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The GLAST-AGILE Support Program (GASP) of
the Whole Earth Blazar Telescope (WEBT)
Claudia M. Raiteri, M. Villata (INAF-OATo) on
behalf of the WEBT collaboration
WEBT
GASP
AGILE
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Mostly optical, but also radio and near-IR
observatories
The WEBT was born in 1997, in the CGRO era, as an
international consortium of astronomers devoted
to blazar studies.
The distribution in longitude allows 24 h/day
continuous monitoring
http//www.oato.inaf.it/blazars/webt/
Up to now, 24 campaigns have been carried out,
usually in conjunction with observations at high
energies.
More than 100 optical telescopes, 3 NIR, 8 radio,
and the Sub-millimeter Array provided the WEBT
with more than 50,000 observations in 20 bands.
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WEBT campaigns one (source) at a time
WEBT President (from 2000 Massimo Villata, OATo)
Observing proposal (anybody)
WEBT officers
The Campaign Manager takes care of campaign
coordination, publication of results, and sends
data to the
Campaign (from a few days to several months/years)
WEBT archive
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GASP all (sources) together now!
In 2007 the WEBT started the GLAST-AGILE Support
Program (GASP)
Selected WEBTers perform continuous monitoring of
28 ?-loud blazars in the optical, near-IR, and
radio bands Light curves are constructed almost
in real time by the WEBT President
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The first one S5 071671
The ?-ray flux variations follow the optical ones
by about 1 day
Villata et al. (2008, AA, 481, L79) Chen et al.
(2008, AA, 489, L37)
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The WEBT and GASP big efforts on 3C 454.3
On the new activity phase in 2007-2008 Raiteri
et al. (2008, AA, 485, L17) Raiteri et al.
(2008, AA, 491, 755) Vercellone et al. (2009,
ApJ, 690, 1018) Donnarumma et al. (in preparation)
On the big 2004-2005 optical outburst and delayed
radio outburst Villata et al. (2006, AA, 453,
817) Villata et al. (2007, AA, 464, L5)
AGILEFermi
AGILE
On the faint state in 2007-2008 and detection of
little and big blue bumps Raiteri et al. (2007,
AA, 473, 819)
On the new observing season
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Optical, millimetric and centimetric light curves
during the 2004-2008 WEBT campaigns
Orange s represent X-ray fluxes, correlated with
the optical ones
The solid line shows the prediction of the
Villata et al. (2006) model for the mm flux.
The big cm outburst is actually the
Doppler-enhanced counterpart of the minor optical
flare in fall 2005
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Spectral energy distribution of 3C 454.3 during
and after the historical outburst of 2005,
obtained from the WEBT campaigns, including
Chandra and XMM-Newton observations
Little blue bump (BLR)
Big blue bump (disc)
The H? broad emission line in some of the 16
spectra taken in Campo Imperatore during the
faint state
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3C 454.3 correlation between the AGILE ?-ray
fluxes and WEBT-GASP optical fluxes
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December 12, 2007 R- band brightness rise of
1.1 mag in 1.5 h, followed by a fall of 1.2 mag
in 1 h
Delay of the ?-ray flux variations with respect
to the optical ones of about 10 hours Monte Carlo
simulations (FR/RSS) ? ?0.5 ? 0.7 d
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The GASP optical light curve of PKS 1510-08
FermiAGILE
Pucella et al. (2008, AA, 491, L21)
DAmmando et al. (in preparation)
Pucella et al. (in preparation)
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AO 023516
WEBT first light
3C 279