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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 63 243 PAH luminosities for starburst galaxies
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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
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Bytes Format Units Label Explanations
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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)
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Note (1): SST24 objects are named <[WH2008] SST24 JHHMMSS.ss+DDMMSS.s> 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,
http://www.astro.ucla.edu/~wright/CosmoCalc.html, 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 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 2006ApJ...653.1129B
2 = Houck et al. 2007, Cat. J/ApJ/671/323;
<[HWL2007] SST24 JHHMMSS.ss+DDMMSS.s> 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 2008ApJ...673..119B;
<[BWD2008] SST24 JHHMMSS.s+DDMMSS> in Simbad.
7 = Weedman et al. 2006ApJ...653..101W 2006ApJ...653..101W
8 = Farrah et al. 2008ApJ...677..957F 2008ApJ...677..957F; in Simbad
9 = new extraction of source in Houck et al. (2005ApJ...622L.105H 2005ApJ...622L.105H,
<[HSW2005] SST24 JHHMMSS.ss+DDMMSS.s> in Simbad) or Weedman et al.
(2006ApJ...638..613W 2006ApJ...638..613W, <[WLH2006] SST24 JHHMMSS.ss+DDMMSS.s>) using v15
data products and the 4 pixel extraction technique described in Weedman
et al. (2006ApJ...653..101W 2006ApJ...653..101W)
10 = Yan et al. 2007ApJ...658..778Y 2007ApJ...658..778Y;
<[YSF2007] SST24 JHHMMSS.ss+DDMMSS.s> in Simbad
11 = Pope et al. 2008ApJ...675.1171P 2008ApJ...675.1171P
12 = Farrah et al. 2007ApJ...667..149F 2007ApJ...667..149F
13 = Imanishi et al. 2007ApJS..171...72I 2007ApJS..171...72I
14 = Sargsyan et al. 2008ApJ...683..114S 2008ApJ...683..114S
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 17-Dec-2010