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J/A+A/528/A35        Infrared luminosity in GOODS fields       (Magnelli+, 2011)

Evolution of the dusty infrared luminosity function from z=0 to z=2.3 using observations from Spitzer. Magnelli B., Elbaz D., Chary R.R., Dickinson M., Le Borgne D., Frayer D.T., Willmer C.N.A. <Astron. Astrophys. 528, A35 (2011)> =2011A&A...528A..35M
ADC_Keywords: Galaxies, IR ; Galaxies, photometry ; Photometry, infrared Keywords: galaxies: evolution - infrared: galaxies - infrared: starburst - cosmology: observations Abstract: We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24um and 70um imaging of the GOODS North and South fields. We perform a stacking analysis to characterize the observed L24/(1+z) vs L70/(1+z) correlation. Then, using spectral energy distribution templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24um and 70um luminosities. We then compute the infrared LF at z=1.55±0.25 and z=2.05±0.25. The redshift evolution of the infrared LF from z=1.5 to z=2 is consistent with a luminosity evolution proportional to (1+z)1.0±0.9 combined with a density evolution proportional to (1+z)-1.1±1.5. At z=2, LIRGs are still the main contributors, at 49%, to the total comoving infrared luminosity density of the Universe while ULIRGs account for 17%. Description: We present our deep GOODS-North and -South 24 to 70um multi-wavelength catalog. The 24um imaging of the GOODS fields were obtained as part of the GOODS Legacy program (PI: M. Dickinson). The 70um data were obtained by Spitzer GO programs (PI: D. Frayer). In the north they cover a region of roughly 10'x16', while in the south they cover a somewhat smaller fraction of the GOODS 24um area, roughly 10'x10'. The Frayer data have been combined with additional 70um observations covering a wider area from the FIDEL program (PI: M. Dickinson), as well as shallower data from Spitzer GTO programs (PI: Rieke). 24 and 70um flux densities are derived using a PSF fitting technique that takes into account, as prior information, the expected position of the sources. Starting from IRAC, we extract all 24 and 70um sources. Our 24um and 70um data were designed to reach the confusion limit of Spitzer. Thus, flux uncertainties are a complex combination of photon and confusion noise. In order to estimate these complex uncertainties we used two different approaches. (i) We estimate flux uncertainties on our residual maps (e_24(70)map). These uncertainties take into account the local quality of our fit but only partially take into account confusion noise. (ii) To estimate the effect of confusion noise we performed extensive Monte-Carlo simulations. Flux uncertainties derived using our Monte-Carlo simulations are denoted as e24(70)(simu). These uncertainties account for nearly all sources of noise, which explains why they are almost always larger than noise estimates based on residual maps. However, these uncertainties are computed independently of the actual position of the sources. In some cases, local effects can dominate the noise as it is the case when two sources are blended. This local effect is better accounted for by e24(70)(map). To be conservative, users should use the higher uncertainty out of e24(70)(map) and e_24(70)simu, but not the quadratic summation of both since they are not independent. Using our Monte Carlo simulations we found that our 24um catalog is 80% complete at 30uJy. This catalog extends down to 20uJy where flux accuracy of our catalog is 33% (i.e, f24/ e24(simu)=3). Our Monte-Carlo simulations show that our deep 70um catalog is 80% complete at 2.5mJy and that the 33% flux accuracy limit is reached at 2mJy. For our shallow 70um data of GOODS-S, the 80% completeness limit is 3mJy, and the 33% flux accuracy limit is reached at 2.5mJy. A complete description can be found in Magnelli et al. 2009A&A...496...57M and present paper. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 97 1976 24/70um photometry of sources in GOODS-North with f24/e24(simu)>5 table2.dat 97 561 24/70um photometry of sources in GOODS-North with 3<f24/e24(simu)<5 table3.dat 97 1864 24/70um photometry of sources in GOODS-South with f24/e24(simu)>5 table4.dat 97 542 24/70um photometry of sources in GOODS-South with 3<f24/e24(simu)<5
See also: II/261 : GOODS initial results (Giavalisco+, 2004) J/MNRAS/371/1891 : GOODS ELAIS-N1 24um flux densities (Rodighiero+, 2006) J/ApJ/666/863 : GOODS MIPS early-type galaxies (Van Der Wel+, 2007) Byte-by-byte Description of file: table1.dat table2.dat table3.dat table4.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [MIPS] 5- 22 A18 --- MIPS Source name, JHHMMSS.s+DDMMSS.s 24- 25 I2 h RAh Right ascension (J2000) 27- 28 I2 min RAm Right ascension (J2000) 30- 34 F5.2 s RAs Right ascension (J2000) 36 A1 --- DE- Declination sign (J2000) 37- 38 I2 deg DEd Declination (J2000) 40- 41 I2 arcmin DEm Declination (J2000) 43- 47 F5.2 arcsec DEs Declination (J2000) 49- 54 F6.1 uJy f24 Spitzer/MIPS 24um flux density in micro-Jansky 56- 60 F5.1 uJy e_f24 24um flux uncertainty from residual map 62- 65 F4.1 uJy sig24 24um flux uncertainty from M-C simulations 68- 72 I5 s cov24 24um exposure time at this position 74 A1 --- l_f70 Limit flag on 70um flux density 75- 79 F5.1 mJy f70 Spitzer/MIPS 70um flux density in milli-Jansky 81- 85 F5.1 mJy e_f70 ?=-99.0 70um flux uncertainty from residual map (1) 87- 91 F5.1 mJy sig70 ?=-99.0 70um flux uncertainty from Monte-Carlo simulations (1) 93- 97 I5 s cov70 70um exposure time at this position
Note (1): If the source is undetected, flux uncertainties are put to -99.0.
Acknowledgements: Benjamin Magnelli, magnelli(at) References: Damen et al., 2011ApJ...727....1D, The SIMPLE Survey: Observations, Reduction, and Catalog Magnelli et al., 2009A&A...496...57M The 0.4<z<1.3 star formation history of the Universe as viewed in the far-infrared
(End) Benjamin Magnelli [CEA, Saclay], Patricia Vannier [CDS] 13-Jan-2011
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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