The role of AGN in galaxy evolution: the InfraRed...

The role of AGN in galaxy evolution:

the InfraRed perspective, from low to high-z

C. Gruppioni (INAF-OABo) Collaborators (OABO+DIFA): L. Vallini (DIFA/OABO), F. Pozzi (DIFA), C. Vignali (DIFA), F. Calura (OABO), G. Lanzuisi (OABO), M. Talia (DIFA)

Bologna OABo Days, 2016 February 18-19

History: far and recent past activities

�  The IR group at OABo started in the late ‘90s, when I came back after a post-doc in UK (Imperial College, London) based on a Large Survey with ISO

�  F. Pozzi started as a PhD student analysing the (very painful and troublesome) ISO data (with C. Lari!)

�  Big involvement in Herschel GT project PACS Evolutionary Probe (PI D. Lutz, MPE): CG leader of the Luminosity Function project Active participation in many PEP-related papers

�  Several degree thesis and PhD students joined the group (lately H. Dominguez-Sanchez, I. Delvecchio)

�  Post-docs: G. Cresci (now OAAR), G. Lanzuisi, L. Vallini

…and what are we doing now? Present Collaborations

!  Collaborations in BO (OABo & DIFA staff) people: F. Pozzi (DIFA), F. Calura (OABO), C. Vignali (DIFA)

!  Italian Collaborations: G. Rodighiero (UniPd), P. Monaco (UniTs), L. Spinoglio (IAPS), L. Hunt (OAAR)

!  EC ITN: I am preparing a proposal for the next call

for a MARIE CURIE Innovative Training Network Title: Spectral Modelling for European Astronomy from Galaxy ObservationaL data (SMEAGOL) Partners (nodes): CG(OABo) – PI, *D. Alexander (UDurham), *A. Alonso-Herrero (CSIC), *M. Baes (UGent), *F. Boquien (Chile), *D. Burgarella (LAM), *A. Efstathiou (EUC), *D. Elbaz (CEA), *J. Fritz (UNAM), *E. Hatzminaouglou (ESO), *C. Maraston (UPortsmouth), *P. Monaco (UniTs), *S. Paltani (UniGe), *G. Rodighiero (UniPD), *M. Salvato (MPE)

Main (future) Project: SPICA Since 2008 I am involved in the scientific exploitations of an European far-IR spectrometer (SAFARI) for a future ESA-JAXA mission: the Space Infrared Telescope for Cosmology and Astrophysics: SPICA Since 2012 I am Scientific Co-I (1/2 per member State of consortium) of SPICA -> Major involvement involvement

SPICA�

Telescope diameter: 2 - 3 m Telescope temperature: < 6 K Wavelength: 20-210 µm (or wider) Total mass: < 3.7 t Orbit: Halo orbit around liberation point S-E L2 Launch: in FT2025 or later by JAXA's H-X Operation: 3 years (nominal), 5 years (goal)

2014-12-31 Hiroshi Shibai (PI of SPICA Project) Presented 2015-1-4 by Matt Bradford COPAG @ AAS Seattle

0

2.5$m&2.5$m&

SMI$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$SAFARI$$3$spec$channels:$$$$$$$$$$$$$$$$$$$$$$$$32band$gra7ng$spectrometer$LRS,$MRS,$HRS$$$$$$$$$$$$$$$$$$$$$$$$$$$$con7nuous$spectroscopy$capability$R~50$to$28000$$$$$$$$$$$$$$$$$$$$$$$$$$$$R~300$+slit2viewer$30237μm$$$$$$$$$$12237$μm$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$$342210$μm$

12$210&

Problems €  NO MONEY FROM ASI SINCE 2009 !!!!

€  NO MONEY FROM INAF (NEVER) FOR FUTURE MISSIONS PREPARATION/EXPLOITATION !!!!

€  All the SPICA meetings (min. 2 x year) have been payed with funds based on different projects

We will no longer be able to maintain our high degree of involvement without

any dedicated grants

Now a bit more into Science

!  Herschel LF & related stuff

!  IR lines as tracers of BH accretion and SF

!  ISM modelling in galaxies and AGN (diffuse, PDR, XDR, …)

!  Perspective for ALMA

Herschel LF @different z

Herschel LF & related stuff

~8000 sources @160μm In GOODS+COSMOS+ECDFS

CG+ 2013, MNRAS, 432, 23

IR LD vs. z

L evolution

ρ evolution

Diff. pop’s

Herschel LF & related stuff

MNRAS 456, L40–L44 (2016) doi:10.1093/mnrasl/slv173

CO luminosity function from Herschel-selected galaxies and thecontribution of AGN

L. Vallini,1,2‹ C. Gruppioni,2 F. Pozzi,1,2 C. Vignali1,2 and G. Zamorani21Dipartimento di Fisica e Astronomia, Universita di Bologna, viale Berti Pichat 6/2, I-40127 Bologna, Italy2INAF - Osservatorio Astronomico di Bologna, via Ranzani 2, I-40127 Bologna, Italy

Accepted 2015 October 29. Received 2015 October 29; in original form 2015 July 3

ABSTRACTWe derive the carbon monoxide (CO) luminosity function (LF) for different rotational tran-sitions [i.e. (1–0), (3–2), (5–4)] starting from the Herschel LF by Gruppioni et al. and usingappropriate LCO–LIR conversions for different galaxy classes. Our predicted LFs fit the data sofar available at z ≈ 0 and 2. We compare our results with those obtained by semi-analyticalmodels (SAMs): while we find a good agreement over the whole range of luminosities at z ≈ 0,at z ≈ 1 and z ≈ 2, the tension between our LFs and SAMs in the faint and bright ends increases.We finally discuss the contribution of luminous active galactic nucleus (LX > 1044 erg s−1) tothe bright end of the CO LF concluding that they are too rare to reproduce the actual CO LFat z ≈ 2.

Key words: galaxies: evolution – galaxies: luminosity function, mass function – infrared:galaxies.

