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One of the best example are Jorstad et al. with BL Lac, GASP large database of radio-optical flux data on BL Lac (other example NRAO 530/PKS 1730-13), emission lines blazar PKS 1510-08,  3C 454.3, 3C 279 (optical magnitude more bright after the ejection of a huge bright superliminal superluminal radio componentcomponents)

Svetlana J.: 1. theoreticians have to pay attention to these behaviors. 2. what theoreticians want from  MW campaigns/observations? 3. there are needs to justifications in maintain VLBI monitor for example. 


Matt   1 SED (nu peak, synch/IC peaks, Compton dominance, SED dependence on optical class? jet kinetic power? other props?);    2 Luminosity functions (beamed vs umbeamedunbeamed, dependence on optical class) ;  3 Nature of unidentified sources (how many are the blazars? can we predict their SEDs at low energies based on Fermi SEDs?);  4. fundamental properties of blazars ? which are the most useful classifications ? (SED peaks, luminosity, frequency, jet Lorentz factor/Doppler factor,  BLR/no-BLR ?).


Benoit L.: BL Lac objects show some correlations i tyerms in terms of blazar sequence-like (biased) schemes but not the FSRQ NOFSRQs.  FSRQ are almost all low-energy peaked so the lack of correlation even if there is very broad luminosity range the range of peak frequencies is narrow.

Small number of misalined AGN (radiogalaxies) detcted detected by the LAT. THis This is a problem for population studies.


Benoit L: More ways to associate unassociated sources ? Please propose potential new further schemes.

Determine the distribution and range of nu-synch-peak for all blazars down to some limiting flux nu-peak*f-peak? How increase the numeber number of known ISP BL Lacs? Broadband blazar surveys ?  Create a way to release and publish and distribute the MW data where one is working ?


Investigators should not be shy about making their data public as fast as possible during the "Fermi Era." Many papers have not used the full array of multifrequency data available, largely because proprietary data has not been forthcoming. AGNs, especially blazars, are an extremely complex and difficult problem in astrophysics, so forget about "solving" the big issues with your own data exclusively. Pooling all of the data gives theorists and modelers the best possible chance of understanding the many interconnections (and lack of connections) observed between wavebands. Observers should work hard to get their data in a readily accessible form as quickly as possible. Fermi has given the research community an incredible opportunity in cracking the puzzle of accretion and outflow associated with super-massive black holes. It would be disturbing not to maximize the support for this mission at as many wavelengths as possible. Of course, like any science program, the complexities may turn out to be just too great, but if we can't make headway during Fermi's mission, what would be the point of continuing long-standing, proprietary blazar monitoring programs after this mission ends. My apologies for not being able to attend this extremely important workshop and the equally important Fermi Symposium. These events unfortunately coincide with an observing run to support Fermi. The Steward Observatory blazar monitoring program stands ready to carefully consider and adopt changes in observing strategy and/or data products made available in response to any recommendations adopted at this workshop. One last point is that I would like to see us develop a central site where all data at all bands obtained during the Fermi mission can be accessed to go along with the final Fermi data archive. Is there any interest within the multifrequency community and at NASA in hosting such a central data repository? It would be a static archive and only contain data obtained while Fermi was observing.
Hi, The Fermi Guest Investigator Program offers joint observation time on a variety of observatories from radio to TeV through arrangements with NRAO, Arecibo, NOAO, INTEGRAL and VERITAS. The observing time available through these opportunities has generally been undersubscribed, in some cases extremely so. In particular, the bulk of the Fermi community may not be even be aware of two of these that were just recently implemented, Arecibo and INTEGRAL, judging from the dearth of requests in Cycle 7 and 8. We strongly encourage you, whether you reside in the US or abroad, to consider proposals for observation programs making use of these resources. Refer to the FSSC web pages for additional details. – Chris.

Stefano C:-- a) Possible idea for a Memorandum of Understanding with e-ROSITA ? This will be soon finally a sensitive all-sky high-energy instrument simultaneous to Fermi LAT for joint high-energy X-ray-gamma-ray survey astronomy and time domain astronomy. -- b) Fermi with additional more 10 years of prolonged mission can be of interest from particle physics side: increase statiatic statistics and limits/detection of DM and new-physics signals + multimessenger astroparticle physics with cross correlations among the next neutrino, gravitational wave and ultra-high energy cosmic ray data coming in the next decade. Without Fermi the multi-messenger science cannot develop and grow well. Remarks for the physics community side. -- c) Without Fermi the sciencew science possible with CTA cannot develop and grow well. Remarks for the physics community side.


Main goals of time-series (variability) analysis:
(1) identifying nature and gain physical understanding of the phenomenon/object producing the observed time series;
(2) forecasting (predicting future behavior and future values of the time series quantity).

What we can learn from short timescales (<1 day) of variability that can be pserberved observed by the LAT for very bright flares.

Search for breaks in the PDS (relation with physics, SMBH mass like for X-rays in Seyferts?).

Can the LAT allows systematic multiwavelength variability studies measuring the PDS-SED-plane (i.e. timescale-energy plane)?.

Broad-band MW studies: cross-correlation and time lags. MW SED modeling. Gamma-ray-synchrotron amplitude ratio studies, orphan flares, physics of the gamma-ray emission in AGN, identification of newly discovered gamma-ray sources, spectral index hysteresis, etc.

PHYSICS OF GAMMA-RAY EMITTING AGN (includes mainly blazars and radio galaxies)