J/ApJ/683/114 IRS spectra of faint IRAS sources (Sargsyan+, 2008) ================================================================================ Spitzer IRS spectra of optically faint IRAS sources. Sargsyan L., Mickaelian A., Weedman D., Houck J. =2008ApJ...683..114S ================================================================================ ADC_Keywords: Active gal. nuclei ; Equivalent widths ; Photometry, infrared ; Redshifts ; Spectra, infrared Keywords: galaxies: active - galaxies: starburst - infrared: galaxies Abstract: Extragalactic sources from the IRAS Faint Source Catalog (FSC) that have the optically faintest magnitudes (E>~18) were selected by spatial coincidence with a source in the FIRST radio survey, and 28 of these sources have been observed with the Infrared Spectrograph on Spitzer (IRS). While an infrared source is always detected with the IRS at the FIRST position, only ~50% of the infrared sources are real FSC detections, as estimated from the number of sources for which the f_v_(25um) determined with the IRS is fainter than the sensitivity limit for the FSC. Sources have 0.12 10, Version 2.0 (Moshir+ 1989) VIII/71 : The FIRST Survey Catalog, Version 03Apr11 (Becker+ 2003) J/ApJ/642/673 : IR-selected obscured AGN candidates (Polletta+, 2006) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 I2 --- Seq Sequence running number 4- 6 A3 --- --- [FSC] 8- 17 A10 --- FSC Source name from the IRAS Faint Source Catalog (II/156) (1) 19- 36 A18 --- FIRST Coordinates for the FIRST source (2) 38- 45 I8 --- AOR Astronomical Observation Request identification number 47- 51 I5 --- Prog Program identification number 53- 55 I3 s Tsl Total integration time for IRS short-low modules 57- 59 I3 s Tll Total integration time for IRS long-low modules 61- 70 A10 "YYYY/MM/DD" Date Date of IRS observation -------------------------------------------------------------------------------- Note (1): Sources are in Simbad. 14589+2329 is a misprint for 14589+2340, corrected at CDS. Note (2): Coordinates for the FIRST source that is closest to the FSC source (HHMMSS.ss+DDMMSS.s, J2000) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 I2 --- Seq Sequence running number 4- 8 I5 --- Id Source number 10- 14 F5.3 --- z Redshift determined from the IRS spectra 15 A1 --- r_z [fg] References for two redshifts (3) 17- 19 I3 mJy F25i IRAS-FSC flux at 25um (Cat. II/156) 21- 25 F5.1 mJy F25s Spitzer/IRS measured flux at 25um 27- 30 F4.1 mag Emag Photographic E magnitude from APS catalog (Cabanela et al., 2003PASP..115..837C) 32 A1 --- l_Jmag Limit flag on Jmag 33- 37 F5.2 mag Jmag 2MASS J magnitude 39- 43 F5.2 mJy F1.4G ? FIRST flux at 1.4GHz 45- 48 F4.2 --- q ? Ratio of infrared to radio flux (4) 50- 54 F5.2 mJy F5.5 Spitzer/IRS flux at 5.5um 56- 60 F5.1 mJy F15 Spitzer/IRS flux at 15um 62 A1 --- l_EW Limit flag on EW 63- 67 F5.3 um EW ? Equivalent width of PAH at 6.2um 69- 73 F5.3 um e_EW ? Uncertainty on EW (5) 75 A1 --- l_F6.2 Limit flag on F6.2um 76- 80 F5.2 zW/cm2 F6.2 ? Total Spitzer/IRS flux of PAH at 6.2um (5) 82- 85 F4.2 zW/cm2 e_F6.2 ? Uncertainty on F6.2 (5) 87 A1 --- l_F11.3 Limit flag on F11.3 88- 92 F5.2 zW/cm2 F11.3 ? Total Spitzer/IRS flux of PAH at 11.3um (5) 94- 97 F4.2 zW/cm2 e_F11.3 ? Uncertainty on F11.3um (5) 99-103 F5.2 --- tau {tau}_si_ measure of the depth of the 9.7um absorption feature (6) -------------------------------------------------------------------------------- Note (3): References as follows: f = Redshift for this object, a red quasar, is the optical redshift from Urrutia et al., 2005ApJ...627...75U g = Redshift for this object, a blazar, is from Perry et al., 1978PASP...90..337P Note (4): In the observed frame, q=log[f_{nu}_(25um)/f_{nu}_(1.4GHz)], using f_{nu}_(1.4GHz) of "peak flux" from FIRST, corresponding to an unresolved source. Note (5): Total flux of feature, fit with a single Gaussian. Uncertainties in fluxes and equivalent widths are statistical uncertainties from fitting the feature and do not include systematic uncertainties of <~10%, which may arise from the fitting procedure chosen, as discussed in text. Note (6): Quantity defined as {tau}_si_=ln[f_{nu}_(abs)/f_{nu}_(cont)], for f_v_(abs) measured at the maximum depth of absorption and f_v_(cont) is the unabsorbed continuum as extrapolated in Spoon et al., 2007ApJ...654L..49S -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 I2 --- Seq Sequence running number 4- 8 I5 --- Id Source number 10- 13 I4 Mpc Dist Luminosity distance (7) 15- 19 F5.2 [10-7W] L5.5 Rest-frame parameter log({nu}L_{nu}_) at 5.5um 21- 25 F5.2 [10-7W] L15 Rest-frame log({nu}L_{nu}_) at 15um 27 A1 --- l_L6.2 Limit flag on L6.2 28- 32 F5.2 [10-7W] L6.2 ? Total luminosity of the 6.2um PAH feature, after subtracting the underlying continuum 34 A1 --- l_Ls Limit flag on Ls 35- 39 F5.2 [10-7W] Ls ? logL(6.2+11.3) 41 A1 --- l_LSB Limit flag on LSB 42- 46 F5.2 [10-7W] LSB ? Total luminosity of starburst (8) 48 A1 --- l_LAGN Limit flag on LAGN 49- 53 F5.2 [10-7W] LAGN ? Luminosity from the dusty torus of the AGN (9) 55 A1 --- l_f(SB) Limit flag on f(SB) 56- 59 F4.2 --- f(SB) ? Fraction of luminosity from starburst (10) -------------------------------------------------------------------------------- Note (7): Luminosity distance determined by E.L. Wright (see http://www.astro.ucla.edu/~wright/DlttCalc.html) for H_0_=71km/s/Mpc, {Omega}_m_=0.27, and {Omega}_{Lambda}_=0.73. Note (8): Total luminosity of starburst, assuming that log[L_IR_(SB)]=log[L(6.2)]+2.7+/-0.1, from Brandl et al. (2006ApJ...653.1129B) and Pope et al. (2008ApJ...675.1171P). Note (9): Total luminosity from the dusty torus of the AGN, assuming log[L_IR_(AGN)]=log[{nu}L_{nu}_(5.5um)]+0.33+/-0.06, from Polletta et al. (2008ApJ...675..960P) and assuming that all continuum luminosity vL_v_(5.5um) arises from an AGN. Note (10): Fraction L(SB)/[L(SB)+L(AGN)]. If a PAH feature is detected, this fraction is shown as a lower limit because some of the continuum at 5.5um, which is attributed to an AGN, actually arises from the starburst. If no PAH feature is detected, this fraction is shown as an upper limit because there is no direct evidence that a starburst is present. Source 9 is a blazar, so the parameters for determining L_IR_(AGN) and L_IR_(SB) are not applicable. -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Emmanuelle Perret [CDS] 26-Nov-2010