TeV Observations of blazars and constraints on their redshift: a detailed study of PG 1553+113 and PKS 1424+240 with MAGIC
TeV Observations of blazars and constraints on their redshift
a detailed study of PG 1553+113 and PKS 1424+240 with MAGIC
Scuola di Dottorato di Ricerca in FisicaCiclo XXIIIDirettore della Scuola: Prof. Attilio StellaSupervisore: Prof. Mos MariottiCorrelatore: Dott. Fabrizio Tavecchio
Dottoranda: Elisa Prandini
Padova, March 16th 2011
OutlineIntroduction: VHE gamma ray astrophysics The Physics case: gamma rays from Active Galactic NucleiMAGIC Observations5 years of PG 1553+113 dataThe source PKS 1424+240Constraints on blazars distancesLimits on the redshiftsA new empirical methodConclusions and Outlook
1The Physics Case: VHE g-rays2Very High Energy g-rays: E > 100 GeV [TeV regime]The Physics Case: VHE g-raysPropagate from cosmological distances:From their interactions cosmology
Ideal messengers of non thermal processes in the UniverseNeutrality
2
Very High Energy g-rays: E > 100 GeV [TeV regime]The VHE gamma-ray sky
3
The VHE gamma-ray sky: Extragalactic ComponentAll but two sources are Active Galactic Nuclei!4Active Galactic Nuclei: the most powerful accelerators
Supermassive black holes (109 solar masses)Are probably at the center of every galaxyIn some cases (radio loud AGNs) there are two narrow jets of particlesThe emitted spectrum is a superposition of several components5Active Galactic Nuclei: the most powerful accelerators Supermassive black holes (109 solar masses)Are probably at the center of every galaxyIn some cases (radio loud AGNs) there are two narrow jets of particlesThe emitted spectrum is a superposition of several components
5The observed radiation depends on the viewing angle Radio galaxiesBlazars FSRQBL Lac Objects
Radio Loud AGNs: Unified Scheme6 Radio galaxiesBlazars FSRQBL Lac Objects
The observed radiation depends on the viewing angleRadio Loud AGNs: Unified Scheme6The blazars Spectral Energy Distributionlog(E)nFneV keV MeV GeV TeVSimplified SEDnon thermal and covers the entire e.m. spectrum beaming effectsTwo bumps structure: Synchrotron emission High energy emissionLeptonic models (Inverse Compton)Hadronic models (p0 decay)
711The blazars SED: Mkn 421 a real example
- Clear two bump structure- High variability8The study of VHE gamma rays from blazars: why?A new unexplored regime! Characterize the emitting regionDiscriminate the emission modelsUp to z~0.5: cosmology!
log(E)nFneV keV MeV GeV TeVSimplified SED9The study of VHE gamma rays from blazars: why?log(E)nFneV keV MeV GeV TeVSimplified SED9HOW?A new unexplored regime! Characterize the emitting regionDiscriminate the emission modelsUp to z~0.5: cosmology!
Detection technique: Imaging Atmospheric Cherenkov Telescopes~ 1oCherenkov cone~ 120 m~ 10 kmVHE gamma rayAtmospheric shower (electromagnetic)
Earth atmosphere10Detection technique: Imaging Atmospheric Cherenkov Telescopes~ 1oCherenkov cone~ 120 m~ 10 km
VHE gamma rayAtmospheric shower (electromagnetic)
Earth atmosphere10Background
ImagesSignal[Gamma-like]
1117IACTs in the world
MAGICH.E.S.S.VERITAS
12The MAGIC Telescopes
SIGNAL TRANSPORTIPEIPEIPECENETACQUISITION SYSTEMMIRRORS
STRUCTURE CAMERA13
The MAGIC TelescopesEnergy threshold 60 GeVEnergy Resolution ~20%FOV 3.5oAngular Resolution ~0.1oSensitivity (5 s in 50 hours) ~1% Crab Nebula flux (> 100 GeV)
MAGIC I (2004)MAGIC II (2009)14OutlineIntroduction: VHE gamma ray astrophysics The Physics case: gamma rays from Active Galactic NucleiMAGIC Observations of AGNs5 years of PG 1553+113 dataThe source PKS 1424+240Constraints on blazars distancesLimits on the redshiftsA new empirical methodConclusions and Outlook
