Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/686/127       Starbursts luminosities based on PAH        (Weedman+, 2008)

The most luminous starbursts in the Universe. Weedman D.W., Houck J.R. <Astrophys. J., 686, 127-137 (2008)> =2008ApJ...686..127W
ADC_Keywords: Galaxies, IR ; Redshifts ; Photometry, infrared ; Spectroscopy Keywords: galaxies: distances and redshifts - galaxies: evolution - galaxies: high-redshift - galaxies: starburst - infrared: galaxies Abstract: A summary of starburst luminosities based on polycyclic aromatic hydrocarbon (PAH) features is given for 243 starburst galaxies with 0<z<2.5, observed with the Spitzer Infrared Spectrograph. Luminosity νLν(7.7um) for the peak luminosity of the 7.7um PAH emission feature is found to scale as log[νLν(7.7µm)]=44.63(±0.09)+2.48(±0.28)log(1+z) for the most luminous starbursts observed. Empirical calibrations of νLν(7.7um) are used to determine bolometric luminosity LIR and the star formation rate (SFR) for these starbursts. The most luminous starbursts found in this sample have logLIR=45.4(±0.3)+2.5(±0.3)log(1+z), in ergs/s, and the maximum star formation rates for starbursts in units of M/yr are log(SFR)=2.1(±0.3)+2.5(±0.3)log(1+z), up to z=2.5. The exponent for pure luminosity evolution agrees with optical and radio studies of starbursts but is flatter than previous results based in infrared source counts. The maximum star formation rates are similar to the maxima determined for submillimeter galaxies; the most luminous individual starburst included within the sample has logLIR=46.9, which gives an SFR=3.4x103M_☉/yr. Description: In this paper, we assemble data from 14 different Spitzer/IRS (InfraRed Spectrograph) programs (listed in "Ref" column of table1) to summarize a wide variety of sources having strong PAH spectral features, providing a total of 243 sources. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 63 243 PAH luminosities for starburst galaxies
See also: J/ApJ/701/1398 : SFR for starburst galaxies (Sargsyan+, 2009) J/ApJ/693/370 : Average Spitzer spectra for galaxies (Weedman+, 2009) J/A+A/508/117 : Spitzer selected starbursts at z∼2 (Fiolet+, 2009) J/A+A/507/713 : Galaxies with strong PAH emission (Haas+, 2009) J/ApJS/184/230 : Spitzer high-resolution MIR spectral atlas (Bernard-Salas+, 2009) J/ApJ/671/323 : Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Source running number 5- 20 A16 --- Name Source identification (1) 22- 23 I2 h RAh Hour of right ascension (J2000) 24- 25 I2 min RAm Minute of right ascension (J2000) 26- 30 F5.2 s RAs Second of right ascension (J2000) 31 A1 --- DE- Declination sign (J2000) 32- 33 I2 deg DEd Degree of declination (J2000) 34- 35 I2 arcmin DEm Arcminute of declination (J2000) 36- 39 F4.1 arcsec DEs Arcsecond of declination (J2000) 41- 46 F6.4 --- z Spectroscopic redshift (from Spitzer IRS) 48- 54 F7.2 mJy Fnu ? Spitzer/IRS flux density at 7.7um (2) 56- 60 F5.2 [10-7W] logLnu Rest-frame luminosity νLν at 7.7um (3) 62- 63 I2 --- Ref Reference (4)
Note (1): SST24 objects are named <[WH2008] SST24> in Simbad Note (2): Observed flux density in mJy at peak of 7.7um PAH feature measured from published spectra or from our own extractions. Typical uncertainties are ±5% for sources with Fν(7.7µm)≳5mJy and ±10% for sources with Fν(7.7µm)∼1mJy. Sources without entries have νLν(7.7um) determined from other PAH features, as explained in note (2). Note (3): Rest-frame luminosity νLν(7.7um) in ergs/s determined using peak Fν(7.7um) and luminosity distances from E. L. Wright,, for H0=71km/s/Mpc, ΩM=0.27, and ΩΛ=0.73. * For ULIRGs in reference 12, νLν(7.7um) is determined using the relation νLν(7.7µm)=28L(6.2µm+11.3µm); * for ULIRGs in references 13 and 14, νLν(7.7um) is determined using the relation νLν(7.7µm)=50L(6.2µm). * For starbursts in reference 1, luminosities also include the correction factor FF given in Brandl et al. (2006ApJ...653.1129B) for flux from the resolved source which is not included in the IRS observing slit. Note (4): References (with more details in section 2.1) as follows: 1 = Brandl et al. 2006ApJ...653.1129B 2 = Houck et al. 2007, Cat. J/ApJ/671/323; <[HWL2007] SST24> in Simbad 3 = new extraction of Bootes source from archival spectra program 20128 (PI: G. Lagache) or 20113 (PI: H. Dole) 4 = new spectral extraction from program 40038 (D. Weedman & J. Houck, 2009, cat J/ApJ/693/370) 5 = new extraction of FLS source from archival spectra program 20128 6 = Brand et al. 2008ApJ...673..119B; <[BWD2008] SST24 JHHMMSS.s+DDMMSS> in Simbad. 7 = Weedman et al. 2006ApJ...653..101W 8 = Farrah et al. 2008ApJ...677..957F; <SWIRE> in Simbad 9 = new extraction of source in Houck et al. (2005ApJ...622L.105H, <[HSW2005] SST24> in Simbad) or Weedman et al. (2006ApJ...638..613W, <[WLH2006] SST24>) using v15 data products and the 4 pixel extraction technique described in Weedman et al. (2006ApJ...653..101W) 10 = Yan et al. 2007ApJ...658..778Y; <[YSF2007] SST24> in Simbad 11 = Pope et al. 2008ApJ...675.1171P 12 = Farrah et al. 2007ApJ...667..149F 13 = Imanishi et al. 2007ApJS..171...72I 14 = Sargsyan et al. 2008ApJ...683..114S
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 17-Dec-2010
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

catalogue service