J/A+A/561/A33 SDSS star-forming galaxies multi-wavelength study (Izotov+, 2014)
Multi-wavelength study of 14000 star-forming galaxies from the
Sloan Digital Sky Survey.
Izotov Y.I., Guseva N.G., Fricke K.J., Henkel C.
<Astron. Astrophys., 561, A33-33 (2014)>
=2014A&A...561A..33I 2014A&A...561A..33I
ADC_Keywords: Galaxies, photometry ; Photometry, SDSS ; Photometry, infrared ;
Photometry, ultraviolet
Keywords: galaxies: abundances
Abstract:
We studied a large sample of ∼14000 dwarf star-forming galaxies with
strong emission lines. These low-metallicity galaxies with oxygen
abundances of 12+logO/H∼7.4-8.5 are selected from the Sloan Digital
Sky Survey (SDSS) and distributed in the redshift range of z∼0-0.6. We
modelled spectral energy distributions (SED) of all galaxies, which
were based on the SDSS spectra in the visible range of
0.38µm-0.92µm and included both the stellar and ionised gas
emission. These SEDs were extrapolated to the UV and mid-infrared
ranges to cover the wavelength range of 0.1µm-22µm. The SDSS
spectroscopic data were supplemented by photometric data from the
GALEX, SDSS, 2MASS, WISE, IRAS, and NVSS all-sky surveys. Using these
data, we derived global characteristics of the galaxies, such as their
element abundances, luminosities, and stellar masses.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 108 96 Observed parameters of the galaxies
table3.dat 88 96 Derived parameters of the galaxies
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1 A1 --- Gr [abc] Group (G1)
3- 12 A10 --- Name Galaxy abbreviated name (JHHMM+DDMM)
14- 15 I2 h RAh Right ascension (J2000)
17- 18 I2 min RAm Right ascension (J2000)
20- 24 F5.2 s RAs Right ascension (J2000)
26 A1 --- DE- Declination sign (J2000)
27- 28 I2 deg DEd Declination (J2000)
30- 31 I2 arcmin DEm Declination (J2000)
33- 37 F5.2 arcsec DEs Declination (J2000)
39- 44 F6.4 --- z Spectroscopic redshift
46- 50 F5.2 mag gmag SDSS g magnitude
52- 56 F5.2 mag FUV ?=- GALEX far-UV magnitude
58- 62 F5.2 mag NUV ?=- GALEX near-UV magnitude
64- 68 F5.2 mag W1mag WISE 3.4um magnitude
70- 74 F5.2 mag W2mag WISE 4.6um magnitude
76- 80 F5.2 mag W3mag WISE 12um magnitude
82 A1 --- l_W4mag Limit flag on W4mag
83- 86 F4.2 mag W4mag WISE 22um magnitude
88-108 A21 --- OName Other names
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1 A1 --- Gr [abc] Group (G1)
3- 12 A10 --- Name Galaxy abbreviated name (JHHMM+DDMM)
14- 17 F4.2 [-] e(O) [7.4/8.6] Oxygen abundance (log(O/H)+12)
19- 21 I3 0.1nm EW(Hb) Rest-frame equivalent width of the Hβ
emission line
23- 28 F6.2 mag gMAG Extinction-corrected absolute SDSS g
magnitude
30- 34 F5.2 [10-7W] logLHb Log of the aperture- and extinction-corrected
Hβ luminosity (in erg/s)
36- 40 F5.2 [10-6W/nm] logLFUV ?=- Log of the extinction-corrected GALEX
far-UV luminosity (in erg/s/Å)
42- 46 F5.2 [10-6W/nm] logLNUV ?=- Log of the extinction-corrected GALEX
near-UV luminosity (in erg/s/Å)
48- 52 F5.2 [10-6W/nm] logLW1 Log of the extinction-corrected WISE 3.4um
luminosity (in erg/s/Å)
54- 58 F5.2 [10-6W/nm] logLW2 Log of the extinction-corrected WISE 4.6um
luminosity (in erg/s/Å)
60- 64 F5.2 [10-6W/nm] logLW3 Log of the extinction-corrected WISE 12um
luminosity (in erg/s/Å)
66 A1 --- l_logLW4 Limit flag on logLW4
67- 71 F5.2 [10-6W/nm] logLW4 Log of the extinction-corrected WISE 22um
luminosity (in erg/s/Å)
73- 77 F5.2 [Msun] logM* Log of the aperture-corrected stellar mass
79- 82 F4.2 [Msun] logMy Log of the aperture-corrected mass of the
young stellar population
84- 88 F5.2 Msun/yr SFR Star formation rate (1)
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Note (1): SFR derived from L(Hα)=2.8L(Hβ) and using relation
SFR(M☉/yr)=4.4x10-42L(Hα)(erg/s) (Kennicutt 1998ARA&A..36..189K 1998ARA&A..36..189K).
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Note (G1): Groups as follows:
a = Galaxies with m(3.4um)-m(4.6um)≥2mag
b = Galaxies with 2mag>m(3.4um)-m(4.6um)≥1.5mag
c = Representative galaxies with m(3.4um)-m(4.6um)<0.5mag
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History:
09-May-2014: From electronic version of the journal
23-Nov-2016: Luminosity units in table3 corrected (fluxes units previously
indicated), thanks to Genoveva Micheva to notice it
and Yuri Izotov to confirm the right units.
(End) Patricia Vannier [CDS] 31-Mar-2014