15The blazarsPG 1553+113 & PKS 1424+240 Is a well known TeV emitterObserved by MAGIC since 2005My analysis: from 2007 to 2009 (only M1)Is a new detected TeV emitterObserved by MAGIC since 2006, detected in 2009My analysis: 2009 (M1) and 2010 (stereo) data analysis Both sources have unknown/uncertain distance (redshift)16The blazarsPG 1553+113 & PKS 1424+240 Is a well known TeV emitterObserved by MAGIC since 2005My analysis: from 2007 to 2009 (only M1)Is a new detected TeV emitterObserved by MAGIC since 2006, detected in 2009My analysis: 2009 (M1) and 2010 (stereo) data analysis Both sources have unknown/uncertain distance (redshift)16The blazarsPG 1553+113 & PKS 1424+240Both sources have uncertain/unknown distance (redshift)Is a new detected TeV emitterObserved by MAGIC since 2006, detected in 2009My analysis: 2009 (M1) and 2010 (stereo) data analysis Is a well known TeV emitterObserved by MAGIC since 2005My analysis: from 2007 to 2009 (only M1)16z > 0.09 [VLT no lines, Sbarufatti et al. 2006a]z > 0.78 [HST, Sbarufatti et al. 2006b]z > 0.25 [HST, new method for gal. magnitude, Treves et al. 2007]0.4 < z < 0.58 [ISM-IGM lines, Danforth et al. 2010]z < 0.58 [TeV, Mazin & Goebel 2007, E.P. et al. 2009]
Largely uncertain:z > 0.06 [PG, Falomo & Scarpa 1995]z > 0.67 [HST, Sbarufatti et al. 2005]PG 1553+113 PKS 1424+240The Distance17
Falomo & Scarpa 1995
Treves et al. 2007PG 1553+113: data analysis and resultsSignal SearchSpectral AnalysisTime AnalysisMultiwavelength View of the SourceSpectral Energy Distribution (SED)
18PG 1553+113: data analysis and results200720082009A clear signal every year
2007 (11.5 hrs): 5.8 s2008 (8.7 hrs): 8.1 s2009 (8.5 hrs): 4.2 s Signal Search
18The MAGIC CollaborationSubmitted to ApJPG 1553+113: data analysis and resultsSignal SearchSpectral AnalysissDifferential energy spectrum
dN/dE = F0 (E/E0)-G YearGF (> 150 GeV)[Crab %]20074.1 0.34 % 1%20084.3 0.311% 1%20093.4 0.55% 1% (Crab Nebula G~2.5)19The MAGIC CollaborationSubmitted to ApJPG 1553+113: data analysis and resultsSignal SearchSpectral AnalysisTime AnalysisOne of the best followed TeV sourcesYearly variations (4%- 11% Crab flux) No clear intra-year variations20The MAGIC CollaborationSubmitted to ApJMultiwavelength PG 1553+11321The MAGIC CollaborationSubmitted to ApJPG 1553+113: data analysis and resultsSignal SearchSpectral AnalysisTime AnalysisMultiwavelength View of the SourceSpectral Energy Distribution (SED)
22Spectral Energy Distribution
Model Parameters
B = 0.5 G R ~1016 cm- Lr= 6 x 1044 erg/s
Assumption: z=0.4All the results are in agreement with the leptonic model!23The MAGIC CollaborationSubmitted to ApJSpectral Energy Distribution
Model Parameters
B = 0.5 G R ~1016 cm- Lr= 6 x 1044 erg/s
Assumption: z=0.4All the results are in agreement with the leptonic model!The MAGIC CollaborationSubmitted to ApJ23Signal SearchSpectral AnalysisTime AnalysisSpectral Energy Distribution (SED)
PKS 1424+240: data analysis and results2420092010 (stereoscopic data)Signal Search
PKS 1424+240: data analysis and results- 2009 (13 hrs): 4.2 s DISCOVERY of the source at TeV (together with VERITAS)! 2010 (16.6 hrs): 5.75 s past MAGIC observations: no signal--ATel #2098--24Signal SearchSpectral Analysis
PKS 1424+240: data analysis and resultsYearGF (> 150 GeV)[Crab %]20094.0 1.36.2 % 2.0%20103.5 0.81.2% 0.5%25Individual years specraMean spectrumThe MAGIC CollaborationPaper in preparationSignal SearchSpectral AnalysisTime Analysis
PKS 1424+240: data analysis and resultsResults: Monthly variations in 2009 Year variations
the source is highly variable (typical of BL Lacs)26The MAGIC CollaborationPaper in preparationSignal SearchSpectral AnalysisTime AnalysisSpectral Energy Distribution (SED)
PKS 1424+240: data analysis and resultsdistance of the source?
