The Stellar Mass Tully-Fisher Relation to z = 1.2 from AEGIS

By S. Kassin, B. Weiner, S. Faber, D. Koo, J. Lotz, J. Diemand, J. Harker, K. Bundy, A. Metevier, A. Phillips and 5 more. 2006

172 citations recorded by the source corpus.

We combine newly measured rotation velocities, velocity dispersions, and stellar masses to construct stellar mass Tully-Fisher relations (M*TFRs) for 544 galaxies with strong emission lines at 0.1 < z < 1.2 from the All-Wavelength Extended Groth Strip International Survey (AEGIS) and the Deep Extragalactic Evolutionary Probe 2 (DEEP2) survey. The conventional M*TFR using only rotation velocity (Vrot) shows large scatter (~1.5 dex in velocity). The scatter and residuals are correlated with morphology in the sense that disturbed, compact, and major merger galaxies have lower velocities for their masses. We construct an M*TFR using the kinematic estimator S0.5, which is defined as 1/2 and accounts for disordered or noncircular motions through the gas velocity dispersion (σg). The new M*TFR, termed S0.5/M*TFR, is remarkably tight over 0.1 < z < 1.2, with no detectable evolution of its intercept or slope with redshift. The average best-fit relation has 0.47 dex scatter in stellar mass, corresponding to ~1.2 "magnitudes," assuming a constant mass-to-light ratio. Interestingly, the S0.5/M*TFR is consistent with the absorption-line-based stellar mass Faber-Jackson relation for nearby elliptical galaxies in terms of slope and intercept, which might suggest a physical connection between the two relations.

Subfields: Astronomy and Astrophysics, Instrumentation

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THE SINS SURVEY: MODELING THE DYNAMICS OF z ∼ 2 GALAXIES AND THE HIGH-z TULLY–FISHER RELATION (2009, methodology): “5 Tully-Fisher relation Kassin et al. (2007) have constructed a stellar mass TFR at z .”
THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, background): “The TF relation appears to be already in place at high-redshifts z ≥ 1 (Kassin et al. 2007; Puech et al. 2008; Epinat et al. 2009; Cresci et al. 2009) and has evolved by a factor of 2.5 at a given mass (Cresci et al. 2009) from z ≃ 2.2 to the present.”
SIMULATION OF THE COSMIC EVOLUTION OF ATOMIC AND MOLECULAR HYDROGEN IN GALAXIES (2009, unknown): “Kassin et al. (2007) noted that S0.”
Evidence for strong dynamical evolution in disc galaxies through the last 11 Gyr. GHASP VIII – a local reference sample of rotating disc galaxies for high‐redshift studies (2009, background): “Kassin et al. (2007) showed from long slit spectroscopy kinematical data and HST restframe B-band morphology that a correlation be- tween peculiar kinematics and peculiar or merger-like morphology exists at z ∼ 1.”
The Tully-Fisher relations of early-type spiral and S0 galaxies (2010, background): “Conselice et al. (2005), Flores et al. (2006) and Kassin et al. (2007) find no evidence for evolution in either the slope or zeropoint of the K-band spiral TFR from the local universe to z ≈ 1.”
THE NEXT GENERATION VIRGO CLUSTER SURVEY (NGVS). I. INTRODUCTION TO THE SURVEY (2012, background): “The NGVS will allow an important first step toward defining a unified set of scaling relations to describe galaxies of different mass and morphology (e.g., Kassin et al. 2007; Dutton et al. 2010, 2011; McLaughlin et al. 2012).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, result): “…we assume does not evolve with redshift (as suggested by a large number of observations at least to z 1:5, and by some to zk 3; Conselice et al. 2005; Flores et al. 2006; Bell et al. 2006b; Kassin et al. 2007; van Dokkum et al. 2004), but we have tried all three estimators and find similar results.”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, background): “‡‡ It is interesting to note that Kassin et al. (2007) also consider the combination of the rotational velocity and velocity dispersion of the gas when studying the redshift evolution of the stellar mass Tully-Fisher relation, but find that the scatter is reduced with respect to using gas…”
The structures of distant galaxies – III. The merger history of over 20 000 massive galaxies at z < 1.2 (2008, background): “These studies have found that galaxies with evidence for merging, both kinematically (e.g., Kassin et al. 2007), and through visual inspection, have high asymmetries, and likewise the non-mergers are not asymmetric.”
Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations (2016, methodology): “This result has been further supported and generalized in Kassin et al. (2007) from z ∼ 1 to z ∼ 0, based on fairly large samples of galaxies from AEGIS and DEEP2 and adopting the indicator S20.”
ZFIRE: THE KINEMATICS OF STAR-FORMING GALAXIES AS A FUNCTION OF ENVIRONMENT AT z ∼ 2 (2016, background): “Observations of field galaxies show that stellar-mass scaling relations stay relatively consistent with local measurements until z ∼ 1.7 (Kassin et al. 2007; Miller et al. 2011; Di Teodoro et al. 2016).”
THE EPOCH OF DISK SETTLING: z ∼ 1 TO NOW (2012, background): “Kassin et al. (2007) (hereafter K07) followed up on Weiner et al. (2006a,b).”
DISSIPATION AND EXTRA LIGHT IN GALACTIC NUCLEI. IV. EVOLUTION IN THE SCALING RELATIONS OF SPHEROIDS (2008, methodology): “This is also reflected in e.g. the baryonic Tully-Fisher relation, which appears to evolve negligibly from z = 0− 2 (Conselice et al. 2005; Flores et al. 2006; Kassin et al. 2007; van Dokkum et al. 2004).”
THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION, AND REDSHIFTS (2012, background): “• The roots of the Tully-Fisher relation are visible out to z ∼ 1 (Kassin et al. 2007).”
An Explanation for the Observed Weak Size Evolution of Disk Galaxies (2006, background): “…particularly in terms of stellar or baryonic mass, remain uncertain, but Conselice et al. (2005) found no evolution in the K-band or stellar mass Tully-Fisher to z ∼ 1, and Kassin et al. (2007) also find no evolution to z ∼ 1 in a redefined version of the stellar mass Tully-Fisher relation16.”
The effects of gas on morphological transformation in mergers: implications for bulge and disc demographics (2009, background): “…(Governato et al. 2007, 2008), and may be seen in observations of high-redshift discs that are perhaps reforming after mergers (van Dokkum et al. 2004; Kassin et al. 2007; Genzel et al. 2008; Puech et al. 2008; Robertson & Bullock 2008a; Shapiro et al. 2008; van Starkenburg et al. 2008).”
The KMOS Redshift One Spectroscopic Survey (KROSS):dynamical properties, gas and dark matter fractions of typical z~1 star-forming galaxies (2016, background): “…morphologies, SFRs, metallicities and gas content etc. of these galaxies (e.g. Doherty et al. 2004, 2006; Bell et al. 2005, 2012; Erb et al. 2006a,b; Kassin et al. 2007, 2012; Buitrago et al. 2008; Dunne et al. 2009; Peng et al. 2010; Geach et al. 2011; van Dokkum et al. 2011; Stott et al.…”
Cool outflows in galaxies and their implications (2020, background): “…rotation velocity and velocity dispersion of the ISM in the host galaxy) and scales with the stellar mass following log S = 0.29 log M∗–0.93, where S is in km s−1 and M∗ is in M (Weiner et al. 2006; Kassin et al. 2007), in low-z star-forming galaxies (Heckman et al. 2015; Simons et al. 2015).”