ZFIRE: The Evolution of the Stellar Mass Tully–Fisher Relation to Redshift ∼2.2

Straatman, Caroline; Glazebrook, Karl; Kacprzak, Glenn G.; Labbé, Ivo; Nanayakkara, Themiya; Alcorn, Leo Y.; Cowley, Michael J.; Kewley, Lisa J.; Spitler, Lee R.; Tran, Kim‐Vy H.; Yuan, Tiantian

doi:10.3847/1538-4357/aa643e

Cited by 34 publications

(43 citation statements)

References 82 publications

(290 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The median points below = z 1.5 are consistent with a flat slope. The points above = z 1.5 are all above this flat line, consistent with a zero-point shift in the modified Tully-Fisher relation at high redshift (Cresci et al 2009;Price et al 2016;Straatman et al 2017;Übler et al 2017). …”

Section: Evolution Of Dynamical Support S 05 With Timesupporting

confidence: 67%

“…Several active processes, including minor and major mergers, smooth accretion, feedback from star formation, and violent disk instabilities, can disrupt or stall disk formation. Indeed, observations indicate that the internal kinematics of star-forming galaxies at this time have large amounts of disordered motions (as measured by the velocity dispersion of the gas s g ) in addition to ordered rotation (V rot ) (e.g., Förster Schreiber et al 2006Schreiber et al , 2009Genzel et al 2006Genzel et al , 2008Law et al 2007Law et al , 2009Law et al , 2012Wright et al 2007;Wright et al 2009;Shapiro et al 2008;Lemoine-Busserolle et al 2010;Jones et al 2010;Swinbank et al 2011;Glazebrook 2013;Newman et al 2013b;Wisnioski et al 2015;Price et al 2016;Simons et al 2016;Mason et al 2017;Straatman et al 2017). Regardless, the majority of massive star-forming galaxies, * >  M M log 10, at this redshift are rotation-dominated ( s > V g rot ), with at least 70% showing disk-like kinematic signatures (Wisnioski et al 2015).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

z ∼ 2: An Epoch of Disk Assembly

Simons

Kassin

Weiner

et al. 2017

ApJ

133

123

View full text Add to dashboard Cite

We explore the evolution of the internal gas kinematics of star-forming galaxies from the peak of cosmic star formation atz 2 to today. Measurements of galaxy rotation velocity V rot , which quantify ordered motions, and gas velocity dispersion s g , which quantify disordered motions, are adopted from the DEEP2 and SIGMA surveys. This sample covers a continuous baseline in redshift over < < z 0.1 2.5, spanning 10 Gyr. At low redshift, nearly all sufficiently massive star-forming galaxies are rotationally supported (By z=2, 50% and 70% of galaxies are rotationally supported at low ( ) stellar mass, respectively. For, the percentage drops below 35% for all masses. From z=2 to now, galaxies exhibit remarkably smooth kinematic evolution on average. All galaxies tend toward rotational support with time, and higher-mass systems reach it earlier. This is largely due to a mass-independent decline in s g by a factor of 3 since z=2. Over the same time period, V rot increases by a factor of 1.5 in low-mass systems but does not evolve at high mass. These trends in V rot and s g are at a fixed stellar mass and therefore should not be interpreted as evolutionary tracks for galaxy populations. When populations are linked in time via abundance matching, s g declines as before and V rot strongly increases with time for all galaxy populations, enhancing the evolution in s V g rot . These results indicate that = z 2 is a period of disk assembly, during which strong rotational support is only just beginning to emerge.

show abstract

Section: Evolution Of Dynamical Support S 05 With Timesupporting

confidence: 67%

Section: Introductionmentioning

confidence: 99%

z ∼ 2: An Epoch of Disk Assembly

Simons

Kassin

Weiner

et al. 2017

ApJ

133

123

View full text Add to dashboard Cite

show abstract

“…We first estimate the galaxy stellar masses from the tight correlation between stellar mass and the dynamical estimator S05 = √ 0.5 × V 2 max + σ 2 (e.g. Weiner et al 2006;Kassin et al 2007;Price et al 2016;Straatman et al 2017; Figure 3. Mg ii (λ2796) rest equivalent width as a function of impact parameter b for galaxy-quasar pairs classified as wind-pairs.…”

