Blazars @ -ray and other frequencies P. Giommi Agenzia Spaziale Italiana

Blazars @ -ray and other frequencies

P. Giommi Agenzia Spaziale Italiana

3 luglio 2007 Astrofisica Gamma dallo Spazio

AGILE e GLAST

AGN : Two main categories 1. Dominated by accretion - disk

emission - AP-AGN2. Dominated by Non-Thermal

radiation - jet emission - NT-AGN

Blazars: NT-AGN viewed at a small angle

w.r.t. jet axisRadio Galaxies:NT-AGN viewed at a large angle

w.r.t. jet axisBroad-line radio galaxies (e.g.

3c120) :A combination of AP-AGN and “mis-directed” NT-AGN

Blazars and the AGN paradigm


AGILE e GLAST

3C 279 : a Low energy peaked Blazar (LBL)


AGILE e GLAST

MKN 421 : a High energy peaked BL Lac (HBL)


AGILE e GLAST


AGILE e GLAST

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AGILE e GLAST

GLA

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Courtesy of P. Padovani


AGILE e GLAST

The SED of 3C454.3 and the Swift-BAT lightcurve in May-June 2005.

( Giommi et al. 2006, A&A, 456, 911)

The giant flare of 3C454.3 in spring 2005


AGILE e GLAST

A multi-frequency catalog of all known blazars

Catalog of confirmed literature blazars. Compiled in support to AGILE and GLAST missions

Massaro et al. 2007. Currently covers

0 < R.A. < 16 hrs : 1510 objects

> 2000 objects when complete (~ end 2007)


AGILE e GLAST

•194 FSRQs•38 BL Lacs•30 Radio galaxies•15 Steep sp. QSO•2 starburst galaxies•2 planetary nebule

•41 unidentified

323 bright sources

The large majority of bright WMAP foreground sources are blazars or radio galaxies

WMAP CMB fluctuation map

Blazars @ -wave frequencies the 3-year WMAP data

Bright foreground source catalog

Planck will be in a vey similar situation to that of GLAST - LAT(thousands of deteced blazars + contribution to unresolved flux).


AGILE e GLAST

CMB spectrum contaminationGiommi & Colafrancesco 2004 A&A 414,7, Giommi et al. 2006 A&A 445, 843


AGILE e GLAST

All microwave selected blazars are X-ray sources.

2007 A&A, 468, 571


AGILE e GLAST

A complete, -wave flux limitedsample of blazars

Based on WMAP 3-year catalogAll sources with F_41 GHz > 1 Jy

166 objects altogether 112 confirmed FSRQ22 Confirmed BL Lacs6 confirmed blazars, not clear if FSRQs or BL Lacs13 radio galaxies7 still optically unidentified (all with blazar-like SED)

Cleaned for source confusion


AGILE e GLAST


Preliminary results

Best fit slope -1.67 LogN-LogSAll blazars


AGILE e GLAST


Preliminary results

Cosmological evolution

FSRQs

<V/Vm> = 0.65 +/- 0.027BL Lacs

<V/Vm> = 0.54 +/- 0.062

M=0.3,=0.7 cosmology


AGILE e GLAST


Preliminary results

Luminosity functionFSRQs


AGILE e GLAST

Swift XRT serendipitous sources in GRBs pointigs :

the “perfect” serendipitous survey ~1 blazar/field expected with radio flux > 10 mJy!


AGILE e GLAST

209 deep (4x104-6x105 seconds) GRB exposures analyzed

~15,500 sources detected with positional uncertainty of 4-6 arscecs.

143 fields are at |bII| > 20 : ~11,500 sources

242 radio/X-ray matches (blazar candidates)

Swift XRT serendipitous survey

in GRB deep fields status as of end of April 2007


AGILE e GLAST


AGILE e GLAST


AGILE e GLAST

GLAST bandpass

Blazar contribution to the extragalactic

X and -ray background

€

I = S ⋅dN

dS⋅dS

S min

S max

∫


AGILE e GLAST


AGILE e GLAST

Max EGRET

Min EGRET


AGILE e GLAST

Dark matter-blazar angular power spectrum Ando Komatsu Narumoto & Totani 2007 Astro-ph/0612467, Colafrancesco & Giommi 2007, in preparation.

Blazars

Dark matter

GLAST expected signal

XRT data

BeppoSAX

High energy peaked BL Lacs (HBL) Tramacere et al. 2007, A&A 467, 501

SED of MRK 421 in 2005: large changes in luminosity and peak energy.

SED of 1H1100 – 230 observed on 30 June (blue) and 13 July 2005 (red). BeppoSAX 1997 and 1998 data are shown as open symbols.

UVOT data

High energy peaked BL Lacs (HBL)

SED of 1ES 1959+650 (19 April 2005)

SED of 1ES 1553+113 observed on 20 April (red), 6 Octobe (blue), and 8 October 2005 (green)


AGILE e GLAST

May 1999

MKN421 in a bright state: the BeppoSAX observation of May 2000Massaro, Perri, Giommi, Nesci, 2004 A&A


AGILE e GLAST

Log parabolic photon spectra can be explainedas due to Synchrotron radiation from a log-parabolic

particle distribution (Massaro et al. 2004a A&A 413, 489, 2004b, A&A 422,103)

SSC from a log parabolic electron distribution(Massaro et al. 2005, in press)


AGILE e GLAST


AGILE e GLAST

Massaro et al. 2006 A&A 448,861.


AGILE e GLAST

Giommi et al. 2007A&A 468, 97ROXA J081009.9+384757.0 is a z = 3.95

Blazar with HBL-like radio/X-ray SED

fx/fr ~ 5x10-11 erg/cm2/s/Jy

Recent Swift observations showed that the

X-ray luminosity of the QSO is larger

than 1047 erg/s.

The SED is consistent with two possibilities• New type of blazar

• Very high power HBL

High-power HBLs ?

See also IGR J2251+2218, Bassani et al. 2007, submitted

INTEGRAL discovered z=3.668 blazar with fx/fr ~ 2x1010 erg/cm2/s/Jy


AGILE e GLAST

High-power HBLs ! The case of BZB J1456+5048 (Z=0.479)

Rosat luminosity ~ 5x1046 erg/s

RosatSDSS data

NVSS

SDSS optical spectrum


AGILE e GLAST

High-power HBLs ! The case of BZB J1456+5048. Swift data.

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Documents

Blazars @ -ray and other frequencies P. Giommi Agenzia Spaziale Italiana