INAF - ISTITUTO DI RADIOASTRONOMIA I. Prandoni – Nov. 2007 ... · lim = 0.06 mJy; Area 2= 0.35...

Surveys & Surveys & ObsObs. Cosmology. Cosmology@ IRA@ IRA

[2004-2007][2004-2007]

INAF - ISTITUTO DI RADIOASTRONOMIA I. Prandoni – Nov. 2007

General Aim:Formation and cosmological evolution ofgalaxies, AGNs and Universe as a whole

(through CMB-related science)

IRA involved in many survey projectsin framework of large

international collaborations

•VVDS Vettolani, Bondi, Gregorini, Zanichelli

•zCOSMOS Zanichelli,Vettolani

•DPS Mignano, Prandoni

IRA Surveys: IRA Surveys: 2004-20072004-2007


•NEP Gioia

•ELAIS, LH Lari

•HELLAS2XMM Lari

X-raysROSATXMM

opt/NIRVLTHSTNTTCFHTSubaru

FIRISO

Spitzer

Radio• CMB-FG Surveys 5• Deep Fields 4PI-ship in radio surveys

ROSAT X-ray colorimage of NEP Region:442 sources with S0.5-

2 keV > 2·10–14

erg/cm2/s (deepestexsposure of RASS). Voges+, 2001

Redshift distributions in the VVDS fields

F10IAB<22.5

F14IAB<22.

5

F22IAB<22.5

F02Deep

IAB<24

•VVDS Vettolani, Bondi, Gregorini, Zanichelli

•zCOSMOS Zanichelli,Vettolani

•DPS Mignano, Prandoni

IRA Surveys: IRA Surveys: 2004-20072004-2007


•NEP Gioia

•ELAIS, LH Lari

•HELLAS2XMM Lari

X-raysROSATXMM

opt/NIRVLTHSTNTTCFHTSubaru

FIRISO

Spitzer

Radio• CMB-FG Surveys 5• Deep Fields 4PI-ship in radio surveys

ROSAT X-ray colorimage of NEP Region:442 sources with S0.5-

2 keV > 2·10–14

erg/cm2/s (deepestexsposure of RASS). Voges+, 2001

Redshift distributions in the VVDS fields

F10IAB<22.5

F14IAB<22.

5

F22IAB<22.5

F02Deep

IAB<24“Lari Method”: A Standardto clean transients (CRs,..)from FIR data (ISO, Spitzer)

NORTHERNNORTHERN CROSS SURVEYSSURVEYS

408 MHz B1: Braccesi+,1965 (E-W only) Slim = 1 Jy; Area = 0.41; sr

B2: Colla+,1970,72,73, Fanti+,1974 Slim = 0.2-0.25 Jy; Area = 1.7 sr

B3: Ficarra+,1985 Slim = 0.1 Jy; Area = 0.78 sr

EXTRAGALACTIC SKY SURVEYS down to 100-200 EXTRAGALACTIC SKY SURVEYS down to 100-200 mJymJyComplement of brighter Complement of brighter ““CambridgeCambridge”” surveys surveys

RFL extended to P<RFL extended to P<PPbreak break (Auriemma et al. 1977)


“Bologna” Surveys:

+ Mosaic technique+ Mosaic technique

ATCA:ATCA: 68x12h VLA:VLA: 30x12h 6 x 22m 6 x 22m bsbsmaxmax = 6 km = 6 km 27 x 25m 27 x 25m bsbsmaxmax = 30 km= 30 km


I - DEEP RADIO FIELDS @ IRAI - DEEP RADIO FIELDS @ IRA

GMRT:GMRT: 30h

30 x 45m bs30 x 45m bsmaxmax=25 km=25 km

+ Mosaic technique+ Mosaic technique

ATCA:ATCA: 68x12h VLA:VLA: 30x12h 6 x 22m 6 x 22m bsbsmaxmax = 6 km = 6 km 27 x 25m 27 x 25m bsbsmaxmax = 30 km= 30 km



GMRT:GMRT: 30h


ATESP5: Prandoni et al. 2006, Mignano et al. 2007a,b 5 GHz5 GHz Slim = 0.4 mJy; Area = 1 deg2

VVDS F02 Deep Field: Bondi et al. 2007 610 MHz610 MHz Slim = 0.2 mJy; Area = 1.0 deg2

Lockman Hole: de Ruiter et al. 1997 1.4 GHz1.4 GHz Slim = 0.12 mJy; Area = 0.35 deg2

