tic r The he e extr xtragala lactic ray sk y sky Thr hree - PowerPoint PPT Presentation

tic γ –r The he e extr xtragala lactic –ray sk y sky

Thr hree a appr pproa oache hes: s: • Ga Gamma-r -ray obse y observationa tional da l data ta from fr om spa space a and g nd ground obse ound observatorie tories: s: e.g e .g. F . Ferm rmi, A i, AGILE, C GILE, Che herenk nkov T v Tele lesc scope opes s • Monte Monte C Carlo sim lo simula ulations of tions of bla laza zar sur surveys s • New m w multi-fr ulti-freque quenc ncy se y sele lecte ted la d large sa sample ples of s of ϒ -r -ray/ y/VH VHE e E emitting b itting bla laza zars s

…b …but f ut fir irst: st: a f few slide w slides a s about b bout bla laza zars s

Ferm rmi (L i (LAT) T) Swift (U Swift (UVOT + XR T + XRT) T) Pla Planc nck (LFI+H (LFI+HFI) FI) A&A 2012, 541, 160

VHE BAND

factor 10 4 !

https https:/ ://tools tools.a .asdc sdc.a .asi.it si.it/SED SED PKS 2155-304 PKS 2155-304

https https:/ ://tools tools.a .asdc sdc.a .asi.it si.it/SED SED PKS 2155-304 PKS 2155-304

The he 1 100 Me MeV-1 -100 Ge GeV sk sky y seen b se n by y Ferm rmi i

Ferm rmi 3 i 3FGL FGL cata talog log: A : Ackerm rmann e nn et a t al. 2 l. 2015, , ApJ pJ 8 810, 1 , 14, a , arXiv:1 rXiv:1501.0 .06054 4 y years of s of P PASS 7 SS 7 da data ta: 3 : 3033 sour sources s

Ferm rmi 2 i 2FH FHL L The he F Ferm rmi-L i-LAT vie T view of w of the the Very H ry High Ene igh Energy Sk gy Sky y Ackermann et al. 2015, submiBed. arXiv:1508.04449

Monte Monte C Carlo Sim lo Simula ulations tions of of b bla laza zars sur s surveys s

MNRAS, 2012, 420, 2899 Occam’s razor approach Monte Carlo survey simula1ons 19

MNRAS, 2012, 420, 2899 Occam’s razor approach Monte Carlo survey simula1ons LBLs/LSPs 20

MNRAS, 2012, 420, 2899 Occam’s razor approach Monte Carlo survey simula1ons LBLs/LSPs HBLs/HSPs 21

Some results • Properties of high flux density radio- and X-ray-selected blazar samples are reproduced: ü BL Lac & FSRQ fractions ü evolutionary properties (<V /V m >) ü redshift distributions ü ν peak distributions ü fraction of BL Lacs without redshift determination • Results are stable to minor changes (e.g., evolution and LF , < δ >) P. Padovani − MG14, GN2 22

Paper II γ -ray ( Fermi ) band P. Padovani − MG14, GN2 23

Predic1ons for ϒ-ray emission Giommi et al. 2013 MNRAS, 431, 1914 Radio luminosity + ν peak + ϒ -ray luminosity Γ (0.1-100 GeV) from observed correlaYon between ν peak and Γ (0.1-100 GeV) No dependence of L radio /L γ on luminosity or redshi/ 24

Ackermann et al. 2012 (Fermi 2LAC clean sample) Simplified view SimulaYon 25

From GeV to VHE emission Power law spectrum with a break at E= 200 GeV Γ (0.1-100 GeV) if E < 200 GeV Γ (100 GeV-10TeV) = Γ (0.1-100 GeV) + 0.5 if E > 200 GeV 26

0.1 MNRAS 2015, 446L, 41 All blazars arXiv 1410.0497 BL Lacs 0.01 FSRQs Unabsorbed N(>S) [deg − 2 ] Absorbed 10 − 3 10 − 4 10 − 5 10 − 12 10 − 11 10 − 10 VHE gamma − ray flux (E>100GeV) [ph cm − 2 s − 1 ]

