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J/ApJ/723/993   Spatial extent of (U)LIRGs in the MIR. I.   (Diaz-Santos+, 2010)

The spatial extent of (U)LIRGs in the mid-infrared. I. The continuum emission. Diaz-Santos T., Charmandaris V., Armus L., Petric A.O., Howell J.H., Murphy E.J., Mazzarella J.M., Veilleux S., Bothun G., Inami H., Appleton P.N., Evans A.S., Haan S., Marshall J.A., Sanders D.B., Stierwalt S., Surace J.A. <Astrophys. J., 723, 993-1005 (2010)> =2010ApJ...723..993D
ADC_Keywords: Galaxies, IR ; Active gal. nuclei ; Spectra, infrared Keywords: galaxies: active - galaxies: evolution - galaxies: interactions - galaxies: starburst - infrared: galaxies Abstract: We present an analysis of the extended mid-infrared (MIR) emission of the Great Observatories All-Sky LIRG Survey sample based on 5-15um low-resolution spectra obtained with the Infrared Spectrograph on Spitzer. We calculate the fraction of extended emission (FEE) as a function of wavelength for the galaxies in the sample, FEEλ, defined as the fraction of the emission which originates outside of the unresolved component of a source at a given distance. We find that the FEEλ varies from one galaxy to another, but we can identify three general types of FEEλ: one where FEEλ is constant, one where features due to emission lines and polycyclic aromatic hydrocarbons appear more extended than the continuum, and a third which is characteristic of sources with deep silicate absorption at 9.7um. The mean size of the LIRG cores at 13.2um is 2.6kpc. However, once the IR luminosity of the systems reaches the threshold of LIR∼1011.8L, slightly below the regime of Ultra-luminous Infrared Galaxies (ULIRGs), all sources become clearly more compact, with FEE13.2um≲0.2, and their cores are unresolved. Our estimated upper limit for the core size of ULIRGs is less than 1.5kpc. Description: The sample on which we base our analysis is the Great Observatories All-Sky LIRG Survey (GOALS; Armus et al. 2009PASP..121..559A). All galaxies in GOALS have been observed in staring and/or mapping mode with the Spitzer/IRS instrument using all instrument modules (SL, LL, SH, and LH). They also have IRAC and MIPS imaging observations at all bandpasses (J. M. Mazzarella et al. 2011, in preparation). The analysis presented in this paper is based on IRS SL staring observations covering the 5 to ∼15um wavelength range with a spectral resolution of R∼60-130. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 88 221 Properties of the sample
See also: J/ApJ/715/572 : GOALS UV and FIR properties (Howell+, 2010) J/MNRAS/405/2505 : Nuclear activity in ULIRGs (Nardini+, 2010) J/ApJ/709/884 : Role of starburst-AGN composites in LIRG mergers (Yuan+, 2010) J/MNRAS/395/1695 : Spitzer mid-IR spectroscopy of LIRGs (Hernan-Caballero+, 2009) J/ApJS/182/628 : Spitzer quasar and ULIRG evolution study (Veilleux+, 2009) J/ApJ/674/172 : Oxygen abundances of LIRGs and ULIRGs (Rupke+, 2008) J/MNRAS/375/115 : ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007) J/ApJ/658/778 : Spitzer mid-IR spectroscopy of z∼2 ULIRGs (Yan+, 2007) J/A+A/467/565 : z=1-3 ULIRGs from the Spitzer SWIRE survey (Berta+, 2007) J/AJ/121/97 : K-band spectroscopy of ULIRGs (Murphy+, 2001) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 20 A20 --- Name Galaxy name (1) 22- 23 I2 h RAh Hour of Right Ascension (J2000) 25- 26 I2 min RAm Minute of Right Ascension (J2000) 28- 31 F4.1 s RAs Second of Right Ascension (J2000) 33 A1 --- DE- Sign of the Declination (J2000) 34- 35 I2 deg DEd Degree of Declination (J2000) 37- 38 I2 arcmin DEm Arcminute of Declination (J2000) 40- 41 I2 arcsec DEs Arcsecond of Declination (J2000) 43- 47 F5.1 Mpc Dist Luminosity distance (2) 49- 53 F5.2 [Lsun] logL Log IR luminosity 55- 58 F4.2 --- FEE Fraction of extended emission at 13.2{MU}m 60- 63 F4.2 --- e_FEE Uncertainty in FEE 65- 69 F5.2 kpc Size Core size, FHWM, at 13.2{MU}m 71- 74 F4.2 kpc e_Size Uncertainty in Size 75 A1 --- u_Size [*:] Unresolved core or uncertain size (3) 77- 82 F6.3 [-] logR ? Log IRAS 60/100um band flux density ratio (4) 84- 88 F5.3 [-] e_logR ? Uncertainty in logR (4)
Note (1): Multiple systems are indicated with the same name but providing the right ascension and declination of the individual galaxies. Note (2): See Armus et al. 2009PASP..121..559A, for details. LogL is accurate to within 0.01 dex (U et al. 2011, in preparation). Note (3): Flag as follows: * = unresolved cores (FWHM within 10% of that of the unresolved stellar PSF). : = galaxy whose IRS spectra has been contaminated by a close companion galaxy. In this cases, the Frac and the core size are not reliable. Note (4): Values are given only for sources with a unique IRAS color, i.e., not associated to two individual galaxies.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 24-Jul-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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