Marano Field: Gruppioni et al. 1997 Slim = 0.2 mJy; Area = 0.36 deg2

ATESP: Prandoni et al. 2000a,b Slim = 0.47 mJy; Area = 25.9 deg2 2967 RSVLA-VVDS [F02 Deep Field]: Bondi et al. 2003 Slim = 0.08 mJy; Area = 1.0 deg2 1054 RSHDF-South: Huynh et al. 2005 Slim = 0.06 mJy; Area = 0.35 deg2

VLA-COSMOS: Schinnerer et al. 2007, Bondi et al. in prep. Slim = 0.05 mJy; Area = 2.0 deg2 3600 RS

+ + Mosaic techniqueMosaic technique

ATCA:ATCA: 68x12h VLA:VLA: 30x12h 6 x 22m 6 x 22m bsbsmaxmax = 6 km = 6 km 27 x 25m 27 x 25m bsbsmaxmax = 30 km = 30 km



GMRT:GMRT: 30h


ATESP5: Prandoni et al. 2006, Mignano et al. 2007a,b 5 GHz5 GHz Slim = 0.4 mJy; Area = 1 deg2

VVDS F02 Deep Field: Bondi et al. 2007 610 MHz610 MHz Slim = 0.2 mJy; Area = 1.0 deg2

Lockman Hole: de Ruiter et al. 1997 1.4 GHz1.4 GHz Slim = 0.12 mJy; Area = 0.35 deg2

Marano Field: Gruppioni et al. 1997 Slim = 0.2 mJy; Area = 0.36 deg2

ATESP: Prandoni et al. 2000a,b Slim = 0.47 mJy; Area = 25.9 deg2 2967 RSVLA-VVDS [F02 Deep Field]: Bondi et al. 2003 Slim = 0.08 mJy; Area = 1.0 deg2 1054 RSHDF-South: Huynh et al. 2005 Slim = 0.06 mJy; Area = 0.35 deg2

VLA-COSMOS: Schinnerer et al. 2007, Bondi et al. in prep. Slim = 0.05 mJy; Area = 2.0 deg2 3600 RS


I - 1.4 GHz RADIO COUNTSI - 1.4 GHz RADIO COUNTSEXCESS @ S<1 EXCESS @ S<1 mJymJy

EMERGENCE OFEMERGENCE OFNEW POPULATION(S)NEW POPULATION(S) Classical RG: ~ 99%Classical RG: ~ 99%

@ S > 60 @ S > 60 mJymJy

SF dominates at µJy fluxes

ETS important at sub-mJy/mJy fluxes

e.g. Richards et al. 99, Gruppioni etal. 99, Haarsma et al. 00, Prandoniet al. 01b, 02, Gruppioni et al. 03,Sullivan et al. 04, Ciliegi et al. 05,Fomalont et al. 06, Prandoni et al.06, Bondi et al. 07, Mignano et al.07b

IRA PapersIRA Papers

IRA, Bo

“Bologna” surveysSlim> 100 mJy

•• SFGsSFGs SF History (z>2)SF History (z>2) ((Dust-enshrouded objDust-enshrouded obj))


I - Scientific DriversI - Scientific Drivers

•• AGNsAGNs BH Accretion HistoryBH Accretion History ( (Type II AGNsType II AGNs)) low/high accr. rateslow/high accr. rates FRI vs. RQQ [QSO vs Radio mode]

RQ/RL dichotomyRQ/RL dichotomy

Ev. Of LLAGNs: Ev. Of LLAGNs: LLAGNs peak at lower z? [NB: LDDE recently found for opt/X-ray AGNs]

•• Connection between SFH & MBH accretionConnection between SFH & MBH accretion

LOFAR, eVLA, eMERLIN, SKA-Pathfinders, SKA

II II –– CMB Foreground Emission CMB Foreground EmissionSurveys @ IRASurveys @ IRA


- PGMS (2.3 GHz Parkes Galactic Meridian Survey) 5x90 deg2 polarized Galactic synchr. emission as CMB-FG Galactic Magnetism

- S-PASS (S-Band Polarization All Sky Survey) Large Project (2000h @ Parkes): whole Southern Sky

- Deep Survey of BOOMERang Region @ 43 GHz extragalactic point sources as FGs of CMB polarization (ATCA)

2.3 GHzlinear polarizedemission @ SGP(Carretti+,08)

[Carretti + IASF,Bo, OAC, ATNF, UCB]

Scientific Drivers:• CMB polarization• Cosmic inflation with next generation CMB space missions (B-POL, Inflation Probe, Planck)

Parkes [2500h]Effelsberg [100h]Medicina [1000h] ATCA [100h]

II II –– CMB Foreground Emission CMB Foreground EmissionSurveys @ IRASurveys @ IRA


- PGMS (2.3 GHz Parkes Galactic Meridian Survey) 5x90 deg2 polarized Galactic synchr. emission as CMB-FG Galactic Magnetism

