SLIDE 1
Optical band Radio/microwave band Infra red band UV band X-ray band Υ-ray band TeV band
Radio/microwave band The electromagnetic spectrum Infra red band - - PowerPoint PPT Presentation
Radio/microwave band The electromagnetic spectrum Infra red band - - PowerPoint PPT Presentation
The he mul ulti ti-wavele elength ngth mul ulti ti-tempor temporal al sk sky Radio/microwave band The electromagnetic spectrum Infra red band Optical band UV band X-ray band -ray band TeV band Radio/microwave band Infra red
SLIDE 2
SLIDE 3
Optical band Radio/microwave band Infra red band UV band X-ray band Υ-ray band TeV band
SLIDE 4
Courtesy of M. Tavani
SLIDE 5
Typical Multi-Wavelength emitters:
- Radio galaxies/Blazars
- Pulsars/Pulsar wind nebulae
(e.g. Crab)
- GRBs
SLIDE 6
Gamma Ray Bursts as multi-frequency emitters
GRBs were discovered in the 70's as gamma-ray sources, but only in the 90’s the precise positions obtained with the X-ray telescopes (e.g. BeppoSAX) enabled follow-up at optical, IR and radio wavelength, discovering the redshift and their host galaxies It is now possible to follow the time evolution of a GRB in a very wide energy range, and
- bserve new features as a supernova related with a GRB
Observations of GRB-SN 980425/1998bw
VERY LARGE ARRAY HUBBLE SPACE TELESCOPE KECK VERY LARGE TELESCOPE
SLIDE 7
Z=0.54 Eiso=2.8x1053 erg GRB 090618
Fermi RT2 Swift AGILE Konus-WIND SUZAKU Faulkes North Gemini North Herschel telescope Newton telescope
SLIDE 8
AGN : Two main categories
1. Dominated by (mostly) thermal emission from accretion disk - Radio quiet AGN (>~90 %) (normal QSO powered by accretion onto a SM black hole) 1. Dominated by Non-Thermal radiation – Jet dominated AGN (< 10%) When Θ < θblazar Blazar
As of today, about 3,150 blazars are known (Bzcat, edition 4.1, Massaro et al. 2012).
This number is increasing rapidly but it remains a small percentage
- f the over one million AGN known
Flesch, E. The Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012) http://quasars.org/milliquas.htm
SLIDE 9
9
The two blazar classes
May 24, 2012
- P. Padovani − Bologna High Energy
Meeting
BL Lac object Flat spectrum radio quasar
SLIDE 10
SLIDE 11
Fermi adattive bin 1GeV light-curve Courtesiy of B. Lott
Preliminary
Accretion onto SMBH
SLIDE 12
SLIDE 13
SLIDE 14
Fermi adattive bin 1GeV light-curve Courtesy of B. Lott
Preliminary
SLIDE 15
SLIDE 16
SLIDE 17
SLIDE 18
SLIDE 19
SLIDE 20
SLIDE 21
21
SLIDE 22
SLIDE 23
Fermi adattive bin 1GeV light-curve Courtesiy of B. Lott
Preliminary
SLIDE 24
SLIDE 25
SLIDE 26
- Large number of sources:
175 blazars observed by Swift when they were in the FOV of Planck: ~160 Swift ToOs
- Simultaneous Planck Swift Fermi + ground based telescopes
- Multi-selection approach. Four flux-limited samples.
Soft X-ray (RASS, sample) Hard X-ray (Swift-BAT sample) γ-ray (Fermi sample) Radio (100 brightest northern sources) Planck Collaboration 2011, A&A 563, A16 and Giommi et al. A&A 2012, 514, 160
Planck, Swift Fermi observations of Radio and high-energy selected blazars
SLIDE 27
3C 273 MKN 501
27
SLIDE 28
3C 279 LBL/LSP
SLIDE 29
3C 454.3 MKN 421 HBL/HSP
SLIDE 30
S5 0716+714 IBL/ISP www.asdc.asi.it
SLIDE 31
31
The distribution of synchrotron peak energies
SLIDE 32
Testing the simplest scenario:
homogeneous SSC
32
(Thomson regime)
SLIDE 33
33
SLIDE 34
34
Compton Dominance
SLIDE 35
35
The distribution of Compton Dominance
SLIDE 36
36
SLIDE 37
37
SLIDE 38
38
SLIDE 39
39
SLIDE 40
40
SLIDE 41
Most (radio selected) FSRQs have Compton Dominance ~ 1 (Log(CD) = 0)
41
SLIDE 42