J/A+A/584/A87 CALIFA sample SFR calibration (Catalan-Torrecilla+, 2015)
Star formation in the local Universe from the CALIFA sample.
I. Calibrating the SFR using integral field spectroscopy data.
Catalan-Torrecilla C., Gil de Paz A., Castillo-Morales A.,
Iglesias-Paramo J., Sanchez S.F., Kennicutt R.C., Perez-Gonzalez P.G.,
Marino R.A., Walcher C.J., Husemann B., Garcia-Benito R., Mast D.,
Gonzalez Delgado R.M., Munoz-Mateos J.C., Bland-Hawthorn J., Bomans D.J.,
Del Olmo A., Galbany L., Gomes J.M., Kehrig C., Lopez-Sanchez A.R.,
Mendoza M.A., Monreal-Ibero A., Perez-Torres M., Sanchez-Blazquez P.,
Vilchez J.M., (the Califa collaboration)
<Astron. Astrophys., 584, A87-87 (2015)>
=2015A&A...584A..87C 2015A&A...584A..87C (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Photometry, H-alpha ; Ultraviolet ;
Photometry, infrared
Keywords: galaxies: star formation - galaxies: spiral - galaxies: evolution -
techniques: photometric - techniques: spectroscopic
Abstract:
The star formation rate (SFR) is one of the main parameters used to
analyze the evolution of galaxies through time. The need for
recovering the light reprocessed by dust commonly requires the use of
low spatial resolution far-infrared data. Recombination line
luminosities provide an alternative, although uncertain
dust-extinction corrections based on narrowband imaging or long-slit
spectroscopy have traditionally posed a limit to their applicability.
Integral field spectroscopy (IFS) is clearly the way to overcome this
kind of limitation. We obtain integrated Hα, ultraviolet (UV)
and infrared (IR)-based SFR measurements for 272 galaxies from the
CALIFA survey at 0.005<z<0.03 using single-band and hybrid tracers. We
aim to determine whether the extinction-corrected Hα
luminosities provide a good measure of the SFR and to shed light on
the origin of the discrepancies between tracers. Updated calibrations
referred to Hα are provided. The well-defined selection criteria
and large statistics allow us to carry out this analysis globally and
split by properties, including stellar mass and morphological type. We
derive integrated, extinction-corrected Hα fluxes from CALIFA,
UV surface and asymptotic photometry from GALEX and integrated WISE
22µm and IRAS fluxes. We find that the extinction-corrected
Hα luminosity agrees with the hybrid updated SFR estimators
based on either UV or Hα plus IR luminosity over the full range
of SFRs (0.03-20M☉/yr). The coefficient that weights the amount
of energy produced by newly-born stars that is reprocessed by dust on
the hybrid tracers, aIR, shows a large dispersion. However, this
coefficient does not became increasingly small at high attenuations,
as expected if significant highly-obscured Hα emission were
missed, i.e., after a Balmer decrement-based attenuation correction is
applied. Lenticulars, early-type spirals, and type-2 AGN host galaxies
show smaller coefficients because of the contribution of optical
photons and AGN to dust heating. In the local Universe, the Hα
luminosity derived from IFS observations can be used to measure SFR,
at least in statistically-significant, optically-selected galaxy
samples, once stellar continuum absorption and dust attenuation
effects are accounted for. The analysis of the SFR calibrations by
galaxies properties could potentially be used by other works to study
the impact of different selection criteria in the SFR values derived,
and to disentangle selection effects from other physically motivated
differences, such as environmental or evolutionary effects.
Description:
The galaxies we studied are part of the CALIFA survey (Sanchez et al.,
2012A&A...538A...8S 2012A&A...538A...8S). The CALIFA mother sample includes 939 galaxies
of all types. A total of ∼600 galaxies will be observed as part of
CALIFA, using the Potsdam Multi-Aperture Spectrophotometer (PMAS) in
the PPak mode mounted at the Calar Alto 3.5m telescope. The survey is
described in detail in the presentation article (Sanchez et al.,
2012A&A...538A...8S 2012A&A...538A...8S).