27OutlineIntroduction: VHE gamma ray astrophysics The Physics case: gamma rays from Active Galactic NucleiMAGIC Observations of AGNs5 years of PG 1553+113 dataThe source PKS 1424+240Constraints on blazars distancesLimits on the redshiftsA new empirical methodConclusions and Outlook
28
xxxVHE photons absorption by the Extragalactic Background LightVHE photon + diffuse light electron-positron pairs productionVHEEBL e+e-29Absorption:
dF/dEobs= (dF/dEem) e-t 40
EBL SEDVHE photon + diffuse light electron-positron pairs productionVHE photons absorption by the Extragalactic Background Light29Hauser and Dwek (2001)VHEEBL e+e-41VHE photon + diffuse light electron-positron pairs productionLarge uncertainties!VHE photons absorption by the Extragalactic Background Light29Dominguez et al. (2011)VHEEBL e+e-42
z = 0.003z = 0.01z = 0.03z = 0.1z = 0.3z = 0.5z = 1g-g opacityOur range of observations30Absorption:
dF/dEobs= (dF/dEem) e-t EBL ModelFranceschini et al. (2008)
z = 0.003z = 0.01z = 0.03z = 0.1z = 0.3z = 1Strong suppression
z = 0.530g-g opacityAbsorption:
dF/dEobs= (dF/dEem) e-t EBL ModelFranceschini et al. (2008)EBL absorption effect31
EBL model:Franceschini et al. (2008)The effect of EBL on blazars spectraThe absorption is related to the distance of the source
EBL: the EMITTED spectrum is deformed
32log(E)eV keV MeV GeV TeVSEDnFn46log(E)eV keV MeV GeV TeVSEDConstraints from the absorption EBL modelHypotheses on the intrinsic spectrumBlazar distance33nFnlog(E)eV keV MeV GeV TeVSEDConstraints from the absorption EBL modelHypotheses on the intrinsic spectrumBlazar distance33nFnMy workConstraints on blazars distances
Abdo et al. (2010)We propose to use the lower energy slope as limiting slope for the TeV de-absorbed spectrum in order to set a limit on the source distance
34EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., MNRAS 405,2010,L7649Constraints on blazars distances
Abdo et al. (2010)Below 100 GeV: Fermi/LAT measure (launched in 2008)
We propose to use the lower energy slope as limiting slope for the TeV de-absorbed spectrum in order to set a limit on the source distance
34EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., MNRAS 405,2010,L7650z*: an upper limit on the distanceOnce assumed an EBL model:
z* : GTeV(deab) = GGeV34EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., MNRAS 405,2010,L76
Abdo et al. (2010)
Results: upper limits on the distances of PG 1553+113 and PKS 1424+240In agreement with previously estimated limitsz* = 0.71 0.08z* = 0.45 0.15In agreement with previously estimated limits(VERITAS SPECTRUm)EP et al. accepted forPublication in POS 35A step further: from limits to estimatesHOW?
Test on known distances sources:Fermi TeV sources + TeV spectra from last generation of Cherenkov Telescopes16 sources with known redshift 2 sources of uncertain redshift (S5 0716+714 and 3C 66A)3653Results: z* VS ztrueAll the limits (z*) are above the bisector
Open points: uncertain redshiftThe slope measured at low energies (0.1 100 GeV) can be used as a LIMIT on the VHE slope for constraining the REDSHIFT of a source
bisectorz*37ztrue54Linear RelationIs there any relation among z* and ztrue?
