J/other/Ap/54.147 Study of 230 IRAS-FSC galaxies (Hovhannisyan+, 2011)
Multiwavelength study of 230 IRAS FSC galaxies
Hovhannisyan A., Sargsyan L.A., Mickaelian A.M., Weedman D.W.
<Astrophysics, 54 147-154 (2011)>
=2011Ap.....54..147H 2011Ap.....54..147H
=2011Afz....45..171H 2011Afz....45..171H
ADC_Keywords: Galaxies, IR ; Galaxies, radio ; Photometry, infrared ;
Ultraviolet
Keywords: galaxies: multiwavelength study
Description:
From the cross-correlation of the IRAS FSC catalog with the radio
FIRST catalog, 230 infrared galaxies were selected having optical
classifications and redshifts from SDSS and NED. To understand the
nature of these objects we have compared them with a sample of bright
ULIRGs with fluxes f>1Jy at 60-micron and with 14 optically faint
IRAS FSC galaxies, showing that IRAS galaxies are not always strong
infrared sources. We also have calibrated Star Formation Rates based
on luminosities of the PAH feature at 7.7-micron and 1.4GHz radio
flux densities, which confirmed the consistency between these two
SFRs. We have estimated the extinction for our 230 objects using SFRs
calibrated from the PAH feature compared to ultraviolet flux, which
shows that only 1% of the ultraviolet continuum typically escapes
extinction by dust within a starburst. As our 230 galaxies have no
spectra available from Spitzer Space Telescope (SST) archive, to
estimate the infrared flux at 7.7 (for SB galaxies) or 8.0 (for AGN
and composite) micron, we have used the median ratios of the IRAS
fluxes at 25-micron to fluxes at 7.7 or 8.0-micron estimated for each
41.0<logL(IR)<41.9, 42.0<logL(IR)<42.9, 43.0<logL(IR)<43.9,
44.0<logL(IR)<44.9, and 45.0<logL(IR)<45.9 luminosity bins, using
objects having spectra from SST archive.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 108 230 The list and fluxes of the 230 IRAS FSC galaxies
table2.dat 64 230 Luminosities and Star Formation Rates
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See also:
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989)
VIII/71 : The FIRST Survey Catalog, Version 03Apr11 (Becker+ 2003)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/230] Galaxy sequential number
5- 15 A11 --- IRAS IRAS FSC name (FHHMMm+DDMM)
17- 18 I2 h RAh Right ascension (J2000)
20- 21 I2 min RAm Right ascension (J2000)
23- 27 F5.2 s RAs Right ascension (J2000)
29 A1 --- DE- Declination sign J2000)
30- 31 I2 deg DEd Declination J2000)
33- 34 I2 arcmin DEm Declination J2000)
36- 39 F4.1 arcsec DEs Declination J2000)
41- 46 F6.4 --- z Redshift
48- 52 F5.1 mJy FFUV ? Far ultraviolet flux from GALEX,
shifted to z=0
54- 57 F4.1 mJy FJ 2MASS flux J band
59- 62 F4.1 mJy F8 ? Infrared flux at 7.7 or 8.0um
65- 69 F5.1 mJy F12 IRAS FSC flux at 12.0um
71- 75 F5.1 mJy F25 IRAS FSC flux at 25.0um
77- 82 F6.1 mJy F60 IRAS FSC flux at 60.0um
84- 89 F6.1 mJy F100 IRAS FSC flux at 100.0um
91- 95 F5.1 mJy S1.4 Radio flux at 1.4GHz from radio FIRST catalog
shifted to z=0
97-101 F5.1 --- IR/opt Infrared to optical flux ratio
103-108 A6 --- Type Activity type (G1)
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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- 3 I3 --- Seq [1/230] Galaxy sequential number
5- 15 A11 --- IRAS IRAS FSC name (FHHMMm+DDMM)
17- 21 F5.2 [Msun/yr] SFR(UV) ? Star Formation Rate from far
ultraviolet flux (log scale)
23- 27 F5.2 [Msun/yr] SFR(IR) ? Star Formation Rate from IR flux at 7.7um
(log scale)
29- 33 F5.2 [Msun/yr] SFR(Rad) ? Star Formation Rate from radio (1.4GHz)
flux (log scale)
35- 39 F5.2 [10-7W] L(UV) ? Far ultraviolet luminosity (log scale)
41- 45 F5.2 [10-7W] L(PAH) ? infrared luminosity at 7.7 or 8.0um
(log scale)
47- 51 F5.2 [10-7W] L(Rad) Radio (1.4GHz) luminosity (log scale)
53- 57 F5.2 [10-7W] L(IR) Total infrared luminosity (log scale)
59- 64 A6 --- Type Activity type (G1)
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Global notes:
Note (G1): Activity type flag as follows:
agn = active galactic nuclei
sb = starbursts
comp = objects with composite spectrum
em+abs = objects with weak emission features and strong absorption
features in the spectrum
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Acknowledgements:
A. Hovhannisyan,
[Department of General Physics and Astrophysics, Yerevan State University]
(End) Patricia Vannier [CDS] 20-Jul-2011