J/MNRAS/495/2265 Velocity dispersions in star-forming galaxies (Varidel+, 2020)
The SAMI galaxy survey: gas velocity dispersions in low-z star-forming galaxies
and the drivers of turbulence.
Varidel M.R., Croom S.M., Lewis G.F., Fisher D.B., Glazebrook K.,
Catinella B., Cortese L., Krumholz M.R., Bland-Hawthorn J., Bryant J.J.,
Groves B., Brough S., Federrath C., Lawrence J.S., Lorente N.P.,
Owers M.S., Richards S.N., Lopez-Sanchez A.R., Sweet S.M., van de Sande J.,
Vaughan S.P.
<Mon. Not. R. Astron. Soc., 495, 2265-2284 (2020)>
=2020MNRAS.495.2265V 2020MNRAS.495.2265V (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Redshifts ; Star Forming Region ;
Velocity dispersion ; Rotational velocities ; Optical
Keywords: methods: data analysis - methods: statistical -
techniques: imaging spectroscopy - galaxies: disc
Abstract:
We infer the intrinsic ionized gas kinematics for 383 star-forming
galaxies across a range of integrated star formation rates
(SFR∈[10-3, 102]M☉/yr) at z~<0.1 using a consistent 3D
forward-modelling technique. The total sample is a combination of
galaxies from the Sydney-AAO Multiobject Integral field Spectrograph
(SAMI) Galaxy survey and DYnamics of Newly Assembled Massive Objects
survey. For typical low-z galaxies taken from the SAMI Galaxy Survey,
we find the vertical velocity dispersion (σv,z) to be
positively correlated with measures of SFR, stellar mass, HI gas mass,
and rotational velocity. The greatest correlation is with SFR surface
density (ΣSFR). Using the total sample, we find σv,z
increases slowly as a function of integrated SFR in the range
SFR∈[10-3, 1] M☉/yr from 17±3 to 24±5km/s followed by a
steeper increase up to σv,z∼80km/s for SFR≳1M☉/yr. This
is consistent with recent theoretical models that suggest a
σv,z floor driven by star formation feedback processes with an
upturn in σv,z at higher SFR driven by gravitational transport
of gas through the disc.
Description:
The SAMI Galaxy Survey was conducted with the SAMI (Croom et al.
2012MNRAS.421..872C 2012MNRAS.421..872C). SAMI was mounted at the Anglo-Australian
Telescope (AAT) that provided a 1° diameter field of view (FoV).
SAMI used 13 fused fibre bundles, known as Hexabundles (Bland-Hawthorn
et al. 2011OExpr..19.2649B 2011OExpr..19.2649B; Bryant et al. 2014MNRAS.438..869B 2014MNRAS.438..869B), with a
75 per cent fill factor. Each bundle contains 61 fibres of 1.6arcsec
diameter, resulting in an approximately 15arcsec diameter FoV. The
integral-field units (IFUs) as well as 26 sky fibres were attached to
pre-drilled plates using magnetic connectors. SAMI fibres were fed to
the double-beam AAOmega spectrograph (Sharp et al.
2006SPIE.6269E..0GS). The 580V grating at 3750-5750Å provides a
resolution of R=1808 (σ=70.4km/s at 4800Å) and the 1000R
grating from 6300-7400Å providing a resolution of R=4304
(σ=29.6km/s at 6850Å; Scott et al. 2018MNRAS.481.2299S 2018MNRAS.481.2299S).
During the survey, observations of over 3000 galaxies were obtained.
Target selection for the SAMI Galaxy Survey is provided in Bryant et
al. (2015MNRAS.447.2857B 2015MNRAS.447.2857B). The redshift range for the observed
galaxies was 0.004<z<0.113 and a stellar mass range of
7.5<log(M*/M☉)<11.6. The full width at half-maximum (FWHM) of
the seeing distribution was 1.10arcsec<FWHMPSF<3.27arcsec. Relevant
data used for the analysis in this paper are from the SAMI Galaxy
Survey DR2 (Scott et al. 2018MNRAS.481.2299S 2018MNRAS.481.2299S). This includes the
aperture spectra, emission line products (Green et al.
2018MNRAS.475..716G 2018MNRAS.475..716G), data cubes (Sharp et al. 2015MNRAS.446.1551S 2015MNRAS.446.1551S),
and input catalogue (Bryant et al. 2015MNRAS.447.2857B 2015MNRAS.447.2857B).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 71 342 Galaxy properties for the sample from the SAMI
Galaxy Survey analysed in this work
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See also:
J/MNRAS/413/971 : Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- ID [8353/6237126] GAMA identifier
8- 16 F9.5 deg RAdeg Right ascension (J2000)
18- 25 F8.5 deg DEdeg Declination (J2000)
27- 31 F5.3 --- zspec Spectroscopic redshift (1)
33- 37 F5.2 [Msun] logM* Logarithm of the stellar mass (2)
39- 43 F5.2 kpc Re Effective radius (2)
45- 48 F4.2 --- e Photometric ellipticity (3)
50- 57 F8.5 [Msun/yr] logSFR ? Logarithm of the star formation rate (4)
59- 61 I3 km/s vtf Tully-Fisher circular velocity at r=2.2Re
(5)
63- 65 I3 km/s vb3d ? Blobby3D inferred circular velocity at
r=2.2Re
67- 68 I2 km/s sigmaLoS Line of sight velocity dispersion
70- 71 I2 km/s sigmaz Vertical velocity dispersion
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Note (1): Spectroscopic redshift from Driver et al. (2011MNRAS.413..971D 2011MNRAS.413..971D,
Cat. J/MNRAS/413/971) and Bryant et al. (2015MNRAS.447.2857B 2015MNRAS.447.2857B)
Note (2): Mass and radius from Taylor et al. (2011MNRAS.418.1587T 2011MNRAS.418.1587T) and
Bryant et al. (2015MNRAS.447.2857B 2015MNRAS.447.2857B)
Note (3): The ellipticity e=1-b/a is taken from Kelvin et al.
(2012MNRAS.421.1007K 2012MNRAS.421.1007K) and Bryant et al. (2015MNRAS.447.2857B 2015MNRAS.447.2857B)
Note (4): Star formation rate from the GAMA survey (Gunawardhana et al.
2013MNRAS.433.2764G 2013MNRAS.433.2764G; Davies et al. 2013MNRAS.433.2764G 2013MNRAS.433.2764G and
Driver et al. 2018MNRAS.475.2891D 2018MNRAS.475.2891D)
Note (5): vtf is calculated using the relationship proposed by Bloom et al.
(2017MNRAS.472.1809B 2017MNRAS.472.1809B)
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 14-Jun-2023