Extragalactic Source Counts in the
                    <i>Spitzer</i>
                    24 Micron Band: What Do We Expect from ISOCAM 15 Micron Data and Models?

Gruppioni, C.; Pozzi, F.; Lari, C.; Oliver, Seb; Rodighiero, G.

doi:10.1086/427552

Cited by 58 publications

(126 citation statements)

References 24 publications

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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: 73%

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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Section: Introductionsupporting

confidence: 73%

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

Franca¹,

Puccetti²,

Sacchi³

et al. 2007

A&A

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“…One of the most extended and comprehensive far-IR observational datasets of galaxies is the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey (Gruppioni et al 2013). By means of such a dataset, Gruppioni et al (2013) studied the evolution of the far-IR galactic luminosity function up to z ∼ 4.…”

Section: Cosmic Dust Budgetmentioning

confidence: 99%

“…By means of such a dataset, Gruppioni et al (2013) studied the evolution of the far-IR galactic luminosity function up to z ∼ 4. In such a work, a galactic counterpart was found for most of the sources (>87%), possibly leaving little room for extra-galactic emission in the far-IR and consequently to large reservoirs of dust outside galaxies.…”

Section: Cosmic Dust Budgetmentioning

confidence: 99%

The cosmic dust rate across the Universe

Gioannini¹,

Matteuccí

Calura

2017

Monthly Notices of the Royal Astronomical Society

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We investigate the evolution of interstellar dust in the Universe by means of chemical evolution models of galaxies of different morphological types, reproducing the main observed features of present day galaxies. We adopt the most updated prescriptions for dust production from supernovae and asymptotic giant branch (AGB) stars as well as for dust accretion and destruction processes. Then, we study the cosmic dust rate in the framework of three different cosmological scenarios for galaxy formation: i) a pure luminosity scenario (PLE), ii) a number density evolution scenario (DE), as suggested by the classical hierarchical clustering scenario and iii) an alternative scenario, in which both spirals and ellipticals are allowed to evolve in number on an observationally motivated basis. Our results give predictions about the evolution of the dust content in different galaxies as well as the cosmic dust rate as a function of redshift. Concerning the cosmic dust rate, the best scenario is the alternative one, which predicts a peak at 2 < z < 3 and reproduces the cosmic star formation rate. We compute the evolution of the comoving dust density parameter Ω dust and find agreement with data for z < 0.5 in the framework of DE and alternative scenarios. Finally, the evolution of the average cosmic metallicity is presented and it shows a quite fast increase in each scenario, reaching the solar value at the present time, although most of the heavy elements are incorporated into solid grains, and therefore not observable in the gas phase.

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“…Murali et al 2002;Kereŝ et al 2005, could conceivably present accretion "peaks" at high redshifts generating bright nuclear SBs and AGN activity, and thus powerful feedback. In either case, the increasing importance of feedback processes at high redshifts is also expected from the sharp increase of the IR luminosity function as derived from the Spectral Energy Distribution (SED) analysis of Herschel/PACS selected galaxies (Gruppioni et al 2013), as well as from the increase in AGN activity (Hopkins et al 2007;Merloni & Heinz 2008;Delvecchio et al 2014). SPICA would indeed measure with unprecedented accuracy and depth the cosmic evolution of AGN activity using both spectroscopic and photometric techniques (see the accompanying papers Spinoglio et al 2017;Gruppioni et al 2017).…”

Section: Introductionmentioning

confidence: 93%

“…How are these outflows related to the steep decline in star formation during this epoch? In the framework of the two-fold evolutionary dichotomy for IR galaxies proposed by Gruppioni et al (2013), with a strong SB-dominated phase accompanied by SMBH growth leading to ellipticals, and a more moderate mode of star-formation that may generate the local spiral population, are feedback processes mainly responsible for the evolution along the SB-SMBH branch? An estimate of the outflow luminosity/momentum function is needed to answer this question.…”

Section: Introductionmentioning

confidence: 99%

Feedback and Feeding in the Context of Galaxy Evolution withSPICA: Direct Characterisation of Molecular Outflows and Inflows

González-Alfonso

Armus

Carrera

et al. 2017

Publ. Astron. Soc. Aust.

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A far-infrared observatory such as the SPace Infrared telescope for Cosmology and Astrophysics (SPICA), with its unprecedented spectroscopic sensitivity, would unveil the role of feedback in galaxy evolution during the last ∼ 10 Gyr of the Universe (z = 1.5 − 2), through the use of far-and mid-infrared molecular and ionic fine structure lines that trace outflowing and infalling gas. Outflowing gas is identified in the far-infrared through P-Cygni line shapes and absorption blueshifted wings in molecular lines with high dipolar moments, and through emission line wings of fine-structure lines of ionized gas. We quantify the detectability of galaxy-scale massive molecular and ionized outflows as a function of redshift in AGN-dominated, starburstdominated, and main-sequence galaxies, explore the detectability of metal-rich inflows in the local Universe, and describe the most significant synergies with other current and future observatories that will measure feedback in galaxies via complementary tracers at other wavelengths.

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Extragalactic Source Counts in the Spitzer 24 Micron Band: What Do We Expect from ISOCAM 15 Micron Data and Models?

Cited by 58 publications

References 24 publications

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

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

The cosmic dust rate across the Universe

Feedback and Feeding in the Context of Galaxy Evolution withSPICA: Direct Characterisation of Molecular Outflows and Inflows

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