0.1 MNRAS 2015, 446L, 41 All blazars arXiv 1410.0497 BL Lacs 0.01 FSRQs 2FHL N(>F (> 50 GeV) = 1.e-11) Unabsorbed N(>S) [deg − 2 ] Absorbed 10 − 3 2FHL N(> F(> 50 GeV) = 1.e-10) 10 − 4 10 − 5 10 − 12 10 − 11 10 − 10 VHE gamma − ray flux (E>100GeV) [ph cm − 2 s − 1 ]

Padovani & Giommi 2014, MNRAS, 446,L41

2015, MNRAS 450, 2404 arXiv:1504.01978

2015, ApJL 800L, 27, arXiv:1501.050301

New la w large sa sample ples of s of high-e high-ene nergy sync gy synchr hrotr otron on pe peaked b d bla laza zars s -T -The he m most pow ost powerful a rful and e nd ene nergetic tic pa partic ticle le a accele lerator tors k s known nown s - and lik nd likely VH ly VHE e E emitte itters -

ν peak > 10 15 Hz VHE-TeV band

A&A 2015, A&A, 2015, 579, 34 DOI: 10.1051/0004-6361/201424148 34

2WH WHSP SP ~1 ~1,6 ,690 obje objects ts Y-L. Chang, B. Arsioli, P. Giommi, P. Padovani, 2015 in preparaYon +90 o +60 o +30 o +0 o 90 o 60 o 30 o 0 o 330 o 300 o 270 o 150 o 120 o 240 o 210 o 180 o 180 o − 30 o − 60 o − 90 o

2FH 2FHL J0213.9-6949 L J0213.9-6949 5 arcmin 0 − 5 − 5 0 5 arcmin

1RXS J 021359.9-695130 1RXS J 021359.9-695130

1RXS J 021359.9-695130 1RXS J 021359.9-695130 <MRK421> <MRK421> re rescaled

The he very high e ry high ene nergy (VH gy (VHE) E) (E > 5 (E > 50 Ge GeV) ) sk sky y

The he VH VHE E sk sky ( (IA IACTs) ) .U . F > ~ 1 > ~ 10 mC.U +90 o +60 o +30 o +0 o 90 o 60 o 30 o 0 o 330 o 300 o 270 o 150 o 120 o 240 o 210 o 180 o 180 o − 30 o − 60 o − 90 o

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL) ) .U . F > ~ 1 > ~ 10 mC.U F > ~ 1 > ~ 10 mC.U .U. . +90 o +60 o +30 o +0 o 90 o 60 o 30 o 0 o 330 o 300 o 270 o 150 o 120 o 240 o 210 o 180 o 180 o − 30 o − 60 o − 90 o

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL+2WH WHSP SP bright bright) .U . .U F > ~ 1 > ~ 10 mC.U F > ~ 1 > ~ 10 mC.U F > ~ 1 > ~ 10 mC.U .U PR PRELIMIN ELIMINARY Y +90 o +60 o +30 o +0 o 90 o 60 o 30 o 0 o 330 o 300 o 270 o 150 o 120 o 240 o 210 o 180 o 180 o − 30 o − 60 o − 90 o

5BZB J1427+2348: an example of Blazar in 2FHL and in the 2WHSP sample − 10 − 10 Log ν f( ν )[erg cm − 2 s − 1 ] Log ν f( ν )[erg cm − 2 s − 1 ] − 12 − 12 − 14 − 14 − 16 − 16 10 10 15 15 20 20 25 25 Log frequency ν [Hz] Log frequency ν [Hz]

5BZU J0221+3556: an example of Blazar in 2FHL but not in the 2WHSP sample − 10 − 10 Log ν f( ν )[erg cm − 2 s − 1 ] Log ν f( ν )[erg cm − 2 s − 1 ] − 12 − 12 − 14 − 14 − 16 − 16 10 10 15 15 20 20 25 25 Log frequency ν [Hz] Log frequency ν [Hz]

