Infrared luminosity in GOODS fields (Magnelli+, 2011)

Details Infrared luminosity in GOODS fields (Magnelli+, 2011) Infrared luminosity in GOODS fields (Magnelli+, 2011)

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ycat..35289035m&link_type=abstract

VizieR On-line Data Catalog: J/A+A/528/A35. Originally published in: 2011A&A...528..A35M

Computer Science

1

Galaxies: Ir, Galaxies: Photometry, Photometry: Infrared

Scientific paper

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.
(4 data files).

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