A Survey of Galaxy Kinematics to<i>z</i>∼1 in the TKRS/GOODS‐N Field. II. Evolution in the Tully‐Fisher Relation

Weiner, Benjamin J.; Willmer, Christopher N. A.; Faber, S. M.; Harker, Justin; Kassin, Susan; Phillips, Andrew C.; Melbourne, J.; Metevier, A. J.; Vogt, Nicole P.; Koo, David C.

doi:10.1086/508922

Cited by 119 publications

(172 citation statements)

References 69 publications

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“…Most other observational studies also derived (or assumed) a TFR slope independent of look-back time (e.g., Bamford et al 2006;Miller et al 2011; we note that these authors also relied on an inverse fit for their analysis). Only Weiner et al (2006) reported an increased TFR slope in the range 0.4 < z < 1; however, their results are not directly comparable to ours since the approach by Weiner et al lacks corrections for disk inclination and, in turn, for the inclination-dependent optical beam smearing effect (see Sect. 4.3).…”

Section: Appendix A: Distant Tully-fisher Relation Slopecontrasting

confidence: 86%

Disk galaxy scaling relations at intermediate redshifts

Boehm¹,

Ziegler²

2016

A&A

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Aims. Galaxy scaling relations such as the Tully-Fisher relation (between the maximum rotation velocity V max and luminosity) and the velocity-size relation (between V max and the disk scale length) are powerful tools to quantify the evolution of disk galaxies with cosmic time. Methods. We took spatially resolved slit spectra of 261 field disk galaxies at redshifts up to z ≈ 1 using the FORS instruments of the ESO Very Large Telescope. The targets were selected from the FORS Deep Field and William Herschel Deep Field. Our spectroscopy was complemented with HST/ACS imaging in the F814W filter. We analyzed the ionized gas kinematics by extracting rotation curves from the two-dimensional spectra. Taking into account all geometrical, observational, and instrumental effects, these rotation curves were used to derive the intrinsic V max .Results. Neglecting galaxies with disturbed kinematics or insufficient spatial rotation curve extent, V max was reliably determined for 124 galaxies covering redshifts 0.05 < z < 0.97. This is one of the largest kinematic samples of distant disk galaxies to date. We compared this data set to the local B-band Tully-Fisher relation and the local velocity-size relation. The scatter in both scaling relations is a factor of ∼2 larger at z ≈ 0.5 than at z ≈ 0. The deviations of individual distant galaxies from the local Tully-Fisher relation are systematic in the sense that the galaxies are increasingly overluminous toward higher redshifts, corresponding to an overluminosity ∆M B = −(1.2 ± 0.5) mag at z = 1. This luminosity evolution at given V max is probably driven by younger stellar populations of distant galaxies with respect to their local counterparts, potentially combined with modest changes in dark matter mass fractions. The analysis of the velocity-size relation reveals that disk galaxies of a given V max have grown in size by a factor of ∼1.5 over the past ∼8 Gyr, most likely through accretion of cold gas and/or small satellites. From scrutinizing the combined evolution in luminosity and size, we find that the galaxies that show the strongest evolution toward smaller sizes at z ≈ 1 are not those that feature the strongest evolution in luminosity, and vice versa.

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Section: Appendix A: Distant Tully-fisher Relation Slopecontrasting

confidence: 86%

Disk galaxy scaling relations at intermediate redshifts

Boehm¹,

Ziegler²

2016

A&A

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“…A galaxy undergoing a slow quench is not necessarily quiescent by the time of observation. This SFH model has previously been shown to appropriately characterise quenching galaxies (Weiner et al 2006;Martin et al 2007;Noeske et al 2007;Schawinski et al 2014). …”

Section: And Charlot 2003 Hereafter Bc03) Assumes a Chabrier Imfmentioning

confidence: 98%

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

Smethurst

Masters

Lintott

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Do the theorised different formation mechanisms of fast and slow rotators produce an observable difference in their star formation histories? To study this we identify quenching slow rotators in the MaNGA sample by selecting those which lie below the star forming sequence and identify a sample of quenching fast rotators which were matched in stellar mass. This results in a total sample of 194 kinematically classified galaxies, which is agnostic to visual morphology. We use u − r and N U V − u colours from SDSS and GALEX and an existing inference package, starpy, to conduct a first look at the onset time and exponentially declining rate of quenching of these galaxies. An Anderson-Darling test on the distribution of the inferred quenching rates across the two kinematic populations reveals they are statistically distinguishable (3.2σ). We find that fast rotators quench at a much wider range of rates than slow rotators, consistent with a wide variety of physical processes such as secular evolution, minor mergers, gas accretion and environmentally driven mechanisms. Quenching is more likely to occur at rapid rates (τ ∼ < 1 Gyr) for slow rotators, in agreement with theories suggesting slow rotators are formed in dynamically fast processes, such as major mergers. Interestingly, we also find that a subset of the fast rotators quench at these same rapid rates as the bulk of the slow rotator sample. We therefore discuss how the total gas mass of a merger, rather than the merger mass ratio, may decide a galaxy's ultimate kinematic fate.

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“…If we apply the maximum likelihood method of Weiner et al (2006) to fit the new line-width data (i.e., all the data in the left panel of Figure 1 except those of McGaugh et al 2000), we obtain a slope x = 3.41 ± 0.08 and an intercept log A = 2.91 ± 0.17. If we perform the same exercise with the rotation curve data in the right panel of Figure 1, we obtain x = 3.94 ± 0.11 and log A = 1.81 ± 0.22.…”

Section: Comparison Of the Datamentioning

confidence: 99%

The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

McGaugh

2012

434

459

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The baryonic Tully-Fisher relation (BTFR) is an empirical relation between baryonic mass and rotation velocity in disk galaxies. It provides tests of galaxy formation models in ΛCDM and of alternative theories like modified Newtonian dynamics (MOND). Observations of gas-rich galaxies provide a measure of the slope and normalization of the BTFR that is more accurate (if less precise) than that provided by star-dominated spirals, as their masses are insensitive to the details of stellar population modeling. Recent independent data for such galaxies are consistent with M b = AV 4 f with A = 47 ± 6 M km −4 s 4 . This is equivalent to MOND with a 0 = 1.3 ± 0.3 Å s −2 . The scatter in the data is consistent with being due entirely to observational uncertainties. It is unclear why the physics of galaxy formation in ΛCDM happens to pick out the relation predicted by MOND. We introduce a feedback efficacy parameter E to relate halo properties to those of the galaxies they host. E correlates with star formation rate and gas fraction in the sense that galaxies that have experienced the least star formation have been most impacted by feedback.

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A Survey of Galaxy Kinematics toz∼1 in the TKRS/GOODS‐N Field. II. Evolution in the Tully‐Fisher Relation

Cited by 119 publications

References 69 publications

Disk galaxy scaling relations at intermediate redshifts

Disk galaxy scaling relations at intermediate redshifts

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

The Baryonic Tully–fisher Relation of Gas-Rich Galaxies as a Test of Λcdm and Mond

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