SIMBAD references

2005A&A...437..135A - Astronomy and Astrophysics, volume 437, 135-139 (2005/7-1)

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

AHARONIAN F., AKHPERJANIAN A.G., AYE K.-M., BAZER-BACHI A.R., BEILICKE M., BENBOW W., BERGE D., BERGHAUS P., BERNLOEHR K., BOISSON C., BOLZ O., BORGMEIER C., BREITLING F., BROWN A.M., BUSSONS GORDO J., CHADWICK P.M., CHOUNET L.-M., CORNILS R., COSTAMANTE L., DEGRANGE B., DJANNATI-ATAIE A., DRURY L.O'C., DUBUS G., ERGIN T., ESPIGAT P., FEINSTEIN F., FLEURY P., FONTAINE G., FUNK S., GALLANT Y.A., GIEBELS B., GILLESSEN S., GORET P., HADJICHRISTIDIS C., HAUSER M., HEINZELMANN G., HENRI G., HERMANN G., HINTON J.A., HOFMANN W., HOLLERAN M., HORNS D., DE JAGER O.C., JUNG I., KHELIFI B., KOMIN N., KONOPELKO A., LATHAM I.J., LE GALLOU R., LEMIERE A., LEMOINE M., LEROY N., LOHSE T., MARCOWITH A., MASTERSON C., McCOMB T.J.L., DE NAUROIS M., NOLAN S.J., NOUTSOS A., ORFORD K.J., OSBORNE J.L., OUCHRIF M., PANTER M., PELLETIER G., PITA S., PUEHLHOFER G., PUNCH M., RAUBENHEIMER B.C., RAUE M., RAUX J., RAYNER S.M., REDONDO I., REIMER A., REIMER O., RIPKEN J., ROB L., ROLLAND L., ROWELL G.P., SAHAKIAN V., SAUGE L., SCHLENKER S., SCHLICKEISER R., SCHUSTER C., SCHWANKE U., SIEWERT M., SOL H., STEENKAMP R., STEGMANN C., TAVERNET J.-P., THEORET C.G., TLUCZYKONT M., VAN DER WALT D.J., VASILEIADIS G., VINCENT P., VISSER B., VOELK H.J. and WAGNER S.J.

Abstract (from CDS):

Observations of the shell-type supernova remnant SN1006 have been carried out with the HESS system of Cherenkov telescopes during 2003 (18.2h with two operating telescopes) and 2004 (6.3h with all four telescopes). No evidence for TeV γ-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 γ-ray luminosity (for E=0.26 to 10TeV, distance d=2kpc) of L_γ<1.7x10³³erg/s, and the total energy in corresponding accelerated protons, W_p<1.6x10⁵⁰erg are estimated (for proton energies E_p∼1.5 to 60TeV and assuming the lowest value n=0.05cm^–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∼1GeV to 3PeV, assuming a differential particle index -2) gives W_p<6.3x10⁵⁰erg. A lower limit on the post-shock magnetic field of B>25µG results when considering the synchrotron/inverse-Compton framework for the observed X-ray flux and γ-ray upper limits.

Abstract Copyright: ∼

Journal keyword(s): gamma rays: observations - ISM: supernova remnants

Simbad objects: 3

Full paper

View the references in ADS

To bookmark this query, right click on this link: simbad:2005A&A...437..135A and select 'bookmark this link' or equivalent in the popup menu