Investigations of the population of radio-active AGN up to z=3.5 not only show that these sources are hosted by galaxies of very large, M*>1010.5 Msun, stellar masses, but also that at all redshifts they reside in very massive dark matter halos, comparable to those associated with groups-to-clusters of galaxies. This result is found both via clustering studies and by directly pinpointing such sources to the cosmological structures they belong to. We also show how intense star-forming activity is encountered in the overwhelming majority of z>1 (massive) galaxies hosts of radio-active AGN, and how this activity is only halted by nuclear feedbacks in the relatively local universe. What emerges from our work is a scenario whereby physical processes at sub-pc/pc (e.g. AGN emission) and kpc scales strongly influence the large-scale structure behavior of the AGN and its host

MAGLIOCCHETTI, MANUELA

Mara Salvato

Marcella Brusa

Paola Popesso

Magliocchetti, Manuela

Popesso, P.

Brusa, M.

Salvato, M.

ZENODO

Hosts and environments of radio-active AGN

Investigations of the population of radio-active AGN up to z=3.5 not only show that these sources are hosted by galaxies of very large, M*>1010.5 Msun, stellar masses, but also that at all redshifts they reside in very massive dark matter halos, comparable to those associated with groups-to-clusters of galaxies. This result is found both via clustering studies and by directly pinpointing such sources to the cosmological structures they belong to. We also show how intense star-forming activity is encountered in the overwhelming majority of z>1 (massive) galaxies hosts of radio-active AGN, and how this activity is only halted by nuclear feedbacks in the relatively local universe. What emerges from our work is a scenario whereby physical processes at sub-pc/pc (e.g. AGN emission) and kpc scales strongly influence the large-scale structure behavior of the AGN and its host.</p

Magliocchetti, Manuela (5262631)

Popesso, P. (5262628)

Brusa, M. (5191615)

Salvato, M. (5201242)