Following previous works:
linear expression for the steepening of the observed TeV slope
z* is also related to the steepening: LINEAR RELATION
Linear fit:z* = A + B ztruez*38EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., MNRAS 405,2010,L76ztrue55Reconstructed redshiftWe can use the fit to estimate the redshift of a source (and not only to set a limit)zrec= (z* - A)/Bz*39ztrue56Test on known distances blazarsDz#Residuals distribution: Dz = (ztrue- zrec)
Sigma of the Gaussian fit: s = 0.054057Test on known distances blazarsResiduals distribution: Dz = (ztrue- zrec)
Sigma of the Gaussian fit: s = 0.05Dz# error on the reconstructed redshift4058Systematics EBL model Not simultaneous data Different instruments [i.e. energy threshold] Nature of the source
4159Conclusions: the distance of PKS 1424+24042EBL ModelFermi CatalogFermi slopez*zul (2 s)z recKneiske5.5 months1.85 0.050.50 0.160.820.24 0.04Franceschini5.5 months1.85 0.050.45 0.100.750.24 0.04Stecker5.5 months1.85 0.050.28 0.080.440.25 0.04Franceschini1 year1.83 0.030.45 0.150.750.26 0.05Dominguez1 year1.83 0.030.45 0.150.750.26 0.05EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., PoS, submitted60Conclusions: the distance of PKS 1424+240EBL ModelFermi CatalogFermi slopez*zul (2 s)z recKneiske5.5 months1.85 0.050.50 0.160.820.24 0.04Franceschini5.5 months1.85 0.050.45 0.100.750.24 0.04Stecker5.5 months1.85 0.050.28 0.080.440.25 0.04Franceschini1 year1.83 0.030.45 0.150.750.26 0.05Dominguez1 year1.83 0.030.45 0.150.750.26 0.05Almost independent from the EBL model considered!
Estimated Redshift:zrec = 0.26 0.05
42EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., PoS, submitted61Conclusions: the distance of PKS 1424+240This is the first estimate on this source distance!Estimated Redshift:zrec = 0.26 0.05
42EBL ModelFermi CatalogFermi slopez*zul (2 s)z recKneiske5.5 months1.85 0.050.50 0.160.820.24 0.04Franceschini5.5 months1.85 0.050.45 0.100.750.24 0.04Stecker5.5 months1.85 0.050.28 0.080.440.25 0.04Franceschini1 year1.83 0.030.45 0.150.750.26 0.05Dominguez1 year1.83 0.030.45 0.150.750.26 0.05EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., PoS, submitted62Conclusions: the distance of PKS 1424+240
Estimated Redshift:zrec = 0.26 0.05
42The MAGIC Collaboration paper, in preparationConclusions:the distance of PG 1553+113Estimated Redshift:
zrec = 0.43 0.05 in agreement with both upper and lower limits from other studies!EBL ModelFermi CatalogFermi slopez*zul (2 s)z recFranceschini1 year1.66 0.030.70 0.080.860.44 0.05Dominguez1 year1.66 0.030.71 0.080.870.43 0.05
43EP et al. in preparationFinal RemarksConclusionsDetailed analysis of two TeV blazarsDevelopment of a new phenomenological law relating GeV and TeV spectra to the blazars distancesEstimate of PG 1553+113 and PKS 1424+240 distancesOutlookPerform coordinated MWL campaigns Apply the law to other sources: many new TeV sources with unknown/uncertain redshift have been discoveredReduce the systematics44
Thank you!Bibliography
PART I: - PG 1553+113: MAGIC Collaboration (E.P. among corresponding authors) ApJ submitted- PKS 1424+240: MAGIC Collaboration (E.P. among corresponding authors) in preparation PART II: - E.P. et al., 31st ICRC (arXiv:0907.0157)- E.P. et al., MNRAS, 405, L76-L80 (2010) - E.P. et al., SciNeGHE 2010, accepted (arXiv:1101.4098)- E.P. et al., MCoS, accepted (arXiv:1101.5005)
Thank you!Backup slides68Radio Loud AGNs: energy budgetTypical Luminosity: L 1047 erg s-1 = 1040 W
Luminosity Components:
