BULGE AND CLUMP EVOLUTION IN HUBBLE ULTRA DEEP FIELD CLUMP CLUSTERS, CHAINS AND SPIRAL GALAXIES

By Bruce G. Elmegreen, D. Elmegreen, María Ximena Fernández, J. Lemonias. 2008

174 citations recorded by the source corpus.

Clump clusters and chain galaxies in the Hubble Ultra Deep Field (UDF) are examined for bulges in Near-Infrared Camera Multi-Object Spectrometer images. Approximately 50% of the clump clusters and 30% of the chains have relatively red and massive clumps that could be young bulges. Magnitudes and colors are determined for these bulgelike objects and for the bulges in spiral galaxies, and for all of the prominent star formation clumps in these three galaxy types. The colors are fitted to population evolution models to determine the bulge and clump masses, ages, star formation rate decay times, and extinctions. The results indicate that bulgelike objects in clump clusters and chain galaxies have similar ages and two to five times larger masses compared to the star formation clumps, while the bulges in spirals have roughly six times larger ages and 20 to 30 times larger masses than the clumps. All systems appear to have an underlying red disk population. The masses of star-forming clumps are typically in a range from 107 to 108 M☉; their ages have a wide range around ∼102 Myr. Ages and extinctions both decrease with redshift. Star formation is probably the result of gravitational instabilities in the disk gas, in which case the large clump mass in the UDF is the result of a high gas velocity dispersion, 30 km s−1 or more, combined with a high gas mass column density, ∼100 M☉ pc−2. Because clump clusters and chains dominate disk galaxies beyond z ∼ 1, the observations suggest that these types represent an early phase in the formation of modern spiral galaxies, when the bulge and inner disk formed.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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In Electrical and Electronic Engineering

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Citations in the corpus

• Rotational support of giant clumps in high-z disc galaxies (2011, background): “The typical ages of the stellar populations in these clumps are crudely estimated to range from one to several hundred Myr (Elmegreen et al. 2009; Förster Schreiber et al. 2009), on the order of ten dynamical times, indicating that the clumps survive for such durations, but do not age unperturbed f”
• The SLUGGS Survey: kinematics for over 2500 globular clusters in 12 early-type galaxies (2012, background): “At this redshift, galaxies are characterized by fast rotating thick discs (Elmegreen et al. 2009) fragmented into superstarforming clumps.”
• Evolution of density profiles in high-z galaxies: compaction and quenching inside-out (2015, background): “Several studies have investigated the stellar mass density distribution within galaxies at high redshifts (e.g., Elmegreen et al. 2009; Förster Schreiber et al. 2011; Wuyts et al. 2012; van Dokkum et al. 2013; Patel et al. 2013; Lang et al. 2014; Morishita et al. 2015).”
• A CANDELS–3D-HST SYNERGY: RESOLVED STAR FORMATION PATTERNS AT 0.7 < z < 1.5 (2013, methodology): “Indeed, such features, and more generally irregular morphologies, have been abundantly reported in high-redshift SFGs (albeit on monochromatic, and often rest-UV or Hα images; see, e.g., Elmegreen et al. 2004, 2009a; Genzel et al. 2008, 2011).”
• SHORT-LIVED STAR-FORMING GIANT CLUMPS IN COSMOLOGICAL SIMULATIONS OF z ≈ 2 DISKS (2010, background): “The short lifetimes we find are consistent with the upper limits of ≈ 300− 500Myr derived for the stellar populations 6 Genel et al. in the clumps (Elmegreen et al. 2009; Förster Schreiber et al. 2011a).”
• FORMATION OF MASSIVE GALAXIES AT HIGH REDSHIFT: COLD STREAMS, CLUMPY DISKS, AND COMPACT SPHEROIDS (2009, background): “Observational evidence for this comes so far only from the thickness of the old stellar disk in “chain” galaxies as indicated by IR measurements, which is comparable to the thickness in the UV, associated with stars in formation and therefore gas (Elmegreen et al. 2009).”
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• 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, methodology): “As argued by Elmegreen et al. (2009a, see also Elmegreen et al. 2009c), the inferred clump ages and the presence of a redder and more massive clump generally closer to the center in clumpy and spiral types are consistent with inward clump migration, and suggest that at least a fraction of the…”
• PHIBSS: Unified Scaling Relations of Gas Depletion Time and Molecular Gas Fractions (2017, background): “…(sSFR), gas fractions, and metallicities as a function of redshift, with only modest changes as compared to z=0 MS-star formation physics (e.g. Elmegreen et al. 2009, Krumholz & Dekel 2010, Elbaz et al. 2010, 2011, Gracia-Carpio et al. 2011, Nordon et al. 2012, Lilly et al. 2013, Peng &…”
• IMAGING THE MOLECULAR GAS IN A SUBMILLIMETER GALAXY AT z = 4.05: COLD MODE ACCRETION OR A MAJOR MERGER? (2010, background): “These star forming regions then migrate to the galaxy center via dynamical friction and viscosity, forming compact stellar bulges (Genzel et al. 2006; Genzel et al. 2008; Bournaud et al. 2008a,b; Elmegreen et al. 2009).”
• THE THICK DISKS OF SPIRAL GALAXIES AS RELICS FROM GAS-RICH, TURBULENT, CLUMPY DISKS AT HIGH REDSHIFT (2009, background): “Observations of galaxies around that epoch show a large population of rotating disks that are clumpy and turbulent (Elmegreen & Elmegreen 2005; Genzel et al. 2008; Shapiro et al. 2008; Elmegreen et al. 2009a,b).”
• Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks (2009, methodology): “This trend continues towards the flocculent and grand design spiral galaxies we observe today (Elmegreen et al. 2009b).”
• NEWLY QUENCHED GALAXIES AS THE CAUSE FOR THE APPARENT EVOLUTION IN AVERAGE SIZE OF THE POPULATION (2013, background): “…morphological diversity of the high redshift galaxy population, which becomes increasingly irregular/clumpy and problematic for model fitting codes (Elmegreen et al. 2009; Oesch et al. 2010), and the stability (i.e., predictability) of its systematic biases, which can thus be robustly corrected,…”
• THE INTERSTELLAR MEDIUM IN DISTANT STAR-FORMING GALAXIES: TURBULENT PRESSURE, FRAGMENTATION, AND CLOUD SCALING RELATIONS IN A DENSE GAS DISK AT z = 2.3 (2011, background): “Thus, the brightest star-forming regions in the galaxy make up approximately ∼ 10 per cent of the total baryonic mass in the disk (see also Genzel et al. 2010; Elmegreen et al. 2009).”
• The ATLAS3D project – III. A census of the stellar angular momentum within the effective radius of early‐type galaxies: unveiling the distribution of fast and slow rotators (2011, background): “…disc-like objects, expected to be relevant mostly at high redshift: in such a situation, strong instabilities lead the galaxy to become ‘clumpy’, with massive gas clouds forming stars and evolving as a N-body system with low N (see e.g. Elmegreen, Bournaud & Elmegreen 2008; Elmegreen et al. 2009).”
• Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, background): “The central regions tend to be redder, at z ∼ 1–4 often surrounded by bluer ‘clumps’, which by comparison to the gas maps can be identified as large star-forming regions, resembling observed galaxies (Genzel et al. 2008; Elmegreen et al. 2009; Cameron et al. 2011; Förster Schreiber et al. 2011).”
• CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “Many star-forming galaxies at z ≈ 2 have compact sizes, high surface densities and high gas fractions (Tacconi et al. 2010), and exhibit star-forming clumps more massive than local star clusters (Elmegreen et al. 2009).”