1 IN T RO D U C T I O N

The study of the star formation (SF) history, and its connectionwith the gas mass accretion/consumption in galaxies, is one of thestill open issues in modern cosmology. A proper description of theevolution of SF across cosmic time needs both (a) a thorough under-standing of the relation between the total/molecular gas mass andthe SF, and (b) sufficiently large samples of galaxies at differentredshifts (z). As dust and gas are intimately associated, the dustinfrared (IR) continuum emission can be a good proxy to infer theinterstellar medium (ISM) mass (Scoville et al. 2014; Groves et al.2015), tracing it on large samples across cosmic time (e.g. Bertaet al. 2013). The state-of-the-art Atacama Large (Sub)MillimeterArray (ALMA) will make it possible in the next future to directlyfollow the molecular gas abundance as a function of redshift withblind searches of carbon monoxide (CO) rotational transitions (e.g.Carilli & Walter 2013, and references therein). So far, only a hand-ful of observational works have attempted to constrain this quan-tity. Keres, Yun & Young (2003) measured for the first time theCO(1–0) luminosity function (LF) at z = 0 using far-infrared (FIR)and optical B-band selected samples (see also Boselli, Cortese &Boquien 2014, for more recent CO(1–0) data at z ≈ 0). At z ≈ 2, wehave some observational constraints by Aravena et al. (2012) andDaddi et al. (2010). More recently, Walter et al. (2014) measuredthe CO LF in three redshift bins (z ≈ 0.3, 1.52, 2.75) based on ablind molecular line scan using the IRAM Plateau de Bure Inter-ferometer. In the near future, the advent of similar searches with

⋆ E-mail: [email protected]

ALMA will enable similar studies to much deeper levels and overlarger areas. On the theoretical side, the method generally adoptedto predict CO (J–(J–1)) LFs is to couple cosmological simulationswith semi-analytical prescriptions that relate the CO emission to thephysical properties of the simulated galaxies such as the intensity ofthe radiation field, the metallicity, the presence of an active galac-tic nucleus (AGN) (e.g. Obreschkow et al. 2009; Fu et al. 2012;Lagos et al. 2012; Popping, Somerville & Trager 2014a). The aimof this Letter is to derive the CO(1–0), CO(3–2), and CO(5–4) LFsat different redshifts by adopting a simple empirical approach thatallows us to convert the state-of-the-art observed IR LF presentedin Gruppioni et al. (2013). As a matter of fact, the CO luminosityis found to correlate with the total IR luminosity (LIR; 8–1000 µm),providing an integrated proxy of the Kennicutt–Schmidt (Kennicuttet al. 1998) relation that links star formation rate (SFR) and themolecular gas surface density. The correlation between these quan-tities relies on the fact that L′

CO1 is a molecular hydrogen tracer,

while LIR is a proxy of the SFR. This is true in homogeneous sam-ples of galaxies with comparable ISM properties, as the correlationbetween LCO and LIR implicitly depends on the dust-to-gas ratiosand metallicity within the galaxies (e.g. Leroy et al. 2013), on thepresence of additional heating due to AGN activity which affectsthe temperature of dust grains, and on the effects of gas streamingmotions on the star-forming properties (e.g. Meidt et al. 2013).

1 In what follows the L′CO notation will be used when the CO luminosity is

expressed in K km s−1 pc2.

C⃝ 2015 The AuthorsPublished by Oxford University Press on behalf of the Royal Astronomical Society

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teneo on February 17, 2016http://m

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MNRAS 439, 2736–2754 (2014) doi:10.1093/mnras/stu130Advance Access publication 2014 February 25

Tracing the cosmic growth of supermassive black holes to z ∼ 3with Herschel⋆

I. Delvecchio,1† C. Gruppioni,2 F. Pozzi,1 S. Berta,3 G. Zamorani,2 A. Cimatti,1

D. Lutz,3 D. Scott,4 C. Vignali,1 G. Cresci,5 A. Feltre,6,7 A. Cooray,8,9 M. Vaccari,10

J. Fritz,11 E. Le Floc’h,12 B. Magnelli,13 P. Popesso,3 S. Oliver,14 J. Bock,9,15

M. Carollo,16 T. Contini,17 O. Le Fevre,18 S. Lilly,16 V. Mainieri,7 A. Renzini19

and M. Scodeggio20

1Dipartimento di Fisica e Astronomia, Universita di Bologna, via Ranzani 1, I-40127 Bologna, Italy2INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy3Max-Planck-Institut for Extraterrestrische Physik (MPE), Postfach 1312, D-85741 Garching, Germany4Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada5INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy6Dipartimento di Fisica e Astronomia, Universita di Padova, vicolo Osservatorio 3, I-35122 Padova, Italy7ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching bei Munchen, Germany8Department of Physics & Astronomy, University of California, Irvine, CA 92697, USA9Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA10Astrophysics Group, Department of Physics, University of Western Cape, Bellville 7535, Cape Town, South Africa11Sterrenkundig Observatorium, Vakgroep Fysica en Sterrenkunde Universeit, Gent, Krijgslaan 281-S9, B-9000 Gent, Belgium12CEA-Saclay, Service d’Astrophysique, F-91191 Gif-sur-Yvette, France13Argelander Institute for Astronomy, Bonn University, Auf dem Hugel 71, D-53121 Bonn, Germany14Astronomy Centre, Department of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UK15California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA16Institute of Astronomy, Swiss Federal Institute of Technology (ETH Honggerberg), CH-8093 Zurich, Switzerland17Institut de Recherche en Astrophysique et Planetologie, CNRS, Universite de Toulouse, 14 avenue E. Belin, F-31400 Toulouse, France18Laboratoire d’Astrophysique de Marseille, CNRS-Universite de Provence, rue Frederic Joliot-Curie 38, F-13388 Marseille Cedex 13, France19INAF – Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy20INAF – IASF Milano, via Bassini 15, I-20133 Milano, Italy

Accepted 2014 January 16. Received 2013 December 30; in original form 2013 November 14

ABSTRACTWe study a sample of Herschel selected galaxies within the Great Observatories Origins DeepSurvey-South and the Cosmic Evolution Survey fields in the framework of the PhotodetectorArray Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the richmultiwavelength photometric data sets available in both fields, we perform a broad-bandspectral energy distribution decomposition to disentangle the possible active galactic nucleus(AGN) contribution from that related to the host galaxy. We find that 37 per cent of theHerschel-selected sample shows signatures of nuclear activity at the 99 per cent confidencelevel. The probability of revealing AGN activity increases for bright (L1−1000 > 1011 L⊙) star-forming galaxies at z > 0.3, becoming about 80 per cent for the brightest (L1−1000 > 1012 L⊙)infrared (IR) galaxies at z ≥ 1. Finally, we reconstruct the AGN bolometric luminosity functionand the supermassive black hole growth rate across cosmic time up to z ∼ 3 from a far-IRperspective. This work shows general agreement with most of the panchromatic estimates fromthe literature, with the global black hole growth peaking at z ∼ 2 and reproducing the observedlocal black hole mass density with consistent values of the radiative efficiency ϵrad (∼0.07).

