THE EPOCH OF DISK SETTLING: z ∼ 1 TO NOW

By S. Kassin, B. Weiner, S. Faber, J. Gardner, C. Willmer, A. Coil, M. Cooper, J. Devriendt, A. Dutton, P. Guhathakurta and 4 more. 2012

132 citations recorded by the source corpus.

We present evidence from a sample of 544 galaxies from the DEEP2 Survey for evolution of the internal kinematics of blue galaxies with stellar masses ranging 8.0 < log M*(M☉) < 10.7 over 0.2 < z < 1.2. DEEP2 provides galaxy spectra and Hubble imaging from which we measure emission-line kinematics and galaxy inclinations, respectively. Our large sample allows us to overcome scatter intrinsic to galaxy properties in order to examine trends in kinematics. We find that at a fixed stellar mass, galaxies systematically decrease in disordered motions and increase in rotation velocity and potential well depth with time. Massive galaxies are the most well ordered at all times examined, with higher rotation velocities and less disordered motions than less massive galaxies. We quantify disordered motions with an integrated gas velocity dispersion corrected for beam smearing (σg). It is unlike the typical pressure-supported velocity dispersion measured for early type galaxies and galaxy bulges. Because both seeing and the width of our spectral slits comprise a significant fraction of the galaxy sizes, σg integrates over velocity gradients on large scales which can correspond to non-ordered gas kinematics. We compile measurements of galaxy kinematics from the literature over 1.2 < z < 3.8 and do not find any trends with redshift, likely for the most part, because these data sets are biased toward the most highly star-forming systems. In summary, over the last ∼8 billion years since z = 1.2, blue galaxies evolve from disordered to ordered systems as they settle to become the rotation-dominated disk galaxies observed in the universe today, with the most massive galaxies being the most evolved at any time.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d672582463d4a807cc6fc2ea3e99cd67ef5c90c6

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Citations in the corpus

ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, methodology): “This indicates that the disk may have entered an epoch of “disk settling”, as seen in the DEEP2 Survey (Kassin et al. 2012) for galaxies of stellar mass 8.0< logM?”
The KMOS Redshift One Spectroscopic Survey (KROSS):dynamical properties, gas and dark matter fractions of typical z~1 star-forming galaxies (2016, methodology): “DEEP2 is based on slit spectroscopy so again may not be directly comparable.”
THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, background): “However, between z ∼ 2 to z ∼ 1 an accurate measurement of the degree of evolution has not been possible due to a lack of consistent or sizeable datasets (e.g. Epinat et al. 2012; Kassin et al. 2012).”
SUPER-CRITICAL GROWTH OF MASSIVE BLACK HOLES FROM STELLAR-MASS SEEDS (2014, background): “Observations show that, at a fixed stellar mass, galaxies systematically increase in disordered motions and decrease in rotation velocity with increasing redshift and decreasing potential (Kassin et al. 2012).”
FORMING COMPACT MASSIVE GALAXIES (2015, background): “They should not be confused with the rotation-corrected gas dispersions within spatiallyresolved disks, such as discussed by, e.g., Kassin et al. (2012) and Förster Schreiber et al. (2014).”
Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, result): “The emergence of such stable gaseous discs at late times is consistent with observational studies (Kassin et al. 2012).”
Dancing in the dark: galactic properties trace spin swings along the cosmic web (2014, background): “…there could be a significant amount of redistribution of angular momentum within the inner regions of haloes (Kimm et al. 2011; Danovich et al. 2012; Dubois et al. 2012b; Kassin et al. 2012a,b; Tillson et al. 2012), and as a consequence, galaxies misalign with the spin of their host halo (see Fig.”
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).”