The CALIFA spectra cover the range 3650-7500Å in two overlapping
setups, one in the red (3745-7500Å) at a spectral resolution of
R∼850 (V500 setup) and one in the blue (3650-4840Å) at R∼1650
(V1200 setup), where the resolutions quoted are those at the
overlapping wavelength range (λ∼4500Å). For the purpose of
deriving extinction-corrected Hα luminosities, we make use of
the V500 setup as we are interested in having both
Hαλ4861Å and Hβλ6563Å emission lines in
the same observing range.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 138 271 Integrated measurements for the CALIFA galaxies
--------------------------------------------------------------------------------
See also:
J/A+A/573/A59 : Gas kinematics in CALIFA survey (Garcia-Lorenzo+, 2015)
J/A+A/576/A135 : CALIFA DR2 (Garcia-Benito+, 2015)
J/A+A/581/A103 : CALIFA survey across the Hubble sequence (Gonzalez+, 2015)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- ID CALIFA identifier
5- 18 A14 --- Name Galaxy name
20- 22 A3 --- Type Morphological type
24- 29 F6.2 Mpc Dist Distance in Mpc calculated from redshift
31- 34 F4.2 --- b/a Minor-to-major axis ratio as given by the
RC3 catalog, i.e., measured in the D25
B-band isophote
36- 43 F8.2 10-19/m2 FHaobs Observed-Hα flux using an elliptical
aperture with a semimajor axis of 36 arcsec
45- 50 F6.2 10-19/m2 e_FHaobs rms uncertainty on F(Haobs)
52- 55 F4.2 mag AHa Attenuation obtained using the Balmer
decrement (1)
57- 60 F4.2 mag e_AHa rms uncertainty on A(Ha)
62- 67 F6.2 10+33W LHaobs Observed Ha luminosity corrected for
aperture effects
69- 73 F5.2 10+33W e_LHaobs rms uncertainty on L(Haobs)
75- 79 F5.2 Msun/yr SFRHacorr Balmer-corrected and aperture-corrected
Ha SFR values
81- 84 F4.2 Msun/yr e_SFRHacorr rms uncertainty on SFR[Hacorr]
86- 90 F5.2 10+35W LFUVobs ?=- observed FUV luminosity
92- 95 F4.2 10+35W e_LFUVobs ? rms uncertainty on L(FUVobs)
97-102 F6.2 10+35W LNUVobs ?=- observed NUV luminosity
104-108 F5.2 10+35W e_LNUVobs ? rms uncertainty on L(NUVobs)
110-113 F4.2 mag F-N ?=- UV color in AB system
115-120 F6.2 10+36W LTIR ?=- TIR luminosity defined as the total
infrared emission in the range 8-1000um
122-126 F5.2 10+36W e_LTIR ? rms uncertainty on L(TIR)
128-133 F6.2 10+35W L22um ?=- 22um (aperture photometry)
luminosity (2)
135-138 F4.2 10+35W e_L22um ? rms uncertainty on L(22um)
--------------------------------------------------------------------------------
Note (1): As explained in Sect. 3.1.4, we have assumed an intrinsic Ha/Hb ratio
of 2.86 (although lower values are also physically possible in HII regions,
depending on the electron density, effective temperature, and therefore on
the chemical abundance. This leads to a number of galaxies for which we
assumed A(Ha)=0 that also appeared in this table).
The errors listed here only use the Ha flux uncertainty, an additional
7% uncertainty in the Hb flux have been taken into account for the errors in
the Ha luminosities and SFRs and in the attenuations used in the paper.
Note (2): As explained in Sect. 3.3, it has been pointed out by several authors
(Wright et al., 2010AJ....140.1868W 2010AJ....140.1868W; Jarrett et al., 2013AJ....145....6J 2013AJ....145....6J;
Brown et al., 2014, Cat. J/ApJS/212/18) that SF galaxies measured with the
WISE 22um filter are systematically brighter by ∼10 % than that inferred from
Spitzer IRS and 24um data. For that reason, the 22um luminosity values given
in L22um have to be multiplied by 1/1.1. Note that galaxies UGC 00987 and
UGC 03973 are classified as type-1 AGN within our sample. As a consequence,
they have been excluded from the SFR analysis.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Catalan-Torrecilla et al. Paper II. 2017ApJ...848...87C 2017ApJ...848...87C Cat. J/ApJ/848/87
(End) Patricia Vannier [CDS] 27-Jan-2016