FigShare

OA@INAF - Istituto Nazionale di Astrofisica

2018Publication Year2022-02-28T15:37:14ZAcceptance in OA@INAFHosts and environments of radio-active AGNTitleMAGLIOCCHETTI, MANUELA; Paola Popesso; Marcella Brusa; Mara SalvatoAuthors10.5281/zenodo.1472829DOIhttp://hdl.handle.net/20.500.12386/31503HandleHOSTS AND ENVIROMENTS OF         RADIO-ACTIVE AGN Manuela Magliocchetti           IAPS-INAF P.Popesso – M. Brusa – M.Salvato  (Magliocchetti+2014;2016,2017, 2018a,2018b) RADIO-EMITTING AGN OR STAR-FORMING GALAXY? AGN!!  AGN?  AGN?/SFG?  AGN???  AGN?/SFG?  CRITERIA FOR AGN/SF DIVISION IN RADIO SURVEYS             (Magliocchetti+2014;2016,2017,2018a,2018b) Radio data from VLA-VIRMOS  (Bondi+ 2003). 1 deg2 complete  to 100mJy: 1054 sources  AGN all sources with P(z)>Pcross(z) SF all sources with P(z)<Pcross(z) [N.B. also includes RQQ] McAlpine+2013	From McAlpine+13 RLF  z evolution of cross-point  from SF-dominated to  AGN-dominated sources:  Log10Pcross(z)=Log10P0,cross+z    @ z<1.8 Log10Pcross=23.5 [W/Hz/sr]         @ z>1.8   P0,cross break of local SF RLF (Magliocchetti+2002;  Mauch& Sadler 2007) AGN AGN AGN AGN AGN AGN A) COSMOS-VLA Survey (Bondi+2008)  Ntot (F1.4GHz>60µJy): 2382    Nz(F1.4GHz>60µJy)=2123 (90%)  NAGN=704 (272 FIR)  -- shallower in radio/FIR but wider area   B) GOODS-N + GOODS-S (Morrison+2010; Miller+2013)  Ntot (F1.4GHz>20µJy): 401 + 142  Nz(F1.4GHz>20µJy):    267 + 114 (≈75%)  NAGN=32+15 (23+8 FIR)-- deeper in radio/FIR but smaller area   FIELD AND DATA SELECTION STELLAR MASSES OF RADIO-AGN HOSTS 90% have M*>1010 Msun. 50% M*>1011Msun COSMOS GOODSN+GOODSS 90% M*>1010.5 Msun	90% M*>1010.5 Msun	50% M*>1011 Msun	 50% M*>1011 Msun	[N=47 – 31 FIR] -  [N=704 -272 FIR] -  HOSTS OF RADIO AGN EXTREMELY MASSIVE GALAXIES AT ALL REDSHIFTS STAR-FORMING ACTIVITY WIHIN RADIO-AGN HOSTS HOSTS OF RADIO EMITTING AGN NOT ONLY VERY MASSIVE BUT SITES  OF INTENSE STAR FORMATION ACTIVITY, PARTICULARLY AT z>1 GN+GS AGN WITH FIR ACTIVITY (66%) COSMOS AGN WITH FIR ACTIVITY (38%) Fraction of FIR emitters amongst radio-selected AGN as a function of radio  luminosity at different cosmological epochs FRACTION AGN WHICH ARE FIR EMITTERS RADIO LUMINOSITY 20% 40% 50% RADIO LUMINOSITY FRACTION AGN WHICH ARE FIR EMITTERS 20% –100% –100% GN+GS COSMOS 0% 0% 40% 0% WHAT HAVE WE LEARNED SO FAR?  1) Radio-emitting AGN are hosted by very massive galaxies at all z 2) Most of them are in the process of forming stars at very high rates  3)  Such  star-forming activity much more intense in the past.       Deepest FIR surveys show that ~100% of high (z>~1) redshift        radio-active AGN are associated to SF events      à AND WHAT ABOUT AGN LARGE-SCALE ENVIRONMENT?  Investigate spatial distribution via 2ptCF and direct pinpoint  on known structures (COSMOS) CLUSTERING ANALYSIS:  COMPARISON OF AGN RESULTS WITH LITERATURE AGN	Peacock& Nicholson 1991 F>500 mJy – z<0.1 Magliocchetti+2004  --  2dF+FIRST F>1 mJy (AGN) -- <z>=0.1  Brand+2005  -- Texas-Oxford+NVSS F>3 mJy -- <z>=0.3 Lindsay+2014 – GAMA+FIRST F>1mJy -- <z>=0.5 Lindsay+2014b – VLA-VIRMOS F>0.09 mJy -- <z>0=2.2 Magliocchetti+2016 – VLA-COSMOS F>0.15 mJy -- <z>=1.3 Except for P&N excellent agreement amongst different results à à INDEPENDENCE OF AGN CLUSTERING PROPERTIES ON   1) REDSHIFT and 2) RADIO LUMINOSITY (P<~ 1024.5-25 W/Hz) RADIO-ACTIVE AGN RESIDE WITHIN THE SAME STRUCTURES AT ALL  RADIO LUMINOSITIES <~1024.5-25 W/Hz. NO EVOLUTION IN PROPERTIES  DURING COSMIC EPOCHS AT LEAST SINCE z~3!    NO DOWNSIZING Lindsay+2014bLindsay+2014Brand+2005Magliocchetti+2004Peacock&Nicholson1991This work AGNREDSHIFT AGN	CLUSTERING RADIUS [Mpc]  MHALOMIN≈1013.5 Msun (groups-to-clusters of galaxies) {	CLUSTERING ANALYSIS:  COMPARISONS OF SF RESULTS WITH LITERATURE Saunders+1992Magliocchetti&Maddox1999Heinis+2007Lin+2012Magliocchetti+2008Starikova+2012Brodwin+2008van Kampen+2012Hickox+2012Magliocchetti+2011Magliocchetti+2013Martin+2012This work SFThis work SF z<1Adapted from Magliocchetti+2014 Red: 60mm RF selection Blue: UV selection Magenta: BzK selection Green: 24mm selection Black: 250mm (RF) selection Cyan: HI selection Gold: radio-SF selection (this work) Peculiar trend of SF clustering.  Jump in the clustering properties  beyond z>1.5.  At variance with AGN  SF hosted by very massive  structures  only  z>1.5 REDSHIFT CLUSTERING RADIUS [Mpc] MHALOMIN≈1013.5 Msun MHALOMIN≈1011.5 Msun DOWNSIZING RELATIONSHIP BETWEEN DARK AND LUMINOUS MATTER IN AGN Mmin from clustering           -----       M* from Laigle+2016 catalogue <M*>/Mmin<10-2.7   relatively small stellar content (large uncertainties) 	DURATION OF RADIO-ACTIVE AGN PHASE Comparison of observed space density of AGN with that expected for  dark matter haloes more massive than Mmin (from clustering results)     Fraction of haloes with Mmin>10 13.6Msun host of a radio-active AGN = 0.4  à about one in two haloes observed to host radio-AGN (a lot!!) If we assume every halo with Mhalo>Mmin hosts a black hole that at some point  becomes radio-active we derive life-time of radio phase t=1 Gyr    t>>a few x10 Myr for radio-bright phase (Blundell & Rawlings 1999) à      Radio active phase is recurrent phenomenon  DEPENDENCE OF ENVIRONMENTAL PROPERTIES ON AGN-GALAXY PHYSICS (218 radio-AGN z<1.2 on COSMOS field. Environments from Darvish+2017) More massive radio-AGN prefer  denser environments  (not only mass-segregation effect.  Ask me!) Most radio-powerful -  P>~1024.6 W/Hz - AGN  prefer denser environments  (cf Peacock & Nicholson clustering results) CONCLUSIONS  1)  Radio-emitting AGN are hosted by very massive galaxies at all z 2) Most of them are in the process of forming stars at very high rates especially      in the past.     Deepest FIR surveys show that ~100% of z>~1 radio-AGN are associated to      SF events à 		3) Hosted by DM halos of masses >1013.5 Msun  (groups-to-clusters of galaxies)    Radio-AGN environmental properties do not depend on radio luminosity     (at least up to P~1024.5-25 W/Hz) and do not evolve with cosmic epoch  4) Stellar content relatively small <M*>/MHALO<10-2.7 	5) From comparison of densities 1 out of 2 massive halos host of radio-AGN        à τ~ 1Gyr à Radio-active phase recurrent phenomenon 	6) Dependence of environmental properties on stellar content/AGN emission at       different λ/radio luminosity (only for very bright sources)     Connection between sub-pc up to Mpc behaviours? 

NEUROSURGERY ENTHUSIASTIC WOMEN SOCIETY

https://openaccess.inaf.it/bitstream/20.500.12386/31503/1/Magliocchetti-AGN13_talk.pdf

Hosts and environments of radio-active AGN

Abstract

Similar works

Full text

Available Versions

ZENODO

FigShare

OA@INAF - Istituto Nazionale di Astrofisica

NEUROSURGERY ENTHUSIASTIC WOMEN SOCIETY