5BZQ J0043+3426: an example of Blazar in 2FHL but not in the 2WHSP sample − 12 − 12 Log ν f( ν )[erg cm − 2 s − 1 ] Log ν f( ν )[erg cm − 2 s − 1 ] − 14 − 14 10 10 15 15 20 20 25 25 Log frequency ν [Hz] Log frequency ν [Hz]

About bout 1 1/3 of of the the Ferm rmi 2 i 2FH FHL b L bla laza zars s ha have ν pe peak < 1 < 10 15 15 Hz z (not not in 2 in 2WH WHSP) SP)

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL+2WH WHSP SP bright bright) .U . .U F > ~ 1 > ~ 10 mC.U F > ~ 1 > ~ 10 mC.U F > ~ 1 > ~ 10 mC.U .U PR PRELIMIN ELIMINARY Y +90 o +60 o +30 o +0 o 90 o 60 o 30 o 0 o 330 o 300 o 270 o 150 o 120 o 240 o 210 o 180 o 180 o − 30 o − 60 o − 90 o

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL+2WH WHSP SP bright bright + faint int) ) PR PRELIMIN ELIMINARY Y F > ~ 1 > ~ 1 mC.U .U +90 o ~ CTA se ~ C sensitvity nsitvity +60 o +30 o +0 o 90 o 60 o 30 o 0 o 330 o 300 o 270 o 150 o 120 o 240 o 210 o 180 o 180 o − 30 o − 60 o − 90 o

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL+2WH WHSP SP bright bright + faint int) ) PR PRELIMIN ELIMINARY Y F > ~ 1 > ~ 1 mC.U .U +90 o +90 o ~ CTA se ~ C sensitvity nsitvity +60 o +60 o +30 o +30 o +0 o +0 o 90 o 90 o 60 o 60 o 30 o 30 o 0 o 0 o 330 o 330 o 300 o 300 o 270 o 270 o 150 o 150 o 120 o 120 o 240 o 240 o 210 o 210 o 180 o 180 o 180 o 180 o − 30 o − 30 o − 60 o − 60 o − 90 o − 90 o IBLs+LBLs from simulaYons

2WH WHSP - F SP - Ferm rmi 2 i 2FH FHL L 0.3 Com ommon sour on sources 0.2 frequency 0.1 0 − 11.5 − 11 − 10.5 − 10 − 9.5 Log(ebl − deabsorbedF >50GeV /fom)

2WH WHSP - F SP - Ferm rmi 2 i 2FH FHL L 2WH WHSP sour SP sources s 0.3 Com ommon sour on sources NOT in F T in Ferm rmi 2 i 2FH FHL 0.2 frequency 0.1 0 − 11.5 − 11 − 10.5 − 10 − 9.5 Log(ebl − deabsorbedF >50GeV /fom)

Log(ebl − deabsorbedF >50GeV /fom) − 11.5 − 11 − 10.5 − 10 15 15.5 16 16.5 Log( ν peak ) 17 17.5 18 18.5

Flux (E> 50GeV) ebl-deabsorbed = 2x10 11 * Sync_peak_flux * 10 (-0.154*log( ν peak)-8.03) PRELIMIN PR ELIMINARY Y − 10 Log(ebl − deabsorbedF >50GeV /fom) − 10.5 − 11 − 11.5 15 15.5 16 16.5 17 17.5 18 18.5 Log( ν peak )

Flux (E> 50GeV) ebl-deabsorbed = 2x10 11 * Sync_peak_flux * 10 (-0.154*log( ν peak)-8.03) PRELIMIN PR ELIMINARY Y − 10 Log(ebl − deabsorbedF >50GeV /fom) − 10.5 F a c t o r o f 2 f r o m b e s t fi t − 11 PRELIMIN PR ELIMINARY Y − 11.5 15 15.5 16 16.5 17 17.5 18 18.5 Log( ν peak )

VHE LogN − LogS 0.1 Fermi 2FHL Simplified view 2WHSP prediction 0.01 N(>S) [deg − 2 ] 10 − 3 10 − 4 10 − 5 10 − 12 10 − 11 10 − 10 10 − 9 VHE gamma − ray flux (> 50GeV) [ph cm − 2 s − 1 ]