Chain Galaxies in the Tadpole Advanced Camera for Surveys Field

By D. Elmegreen, Bruce G. Elmegreen, Clara M. Sheets. 2004

148 citations recorded by the source corpus.

Colors and magnitudes were determined for 69 chain galaxies, 58 other linear structures, 32 normal edge-on galaxies, and all of their large star formation clumps in the Hubble Space Telescope Advanced Camera for Surveys field of the Tadpole galaxy. Redshifts of 0.5-2 are inferred from comparisons with published color-evolution models. The linear galaxies have no red nuclear bulges like the normal disk galaxies in our field, but the star formation clumps in each have about the same colors and magnitudes. Light profiles along the linear galaxies tend to be flat, unlike the exponential profiles of normal galaxies. Although the most extreme of the linear objects look like beaded filaments, they are all probably edge-on disks that will evolve to late Hubble type galaxies. The lack of an exponential profile is the result of either a dust scale height that is comparable to the stellar scale height or an intrinsically irregular structure. Examples of galaxies that could be face-on versions of linear galaxies are shown. They have an irregular clumpy structure with no central bulge and with clump colors and magnitudes that are comparable to those in the linear galaxies. Radiative transfer solutions to the magnitudes and surface brightnesses of inclined dusty galaxies suggest that edge-on disks should become more prominent near the detection limit for surface brightness. The surface brightness distribution of the edge-on galaxies in this field confirm this selection effect. The star formation regions are much more massive than in modern galaxies, averaging up to ~109 M☉ for kiloparsec scales.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/5ec49c0eba305d98ab85fa32fc6bb3fe0dd5cdc7

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Citations in the corpus

EVIDENCE FOR A CLUMPY, ROTATING GAS DISK IN A SUBMILLIMETER GALAXY AT z = 4 (2012, background): “Rest–frame UV/optical imaging shows that, unlike low–redshift galaxies, their disks tend to be broken into multiple giant clumps of ∼1 kpc and 109 M⊙ (Elmegreen et al. 2004; Elmegreen & Elmegreen 2005; Förster Schreiber et al. 2006; Genzel et al. 2008).”
EVOLVING GRAVITATIONALLY UNSTABLE DISKS OVER COSMIC TIME: IMPLICATIONS FOR THICK DISK FORMATION (2011, background): “A whole class of galaxies has been observed whose images are dominated by large luminous clumps of gas (Elmegreen et al. 2004, 2005; Förster Schreiber et al. 2009), while measurements of the velocity dispersion of such massive star-forming galaxies have found values near 50 km/s spread across the…”
THE LONG LIVES OF GIANT CLUMPS AND THE BIRTH OF OUTFLOWS IN GAS-RICH GALAXIES AT HIGH REDSHIFT (2013, background): “…galaxies apparent shapes range from round to linear, with the respective fractions expected for face-on to edge-on disks (with ≈ 1 kpc scaleheights, Elmegreen et al. 2004) and disk-like kinematics with high turbulent velocity dispersions in both Hα and CO (Genzel et al. 2006; Shapiro et al.…”
Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation (2014, background): “It does not attain a classical bulge, but may appear as a chain galaxy [253, 254] if it experiences a disk-wide star-burst about 11 Gyr ago which would have build a thick disk [255].”
Bars in Disk-dominated and Bulge-dominated Galaxies at z ~ 0: New Insights from ~3600 SDSS Galaxies (2007, methodology): “Subsequent studies (Jogee et al. 2004; Elmegreen et al. 2004a; Sheth et al. 2003; Zheng et al. 2005) ruled out a dramatic orderof-magnitude decline, and reported a fairly constant optical fraction of strong bars or prominent bars ( 23%Y30”
GOODS-Herschel: the far-infrared view of star formation in active galactic nucleus host galaxies since z ≈ 3 (2011, background): “Since main-sequence galaxies at high redshifts (i.e.,z> 1) are often dominated by gravitationally unstable, clumpy disks (e.g., Cowie et al. 1996; Elmegreen et al. 2004; Elmegreen et al. 2007; Förster Schreiber et al. 2006, 2009; Genzel et al. 2008), wespeculate that disk instabilities are driving…”
BULGE AND CLUMP EVOLUTION IN HUBBLE ULTRA DEEP FIELD CLUMP CLUSTERS, CHAINS AND SPIRAL GALAXIES (2008, background): “The distribution of the ratio of axes among clump cluster and chain galaxies suggests that the chains are edge-on clump clusters (Elmegreen et al. 2004a; Elmegreen & Elmegreen 2005).”
Rotational support of giant clumps in high-z disc galaxies (2011, background): “…light is emitted from a few giant clumps, each of a mass∼ 109M⊙, a characteristic size ∼ 1 kpc that is resolved in HST imaging, and a star-formation rate (SFR) that could reach tens of M⊙ yr −1 (Elmegreen et al. 2004; Elmegreen & Elmegreen 2005; Förster Schreiber et al. 2006; Genzel et al. 2008).”
THE SINS SURVEY OF z ∼ 2 GALAXY KINEMATICS: PROPERTIES OF THE GIANT STAR-FORMING CLUMPS (2010, background): “…Noeske et al. 2007; Daddi et al. 2007; Cameron et al. 2010) are irregular and often dominated by several giant (kpc size) star-forming clumps (Cowie et al. 1995; van den Bergh et al. 1996; Elmegreen et al. 2004, 2007, 2009; Elmegreen & Elmegreen 2005, 2006; Förster Schreiber et al. 2009, 2011).”
SINFONI Integral Field Spectroscopy of z ~ 2 UV-selected Galaxies: Rotation Curves and Dynamical Evolution (2006, methodology): “In the context of the Elmegreen et al. (2004a, 2004b) analysis, SSA22a-MD41 resembles a ‘‘tadpole’’ system, with two bright knots dominating one side of a clumpy disk or ring embedded in a more diffuse emission.”
Bulge Formation by the Coalescence of Giant Clumps in Primordial Disk Galaxies (2008, background): “The earliest stages resemble high-redshift chain galaxies and clump clusters, with kpc-size, 108 M clumps (Cowie et al. 1995; van den Bergh et al. 1996; Elmegreen et al. 2004; Conselice et al. 2004).”
FORMATION OF MASSIVE GALAXIES AT HIGH REDSHIFT: COLD STREAMS, CLUMPY DISKS, AND COMPACT SPHEROIDS (2009, background): “…is that the disk tends to be broken into several giant clumps, of ∼ 1 kpc in size and up to a few times 109M⊙ each, in which most of the star formation occurs (van den Bergh et al. 1996; Elmegreen et al. 2004; Elmegreen & Elmegreen 2005; Förster Schreiber et al. 2006; Genzel et al. 2008).”
THE CLUSTER LENSING AND SUPERNOVA SURVEY WITH HUBBLE: AN OVERVIEW (2011, background): “These galaxies tend to exhibit large star forming “clumps” (Cowie et al. 1995; van den Bergh 1996; Elmegreen et al. 2004a,b), although at least some of these galaxies may form disks with coherent rotation (Genzel et al. 2010).”
Star formation sustained by gas accretion (2014, background): “…at 1 < z < 3 are often clumpy disks (e.g. Glazebrook et al. 1995; Abraham et al. 1996a,b; van den Bergh et al. 1996; Cowie et al. 1995; Im et al. 1999; Elmegreen et al. 2004, 2005, 2007b, 2009; Förster Schreiber et al. 2009) with large SFR in excess of 100 M yr −1 (e.g., Bauer et al. 2011).”