TRANSNATIONAL ACCESS ACTIVITIES. Discussion on access to observatories Purpose :
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Discussion on access to observatories
Implementation of a Virtual Observatory with a collection of Cosmic Rays and High-Energy Gamma Rays data archives and software tools to form a scientific research environment in which multi-messenger astroparticle research programs can be conducted.
INFN & University of Roma Tor Vergata
19-20 February, 2007
High galactic latitudes (background Fb=2 10-5g cm-2 s-1 sr -1 (100 MeV/E)1.1). Cerenkov telescopes sensitivities (Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations. Large field of view detectors sensitivities (AGILE, GLAST, Milagro, ARGO) are for 1 year of observation.
The Roma Computing Center in Rome “Tor Vergata” will have the task to support the storage, the management and the utilization of the PAMELA Data Archiveand AGILE and GLAST Data ArchiveMirrors
Total 689 760 €
Access to and exchange of data
• A ( web-based) database of astro-particle observations and the exchange of inter-disciplinary data
• Computer modelling and simulations
•Correlate observations of space experiments (AGILE, GLAST) and ground observations
( H.E.S.S., MAGIC, ARGO).
Multiwavelength (MW) studies are intimately related to essentially all the astrophysical topics of gamma-ray astrophysics. All of the gamma ray observations will require observational programs at other wavelengths to extract their full value.
We envision three types of multiwavelength study:
identification of sources in known classes, such as blazars and pulsars,
ii) discovery of new sources classes,
iii) intensive, MW explorations of the brightest and most variable sources that will allow deep study of the source physics.
after 18 months :
Whole Earth Blazar Telescope [WEBT]
European Network for the Investigation of Galactic Nuclei through Multifrequency Analysis [ENIGMA] (http://www.lsw.uni heidelberg.de/users/swagner/enigma.html).
and space and ground gamma-ray observation
40 * double 3.2 GHz processor computers, 50 TByte storage system and 20 TB Disks.
<-- no more
PAMELA launched June 2006
AGILE launch end of March 2007
GLAST launch November 2007
After the initial on-orbit checkout, verification, and calibrations,
the first year of science operations will be an all-sky survey.
–all GBM data released
–LAT data on flaring sources, transients, and “sources of interest”
will be released, with caveats (see following slide)
–first-year LAT individual photon candidate events initially used for
detailed instrument characterization, refinement of the alignment,
and key projects (source catalog, diffuse background models, etc.)
needed by the community. Individual photon data released at the
end of year one. Subsequent photon data released immediately
–burst alerts and repoints for bright bursts
–extraordinary ToO’s supported
–workshops for guest observers on science tools and mission
characteristics for proposal preparation
•Observing plan in subsequent years driven by guest observer
proposal selections by peer review - default is sky survey mode.
Data released through the science support center (GSSC).
red: 0.1-0.4 GeV
green: 0.4-1.6 GeV
blue: >1.6 GeV
> 9000 sources are foreseen
First GLAST Symposium Feb. 2007
AGILE data will be available through a Guest Observers Program (GOP) that will be open to the international astrophysical community.
GOP data will be allocated through the DATA Allocation Committee (ADAC) by means of yearly AO.
• insertion in the data base of HESS MAGIC PAMELA and ARGO published data for cross-correlation with AGILE and GLAST data
• organize from now Data Policy for CTA