High-Energy Astrophysics with AGILE. Moriond 2009. AGILE. AGILE challenge…. only ~100 kg of Payload only ~100 W of PL absorbed power only 350 kg of satellite… Small Mission budget and resources. The AGILE Payload.
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combines for the first time agamma-ray imager (30 MeV- 30 GeV)with a hard X-ray imager (18-60 keV)with large FOVs (1-2.5 sr) and optimal angular resolution
HARD X-RAY IMAGER (SUPER-AGILE)
~9150 orbits, January 30, 2009.
Healthy Scientific Instrument
AGILE Cycle-2 on going
Nominal scientific performance of all subsystems
The AGILE gamma-ray exposure (E > 100 MeV)
more than 1 yr. exposure: July 2007 – 15 Sept. 2008
average flux above 100 MeV
In about 9 months of scientific life, AGILE reached EGRET exposure level in the Vela region.
(Pellizzoni et al. Ap.J. in press)
Method: simultaneous radio coverage allows us to perform proper phasing accounting for timing noise in the folding process.
We fit radio timing residuals with polynomial harmonic functions in addition to standard ephemeris parameters (pulsars frequency and its derivatives).
This improves the phasing precision and resolution (especially with >6 months long AGILE data spans) properly accounting for timing noise and then matching the *actual* shape of the pulsar light-curve in gamma-rays.
0.7 ms bins
E > 1 GeV
E > 100 MeV
30 - 100 MeV
E > 1 GeV
E > 100 MeV
30 - 100 MeV
100 - 1500 MeV
Halpern et al., 2008
EROT= 2.2x1036 erg/s
P = 3 ms
d = 4.9 kpc
A new variable millisecond gamma-ray pulsar in a globular cluster
Gamma-ray model based on (ASDC)CO maps
Gamma-ray intensity map
TeV source (MAGIC,VERITAS)
Very difficult to react in such a short time
3EG 1835+5918 443
The Next Geminga
even more difficult than the original one
In g rays 5 times fainter than Geminga
In X-rays 10 times fainter than Geminga
In the optical 20 times fainter than Geminga
No radio detection, no X-ray pulsation
LSI +61°303 443
GRID Galactic anticenter observation
15 GRBs localized by SuperAGILE since July 2007 => ~1 GRB/month;
The uncertainty on the localization is 3 arcmin and the minimum detected fluence is ~5 10-7 erg cm-2;
11 follow-ups by Swift/XRT and the X-ray afterglow was always found;
About 1 GRB/week detected by MCAL and 1 – 2 GRBs/month detected by SuperAGILE (outside FoV) and provided to IPN for triangulation;
One firm detection in gamma rays (GRB 080514B, Giuliani et al., 2008, A&A) and two less significant detections (GRB 080721 and GRB 081001);
GRID field of view
SA field of view
Up to June 2008
The most off-axis:
In the period July '07 – August '08: 64 GRBs detected (~1 GRB / week)
10 localized by SWIFT
8 localized by IPN (many more expected)
1 localized by SuperAGILE (other 4 SuperAGILE localizations without MCAL detection)
out of GRID FOV
AGILE first gamma-ray detection of a GRB: 443 GRB 080514B (Giuliani et al., A&A 2008)
SuperAGILE – Mars Odyssey annulus
GRB 080514B has been localized jointly by SuperAGILE and IPN.
Follow-up by Swift provided the afterglow in X-rays.
Many telescopes participated in the observation of the optical afterglow yielding the redshift
trigger date and time
temporal bin: 100 ms! time scale: < 5 ms