Key words: galaxies: evolution – galaxies: nuclei – infrared: galaxies.

⋆Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation

from NASA.†E-mail: [email protected]


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A&A 554, A70 (2013)DOI: 10.1051/0004-6361/201321651c� ESO 2013

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Astrophysics

Herschel PEP/HerMES: the redshift evolution (0 z 4) of dustattenuation and of the total (UV+IR) star formation rate density?

D. Burgarella1, V. Buat1, C. Gruppioni2, O. Cucciati2, S. Heinis1, S. Berta3, M. Béthermin4, J. Bock5,6, A. Cooray7,5,J. S. Dunlop8, D. Farrah9,10, A. Franceschini11, E. Le Floc’h4, D. Lutz3, B. Magnelli3, R. Nordon3, S. J. Oliver9,

M. J. Page12, P. Popesso3, F. Pozzi13, L. Riguccini4, M. Vaccari11,14, and M. Viero5

1 Aix–Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, Francee-mail: [email protected]

2 INAF–Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy3 Max-Planck-Institut für Extraterrestrische Physik (MPE), Postfach 1312, 85741 Garching, Germany4 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris Diderot, CE-Saclay, pt courrier 131,

91191 Gif-sur-Yvette, France5 California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA6 Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA7 Dept. of Physics & Astronomy, University of California, Irvine, CA 92697, USA8 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK9 Astronomy Centre, Dept. of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK

10 Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA11 Dipartimento di Fisica e Astronomia, Università di Padova, vicolo Osservatorio, 3, 35122 Padova, Italy12 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK13 INAF – Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monte Porzio Catone, Italy14 Astrophysics Group, Physics Department, University of the Western Cape, Private Bag X17, 7535 Bellville, Cape Town,

South AfricaReceived 5 April 2013 / Accepted 29 April 2013

ABSTRACT

Using new homogeneous luminosity functions (LFs) in the far-ultraviolet (FUV) from VVDS and in the far-infrared (FIR) fromHerschel/PEP and Herschel/HerMES, we studied the evolution of the dust attenuation with redshift. With this information, we wereable to estimate the redshift evolution of the total (FUV + FIR) star formation rate density (SFRDTOT). By integrating SFRDTOT, wefollowed the mass building and analyzed the redshift evolution of the stellar mass density (SMD). This article aims at providing acomplete view of star formation from the local Universe to z ⇠ 4 and, using assumptions on earlier star formation history, comparesthis evolution with previously published data in an attempt to draw a homogeneous picture of the global evolution of star formationin galaxies. Our main conclusions are that: 1) the dust attenuation AFUV is found to increase from z = 0 to z ⇠ 1.2 and then starts todecrease until our last data point at z = 3.6; 2) the estimated SFRD confirms published results to z ⇠ 2. At z > 2, we observe eithera plateau or a small increase up to z ⇠ 3 and then a likely decrease up to z = 3.6; 3) the peak of AFUV is delayed with respect tothe plateau of SFRDTOT and a probable origin might be found in the evolution of the bright ends of the FUV and FIR LFs; 4) usingassumptions (exponential rise and linear rise with time) for the evolution of the star formation density from z = 3.6 to zform = 10, weintegrated SFRDTOT and obtained a good agreement with the published SMDs.

Key words. early Universe – cosmology: observations – galaxies: star formation – infrared: galaxies – galaxies: starburst –ultraviolet: galaxies

1. Introduction

One of the main objectives in astrophysics during the past15 years has been to follow the cosmic star formation rate den-sity (SFRD) at ever earlier epochs. But whenever optical data areused, one must apply a dust correction to the luminosity densi-ties (LDs) and a calibration into SFRDs (with their associateduncertainties) to obtain a relevant estimate. Knowing how thedust attenuation evolves in redshift is therefore mandatory if onewishes to study the redshift evolution of the SFRD.

For instance, Takeuchi et al. (2005) estimated the cosmicevolution of the SFRD from the far-ultraviolet (FUV) and far-infrared (FIR = bolometric IR). They found an increase of the

? Herschel is an ESA space observatory with science instrumentsprovided by European-led Principal Investigator consortia and with im-portant participation from NASA.

fraction of hidden SFR from 56% locally to 84% at z = 1. TheLDs show a significant evolution because the FIR LD evolvesfaster than the FUV. Their ratio ⇢FIR/⇢FUV increases from ⇠ 4(AFUV ⇠ 1.3 mag) locally to ⇠15 (AFUV ⇠ 2.3 mag) at z = 1.Cucciati et al. (2012) used the VIMOS-VLT Deep Survey toshow from the FUV only that the mean dust attenuation AFUVagrees with Takeuchi et al. (2005) over the range 0 < z < 1.Then it remains at the same level to z ⇠ 2, and declines to ⇠ 1mag at z ⇠ 4.

In this article, we use the FUV luminosity functions (LFs)published in Cucciati et al. (2012) from the VLT along withthe FIR LFs from Herschel/PACS and SPIRE data1 of a

1 From two Herschel large programmes: PACS evolutionary probe(PEP, Lutz et al. 2011) and the Herschel Multi-tiered ExtragalacticSurvey (HerMES, Oliver et al. 2012).

