Hide/Show Apps

Upper limits to the SN1006 multi-TeV gamma-ray flux from HESS observations

Download
2005-07-01
Aharonian, F
Akhperjanian, AG
Aye, KM
Bazer-Bachi, AR
Beilicke, M
Benbow, W
Berge, D
Berghaus, P
Bernlohr, K
Boisson, C
Bolz, O
Borgmeier, C
Breitling, F
Brown, AM
Gordo, JB
Chadwick, PM
Chounet, LM
Cornils, R
Costamante, L
Degrange, B
Djannati-Atai, A
Drury, LOC
Dubus, G
Ergin, Tülün
Espigat, P
Feinstein, F
Fleury, P
Fontaine, G
Funk, S
Gallant, YA
Giebels, B
Gillessen, S
Goret, P
Hadjichristidis, C
Hauser, M
Heinzelmann, G
Henri, G
Hermann, G
Hinton, JA
Hofmann, W
Holleran, M
Horns, D
de Jager, OC
Jung, I
Khelifi, B
Komin, N
Konopelko, A
Latham, IJ
Le Gallou, R
Lemiere, A
Lemoine, M
Leroy, N
Lohse, T
Marcowith, A
Masterson, C
McComb, TJL
de Naurois, M
Nolan, SJ
Noutsos, A
Orford, KJ
Osborne, JL
Ouchrif, M
Panter, M
Pelletier, G
Pita, S
Puhlhofer, G
Punch, M
Raubenheimer, BC
Raue, M
Raux, J
Rayner, SM
Redondo, I
Reimer, A
Reimer, O
Ripken, J
Rob, L
Rolland, L
Rowell, GP
Sahakian, V
Sauge, L
Schlenker, S
Schlickeiser, R
Schuster, C
Schwanke, U
Siewert, M
Sol, H
Steenkamp, R
Stegmann, C
Tavernet, JP
Theoret, CG
Tluczykont, M
van der Walt, DJ
Vasileiadis, G
Vincent, P
Visser, B
Volk, HJ
Wagner, SJ
Observations of the shell-type supernova remnant SN1006 have been carried out with the HESS system of Cherenkov telescopes during 2003 (18.2 h with two operating telescopes) and 2004 (6.3 h with all four telescopes). No evidence for TeV gamma-ray emission from any compact or extended region associated with the remnant is seen and resulting upper limits at the 99.9% confidence level are up to a factor 10 lower than previously-published fluxes from CANGAROO. For SN1006 at its current epoch of evolution we define limits for a number of important global parameters. Upper limits on the gamma-ray luminosity (for E = 0.26 to 10 TeV, distance d = 2 kpc) of L-gamma < 1.7 x 10(33) erg s(-1), and the total energy in corresponding accelerated protons, W-p < 1.6 x 10(50) erg are estimated ( for proton energies E-p similar to 1.5 to 60 TeV and assuming the lowest value n = 0.05 cm(-3) of the ambient target density discussed in literature). Extending this estimate to cover the range of proton energies observed in the cosmic ray spectrum up to the knee (we take here E-p similar to 1 GeV to 3 PeV, assuming a differential particle index -2) gives W-P < 6.3 x 10(50) erg. A lower limit on the post-shock magnetic field of B > 25 G results when considering the synchrotron/inverse-Compton framework for the observed X-ray flux and gamma-ray upper limits.