Section: Stellar Massmentioning

confidence: 99%

MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

Schroetter

Bouché

Zabl

et al. 2019

Monthly Notices of the Royal Astronomical Society

136

141

View full text Add to dashboard Cite

We present results from our on-going MusE GAs FLOw and Wind (MEGAFLOW) survey, which consists of 22 quasar lines-of-sight, each observed with the integral field unit (IFU) MUSE and the UVES spectrograph at the ESO Very Large Telescopes (VLT). The goals of this survey are to study the properties of the circum-galactic medium around z ∼ 1 star-forming galaxies. The absorption-line selected survey consists of 79 strong Mg ii absorbers (with rest-frame equivalent width (REW) 0.3Å) and, currently, 86 associated galaxies within 100 projected kpc of the quasar with stellar masses (M ) from 10 9 to 10 11 M . We find that the cool halo gas traced by Mg ii is not isotropically distributed around these galaxies from the strong bi-modal distribution in the azimuthal angle of the apparent location of the quasar with respect to the galaxy major-axis. This supports a scenario in which outflows are bi-conical in nature and co-exist with a coplanar gaseous structure extending at least up to 60 to 80 kpc. Assuming that absorbers near the minor axis probe outflows, the current MEGAFLOW sample allowed us to select 26 galaxy-quasar pairs suitable for studying winds. From this sample, using a simple geometrical model, we find that the outflow velocity only exceeds the escape velocity when M 4 × 10 9 M , implying the cool material is likely to fall back except in the smallest halos. Finally, we find that the mass loading factor η, the ratio between the ejected mass rate and the star formation rate (SFR), appears to be roughly constant with respect to the galaxy mass.

show abstract

“…The success of the angular momentum conservation model put forward by MMW in predicting the structural properties of disc galaxies has been suggested in several works (Somerville et al 2008, Lapi et al 2018b, Kravtsov 2013, Huang et al 2017, Somerville et al 2018, Straatman et al 2017. For instance, Kravtsov 2013 (K13 hereafter) found that a linear relationship between the sizes of galaxies and their haloes, as predicted by eq.…”

Section: Introductionmentioning

confidence: 98%

Galaxy sizes and the galaxy–halo connection – I. The remarkable tightness of the size distributions

Zanisi

Shankar

Lapi

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The mass and structural assembly of galaxies is a matter of intense debate. Current theoretical models predict the existence of a linear relationship between galaxy size (R e ) and the host dark matter halo virial radius (R h ). By making use of semi-empirical models compared to the size distributions of central galaxies from the Sloan Digital Sky Survey, we provide robust constraints on the normalization and scatter of the R e − R h relation. We explore the parameter space of models in which the R e − R h relation is mediated by either the spin parameter or the concentration of the host halo, or a simple constant the nature of which is in principle unknown. We find that the data require extremely tight relations for both early-type and latetype galaxies (ETGs,LTGs), especially for more massive galaxies. These constraints challenge models based solely on angular momentum conservation, which predict significantly wider distributions of galaxy sizes and no trend with stellar mass, if taken at face value. We discuss physically-motivated alterations to the original models that bring the predictions into better agreement with the data. We argue that the measured tight size distributions of SDSS disk galaxies can be reproduced by semi-empirical models in which the R e − R h connection is mediated by the stellar specific angular momenta j st ar . We find that current cosmological models of galaxy formation broadly agree with our constraints for LTGs, and justify the strong link between R e and j st ar that we propose, however the tightness of the R e − R h relation found in such ab-initio theoretical models for ETGs is in tension with our semi-empirical findings.

show abstract

ZFIRE: The Evolution of the Stellar Mass Tully–Fisher Relation to Redshift ∼2.2

Cited by 34 publications

References 82 publications

z ∼ 2: An Epoch of Disk Assembly

z ∼ 2: An Epoch of Disk Assembly

MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

Galaxy sizes and the galaxy–halo connection – I. The remarkable tightness of the size distributions

Contact Info

Product

Resources

About