Article published by EDP Sciences A70, page 1 of 6

A&A 558, A15 (2013)DOI: 10.1051/0004-6361/201321396c⃝ ESO 2013

Astronomy&

Astrophysics

Cosmological model dependence of the galaxy luminosityfunction: far-infrared results in the Lemaître-Tolman-Bondi model

A. Iribarrem1,2, P. Andreani2, C. Gruppioni3, S. February4, M. B. Ribeiro5, S. Berta6, E. Le Floc’h7, B. Magnelli6,R. Nordon6, P. Popesso6, F. Pozzi8, and L. Riguccini7

1 Observatório do Valongo, Universidade Federal do Rio de Janeiro, Ladeira Pedro Antonio 43, 20080-090 Rio de Janeiro, Brazile-mail: [email protected]

2 European Southern Observatory (ESO),Karl-Schwarzschild-Straße 2, 85748 Garching, Germany3 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy4 Astrophysics, Cosmology and Gravitation Centre, and Department of Mathematics and Applied Mathematics,

University of Cape Town, Rondebosch 7701, Cape Town, South Africa5 Instituto de Física, Universidade Federal do Rio de Janeiro, CP 68532, 21941-972 Rio de Janeiro, Brazil6 Max-Planck-Institut für Extraterrestrische Physik (MPE), Postfach 1312, 85741 Garching, Germany7 CEA-Saclay, Service d’Astrophysique, 91191 Gif-sur-Yvette, France8 Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy

Received 1 March 2013 / Accepted 24 July 2013

ABSTRACT

Aims. This is the first paper of a series aiming at investigating galaxy formation and evolution in the giant-void class of theLemaître-Tolman-Bondi (LTB) models that best fits current cosmological observations. Here we investigate the luminosity func-tion (LF) methodology, and how its estimates would be affected by a change on the cosmological model assumed in its computation.Are the current observational constraints on the allowed cosmology enough to yield robust LF results?Methods. We used the far-infrared source catalogues built on the observations performed with the Herschel/PACS instrument andselected as part of the PACS evolutionary probe (PEP) survey. Schechter profiles were obtained in redshift bins up to z ≈ 4, assumingcomoving volumes in both the standard model, that is, the Friedmann-Lemaître-Robertson-Walker metric with a perfect fluid energy-momentum tensor, and non-homogeneous LTB dust models, parametrized to fit the current combination of results stemming from theobservations of supernovae Ia, the cosmic microwave background, and baryonic acoustic oscillations.Results. We find that the luminosity functions computed assuming both the standard model and LTB void models show in generalgood agreement. However, the faint-end slope in the void models shows a significant departure from the standard model up to red-shift 0.4. We demonstrate that this result is not artificially caused by the used LF estimator which turns out to be robust under thedifferences in matter-energy density profiles of the models.Conclusions. The differences found in the LF slopes at the faint end are due to variation in the luminosities of the sources that dependon the geometrical part of the model. It follows that either the standard model is over-estimating the number density of faint sourcesor the void models are under-estimating it.

Key words. galaxies: luminosity function, mass function – galaxies: distances and redshifts – infrared: galaxies –cosmology: theory – galaxies: evolution

1. Introduction

The luminosity function (LF) is an important observational toolfor galaxy evolution studies because it encodes the observed dis-tribution of galaxies in volumes and luminosities. However, acosmological model must be assumed in its estimation, render-ing it model dependent. On the other hand, the precision of thecurrent constraints on the cosmological model might arguablybe enough to yield an LF that has the same shape in all mod-els allowed by the observations. To investigate this assertion,it is necessary to compute the LF considering one such alter-native model, and perform a statistical comparison with the LFobtained assuming the standard model.

The currently favoured theory for explaining the shape andredshift evolution of the LF is that the dark matter haloes growup hierarchically by merging, and that baryonic matter trappedby these haloes condense to form galaxies. Astrophysical pro-cesses (gas cooling, high redshift photoionization, feedbacks),

are then responsible for reproducing the shape of the luminosityfunction of galaxies starting from the dark matter halo massfunction (Benson et al. 2003). The usual approach in the contextof the standard model is either to use semi-analytical models toparameterize these processes (e.g. Neistein & Weinmann 2010),or to use empirical models (e.g. Yang et al. 2003; Skibba & Sheth2009; Zehavi et al. 2011) to allocate galaxies as a function ofhalo mass, both built on a dark matter hierarchical merger treecreated by simulations, like the Millennium simulation (Springelet al. 2005; Boylan-Kolchin et al. 2009).

It has been well-established by observations made atmany different wavelengths (some recent examples includevan der Burg et al. 2010; Ramos et al. 2011; Cool et al. 2012;Simpson et al. 2012; Patel et al. 2013; Stefanon & Marchesini2013), and particularly in the IR (Babbedge et al. 2006; Caputiet al. 2007; Rodighiero et al. 2010; Magnelli et al. 2011; Heiniset al. 2013), that the LF shows significant evolution with redshift.In practice the LF is traditionally computed using the comoving


MNRAS 451, 3419–3426 (2015) doi:10.1093/mnras/stv1204

Star formation in Herschel’s Monsters versus semi-analytic models

C. Gruppioni,1‹ F. Calura,1 F. Pozzi,2 I. Delvecchio,2 S. Berta,3 G. De Lucia,4

F. Fontanot,4 A. Franceschini,5 L. Marchetti,6 N. Menci,7 P. Monaco8 and M. Vaccari91Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy2Dipartimento di Fisica e Astronomia, Universita di Bologna, viale Berti Pichat 6, I-40127 Bologna, Italy3Max-Planck-Institut fur Extraterrestrische Physik (MPE), Postfach 1312, D-85741 Garching, Germany4Istituto Nazionale di Astrofisica - Osservatorio Astronomico di Trieste, Via Tiepolo 11, I-34143 Trieste, Italy5Dipartimento di Astronomia, Universita di Padova, vicolo dell’Osservatorio 3, I-35122 Padova, Italy6Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK7INAF Osservatorio Astronomico di Roma, via di Frascati 33, I-00040 Monte Porzio Catone, Italy8Dipartimento di Fisica, Sezione di Astronomia, via Tiepolo 11, I-34143 Trieste, Italy9Astrophysics Group, Department of Physics, University of Western Cape, Bellville 7535, Cape Town, South Africa

Accepted 2015 May 25. Received 2015 May 6; in original form 2015 March 17

ABSTRACTWe present a direct comparison between the observed star formation rate functions (SFRFs)and the state-of-the-art predictions of semi-analytic models (SAMs) of galaxy formation andevolution. We use the PACS Evolutionary Probe Survey and Herschel Multi-tiered Extragalac-tic Survey data sets in the COSMOS and GOODS-South fields, combined with broad-bandphotometry from UV to sub-mm, to obtain total (IR+UV) instantaneous star formation rates(SFRs) for individual Herschel galaxies up to z ∼ 4, subtracted of possible active galacticnucleus (AGN) contamination. The comparison with model predictions shows that SAMsbroadly reproduce the observed SFRFs up to z ∼ 2, when the observational errors on the SFRare taken into account. However, all the models seem to underpredict the bright end of theSFRF at z ! 2. The cause of this underprediction could lie in an improper modelling of severalmodel ingredients, like too strong (AGN or stellar) feedback in the brighter objects or too lowfallback of gas, caused by weak feedback and outflows at earlier epochs.

