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We are organizing a multi-frequency monitoring of the TeV blazar Mrk421. Such campaign will start on December 8th 2009 and will last till December 2010.
The main goal of the campaign is to study the flux and spectral evolution of the broad-band emission, from radio to multi-TeV, of Mrk421.
The most important part of the campaign will be between Mid-December 2009 to Mid-June 2010; this is the time interval with good visibility for optical/TeV instruments. The goal for this time interval is to sample DAILY the peaks of the 2 bumps in the SED of Mrk421 (optical/X-ray and GeV/TeV). We have already allocated resources to do that at various energy ranges with various insrtruments (GRT,KVA,RXTE,MAGIC). I am currently trying to involve many other instruments. The current (very preliminary) observing schedule can be found here. This schedule will be updated during the following days with new instrument observations.
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The Fermi/AGN group is organizing a long multi-frequency monitoring on the object Mrk421. This campaign will start Mrk421,starting on December 8th 2009 and will last lasting 1 year. Specially critical are the frequencies energies around the peaks of the Synchrotron (~keV) and Inverse Compton (10-100 ~100 GeV) bumps. Swift observations are important to provide information from energies in the range 0.2-10 keV (which complements the observations from RXTE/PCA above 3 keV) , as well as information at the Ultraviolet UV frequencies (which are not affected by the host galaxy emission). Note that observations at UV frequencies can only be provided by Swift. Both X-rays and UV frequencies are very valuable for the correct modeling of the Synchrotron bump, and hence Swift observations will play a key role in the understanding of the physical processes occurring in this blazar.
The source is bright at both X-rays and UV frequencies, and hence 1 ks observation is long enough to have very long observations are sufficient for significant detections with both XRT and UVOT instruments. We request Swift 1ks long observations every 2 days starting from December 8th and finishing on March 31st 2010. This is 58 ks in total. We submitted a Swift Cycle-6 proposal that (in case of being approved) could be used for the observations after March 31st. Those Swift observations will be combined with the already scheduled optical,X-ray and TeV observations, as well as with Fermi/LAT, which operates in survey mode and hence is "constantly" observing Mrk421.
The current schedule of the multi-frequency observations from this campaign can be found at the following URL: https://confluence.slac.stanford.edu/display/GLAMCOG/Campaign+on+Mrk421+%28December+2009+to+December+2010%29
The scientific return of the Swift data will be maximized if the observations are taken close in time to the (almost simultaneous) optical, RXTE and IACT observations. Yet we want to stress that these observations are requested within the constraints of the primary Swift observing program. We are aware of the very tight Swift observing schedule, and thus we only ask for a "best effort" from the Swift team.