E07-007 & E08-025 status report Maxime DEFURNE CEA-Saclay/Irfu/SPhN 1.
The γ-ray sky above 10 GeV seen by the Fermi satellite Grenoble, December 5, 2011 Jean Ballet (AIM,...
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Transcript of The γ-ray sky above 10 GeV seen by the Fermi satellite Grenoble, December 5, 2011 Jean Ballet (AIM,...
The γ-ray sky above 10 GeV seen by the Fermi satellite
Grenoble, December 5, 2011
Jean Ballet(AIM, CEA Saclay, France)
Above 1 GeV
2FGL: 1873 sources (ArXiv1108.1435)
Above 10 GeV
Many fewer events (2 years data)
Galactic diffuse emission not dominant, except in the Ridge
Fermi bubbles
Spatial resolution
PSF improves considerably with energy up to 10 GeV
R68 approximately constant at 0.2° above 10 GeV (in flight)
Not as good as simulation. Could still be improved.
Fermi sources > 100 GeV
Neronov et al 2010 (A&A 519, L6) have found 8 Fermi sources above 100 GeV, among which one was not a previously known TeV source
IC 310 in Perseus cluster: 3 events within 0.1° over 18 months
0.6°
1 – 10 GeV 10 – 100 GeV 100 – 300 GeV
Fermi sources > 10 GeV
> 300 sources over 2 years
Integral flux above 50 GeV estimated from power-law fit above 10 GeV
Even though AGN are variable, flux above 50 GeV is a good indicator of TeV detectability
Several Fermi-based TeV detections already
Paneque et al 2011,Fermi Symposium (2 years)
Fermi sources > 10 GeV
AG
N
SNR
PSR
PWN
LMXB
LBV
LMC
Paneque et al 2011,Fermi Symposium (2 years)
Preliminary
Mostly AGN
Tail of bright pulsars
Hard Galactic sources (SNR, PWN)
Individuals
Crab pulsar
Crab pulsar has been detected by MAGIC then VERITAS over 100 GeV
Clearly incompatible with exponential decay
Not obvious this can happen in older less energetic pulsars, but worth looking
McCann 2011, ICRC
Special case when the pulsar itself was not detected by Fermi
PWN normally much harder to detect on top of bright pulsar, but possible with phase selection
Pulsar Wind Nebulae
HESS J1825-137Grondin et al 2011, ApJ 738, 42
Fermi HESS
TS > 10 GeV + HESS contours
PWN will remain much easier to detect at TeV than GeV energies
Main help from Fermi in pulsar itself for interpretation (power input)
Brightest TeV SNR
Very faint, hard Fermi source in a complicated region of the Galactic plane, not detected below 5 GeV
Extended, compatible with HESS image
Clearly below the extrapolation of hadronic models, in line with leptonic models
Does not mean that protons are absent, but that density is low (as indicated by absence of thermal X-rays).
Supernova remnants RX J1713.7-3946
Abdo et al 2011, ApJ 734, 28
Fermi HESS
Hadronic
Leptonicmodel
1 GeV 10 TeV
Older SNR, between 3 and 30 kyr
Extended, emission where molecular clouds interact with the SNR, does not follow radio contours
Break frequency at ~ 3 GeV, corresponding to 20 GeV on proton spectrum.
Probably reflects the maximum energy reached by freshly accelerated particles
Clearly hadronic, but soft (Γ = 2.9 at TeV)
Old SNRs: IC 443
Abdo et al 2010, ApJ 712, 459
Albert et al 2007, ApJ 664, L87Acciari et al 2009, ApJ 698, L133
FermiTeV
1 GeV 1 TeV
Very large diversity in SNR spectra, depending on age (shock speed) and surroundings (density)
Global emission very slowly variable: no need for coincidence
GeV and TeV observations are very complementary
FSRQsBL Lacsother AGNs
B. Lott at Fermi meets Jansky 2011 Abdo, A. A. et al., accepted by ApJ, arXiv:1108.1420
886 high-confidence AGN
Nearly flux-limited sample in terms of energy flux over full band
Follows nicely blazar sequence
395 BL Lacs in 2LAC (291 in 1LAC)
Longer exposure time favors hard sources
100 MeV to 100 GeV
AGN – 2LAC
AGN: GeV - TeV
connection
Abdo et al. 2009, ApJ 707, 1310
Fermi spectra of known TeV AGN
Fermi: average flux
Comparison difficult due to intrinsic variability
Fermi is not well suited to MW studies of correlated variability
Compare spectral index rather than flux
39/45 TeV AGNs are in the 2LAC (34 in clean sample)
26 AGN are well fitted with simple power law in the LAT band
17 HSP, 2 ISP, 2LSP, 5 unknown
Deficit of distant sources with small values of ΔΓ
EBL: softening of the VHE spectrum dependent on z
AGN: GeV - TeV connection
B. Lott at Fermi meets Jansky 2011 Updated from Abdo et al. 2009, ApJ 707, 1310
When variability is detected, large relative variations
Fermi can characterize variability on long time scales, but short time scales not reachable for most sources
AGN: variability
1FGL: Abdo et al 2010, ApJS 188, 405
TeV instruments can characterize short term (but not long term) variability
GeV and TeV observations are very complementary for statistical studies
• Automated search for flaring sources on 6 hour, 1 day and 1 week timescales.– LAT scientists perform follow-up
analyses, produce ATels, and propose ToOs
• >100 Astronomers telegrams – Discovery of new gamma-ray blazars– Flares from known gamma-ray blazars
Flaring sources
Fermi is an excellent all-sky monitor
Detects flaring sources at low energy, but TeV behavior can be guessed from average spectrum
This one is very soft, no good for TeV
• Consistent with Band function from 10 keV to 10 GeV• No evidence for rolloff or γγ absorption Γ ≥ 900• No evidence for Compton component
Alpha = -1.02 ± 0.02Beta = -2.21 ± 0.03Epeak = 1170 ± 142 keV
GRB 080916CAbdo et al 2009,Science 323, 1688
Gamma-ray Bursts
Fermi has shown that GeV emission can extend up to 10 minutes in some GRBs
Hard sources limited by source count rate
Detection threshold improves faster than 1 / √t
P7Source_V6
Rocking angle 50°
|Latitude| > 10°
E-2.5E-1.5
Soft sourceslimited by:
- Knowledge of diffuse background (5% precision)
- Source density (extrapolated from measured logN logS)
Power-law detection threshold
• Spatial resolution 0.2° limiting in Galactic plane
• Detects 100s of sources above 10 GeV
• All-sky survey: reservoir of TeV targets
• Excellent GeV – TeV complementarity for SNRs
• PWN: can detect pulsar inside and measure power
• AGN: blazar sequence, variability over long time scales
• GRBs await detection at TeV energies. Need to be fast.
• Good prospects for hard sources with increasing exposure
Fermi at high energy
It costs NASA money to operate Fermi
5-year operations are guaranteed (up to mid 2013)
Good prospects to extend it for two more years, hopefully five
But not indefinitely, and no other GeV instrument in sight