Key words: galaxies: evolution – galaxies: formation – galaxies: star formation – cosmology:observations – infrared: galaxies.


The study of how the star formation rate (SFR) in galaxies evolveswith redshift provides important constraints to the galaxy formationand evolution theories. In particular, semi-analytic models (SAMs;e.g. White & Frenk 1991; Kauffmann, White & Guiderdoni 1993;Springel et al. 2001; Monaco, Fontanot & Taffoni 2007; Guo et al.2011; Benson et al. 2012; Menci, Fiore & Lamastra 2012; Henriqueset al. 2013) need to be directly compared with observations to obtaininsight of the relevant physical processes. The first and most pop-ular SAMs are three, commonly named ‘Munich’ (starting withthe models of Kauffmann et al. 1993), ‘Durham’ (beginningwith the models of Cole et al. 1994), and ‘Santa Cruz’ (begin-ning with the models of Somerville & Primack 1999); more recentSAMs include, i.e. Croton et al. 2006; Bower et al. 2006; Somervilleet al. 2008; Fontanot et al. 2009; Guo et al. 2011; Somerville et al.2012. The main differences between these models lie in the pre-scriptions adopted for some of the most basic baryonic processes,


such as star formation, gas cooling, and feedback. One of the pro-cesses that must be modelled and compared to data is the evolutionof the SFR over the cosmic time. However, the derivation of anaccurate SFR from observational data is difficult, due to the manyuncertainties involved in its reconstruction. An important source ofuncertainty comes from dust extinction. The rest-frame ultraviolet(UV) light emitted by young and massive stars, strictly connected tothe instantaneous SFR in galaxies, is strongly absorbed by dust, andre-radiated in the infrared (IR) bands. Dust attenuation, as well asother galaxy physical properties, evolve with cosmic time and showa peak between z ∼ 1 and 2 (e.g. Burgarella et al. 2013). Knowinghow dust attenuation evolves in redshift is therefore crucial to studythe redshift evolution of the SFR: to this purpose, combining UVinformation with direct observations in the IR region is probably thebest tool to account for the total SFR (e.g. Kennicutt 1998). In fact,IR surveys covering a wide range of redshifts are extremely usefulto estimate the global IR luminosity, since they provide a directmeasurement of the amount of energy absorbed and re-emitted bydust (e.g. what is missed by UV surveys).

Herschel (Pilbratt et al. 2010), with its 3.5 m mirror, hasbeen the first telescope which allowed us to detect the far-IR


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Astronomy&

Astrophysics

The evolution of galaxy star formation activity in massive haloes⋆

P. Popesso1,2, A. Biviano3, A. Finoguenov2, D. Wilman2, M. Salvato2, B. Magnelli2, C. Gruppioni4, F. Pozzi5,G. Rodighiero6, F. Ziparo2, S. Berta2, D. Elbaz7, M. Dickinson8, D. Lutz2, B. Altieri9, H. Aussel7, A. Cimatti6,

D. Fadda10, O. Ilbert11, E. Le Floch7, R. Nordon2, A. Poglitsch2, and C. K. Xu12

1 Excellence Cluster Universe, Boltzmannstr. 2, 85748 Garching, Germanye-mail: [email protected]

2 Max-Planck-Institut für Extraterrestrische Physik (MPE), Postfach 1312, 85741 Garching, Germany3 INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34143 Trieste, Italy4 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy5 Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy6 Dipartimento di Astronomia, Università di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy7 Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service d’Astrophysique, Bât. 709, CEA-Saclay,

91191 Gif-sur-Yvette Cedex, France8 National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA9 Herschel Science Centre, European Space Astronomy Centre, ESA, Villanueva de la Cañada, 28691 Madrid, Spain

10 NASA Herschel Science Center, Caltech 100-22, Pasadena, CA 91125, USA11 Institute for Astronomy 2680 Woodlawn Drive Honolulu, HI 96822-1897, USA12 IPAC, Caltech 100-22, Pasadena, CA 91125, USA

Received 30 July 2014 / Accepted 13 October 2014

ABSTRACT

Context. There is now a large consensus that the current epoch of the cosmic star formation history (CSFH) is dominated by low massgalaxies while the most active phase, between redshifts 1 and 2, is dominated by more massive galaxies, which evolve more quickly.Aims. Massive galaxies tend to inhabit very massive haloes, such as galaxy groups and clusters. We aim to understand whetherthe observed “galaxy downsizing” could be interpreted as a “halo downsizing”, whereas the most massive haloes, and their galaxypopulations, evolve more rapidly than the haloes with lower mass.Methods. We studied the contribution to the CSFH of galaxies inhabiting group-sized haloes. This is done through the study of theevolution of the infra-red (IR) luminosity function of group galaxies from redshift 0 to redshift ∼1.6. We used a sample of 39 X-ray-selected groups in the Extended Chandra Deep Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOSfield, where the deepest available mid- and far-IR surveys have been conducted with Spitzer MIPS and with the Photodetector ArrayCamera and Spectrometer (PACS) on board the Herschel satellite.Results. Groups at low redshift lack the brightest, rarest, and most star forming IR-emitting galaxies observed in the field. TheirIR-emitting galaxies contribute ≤10% of the comoving volume density of the whole IR galaxy population in the local Universe. Atredshift !1, the most IR-luminous galaxies (LIRGs and ULIRGs) are mainly located in groups, and this is consistent with a rever-sal of the star formation rate (SFR) vs. density anti-correlation observed in the nearby Universe. At these redshifts, group galaxiescontribute 60–80% of the CSFH, i.e. much more than at lower redshifts. Below z ∼ 1, the comoving number and SFR densities ofIR-emitting galaxies in groups decline significantly faster than those of all IR-emitting galaxies.Conclusions. Our results are consistent with a “halo downsizing” scenario and highlight the significant role of “environment”quenching in shaping the CSFH.