- S-PASS (S-Band Polarization All Sky Survey) Large Project (2000h @ Parkes): whole Southern Sky

- Deep Survey of BOOMERang Region @ 43 GHz extragalactic point sources as FGs of CMB polarization (ATCA)

2.3 GHzlinear polarizedemission @ SGP(Carretti+,08)

[Carretti + IASF,Bo, OAC, ATNF, UCB]

Scientific Drivers:• CMB polarization• Cosmic inflation with next generation CMB space missions (B-POL, Inflation Probe, Planck)

Parkes [2500h]Effelsberg [100h]Medicina [1000h] ATCA [100h]

- All Northern Sky Survey @ 20 GHz with Medicina (Slim ~ 50 mJy) Carretti, Mack, Prandoni, Zanichelli + 2 PhD Students: S. Righini, R. Verma

extragalactic point sources as FGs of CMB study of flat/inverted spectrum RS (Blazars/HFP)

1st Antenna in the North with a 7-horn 20 GHzMultibeam (FOV= 2FOV= 2’’ x7 beams x7 beams )

It will complement the AT20G [all Southern sky survey to Slim~50 mJy]

- Followed by deeper 20 GHz survey with SRT-64m (FOV~50 (FOV~50”” x 7 beams) x 7 beams)

EXTRACTION OF COMPLETE SAMPLESEXTRACTION OF COMPLETE SAMPLES FOR FOLLOW-UP STATISTICAL STUDIES FOR FOLLOW-UP STATISTICAL STUDIES

B3-VLA B3-VLA RGs RGs [L. Gregorini, K-H Mack, M. Vigotti]

QZ4 QZ4 BAL-Quasars BAL-Quasars [K-H Mack, F. Montenegro-Montes, M. Vigotti]

KuhrKuhr 18.5 18.5 Blazars Blazars [I. Prandoni]

NEP/VLA NEP/VLA Cluster RS Cluster RS [M. Branchesi, I. Gioia, R. Fanti, C. Fanti]

VVDS-WIDE/FIRST VVDS-WIDE/FIRST mJy radio sources mJy radio sources [L. Gregorini, A. Zanichelli]

III - SURVEYS as DATABASESIII - SURVEYS as DATABASES


PI-shipPI-ship


Local clusters by Fanti et al.(1984) and Ledlow & Owen(1996)

Instruments used: 1) VLA - 24 hours (1.4 GHz) 2) CFHT - 10 hours

III - RLF of Distant X-ray selectedIII - RLF of Distant X-ray selectedCluster Radio GalaxiesCluster Radio Galaxies

NEP clusters (0.3<z<0.8)

XLocal clusters (z<0.1)

Evolution of RLF of cluster galaxies with redshift[both in amplitude and slope]

Branchesi et al. 2006, A&A 446, 97

Resources Resources [2004-2007][2004-2007]


L. Gregorini, C. Fanti, R. Fanti(UniBO), H. de Ruiter (OABo)

- Collaborations: INAF Institutes, Univ. (OABo, OAB, IASF, UniBO, ...) + Foreign Inst. & Univ. (ATNF, ESO, MPIA, NRAO, ...)- External Funds: Bilateral Agreements (CNR-CSIRO; INAF-IAC) EU Networks (e.g. ESTRELA, Radionet) PRIN (MIUR/INAF, Spain), ASI (SPOrt[<2006]; COFIS-2, ...)

M. Bondi, E. Carretti, I. Gioia, C.Lari, K.-H. Mack, P. Parma, I.Prandoni, T. Venturi, G. Vettolani,M. Vigotti, A. Zanichelli

F. Montenegro-Montes (Spain),S. Righini, R. Verma (India)

M. Branchesi, A. Mignano

IRA-Staff

Associates

Postdoc

PhD

114

2

3- Personnel:

- - Publications (refereed journals)Publications (refereed journals):: 85 since 2004 (in press not included)


SummarySummary IRA involved in many large international survey projects:

from X-ray to FIR + several radio surveys (PI-ship):

Aims cosmological statistical studies Formation & Ev. of galaxies, AGNs and Universe as a whole

Points of strength: Widely Recognized expertise in (radio) surveys Close collaborations with Italian & foreign Inst. & Univ. High publication rate

Critical issues: Insufficient funding for a regular fellowship program

Deep Fields [Radio/FIR/opt/X-ray] CMB-Foreground surveys

INAF - ISTITUTO DI RADIOASTRONOMIA I. Prandoni – Nov. 2007 ... · lim = 0.06 mJy; Area 2= 0.35...

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Transcript of INAF - ISTITUTO DI RADIOASTRONOMIA I. Prandoni – Nov. 2007 ... · lim = 0.06 mJy; Area 2= 0.35...