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tic 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

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SLIDE 1

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

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SLIDE 2

Thr hree a appr pproa

  • ache

hes: s:

  • Ga

Gamma-r

  • ray obse

y observationa tional da l data ta fr from

  • m spa

space a and g nd ground obse

  • und observatorie

tories: s: e e.g .g. F . Ferm rmi, A i, AGILE, C GILE, Che herenk nkov T v Tele lesc scope

  • pes

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

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SLIDE 3

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

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SLIDE 4

Pla Planc nck (LFI+H (LFI+HFI) FI) Swift Swift (U (UVOT + XR T + XRT) T) Ferm rmi (L i (LAT) T)

A&A 2012, 541, 160

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SLIDE 5

VHE BAND

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SLIDE 6

factor 104 !

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SLIDE 7

PKS 2155-304 PKS 2155-304

https https:/ ://tools tools.a .asdc sdc.a .asi.it si.it/SED SED

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SLIDE 8

PKS 2155-304 PKS 2155-304

https https:/ ://tools tools.a .asdc sdc.a .asi.it si.it/SED SED

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SLIDE 9

The he 1 100 Me MeV-1

  • 100 Ge

GeV sk sky y se seen b n by y Ferm rmi i

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SLIDE 10
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SLIDE 11

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

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SLIDE 12
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SLIDE 13
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SLIDE 14
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SLIDE 15

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

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SLIDE 16
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SLIDE 17
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SLIDE 18

Monte Monte C Carlo Sim lo Simula ulations tions

  • f
  • f b

bla laza zars sur s surveys s

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SLIDE 19

19

MNRAS, 2012, 420, 2899 Monte Carlo survey simula1ons

Occam’s razor approach

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SLIDE 20

20

MNRAS, 2012, 420, 2899 Monte Carlo survey simula1ons

Occam’s razor approach

LBLs/LSPs

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SLIDE 21

21

MNRAS, 2012, 420, 2899 Monte Carlo survey simula1ons

Occam’s razor approach

LBLs/LSPs HBLs/HSPs

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SLIDE 22
  • Properties of high flux density radio- and X-ray-selected

blazar samples are reproduced: ü BL Lac & FSRQ fractions ü evolutionary properties (<V /Vm>) ü redshift distributions ü νpeak distributions ü fraction of BL Lacs without redshift determination

  • Results are stable to minor changes (e.g., evolution and LF

, <δ>)

22

Some results

  • P. Padovani − MG14, GN2
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SLIDE 23

23

Paper II

  • P. Padovani − MG14, GN2

γ-ray (Fermi) band

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SLIDE 24

24

Predic1ons for ϒ-ray emission

Radio luminosity + νpeak + Γ(0.1-100 GeV) from observed correlaYon between

νpeak and Γ(0.1-100 GeV)

No dependence of Lradio/Lγ on luminosity or redshi/

ϒ-ray luminosity

Giommi et al. 2013 MNRAS, 431, 1914

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SLIDE 25

Ackermann et al. 2012 (Fermi 2LAC clean sample)

25

Simplified view SimulaYon

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SLIDE 26

26

From GeV to VHE emission

Power law spectrum with a break at E= 200 GeV

Γ(100 GeV-10TeV) =

Γ(0.1-100 GeV) if E < 200 GeV Γ(0.1-100 GeV) + 0.5 if E > 200 GeV

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SLIDE 27

MNRAS 2015, 446L, 41 arXiv 1410.0497

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

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SLIDE 28

MNRAS 2015, 446L, 41 arXiv 1410.0497

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

2FHL N(>F (> 50 GeV) = 1.e-11)

2FHL N(> F(> 50 GeV) = 1.e-10)

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SLIDE 29

Padovani & Giommi 2014, MNRAS, 446,L41

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SLIDE 30

2015, MNRAS 450, 2404 arXiv:1504.01978

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SLIDE 31

2015, ApJL 800L, 27, arXiv:1501.050301

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SLIDE 32

New la w large sa sample ples of s of high-e high-ene nergy sync gy synchr hrotr

  • tron
  • n

pe peaked b d bla laza zars s

  • T
  • The

he m most pow

  • st powerful a

rful and e nd ene nergetic tic pa partic ticle le a accele lerator tors k s known nown and lik nd likely VH ly VHE e E emitte itters - s -

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SLIDE 33

νpeak > 1015Hz

VHE-TeV band

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

34

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+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

2WH WHSP SP ~1 ~1,6 ,690 obje

  • bjects

ts

Y-L. Chang, B. Arsioli, P. Giommi, P. Padovani, 2015 in preparaYon

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2FH 2FHL J0213.9-6949 L J0213.9-6949

−5 5 −5 5 arcmin arcmin

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SLIDE 37

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

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

<MRK421> <MRK421> re rescaled

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The he very high e

ry high ene nergy (VH gy (VHE) E) (E > 5 (E > 50 Ge GeV) )

sk sky y

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The he VH VHE E sk sky ( (IA IACTs) )

F > ~ 1 > ~ 10 mC.U .U.

+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

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SLIDE 41

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL) )

F > ~ 1 > ~ 10 mC.U .U. F > ~ 1 > ~ 10 mC.U .U. .