Key words. galaxies: evolution – galaxies: clusters: general – galaxies: luminosity function, mass function – galaxies: groups: general

1. Introduction

One of the most fundamental correlations between the propertiesof galaxies in the local Universe is the so-called morphology-density relation. Since the early work of Dressler (1980), aplethora of studies utilizing multi-wavelength tracers of activ-ity have shown that late type star-forming galaxies favour low-density regimes in the local Universe (e.g. Gómez et al. 2003). Inparticular, the cores of massive galaxy clusters are galaxy grave-yards of massive spheroidal systems dominated by old stellarpopulations. Much of the current debate centres on whether the

⋆ Herschel is an ESA space observatory with science instrumentsprovided by European-led Principal Investigator consortia and with im-portant participation from NASA.

relation arises early on during the formation of the object, orwhether it is caused by environment-driven evolution. However,as we approach the epoch when the quiescent behemoths shouldbe forming the bulk of their stars at z ! 1.5 (e.g. Rettura et al.2010), the relation between star formation (SF) activity and en-vironment should progressively reverse. Elbaz et al. (2007) andCooper et al. (2008) observe the reversal of the star formationrate (SFR) vs. density relation already at z ∼ 1 in the GOODSand the DEEP2 fields, respectively. Using Herschel PACS data,Popesso et al. (2011) show that the reversal is mainly observed inhigh-mass galaxies and is due to a higher fraction of active galac-tic nuclei (AGN), which exhibit slightly higher SFR than galax-ies of the same stellar mass (Santini et al. 2012). On the otherhand, Feruglio et al. (2010) find no reversal in the COSMOS


ARE THE BULK OF >z 2 HERSCHEL GALAXIES PROTO-SPHEROIDS?

F. Pozzi1,2, F. Calura2, C. Gruppioni2, G. L. Granato3, G. Cresci4, L. Silva3, L. Pozzetti2,F. Matteucci3,5, and G. Zamorani2

1 Dipartimento di Fisica e Astronomia, Università degli Studi di Bologna, Viale Berti Pichat 6/2, I-40127 Bologna, Italy; [email protected] INAF—Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy

3 INAF—Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, I-34131, Trieste, Italy4 INAF—Osservatorio Astronomico di Arcetri, Via Largo Enrico Fermi 5, I-50125 Firenze, Italy5 Dipartimento di Fisica, Università degli Studi di Trieste, Via Valerio 2, I-34127 Bologna, Italy

Received 2014 July 30; accepted 2015 February 10; published 2015 April 13

ABSTRACT

We present a backward approach for the interpretation of the evolution of the near-IR and the far-IR luminosityfunctions (LFs) across the redshift range < <z0 3. In our method, late-type galaxies are treated by means of aparametric phenomenological method based on PEP/HerMES data up to z ∼ 4, whereas spheroids are described bymeans of a physically motivated backward model. The spectral evolution of spheroids is modeled by means of asingle-mass model, associated with a present-day elliptical with a K-band luminosity comparable to the break ofthe local early-type LF. The formation of proto-spheroids is assumed to occurr across the redshift range ⩽ ⩽z1 5.The key parameter is represented by the redshift z0.5 at which half of all proto-spheroids are already formed. Forthis parameter, a statistical study indicates values between =z 1.50.5 and =z 30.5 . We assume ~z 20.5 as thefiducial value and show that this assumption allows us to describe accourately the redshift distributions and thesource counts. By assuming ~z 20.5 at the far-IR flux limit of the PEP-COSMOS survey, the PEP-selected sourcesobserved at >z 2 can be explained as progenitors of local spheroids caught during their formation. We also testthe effects of mass downsizing by dividing the spheroids into three populations of different present-day stellarmasses. The results obtained in this case confirm the validity of our approach, i.e., that the bulk of proto-spheroidscan be modeled by means of a single model that describes the evolution of galaxies at the break of the present-dayearly-type K-band LF.

Key words: galaxies: evolution – galaxies: formation – galaxies: luminosity function, mass function – infrared:galaxies

1. INTRODUCTION

Achieving a complete understanding of the origin of thelocal dichotomy of spheroids and disk galaxies has been one ofthe main objectives in astrophysics during the past severalyears, as well as obtaining an accurate measure of the starformation history over cosmic time.

From the pioneering IRAS satellite results in the localuniverse (e.g., Soifer et al. 1987) and the detection of a cosmicinfrared (IR) background as energetic as the optical/near-IRbackground (e.g., Puget et al. 1996), it is now well establishedthat most energy radiated by newly formed stars is heavilyabsorbed by dust and re-emitted in the IR band. In the lastdecade, the ISO and the Spitzer satellite individually detectedIR sources up to z ∼ 1 (e.g., Elbaz et al. 1999; Gruppioniet al. 2002) and z ∼ 2 (e.g., Papovich et al. 2004; Shupeet al. 2008) in the mid-IR band, but their capabilities at far-IRwavelengths (i.e., where the dust reprocessed emission peaks)were still strongly limited by source confusion.

More recently, the Herschel Space Observatory (Pilbrattet al. 2010) has allowed us to properly measure the IRluminosity function (LF) of galaxies up to z ∼ 4 (Gruppioniet al. 2013, hereafter GPR13; see also Magnelli et al. 2013),thanks to its mirror of 3.5 m and observing spectral rangebetween 60 and 670 μm. The derived IR luminosity density(rIR) confirms the Spitzer 24 μm based results (e.g., Caputiet al. 2007; Magnelli et al. 2009; Rodighiero et al. 2010) up to z∼ 2, revealing that the IR luminosity density increases steeplyfrom z = 0 up to z ∼ 1, then flattens between z ∼ 1 and z ∼ 3, todecrease at >z 3.

