<i>Spitzer</i>70 and 160 μm Observations of the Extragalactic First Look Survey

Frayer, David; Fadda, D.; Yan, Lin; Marleau, F.; Choi, Philip; Hélou, G.; Soifer, B. T.; Appleton, P. N.; Armus, L.; Beck, R.; Dole, H.; Engelbracht, C. W.; Fan, Fang; Gordon, K. D.; Heinrichsen, I.; Henderson, David; Hesselroth, Ted; Im, Myungshin; Kelly, Douglas; Lacy, Mark; Laine, Seppo; Latter, William B.; Mahoney, W. A.; Makovoz, David; Masci, Frank J.; Morrison, J.; Moshir, M.; Noriega-Crespo, A.; Padgett, Deborah; Pesenson, Meyer Z.; Shupe, D. L.; Squires, G.; Storrie-Lombardi, L. J.; Surace, J.; Teplitz, Harry I.; Wilson, G. W.

doi:10.1086/498690

Cited by 108 publications

(96 citation statements)

References 43 publications

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“…The contribution from resolved sources reaches a maximum at z < 0.3 and strongly decreases toward higher redshift, in agreement with the identifications of Frayer et al (2006a). The AGN contribution is rather constant with redshift; the relative contribution of AGN thus increases with redshift.…”

Section: The 160 μM Background: Its History Since Z =supporting

confidence: 88%

“…The use of this method is justified for two reasons: 1) The 24 μm population is a good proxy for the 70 μm and 160 μm populations making up most of the CIB near its peak Bethermin et al 2010a). 2) Only a few sources are individually detected at FIR wavelengths and do not resolve much of the background Frayer et al 2006a;Frayer et al 2006b;Dole et al 2006;Frayer et al 2009). We note that stacking may be affected by galaxy clustering, since the stacked image shows two dimensions the two point angular correlation function Bavouzet 2008;Bethermin et al 2010a).…”

Section: Stacking Analysismentioning

confidence: 99%

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The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Jauzac

Dole

Floc’h

et al. 2010

A&A

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Context. The cosmic far-infrared background (CIB) at wavelengths around 160 μm corresponds to the peak intensity of the whole extragalactic background light, which is being measured with increasing accuracy. However, the build up of the CIB emission as a function of redshift is still not well known. Aims. Our goal is to measure the CIB history at 70 μm and 160 μm at different redshifts, and provide constraints for infrared galaxy evolution models. Methods. We used deep Spitzer 24 μm catalogs complete to about 80 μJy with spectroscopic and photometric redshift identifications, derived using the GOODS and COSMOS deep infrared surveys covering 2 square degrees total. After cleaning the Spitzer/MIPS 70 μm and 160 μm maps of detected sources, we stacked the far-IR images at the positions of the 24 μm sources in different redshift bins. We measured the contribution of each stacked source to the total 70 and 160 μm light, and compared with model predictions and far-IR measurements obtained for Herschel/PACS data of smaller fields. Results. We detect components of the 70 and 160 μm backgrounds in different redshift bins up to z ∼ 2. The contribution to the CIB reaches a maximum at 0.3 ≤ z ≤ 0.9 at 160 μm (and z ≤ 0.5 at 70 μm). A total of 81% (74%) of the 70 (160) μm background was emitted at z < 1. We estimate that the AGN contribution to the far-IR CIB is less than about 10% at z < 1.5. We provide a comprehensive view of the CIB buildup at 24, 70, 100 and 160 μm. Conclusions. We find that IR galaxy models predicting a major contribution to the CIB from sources at z < 1 agree with our measurements, while our results exclude other models that predict a peak of the background at higher redshifts. The consistency of our results with those obtained by the direct study of Herschel far-IR data at 160 μm confirms that the stacking analysis method is a valid approach to estimate the components of the far-IR background using prior information about resolved mid-IR sources.

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Section: The 160 μM Background: Its History Since Z =supporting

confidence: 88%

Section: Stacking Analysismentioning

confidence: 99%

The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Jauzac

Dole

Floc’h

et al. 2010

A&A

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“…At 70 μm no reliable empirical PSF could be constructed because only a few isolated sources could be found in each map. We then decided to use the appropriate 70 μm Point Response Function (PRF) estimated on the extragalactic First Look Survey mosaic (xFLS; Frayer et al 2006a) and available on the Spitzer web site. At both wavelengths an aperture correction is applied to all flux densities to account for the finite size of our PSFs.…”

Section: Appendix B: Source Listmentioning

confidence: 99%

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

Magnelli

Elbaz

Chary

et al. 2011

A&A

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422

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Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields. Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) ∼20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L 24/(1+z) vs. L 70/(1+z) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at z ∼ 1.55 ± 0.25 and z ∼ 2.05 ± 0.25. Results. We observe the break in the infrared LF up to z ∼ 2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 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, luminous infrared galaxies (LIRGs: 10 11 L < L IR < 10 12 L ) are still the main contributors to the total comoving infrared luminosity density of the Universe. At z ∼ 2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 10 12 L < L IR ) account for ∼49% and ∼17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.

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“…The pioneering exploration of the IR sky by the IRAS satellite revealed the rapid evolution of the infrared (IR) LLF (Saunders et al 1990), illustrating the importance of local studies at infrared (IR) wavelengths. ISO was later able to follow the evolution of the IR LF up to z 1 (Pozzi et al 2004), while Spitzer studies using the MIPS 24 μm (Le Floc'h et al 2005;Marleau et al 2007;Rodighiero et al 2010) and 70 μm (Frayer et al 2006; Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. Huynh et al 2007;Magnelli et al 2009) channels have both extended our reach to higher redshifts and improved our constraints on the IR bolometric (8−1000 μm) luminosity of detected sources.…”

Section: Introductionmentioning

confidence: 99%

The HerMES SPIRE submillimeter local luminosity function

Vaccari¹,

Marchetti²,

Franceschini³

et al. 2010

A&A

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Local luminosity functions are fundamental benchmarks for high-redshift galaxy formation and evolution studies as well as for models describing these processes. Determining the local luminosity function in the submillimeter range can help to better constrain in particular the bolometric luminosity density in the local Universe, and Herschel offers the first opportunity to do so in an unbiased way by imaging large sky areas at several submillimeter wavelengths. We present the first Herschel measurement of the submillimeter 0 < z < 0.2 local luminosity function and infrared bolometric (8−1000 μm) local luminosity density based on SPIRE data from the HerMES Herschel key program over 14.7 deg 2 . Flux measurements in the three SPIRE channels at 250, 350 and 500 μm are combined with Spitzer photometry and archival data. We fit the observed optical-to-submillimeter spectral energy distribution of SPIRE sources and use the 1/V max estimator to provide the first constraints on the monochromatic 250, 350 and 500 μm as well as on the infrared bolometric (8−1000 μm) local luminosity function based on Herschel data. We compare our results with modeling predictions and find a slightly more abundant local submillimeter population than predicted by a number of models. Our measurement of the infrared bolometric (8−1000 μm) local luminosity function suggests a flat slope at low luminosity, and the inferred local luminosity density, 1.31 +0.24 −0.21 × 10 8 L Mpc −3 , is consistent with the range of values reported in recent literature.

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Spitzer70 and 160 μm Observations of the Extragalactic First Look Survey

Cited by 108 publications

References 43 publications

The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

The cosmic far-infrared background buildup since redshift 2 at 70 and 160 microns in the COSMOS and GOODS fields

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

The HerMES SPIRE submillimeter local luminosity function

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