+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

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SLIDE 42

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL+2WH WHSP SP bright bright)

PR PRELIMIN ELIMINARY Y

+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

F > ~ 1 > ~ 10 mC.U .U F > ~ 1 > ~ 10 mC.U .U. F > ~ 1 > ~ 10 mC.U .U

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SLIDE 43

10 15 20 25 −16 −14 −12 −10 Log νf(ν)[erg cm−2s−1] Log frequency ν [Hz] 10 15 20 25 −16 −14 −12 −10 Log νf(ν)[erg cm−2s−1] Log frequency ν [Hz]

5BZB J1427+2348: an example of Blazar in 2FHL and in the 2WHSP sample

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10 15 20 25 −16 −14 −12 −10 Log νf(ν)[erg cm−2s−1] Log frequency ν [Hz] 10 15 20 25 −16 −14 −12 −10 Log νf(ν)[erg cm−2s−1] Log frequency ν [Hz]

5BZU J0221+3556: an example of Blazar in 2FHL but not in the 2WHSP sample

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SLIDE 45

10 15 20 25 −14 −12 Log νf(ν)[erg cm−2s−1] Log frequency ν [Hz] 10 15 20 25 −14 −12 Log νf(ν)[erg cm−2s−1] Log frequency ν [Hz]

5BZQ J0043+3426: an example of Blazar in 2FHL but not in the 2WHSP sample

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SLIDE 46

About bout 1 1/3 of

  • f the

the Ferm rmi 2 i 2FH FHL b L bla laza zars s ha have νpe

peak < 1

< 1015

15Hz

z (not not in 2 in 2WH WHSP) SP)

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SLIDE 47

The he VH VHE E sk sky ( (IA IACTs+ s+Ferm rmi 2 2FH FHL+2WH WHSP SP bright bright)

PR PRELIMIN ELIMINARY Y

+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

F > ~ 1 > ~ 10 mC.U .U F > ~ 1 > ~ 10 mC.U .U. F > ~ 1 > ~ 10 mC.U .U

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SLIDE 48

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

+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

F > ~ 1 > ~ 1 mC.U .U ~ C ~ CTA se sensitvity nsitvity

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SLIDE 49

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

+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

F > ~ 1 > ~ 1 mC.U .U ~ C ~ CTA se sensitvity nsitvity

+90o −90o −60o −30o +0o +30o +60o 180o 180o 0o 30o 60o 90o 120o 150o 210o 240o 270o 300o 330o

IBLs+LBLs from simulaYons

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SLIDE 50

−11.5 −11 −10.5 −10 −9.5 0.1 0.2 0.3 frequency Log(ebl−deabsorbedF>50GeV/fom)

2WH WHSP - F SP - Ferm rmi 2 i 2FH FHL L Com

  • mmon sour
  • n sources
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SLIDE 51

−11.5 −11 −10.5 −10 −9.5 0.1 0.2 0.3 frequency Log(ebl−deabsorbedF>50GeV/fom)

2WH WHSP - F SP - Ferm rmi 2 i 2FH FHL L Com

  • mmon sour
  • n sources

2WH WHSP sour SP sources s NOT in F T in Ferm rmi 2 i 2FH FHL

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

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

PR PRELIMIN ELIMINARY Y

Flux (E> 50GeV)ebl-deabsorbed = 2x1011*Sync_peak_flux*10(-0.154*log(νpeak)-8.03)

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

F a c t

  • r
  • f

2 f r

  • m

b e s t fi t PR PRELIMIN ELIMINARY Y

Flux (E> 50GeV)ebl-deabsorbed = 2x1011*Sync_peak_flux*10(-0.154*log(νpeak)-8.03)

PR PRELIMIN ELIMINARY Y

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SLIDE 55

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

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−12 −11.8 −11.6 −11.4 −11.2 −11 −10.8 20 40 60 80 Percentage Log (flux,(E>50 GeV)ph/cm2/s) Log(νpeak) > 15) 14 < Log(νpeak) < 15) Log(νpeak) < 14

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0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 0.1 0.2 0.3 0.4 Normalized fraction Observed redshift 1.e−12 < Fabsorbed( E> 30 Gev) < 3.e−12 3.e−12 < Fabsorbed( E> 30 Gev) < 1.e−11 Fabsorbed( E> 30 Gev) > 1.e−11

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The cumulaYve neutrino emission from BL Lacs

58

MNRAS, 2015, 452, 1877

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TheoreYcal modelling

59

Input:

  • electrons and

protons accelerated by some mechanism

  • injected isotropically

in the blob, constant rate

  • interaction with

magnetic field, production of secondaries

δ

R(cm) B(G)

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SLIDE 60

TheoreYcal modelling

July 16, 2015

Output: five stable particle populations

  • protons lose energy by:

ü synchrotron radiation, Bethe-Heitler (pe) pair production (p+γà e+ + e-), photopion interaction

  • electrons lose energy by:

ü synchrotron radiation, inverse Compton scattering

  • photons: gain and lose energy in various ways
  • neutrons: escape
  • neutrinos: escape

Interplay of the processes described by a set of time- dependent kinetic equations, solved by a numerical code.

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Neutrino spectra

61

EνF(Eν )∝YνγEν

1−s exp(−Eν / E0)Fγ(>10GeV)

E0 ≅ 17.5PeV (1+ z)2 ( δ 10)2(νsynch,peak 1016Hz )−1

Plus: γ-ray luminosity function, evolution, source class, etc.

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SLIDE 62

The big picture

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