In a recent paper by Burgarella et al. (2013), the IR HerschelLF derived by GPR13 has been combined with the LF in thefar-UV from Cucciati et al. (2012) in order to achieve anestimate of the redshift evolution of the total (far-UV + IR) starformation rate density (SFRD). The SFRD is alwaysdominated by the IR emission, whereas the UV contributionincreases steeply from z = 0 up to z ∼ 2.5, where it flattens andsettles on a plateau up to the highest redshift sampled by thesurvey (z ∼ 3.6). This suggests that the peak of the dustattenuation, occurring at z ∼ 1, is delayed with respect to theSFRD plateau (z ∼ 2−3), derived from the far-UV.The accurate determination of the star formation history up

to z ∼ 4 has rendered particularly urgent the issue oftheoretically explaining this behavior as well as understandinghow the observed SFRD evolution is linked to the galaxyformation process.Within the current “concordance” cosmological paradigm,

which employs a Λ cold dark matter (ΛCDM)-dominateduniverse, the formation of structures is hierarchical since smalldark matter (DM) halos are the first to collapse, then interactand merge to assemble into larger halos (e.g., Laceyet al. 2008; Fontanot et al. 2009).In cosmological ΛCDM-based semi-analytical models

(SAMs) for galaxy formation, the most uncertain assumptionsconcern the behavior of the baryonic matter. In the firstclassical SAM implementations, baryonic matter was assumedto follow the DM in all the interaction and merging processesand spheroid galaxies were formed from several mergingepisodes of smaller sub-units with the most massive galaxies asthe last systems to assemble. Indeed, more recent results

The Astrophysical Journal, 803:35 (16pp), 2015 April 10 doi:10.1088/0004-637X/803/1/35© 2015. The American Astronomical Society. All rights reserved.

1

MNRAS 438, 2547–2564 (2014) doi:10.1093/mnras/stt2375Advance Access publication 2014 January 10

Exploring the early dust-obscured phase of galaxy formation with blindmid-/far-infrared spectroscopic surveys

M. Bonato,1,2‹ M. Negrello,2 Z.-Y. Cai,3 G. De Zotti,2,3 A. Bressan,3 A. Lapi,3,4

C. Gruppioni,5 L. Spinoglio6 and L. Danese3

1Dipartimento di Fisica e Astronomia ‘G.Galilei’, Universita degli Studi di Padova, Vicolo Osservatorio 3, I-35122 Padova, Italy2INAF, Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, I-35122 Padova, Italy3SISSA, Via Bonomea 265, I-34136 Trieste, Italy4Dipartimento di Fisica, Universita ‘Tor Vergata’, Via della Ricerca Scientifica 1, I-00133 Roma, Italy5INAF, Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy6Istituto di Astrofisica e Planetologia Spaziali, INAF-IAPS, Via Fosso del Cavaliere 100, I-00133 Roma, Italy

Accepted 2013 December 6. Received 2013 November 18; in original form 2013 August 26

ABSTRACTWhile continuum imaging data at far-infrared to submillimetre wavelengths have provided tightconstraints on the population properties of dusty star-forming galaxies up to high redshifts,future space missions like the Space Infrared Telescope for Cosmology and Astrophysics(SPICA) and ground-based facilities like the Cerro Chajnantor Atacama Telescope (CCAT)will allow detailed investigations of their physical properties via their mid-/far-infrared lineemission. We present updated predictions for the number counts and the redshift distributions ofstar-forming galaxies spectroscopically detectable by these future missions. These predictionsexploit a recent upgrade of evolutionary models, that include the effect of strong gravitationallensing, in the light of the most recent Herschel and South Pole Telescope data. Moreover therelations between line and continuum infrared luminosity are re-assessed, considering alsodifferences among source populations, with the support of extensive simulations that takeinto account dust obscuration. The derived line luminosity functions are found to be highlysensitive to the spread of the line to continuum luminosity ratios. Estimates of the expectednumbers of detections per spectral line by SPICA/SpicA FAR-infrared Instrument (SAFARI)and by CCAT surveys for different integration times per field of view at fixed total observingtime are presented. Comparing with the earlier estimates by Spinoglio et al. we find, in thecase of SPICA/SAFARI, differences within a factor of 2 in most cases, but occasionally muchlarger. More substantial differences are found for CCAT.

Key words: galaxies: active – galaxies: evolution – galaxies: luminosity function, mass func-tion – galaxies: starburst – infrared: galaxies.


The rest-frame mid- to far-infrared (IR) spectral region offersa rich suite of spectral lines that allow us to probe all phasesof the interstellar medium (ISM): ionized, atomic and molecular(Spinoglio & Malkan 1992). Measurements of these lines provideredshifts and key insight on physical conditions of dust-obscuredregions and on the energy sources controlling their temperature andpressure. This information is critically important for investigatingthe complex physics ruling the dust-enshrouded active star-formingphase of galaxy evolution and the relationship with nuclear activity.


A major progress in this field is therefore expected with plannedor forthcoming projects specifically devoted to mid- to far-IR spec-troscopy such as the Space Infrared Telescope for Cosmology andAstrophysics (SPICA)1 with its SpicA FAR-infrared Instrument(SAFARI; Roelfsema et al. 2012) and the Cerro Chajnantor At-acama Telescope (CCAT; Woody et al. 2012).2 SAFARI is an imag-ing spectrometer designed to fully exploit the extremely low far-IR background environment provided by the SPICA observatory,whose telescope will be actively cooled at 6 K. In each integrationit will take complete 34–210 µm spectra with three bands (34–60,

1 http://www.ir.isas.jaxa.jp/SPICA/SPICA_HP/index-en.html2 http://www.ccatobservatory.org


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The star-formation rate density from z = 1-6 ⋆

Michael Rowan-Robinson1 , Seb Oliver2, Lingyu Wang3,Lucia Marchetti4, Duncan Farrah5, Carlotta Gruppioni6, Mattia Vaccari71Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK2Astronomy Centre, Dept. of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK,3Department of Physics, Durham University, South Rd, Durham DH1 3LE, UK,4Department of Physical Science, The Open University, Milton Keynes MK7 6AA, UK5Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA6INAF, - Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy7Astrophysics Group, University of the Western Cape, Private Bag X17, 7535, Bellville, Cape Town, South Africa

4 February 2016

ABSTRACT

We use Herschel-SPIRE data from the HerMES Lockman, ES1 and XMM-LSS areasto estimate the star-formation rate density at z = 1-6.

