dc.contributor.author |
Britto, R. J |
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dc.contributor.author |
Acharya, B. S |
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dc.contributor.author |
Anupama, G. C |
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dc.contributor.author |
Bhattacharjee, P |
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dc.contributor.author |
Chitnis, V. R |
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dc.contributor.author |
Cowsik, R |
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dc.contributor.author |
Dorji, N |
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dc.contributor.author |
Duhan, S. K |
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dc.contributor.author |
Gothe, K. S |
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dc.contributor.author |
Kamath, P. U |
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dc.contributor.author |
Mahesh, P. K |
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dc.contributor.author |
Manoharan, J |
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dc.contributor.author |
Nagesh, B. K |
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dc.contributor.author |
Parmar, N. K |
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dc.contributor.author |
Prabhu, T. P |
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dc.contributor.author |
Rao, S. K |
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dc.contributor.author |
Saha, L |
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dc.contributor.author |
Saleem, F |
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dc.contributor.author |
Saxena, A. K |
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dc.contributor.author |
Sharma, S. K |
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dc.contributor.author |
Shukla, A |
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dc.contributor.author |
Singh, B. B |
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dc.contributor.author |
Srinivasan, R |
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dc.contributor.author |
Srinivasulu, G |
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dc.contributor.author |
Sudersanan, P. V |
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dc.contributor.author |
Tsewang, D |
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dc.contributor.author |
Upadhya, S. S |
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dc.contributor.author |
Vishwanath, P. R |
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dc.date.accessioned |
2011-12-16T14:34:17Z |
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dc.date.available |
2011-12-16T14:34:17Z |
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dc.date.issued |
2011-12 |
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dc.identifier.citation |
SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem, R. Samadi and D. Valls-Gabaud, pp.535 - 538 |
en |
dc.identifier.uri |
http://hdl.handle.net/2248/5642 |
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dc.description.abstract |
The High Altitude GAmma-Ray (HAGAR) experiment is the highest altitude atmospheric Cherenkov sampling array, set up at 4300 m amsl in the Himalayas (Northern India). It constitutes 7 telescopes, each one with seven 90 cm-diameter mirrors, a field of view of 3 degrees, and was designed to reach a relatively low threshold (currently around 200 GeV) with quite a low total mirror area (31 m^2). In order to remove the strong isotropic background of charged cosmic rays, data are collected by tracking separately ON-source followed by OFF-source regions, or vice-versa. Typical observations period is about 30-40 min. ON-OFF data pairs are then selected according to quality parameters such as stability of the trigger rate and the comparison of average trigger rates between ON and OFF-source data sets. Signal extraction from point sources is done by performing analysis cuts on the count rate excess, rejecting off-axis events. Validation of method and systematics are evaluated through the analysis of fake sources (OFF-OFF pairs) located at similar declination as the observed point sources. Spurious signal, if any, would show up in this study. |
en |
dc.language.iso |
en |
en |
dc.publisher |
French Society of Astronomy and Astrophysics |
en |
dc.relation.uri |
http://sf2a.cesr.fr/2011/2011sf2a.conf..0535B.pdf |
en |
dc.rights |
© French Society of Astronomy and Astrophysics |
en |
dc.subject |
Gamma rays: atmospheric |
en |
dc.subject |
Cherenkov technique |
en |
dc.subject |
Methods: data analysis |
en |
dc.subject |
Telescopes: HAGAR |
en |
dc.title |
Data analysis method for the search of point sources of gamma rays with the HAGAR telescope array |
en |
dc.type |
Article |
en |