AccretionEjection
6Blazars SED: beaming effects Collimation (sinq=1/g)Time: Dtobs= Dtem/dEnergy: nobs = d nemLuminosity: Lobs = dp Lem
Rs < cDtvar / (1+z)70log(E)nFneV keV MeV GeV TeVSimplified SED= Doppler factor, ~10p ~ 470Cherenkov light spectrum
71Detection technique
72MAGIC CameraM1: 377 0.1o PMTs, 180 0.2o M2: 1039 0.1o PMTsQE ~ 30%73
MAGIC Trigger Multi-level:L0: thresholdL1: temporal and spatial coincidence (topology) L2: topological constraints to the images (flag mode)L3: stereo coincidence74MAGIC Sensitivity
75PG 1553+113: Optical-TeV correlation21Probability 76%SSC Model (PG 1553+113)
77Signal SearchSpectral AnalysisTemporal AnalysisMwl view
PKS 1424+240: data analysis and resultsResults:High state in 2009 also in optical and X-rays Not conclusive correlation studies: more coverage needed78Blazar observed spectrumIngredients
EBL modelBlazar emitted spectrumBlazar distanceMy work33EBL Measurements Direct PB: zodiacal dust and other foregrounds IndirectSource number countsOpacity to TeV photonsStatistical analysesStacking techniqueFluctuation technique80
Chary & Pope 2010EBL Models (following Dominguez et al 2010)Forward evolutionAssume determined cosmological conditions in the past as a starting point Backward evolutionEvolution of existing galaxies backward in timeInferred galaxy evolutionStarts from observed quantities (i.e. star formation rate)Observed Galaxy evolution Observed galaxy evolution81Absorption coefficient
82cosmologycross sectionEBL model
Opacity: models Comparison
83EBL absorption effect
84old criteriaMax slope -1.5 standard scenario (Aharonian et al. 2006)0.67 extreme model (Katarzynski et al. 2006)
No third peak at high energies
85
Spectral break Fermi TeV sources (from Abdo et al. 2009) + TeV spectra from last generation of Cherenkov Telescopes (MAGIC, VERITAS, H.E.S.S.)14 sources with well known redshift 2 sources of uncertain redshift (S5 0716+714 and 3C 66A)
Spectral breakHEVHE (observed)86EP, Bonnoli G.,Maraschi L.,Mariotti M. & Tavecchio F., MNRAS 405,2010,L7686Comparison between different EBL ModelsSimilar results with extreme EBL models:Low EBL: Kneinske & Dole 2010Mean EBL: Franceschini et al. 2008High EBL: Stecker et al. 2006
87Linear fit has a probability of ~60%87Results: z* VS ztrue in LINEAR SCALE88
88SourceztrueG (0.1-100 GeV)z*zrecMkn 4210.0301.81 0.020.07 0.020.02 0.05Mkn 5010.0341.85 0.040.07 0.02 0.02 0.051ES 2344+5140.0441.57 0.170.18 0.03 0.09 0.05Mkn 1800.0451.86 0.110.20 0.11 0.11 0.051ES 1959+6500.0472.09 0.050.07 0.030.02 0.05BL Lacertae0.0692.37 0.04 0.26 0.150.14 0.05PKS 2155-4890.0711.90 0.060.18 0.030.09 0.05W Comae0.1022.06 0.040.23 0.050.13 0.05PKS 2155-3040.1161.91 0.020.21 0.010.11 0.05RGB J0710+5910.1251.28 0.210.20 0.060.11 0.051ES 0806+5240.1382.09 0.100.22 0.150.12 0.05H 2356-3090.1652.10 0.170.16 0.070.08 0.051ES1218+3040.1821.70 0.080.20 0.080.11 0.051ES 1101-2320.1861.36 0.580.22 0.100.12 0.051ES 1011+4960.2121.93 0.040.60 0.180.36 0.05S5 0716+7140.310*2.15 0.030.22 0.100.12 0.05PG 1553+1130.4001.66 0.030.75 0.070.45 0.053C 66A0.444*1.92 0.020.38 0.050.22 0.05The Dataset89S5 0716+714
903C 66A
91The VHE g-ray sky: a new field
92Steepening of blazars spectra
93Stecker & Scully, 2010Cosmic Rays
Many open questions:Up to which energies?Antimatter content?Which is their origin? 22
Neutral Messangerapparent sourcedirection Charged particleCRsourceCosmic Rays originUHECR (E>1018eV)Cosmic RaysMany open questions:Up to which energies?Antimatter content?Which is their origin?
