# Presentation: 713996

## Multi-wavelength AGN spectra and modeling  Paolo GiommiASI

## Stars+Galaxies (black body)

- AP-AGN (accretion onto SMBH)

- Radio Galaxies
- non-thermal emission

## AGN Types

**AGN Types**

## Blazars

**Blazars**

**AGN **
**Highly variable at all frequencies **
**Highly polarized**
**Radio core dominance**
**Superluminal speeds**

**Observed at a small angle to the jet and therefore rare AGN : 5-8% of all AGN**
**(but only at optical or X-ray frequencies!)**
**Blazars are the dominant population of extragalactic point sources at**

-  **Gamma-ray**
** ****TeV**
** ****Microwave frequencies**

## Normally the electromagnetic emission from blazars is assumed to be due to the Synchrotron-Self Compton mechanism (SSC) or SSC+External Component of a population of electrons in a jet of material that is moving at relativistic speed at a small angle with respect to the observer.

## Slide 6

## Swift/AGILE ToO observations of S5 0716+714 (Oct-Nov 2007)

- Giommi et al. 2008, A&A in press, arXiv:0806.1855

## Swift observations of 3C454.3during the giant flare of May 2005Giommi et al. 2006, A&A 456, 911

## TeV dectected BL LacsTramacere et al. 2006

- TeV dectected BL LacsTramacere et al. 2006

- 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

## TeV dectected BL Lacs

- 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)

## MKN421 in a bright state: 

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

## Log parabolic photon spectra can be explained as 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)

- (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)

## Slide 13

## Slide 14

## Spectral curvature observed around the Synchrotron peak is due to intrinsic curvature of emitting particle distribution
SSC of a particle distribution distributed as a Log-Parabola implies intrinsic curvature around Inverse Compton peak leaving little room for curvature resulting from EBL absorption 
Absorption due to EBL could be significantly lower than previously thought
Supported also by 
Aharonian et al. 2005 A&A 437, 395 
    Cut off energy in TeV spectrum of MKN421 (3.1TeV) lower than that of MKN501 (6.2 TeV), but redshift is very similar 
Aharonian et al. 2005 astro/ph 0508073
     HESS detection of the “high redshift” Blazars: 
     H2356-309 (z=0.165) and 1ES1101-232

- SSC of a particle distribution distributed as a Log-Parabola implies intrinsic curvature around Inverse Compton peak leaving little room for curvature resulting from EBL absorption
- Absorption due to EBL could be significantly lower than previously thought
- Supported also by
- Aharonian et al. 2005 A&A 437, 395
-     Cut off energy in TeV spectrum of MKN421 (3.1TeV) lower than that of MKN501 (6.2 TeV), but redshift is very similar
- Aharonian et al. 2005 astro/ph 0508073
-      HESS detection of the “high redshift” Blazars:
-      H2356-309 (z=0.165) and 1ES1101-232

## Slide 16

## Swift observation of MKN421 in 2006Tramacere et al. 2008 in preparation

## WMAP bright foreground 

**source catalog**** **

**140 FSRQs**
**23 BL Lacs**
**13 Radio galaxies**
**5 Steep Spectrum QSOs**
**2 starburst galaxies**
**2 planetary nebule**
**17 unidentified**
**6 without radio counterpart**
**  ****(probably spurious) **

**208 bright sources, of which**

**The vast majority of bright WMAP **
**foreground sources are Blazars**

**WMAP CMB fluctuation map**

## Slide 19

## Slide 20

## Boomerang 90 GHz CMB MAP

**Boomerang 90 GHz CMB MAP**
**De Bernardis et al. 2000**

## Slide 22

## Slide 23

## WMAP SEDs

## The Blazar LogN-LogS 

## Giommi & Colafrancesco 2003

## Slide 27

## 2007 A&A, 468, 571 

- All microwave selected blazars are X-ray sources.

- 2007 A&A, 468, 571

## From wave flux to X-rays and vice-versa

- f94GHz = f1keV • 106.41 x**>**** **

- f94GHz = 10 0.086.41 • f94GHz
- f94GHz ~ 3 • f94GHz

- f94GHz = 106.85 • f1keV

**Microwave fluxes can be estimated from X-ray flux**
**to within a factor ******** 3**

- f94GHz = 7.1 • 106 f1keV

- Effect of  3 variability

**LBL ****Blazar contribution to soft CXB: 4%, total (LBL+HBL 12%)**

## From -wave to X-rays

## Hard-Xray/Soft Gamma-Ray Cosmic Background

## Contribution to the X and -ray backgrounds

## Radio — -ray flux ratio & duty cycle

| Blazar Name |  | f-source/<background>
(background=-0.994) |
| --- | --- | --- |
| BZQ J0204+1514 | -0.892 | 14.5 |
| BZU J0210-5101 | -0.887 | 16.6 |
| BZB  J0339-0146 | -0.902 | 11.2 |
| BZQ J0423-0120 | -0.907 | 9.7 |
| BZQ J0455-4615 | -0.913 | 8.3 |
| BZQ J0457-2324 | -0.908 | 9.6 |
| BZU J0522-3627  | -0.926 | 6.0 |
| BZB J0538-4405 | -0.892 | 14.4 |
| BZQ J1256-0547 (3C 279) | -0.870 | 25.5 |

- Define a slope/trend:

| Duty cycle
(%) |
| --- |
| 6.9 |
| 6.0 |
| 8.9 |
| 10.3 |
| 12.0 |
| 10.4 |
| 16.7 |
| 6.9 |
| 3.9 |

## Slide 34

## Slide 35

## A ~10 mJy Blazar