A transition mass in the local Tully–Fisher relation

Simons, Raymond C.; Kassin, Susan; Weiner, Benjamin J.; Heckman, Timothy M.; Lee, Janice; Lotz, Jennifer M.; Peth, Michael; Tchernyshyov, Kirill

doi:10.1093/mnras/stv1298

Cited by 63 publications

(95 citation statements)

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“…Fig 8 shows our TFR in comparison with those from Green et al (2013) and Simons et al (2015) and our linear fit from Fig. 3 in comparison to that from Reyes et al (2011).…”

Section: D Spatially Resolved Tfrmentioning

confidence: 99%

“…There have been extensive TFR studies with single slit and fibre measurements [Tully & Fisher (1977), Courteau (1997), Böhm et al (2004), Mocz et al (2012) and others]. Despite the success of fibre and slit-based measurements in determining the TFR, they are vulnerable to potential errors introduced by slit placement (Spekkens et al 2005;Oh et al 2011;Simons et al 2015) and aperture effects. It is also difficult to investigate spatial variation across an extended source using a single slit.…”

Section: Introductionmentioning

confidence: 99%

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The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

Bloom

Croom

Bryant

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate the Tully-Fisher Relation (TFR) for a morphologically and kinematically diverse sample of galaxies from the SAMI Galaxy Survey using 2 dimensional spatially resolved Hα velocity maps and find a well defined relation across the stellar mass range of 8.0 < log(M * /M ) < 11.5.We use an adaptation of kinemetry to parametrise the kinematic Hα asymmetry of all galaxies in the sample, and find a correlation between scatter (i.e. residuals off the TFR) and asymmetry. This effect is pronounced at low stellar mass, corresponding to the inverse relationship between stellar mass and kinematic asymmetry found in previous work. For galaxies with log(M * /M ) < 9.5, 25 ± 3% are scattered below the root mean square (RMS) of the TFR, whereas for galaxies with log(M * /M ) > 9.5 the fraction is 10 ± 1%We use 'simulated slits' to directly compare our results with those from long slit spectroscopy and find that aligning slits with the photometric, rather than the kinematic, position angle, increases global scatter below the TFR. Further, kinematic asymmetry is correlated with misalignment between the photometric and kinematic position angles. This work demonstrates the value of 2D spatially resolved kinematics for accurate TFR studies; integral field spectroscopy reduces the underestimation of rotation velocity that can occur from slit positioning off the kinematic axis.

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“…Fig 8 shows our TFR in comparison with those from Green et al (2013) and Simons et al (2015) and our linear fit from Fig. 3 in comparison to that from Reyes et al (2011).…”

Section: D Spatially Resolved Tfrmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

Bloom

Croom

Bryant

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…As a result, low-mass galaxies are thought to have highly stochastic and bursty SFRs (for example, Gerola et al 1980;Stinson et al 2007;McQuinn et al 2010;Weisz et al 2011;González-Samaniego et al 2014), which in turn can have significant effects on these galaxies' dynamical and morphological evolution. For instance, bursty star formation may explain the lack of coherent, rotationally supported disks in galaxies with M star 10 9.5 M e Muratov et al 2015;Simons et al 2015) and the fact that starforming galaxies are more likely to be dispersion-supported at low mass than at high mass (Roychowdhury et al 2010;Sánchez-Janssen et al 2010;Teyssier et al 2013;Wheeler et al 2015). Many studies have shown that stellar feedback-driven gas outflows can displace a significant fraction of a galaxy's total gas mass (for example, Mathews & Baker 1971;Haehnelt 1995;Christensen et al 2015;Muratov et al 2015), and several recent works have investigated how the resulting time-varying potential can transfer orbital energy to dark matter.…”

Section: Introductionmentioning

confidence: 99%

Breathing Fire: How Stellar Feedback Drives Radial Migration, Rapid Size Fluctuations, and Population Gradients in Low-Mass Galaxies

El-Badry

Wetzel

Geha

et al. 2016

ApJ

273

306

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We examine the effects of stellar feedback and bursty star formation on low-mass galaxies (M star =2×10 6 −5×1010 M e ) using the Feedback in Realistic Environments (FIRE) simulations. While previous studies emphasized the impact of feedback on dark matter profiles, we investigate the impact on the stellar component: kinematics, radial migration, size evolution, and population gradients. Feedback-driven outflows/ inflows drive significant radial stellar migration over both short and long timescales via two processes: (1) outflowing/infalling gas can remain star-forming, producing young stars that migrate ∼1 kpc within their first 100 Myr, and (2) gas outflows/inflows drive strong fluctuations in the global potential, transferring energy to all stars. These processes produce several dramatic effects. First, galaxies' effective radii can fluctuate by factors of >2 over ∼200 Myr, and these rapid size fluctuations can account for much of the observed scatter in the radius at fixed M star . Second, the cumulative effects of many outflow/infall episodes steadily heat stellar orbits, causing old stars to migrate outward most strongly. This age-dependent radial migration mixes-and even inverts-intrinsic age and metallicity gradients. Thus, the galactic-archaeology approach of calculating radial star formation histories from stellar populations at z=0 can be severely biased. These effects are strongest at M star ≈10 7-9.6 M e , the same regime where feedback most efficiently cores galaxies. Thus, detailed measurements of stellar kinematics in low-mass galaxies can strongly constrain feedback models and test baryonic solutions to small-scale problems in ΛCDM.

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“…Locally: the majority of high mass galaxies are ordered rotating disks, with kinematically disordered galaxies appearing only below a stellar mass of log M * /M < 9.5 (Simons et al 2015). However, it is unclear whether the kinematic downsizing picture extends beyond z ∼ 1.2 and into the peak of cosmic star-formation.…”

Section: Introductionmentioning

confidence: 99%

KINEMATIC DOWNSIZING AT z ∼ 2

Simons

Kassin

Trump

et al. 2016

ApJ

Self Cite

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We present results from a survey of the internal kinematics of 49 star-forming galaxies at z ∼ 2 in the CANDELS fields with the Keck/MOSFIRE spectrograph (SIGMA, Survey in the near-Infrared of Galaxies with Multiple position Angles). Kinematics (rotation velocity V rot and integrated gas velocity dispersion σ g ) are measured from nebular emission lines which trace the hot ionized gas surrounding star-forming regions. We find that by z ∼ 2, massive star-forming galaxies (log M * /M 10.2) have assembled primitive disks: their kinematics are dominated by rotation, they are consistent with a marginally stable disk model, and they form a Tully-Fisher relation. These massive galaxies have values of V rot /σ g which are factors of 2-5 lower than local well-ordered galaxies at similar masses. Such results are consistent with findings by other studies. We find that low mass galaxies (log M * /M 10.2) at this epoch are still in the early stages of disk assembly: their kinematics are often supported by gas velocity dispersion and they fall from the Tully-Fisher relation to significantly low values of V rot . This "kinematic downsizing" implies that the process(es) responsible for disrupting disks at z ∼ 2 have a stronger effect and/or are more active in low mass systems. In conclusion, we find that the period of rapid stellar mass growth at z ∼ 2 is coincident with the nascent assembly of low mass disks and the assembly and settling of high mass disks.

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A transition mass in the local Tully–Fisher relation

Cited by 63 publications

References 100 publications

The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation

Breathing Fire: How Stellar Feedback Drives Radial Migration, Rapid Size Fluctuations, and Population Gradients in Low-Mass Galaxies

KINEMATIC DOWNSIZING AT z ∼ 2

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