SpitzerView on the Evolution of Star‐forming Galaxies fromz= 0 toz∼ 3

Pérez‐González, Pablo G.; Rieke, G. H.; Egami, Eiichi; Alonso‐Herrero, A.; Dole, H.; Papovich, C.; Blaylock, Myra L.; Jones, J.B.; Rieke, M. J.; Rigby, J. Keith; Barmby, P.; Fazio, G. G.; Huang, Jia-Sheng; Martin, Christopher

doi:10.1086/431894

Cited by 478 publications

(667 citation statements)

References 156 publications

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“…We find a slight decrease of the IR LD from z = 1.3 to z = 2.3 due to a decrease in the contribution of LIRGs and "normal" galaxies. At z ∼ 2 the IR LD of the Universe is still dominated by LIRGs and not by ULIRGs, contrary to previous claims (e.g., Pérez-González et al 2005). Using the best fit of our infrared LF, we infer that at z ∼ 2 LIRGs and ULIRGs have an IR LD of 4.5 × 10 8 L Mpc −1 and 1.5 × 10 8 L Mpc −1 respectively and that they account for 49% and 17% of the total IR LD respectively.…”

Section: Discussioncontrasting

confidence: 90%

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: Discussioncontrasting

confidence: 90%

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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“…These results are now confirmed and extended by the data coming from the Spitzer Space Telescope (e.g. Gruppioni et al 2005;Le Floc'h et al 2005;Pérez-González et al 2005;Babbedge et al 2006;Caputi et al 2007). On the contrary, the evolution of AGN at MIR wavelengths are similar to what has been measured in the optical and X-ray bands for type 1 AGN (AGN1) and even slower for type 2 AGN (Matute et al 2002(Matute et al , 2006.…”

Section: Introductionsupporting

confidence: 74%

AGN counts at 15$\mu{\rm m}$

Franca¹,

Puccetti²,

Sacchi³

et al. 2007

A&A

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Context. The counts of galaxies and AGN in the mid infra-red (MIR) bands are important instruments for studying their cosmological evolution. However, the classic spectral line ratios techniques can become misleading when trying to properly separate AGN from starbursts or even from apparently normal galaxies. Aims. We use X-ray band observations to discriminate AGN activity in previously classified MIR-selected starburst galaxies and to derive updated AGN1 and (Compton thin) AGN2 counts at 15 µm. Methods. XMM observations of the ELAIS-S1 15 µm sample down to flux limits ∼2 × 10 −15 erg cm −2 s −1 (2-10 keV band) were used. We classified as AGN all those MIR sources with a unabsorbed 2-10 keV X-ray luminosity higher that ∼10 42 erg s −1 . Results. We find that at least about 13 ± 6% of the previously classified starburst galaxies harbor an AGN. According to these figures, we provide an updated estimate of the counts of AGN1 and (Compton thin) AGN2 at 15 µm. It turns out that at least 24% of the extragalactic sources brighter than 0.6 my at 15 µm are AGN (∼13% contribution to the extragalactic background produced at fluxes brighter than 0.6 mJy).

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“…All infraredbased estimates are compared to the optical/rest-frame UV estimates compiled in Hopkins & Beacom (2006) which have been corrected for dust extinction, and therefore represent an approximation to the total star formation rate density in the Universe at a given epoch. The total infrared estimates from the literature (integrated over ∼10 8 − 10 13.5 L ) come from Spitzer samples Pérez-González et al, 2005;Caputi et al, 2007;Rodighiero et al, 2010;Magnelli et al, 2011) and Herschel samples . In contrast, several samples from the submm and mm are also included; although they are known to be incomplete, they provide a benchmark lower limits for the true contributions from their respective populations.…”

Section: Contribution To Cosmic Star Formation Rate Densitymentioning

confidence: 99%

“…L < 10 11 L ) in blue, the LIRG population (10 11 < L < 10 12 L ) in yellow-orange, and the ULIRG population (10 12 < L < 10 13 L ) in red. The literature sources of each estimate are given by different symbols or line-types as indicated Pérez-González et al, 2005;Hopkins & Beacom, 2006;Caputi et al, 2007;Magnelli et al, 2011Magnelli et al, , 2013bMurphy et al, 2011;Casey, 2012). Note that not all literature derivations of different luminosity bins are computationally equivalent since some luminosities are derived directly from the far-infrared bands while others are extrapolations from mid-infrared bands.…”

Section: Contribution To Cosmic Star Formation Rate Densitymentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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SpitzerView on the Evolution of Star‐forming Galaxies fromz= 0 toz∼ 3

Cited by 478 publications

References 156 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

AGN counts at 15$\mu{\rm m}$

Dusty star-forming galaxies at high redshift

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