UHECRsNeutral Messangers:
Neutrinos Gamma-rays
2
] [_0 10 20 30 40 50 60 70 80 90
even
tsN
1000
2000
3000
4000
5000
6000
7000
8000
173.5 Non = 30098.0 169.4 Noff measured (Normalized) = 28698.0
242.5 Nex (ON - OFF measured) = 1400.0 Significance = 5.77, Nex/(Nbg*NormFactor) = 0.05
] [_0 10 20 30 40 50 60 70 80 90
even
tsN
0
200
400
600
800
1000
60.7 Non = 3688.0 32.4 Noff measured (Normalized) = 3146.0
68.8 Nex (ON - OFF measured) = 542.0 Significance = 8.09, Nex/(Nbg*NormFactor) = 0.17
] [_0 10 20 30 40 50 60 70 80 90
even
tsN
100
200
300
400
500
600
700
45.3 Non = 2048.0 24.7 Noff measured (Normalized) = 1835.3
51.6 Nex (ON - OFF measured) = 212.7 Significance = 4.20, Nex/(Nbg*NormFactor) = 0.12
Energy [GeV]210
]-1 T
eV-1
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dN/
dE [c
m
-1410
-1310
-1210
-1110
-1010
-910
-810
20072008 2009Crab Flux (Albert et al. 2008a)
2005 2006 2007 2008 2009
Time [MJD]53500 54000 54500 55000
]-1 s-2
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-11
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GeV)
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0 ]-1 s-2
[cm
Time [MJD]
2005 2006 2007 2008 2009
0
5
10VHE gamma-rays (MAGIC)
5
10
15 Optical (KVA+Tuorla)
2
4 X-rays (Swift/XRT)
53500 54000 54500 55000
0
0.02
0.04HE gamma-rays (Fermi/LAT)
2e0 0.05 0.1 0.15 0.2 0.25 0.3 0.35 0.4 0.45 0.5
even
tsN
0
200
400
600
800
1000
1200
1400
1600
1800 88.4 Non = 7812.0 49.6 Noff measured (Normalized) = 7394.0
101.4 Nex (ON - OFF measured) = 418.0 Significance = 4.16, Nex/(Nbg*NormFactor) = 0.06
2e0 0.1 0.2 0.3 0.4
even
tsN
0
200
400
600
800
1000
1200
1400
1600Time = 16.65 h
46.0 = 2203.0 off
= 2597; NonN = 394.0exN
mSignificance (Li&Ma) = 5.75
Energy [GeV]210
]-1 T
eV-1
s-2
dN/
dE [c
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-1210
-1110
-1010
-910 2009 (mono)2010 (stereo)
Energy [GeV]210
]-1 T
eV-1 s
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N/dE
[cm
-1210
-1110
-1010
-910 MAGIC 2009/10VERITAS 2009
Time [MJD]54880 54900 54920 54940 54960 54980 55000
]-1 s-2
[cm
-11
F (>
150
GeV
) x 1
0
1
2
3
4
5
6
7
MAGIC
VERITAS
Time [MJD]55270 55275 55280 55285 55290 55295 55300 55305
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[cm
-11
F (>
150
GeV
) x 1
0
0.5
1
1.5
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MAGIC 2009
VERITAS 2009
MAGIC 2010
0.1 1 10 100 1000 [m]
1
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100I [nWm2sr1]
this workFranceschini+ 08Gilmore+ 10Aharonian+ 06Mazin & Raue 07 - realisticMazin & Raue 07 - extremeAlbert+ 08Schlegel+ 98Hauser+ 98Finkbeiner+ 00Lagache+ 00Gardner+ 00Gorjian+ 00Cambresy+ 01Madau & Pozzetti 01Metcalfe+ 03Chary+ 04Fazio+ 04; Franceschini+ 08Xu+ 05Matsumoto+ 05Frayer+ 06Bernstein+ 07Levenson & Wright 08Matsuura+ 10Hopwood+ 10Bethermin+ 10Berta+ 10Keenan+ 10
truez-110
z*
-110
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1
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#
0
1
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F[Jy]0.008 0.01 0.012 0.014 0.016
]-1 s-2
F >
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-10
0
10
20
30
40
50
60
70
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-11F (
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ounts
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Time [MJD]
2006 2007 2008 2009 2010
0
2
4
6 -rays (MAGIC)aVHE
5
10 Optical (KVA + Tuorla)
53800 54000 54200 54400 54600 54800 55000 55200 55400
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0.1 1 10 100 1000 [m]
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100I [nWm2sr1]
this workFranceschini+ 08Gilmore+ 10Aharonian+ 06Mazin & Raue 07 - realisticMazin & Raue 07 - extremeAlbert+ 08Schlegel+ 98Hauser+ 98Finkbeiner+ 00Lagache+ 00Gardner+ 00Gorjian+ 00Cambresy+ 01Madau & Pozzetti 01Metcalfe+ 03Chary+ 04Fazio+ 04; Franceschini+ 08Xu+ 05Matsumoto+ 05Frayer+ 06Bernstein+ 07Levenson & Wright 08Matsuura+ 10Hopwood+ 10Bethermin+ 10Berta+ 10Keenan+ 10
