphological and dynamical studies do find evidence of mergers among these galaxies (e.g., Elmegreen et al. 2007; Förster Schreiber et al. 2009), but being on the MS (Kartaltepe et al. 2011) implies their star-formation is not strongly enhanced by these interactions (Di Matteo et al. 2008).”
• CONSTRAINTS ON THE ASSEMBLY AND DYNAMICS OF GALAXIES. II. PROPERTIES OF KILOPARSEC-SCALE CLUMPS IN REST-FRAME OPTICAL EMISSION OF z ∼ 2 STAR-FORMING GALAXIES (2011, background): “They are found in all types of galaxies atz & 1 including disks identified as such on the basis of their structural properties (Elmegreen & Elmegreen 2005a; Elmegreen et al. 2005b, 2007, 2009a) as well as their kinematics (Genzel et al. 2006, 2008, 2011; Bournaud et al. 2008; Jones et al. 2010).”