The Local Luminosity Function at 25 Microns

Shupe, D. L.; Fan, Fang; Hacking, P.; Huchra, J. P.

doi:10.1086/305825

Cited by 43 publications

(82 citation statements)

References 33 publications

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“…Comparing to the local reference of Xu (2000) and with the z ∼ 0.55, z ∼ 0.85 and z ∼ 1.15 reference of Magnelli et al (2009), we note the strong evolution of this LF with redshift. Figure A.3 presents the rest-frame 25 μm LF derived in our two redshift bins using the 1/V max method as well as the local reference of Shupe et al (1998). Finally Fig.…”

Section: Resultsmentioning

confidence: 99%

“…Finally Fig. A.4 presents the rest-frame 35 μm LF derived in our two redshift bins using the 1/V max method as well as the local reference derived from Shupe et al (1998), and the LFs derived in Magnelli et al (2009) at z ∼ 0.55, z ∼ 0.85 and z ∼ 1.15.…”

Section: Resultsmentioning

confidence: 99%

“…Red squares are obtained using scaled CE01 templates which best fit the L 24 μm/(1+z) − L 70 μm/(1+z) correlation. Asterisks show the local reference taken from Shupe et al (1998) and the dotted line presents the best-fit to these data points with a double power law function with fixed slopes (see Table A.1). The dark shaded area span all the solutions obtained with the χ 2 minimization method and compatible, within 1σ, with our data points.…”

Section: Appendix B: Source Listmentioning

confidence: 99%

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

Magnelli

Elbaz

Chary

et al. 2011

A&A

352

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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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Section: Appendix B: Source Listmentioning

confidence: 99%

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

Magnelli

Elbaz

Chary

et al. 2011

A&A

352

422

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show abstract

“…Therefore we constructed a local reference from the rest-frame 25 microns LF of Shupe et al (1998) derived using the IRAS Faint Source Survey. Using a bivariate method and the CE01 library, we converted the 25 microns LF into a rest-frame 35 microns LF.…”

Section: Methodsmentioning

confidence: 99%

“…8 in the GOODS and EGS fields, respectively. Asterisks show the local reference taken from Shupe et al (1998) and the dotted line presents the best-fit to these data points with a double power law function (see text). In the intermediate redshift panel, we reproduced the best fit of the LF obtained in the two other redshift bins (i.e.…”

Section: Constraining the Faint End 35 Microns Lf Through Stackingmentioning

confidence: 99%

The 0.4 $\mathsf{<}$ z $\mathsf{<}$ 1.3 star formation history of the Universe as viewed in the far-infrared

Magnelli¹,

Elbaz²,

Chary

et al. 2009

A&A

385

563

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Aims. We use the deepest existing mid-and far-infrared observations (reaching ∼3 mJy at 70 μm) obtained with Spitzer in the Great Observatories Origins Deep Survey (GOODS) and Far Infrared Deep Extragalactic Legacy survey (FIDEL) fields to derive the evolution of the rest-frame 15 μm, 35 μm, and total infrared luminosity functions of galaxies spanning z < 1.3. We thereby quantify the fractional contribution of infrared luminous galaxies to the comoving star formation rate density over this redshift range. In comparison with previous studies, the present one takes advantage of deep 70 μm observations that provide a more robust infrared luminosity indicator than 24 μm affected by the emission of PAHs at high redshift (z ∼ 1), and we use several independent fields to control cosmic variance. Methods. We used a new extraction technique based on the well-determined positions of galaxies at shorter wavelengths to extract the 24 and 70 μm flux densities of galaxies. It is found that sources separated by a minimum of 0.5 × FWHM are deblended by this technique, which facilitates multi-wavelength associations of counterparts. Using a combination of photometric and spectroscopic redshifts that exist for ∼80% of the sources in our sample, we are able to estimate the rest-frame luminosities of galaxies at 15 μm and 35 μm. By complementing direct detections with a careful stacking analysis, we measured the mid-and far-infrared luminosity functions of galaxies over a factor ∼100 in luminosity (10 11 L <∼ L IR <∼ 10 13 L ) at z < 1.3. A stacking analysis was performed to validate the bolometric corrections and to compute comoving star-formation rate densities in three redshift bins 0.4 < z < 0.7, 0.7 < z < 1.0 and, 1.0 < z < 1.3. Results. We find that the average infrared spectral energy distribution of galaxies over the last 2/3 of the cosmic time is consistent with that of local galaxies, although individual sources do present significant scatter. We also measured both the bright and faint ends of the infrared luminosity functions and find no evidence for a change in the slope of the double power law used to characterize the luminosity function. The redshift evolution of infrared luminous galaxies is consistent with pure luminosity evolution proportional to (1 + z) 3.6±0.4 up to z ∼ 1.3. We do not find evidence of differential evolution between LIRGs and ULIRGs up to z ∼ 1.3, in contrast with previous claims. The comoving number density of infrared luminous galaxies has increased by a factor of ∼100 between 0 < z < 1. By z ∼ 1.0, LIRGs produce half of the total comoving infrared luminosity density.

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X‐Ray counts and contribution to the X‐ray background of an IR population of starburst and active galaxies

Polletta¹,

Lonsdale

et al. 2003

Astron Nachr

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The Local Luminosity Function at 25 Microns

Cited by 43 publications

References 33 publications

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

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

The 0.4 $\mathsf{<}$ z $\mathsf{<}$ 1.3 star formation history of the Universe as viewed in the far-infrared

X‐Ray counts and contribution to the X‐ray background of an IR population of starburst and active galaxies

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