500 µm sources are associated first with 350 and 250 µm sources, and then withSpitzer 24 µm sources from the SWIRE photometric redshift catalogue. The infraredand submillimetre data are fitted with a set of radiative-transfer templates correspond-ing to cirrus (quiescent) and starburst galaxies. Lensing candidates are removed via aset of colour-colour and colour-redshift constraints. Star-formation rates are found toextend from < 1 to 20,000 M⊙yr−1.

Star-formation rate functions are derived in a series of redshift bins from 0-6, com-bined with earlier far-infrared estimates, where available, and fitted with a Saundersfunctional form. The star-formation-rate density as a function of redshift is derivedand compared with other estimates. There is good agreement with both infrared andultraviolet estimates for z < 3, but we find significantly higher star-formation-ratedensities than ultraviolet estimates at z = 3-6.

Key words: infrared: galaxies - galaxies: evolution - star:formation - galaxies: star-burst - cosmology: observations

1 INTRODUCTION

The history of the determination of the evolution of the in-tegrated star-formation rate density has been controversial.Lilley at al (1996) and Madau et al (1996) gave estimatesbased purely on the ultraviolet (uv) light from galaxies, witha correction for extinction based on a screen model. Rowan-Robinson et al (1997) showed from ISO data that this es-timate was likely to be significantly underestimated. Morerecent uv surveys (e.g. Wyder et al 2005, Schiminvich et al2005, Dahlen et al 2007, Reddy and Steidel (2009), Cucciatiet al 2012) and infrared (ir) surveys (eg Sanders et al 2003,Takeuchi et al 2003, Magnelli et al 2011, 2013, Gruppioni etal 2013) are now in good agreement for z < 3. The Grup-pioni et al (2013) study of Herschel sources at 70, 90 and160 µm is especially significant in capturing the total far

⋆ Herschel is an ESA space observatory with science instrumentsprovided by European-led Principal Investigator consortia andwith important participation from NASA.

infrared luminosity, and hence a more accurate estimate ofthe star- formation rate. Madau and Dickinson (2014) havegiven a comprehensive review of the current situation.

At higher redshifts we have only ultraviolet estimates(Bouwens et al 2012a,b, Schenker et al 2013) and so theproblem remains: is the contribution of dust-shrouded star-formation being properly accounted for ? The problem canbe seen clearly by imagining external observations of ourown Galaxy. The blue and ultraviolet light would be dom-inated by young stars which would be subject to an aver-age extinction of a few tenths of a magnitude, due to thedust spread through the interstellar medium. The infraredemission from this optically thin dust makes up the infraredcirrus. However the contribution of newly formed stars em-bedded in dense molecular clouds would not be accountedfor. In the case of our Galaxy this would result in an under-estimate of the total star-formation rate by only about 10%,but for luminous starbursts the underestimate could be overa factor of 100.

To address this question we really need to analyse

c⃝ 0000 RAS

2016 2016 (submitted)

AGN fraction

Netzer+'2007'slope'

CT?

MIR: for AGN

FIR: for SF

LIR from re-emitted stellar light (LIR[8-1000μm] is a proxy) Lbol from AGN torus model

SF

AGN

CG+ 2016, MNRAS in press

IR lines as tracers of BH accretion and SF

LIRSF

L IR(line

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AGN fraction Herschel LF

CG+ 2013

LINE LF



z-distributions of objs detectable in the different IR lines with MIRI/JWST and SMI+SAFARI/SPICA

Far-IR Line Luminosity as a tracer of BHAR 19

Figure 12. Redshift distribution (per unit area) of sources with fluxes of the different mid-IR lines larger than the MIRI-JWSTsensitivities (5σ, 10000s; left) and the SPICA ones (5σ, 10,000s; right), as expected based on the method described in this work. Thetotal (e.g., AGN+galaxies) number of sources per unit area (for SPICA it is the number detectable by both SMI and SAFARI instruments)is shown as grey-filled histogram, while the AGN contribution is shown in red. The yellow and green histograms enlighten the SMI totaland AGN contribution respectively.

MNRAS 000, 1–23 (2015)



In principle with any future IR/sub-mm

facilities

PREDICTIVE POWER OF THIS WORK

"  $SF$bolometric$luminosity$(Gruppioni+2016)$"  $AGN$bolometric$luminosity$(Grupponi+2016)$"  $MIR/FIR$(Spitzer/Herschel)$and$sub2millimeter$(ALMA)$spectroscopic$data$

Observations

INPUTS&&&&&&&&&

1.   Starburst99$spectrum$2.   AGN$spectrum$$3.  gas&density&4.  distance&from&the&source&

OUTPUTS&&&&&&&&&

A.   line$luminosi7es$B.  emiBed&conCnuum&C.  gas&and&grain&temperature&

Cloudy Modelling

Vallini, CG, Pozzi+ in prep.&

ISM modelling in galaxies and AGN &

[Ne&V&24]/[Ne&II&12]&observed&value&of&[NeV]/[NeII]&&

observed&value&of&[OIV]/[NeII]&&

green&contours&with&numbers&=&[OIV]/[NeII]& to&be&compared&with&&observed&value&of&[OIV]/[NeII]&&

backgroud&image&=&[NeV]/[NeII]& to&be&compared&with&&observed&value&of&[NeV]/[NeII]&&


log&(Lbol,agn)&=&43.0&



[Ne&V&24]/[Ne&II&12]&

NGC4051&

NGC4151&

At$fixed$Lbol,$SB=1043$erg/s$


ISM modelling in galaxies and AGN &

ALMA$CO(625)$of$NGC7130$(Pozzi+$in$prep)$ SpaCal&informaCon&that&can&help&in&constraining&the&

distance&parameter&in&the&Cloudy&modeling&

Lbol,SB&known&from&CG+2016&Lbol,AGN&from&X$ray&data&

ProperCes&of&the&emiYng&gas&and&effect&of&the&AGN&

on&the&CO&SLED&

Perspective for ALMA

Pozzi, Talia, Vallini, CG+ in prep.&

Perspective for ALMA

Vallini, CG, Pozzi+ 2016&

CO Luminosity Function

Thank You !

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