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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

HEAPnet meeting


19-20 February, 2007

Sensitivity of g-ray detectors

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.

Ta1 access to virtual data ta vida1
TA1: Access to “Virtual Data”(TA-ViDa1 )









TA1: Access to “Virtual Data” (TA-ViDa1 )

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

TA1: Access to “Virtual Data” (TA-ViDa1 )(cont.)

TA1: Access to “Virtual Data” (TA-ViDa1 )(cont.)

Total 689 760 €

Transnational access
Transnational Access

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

Expected impact
expected impact:

•Correlate observations of space experiments (AGILE, GLAST) and ground observations


  • Multi-wavelengths programs including x-rays, radio, IR, Optical ....

  • Develop observation methods for transient sources: alert systems and combination of space and ground observations .

  • Correlate observations with  and CR observations.

  • Evaluate potential discovery and physics outcome.

Description of work:

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 :

  • Definition of a Coordination between ground and space gamma ray observatories

  • ii) Definition of a Coordination between existing MW programs such as:

    Whole Earth Blazar Telescope [WEBT]



    European Network for the Investigation of Galactic Nuclei through Multifrequency Analysis [ENIGMA] (http://www.lsw.uni

    and space and ground gamma-ray observation

Advantages of a virtual observatory
Advantages of a Virtual Observatory

  • The advantages of a Virtual Observatory approach are several.

  • The data collected by each high energy experiment can be used multiple times by different teams and for different scientific purposes, thus increasing the overall efficiency.

  • The data are collected in a controlled and uniform fashion, ensuring long-term scientific utilization by different users.

  • The worldwide accessibility via web to the Virtual Observatory makes it a powerful scientific source that is available to any community, including those that are economically disfavoured.

  • A Virtual Observatory can also be used as a powerful and stimulating educational tool.

Roma computing center
Roma Computing Center experiments and other centers could be interested to join it.

  • The Roma Computing Center is located in the Department of Physics at the University of Rome “Tor Vergata”.

  • The infrastructure construction started in summer 2004 and is in its final setup phase thanks to INFN, ASI and MIUR funding. It will be fully operative by the end of 2005, in order to be ready for reception, distribution, analysis and storage of data of the PAMELA instrument. The expected PAMELA data flow is approximately 8 Gbyte/day.

  • In Feb.2006 AGILE satellite should be in orbit and starting to send data to the Center. The expected AGILE data flow is approximately 6Gbyte/day.

  • The Center is near the INFN Clean-Rooms facility, where the Pamela Flight Model has been integrated. Its location in the contest of the University of Rome “Tor Vergata” ( ensures a very stimulating scientific environment, from which visiting scientists may benefit.

  • An user room with different working stations which permits a collaborative work is already operative. The main hardware components of the Roma Computing Center are a 20 TByte storage system; a back-up system; 10 double 3.2 GHz processor computers.

  • The Center is connected to the main INFN computer center (CNAF, for any need of storage and CPU computer power .

  • CNAF is integrated in the European Data-Grid network

Paris data center
Paris Data Center experiments and other centers could be interested to join it.

  • The Paris Data Center is located at the APC (Astroparticle and Cosmology) Laboratory and is dedicated to multi-wavelength studies in a wide energy range starting from radio to very high energy gamma-rays. The current setup includes a double 3.2 GHz processor computer with TByte storage capacity at APC as an interface to the Center for Computing of In2p3 (CCPN/Lyon, through a fast connection. The H.E.S.S. Data processing and storage consumes about 7% of CCPN/Lyon total capacity which has about 1 TFlops of computing power (~200 3 GHz PCs) and 20+280 TB (disks + tapes).

Munich data center
Munich Data Center experiments and other centers could be interested to join it.

  • The Munich Data Center is located at the Max Planck Institute for Physics and it is mainly dedicated to the MAGIC data analysis. The current setup includes a

    40 * double 3.2 GHz processor computers, 50 TByte storage system and 20 TB Disks.

  • The Center will be integrated in the European Data-Grid network

Towards fp7
Towards FP7 experiments and other centers could be interested to join it.

  • TA weaknesses of FP6:

  • satellites not yet launched

  • only small part of HESS and MAGIC data goes to guest programs

<-- no more

PAMELA launched June 2006

AGILE launch end of March 2007

GLAST launch November 2007

Glast data policy
GLAST DATA POLICY experiments and other centers could be interested to join it.

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

after processing.

–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).


  • 271 sources



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 policy

AGILE Data Policy for GLAST.

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.

AGILE Data Policy (2) for GLAST.

  • Data rights for Targhet of Opportunity (TOO) sources belongs to the proposers thereof with participation of AGILE Team members who are essential for data processing.

  • Some items belong to the AGILE Team:

  • Diffuse Radiation,

  • Extragalactic background,

  • Unidentified transient sources

Pamela data policy
PAMELA Data Policy for GLAST.

  • The PAMELA scientific primary goals are the search for heavy nuclei and non baryonic particles outside the Standard Model, for the understanding of the formation and evolution of our Galaxy and the Universe and for the exploring of the cycles of matter and energy in the Universe.

  • Additional objectives of PAMELA are the study of galactic cosmic rays in the heliosphere, Solar flares, distribution and acceleration of solar cosmic rays (SCR's) in the internal heliosphere, magnetosphere and magnetic field of the Earth, stationary and disturbed fluxes of high energy particles in the Earth's magnetosphere and anomalous component of cosmic rays.

  • Alerts for transient events, Solar flares will be immediately available on-line, or through other appropriate data distribution means within the limits of the resources available

Only small part of hess and magic data goes to guest programs
--> only small part of HESS and MAGIC data goes to guest programs

  • Possible solution :

  • HESS, MAGIC, ARGO data not public but exchange between the experiments

    • 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

Roma international conference on astroparticle physics roma 20 22 june 2007
Roma International Conference on Astroparticle Physics programs Roma 20-22 June 2007