2009A&A...508.1135H


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.08CET02:32:48

2009A&A...508.1135H - Astronomy and Astrophysics, volume 508, 1135-1140 (2009/12-4)

HESS upper limits on very high energy gamma-ray emission from the microquasar GRS 1915+105.

HESS COLLABORATION, ACERO F., AHARONIAN F., AKHPERJANIAN A.G., ANTON G., BARRES DE ALMEIDA U., BAZER-BACHI A.R., BECHERINI Y., BEHERA B., BERNLOEHR K., BOCHOW A., BOISSON C., BOLMONT J., BORREL V., BRUCKER J., BRUN F., BRUN P., BULIK T., BUESCHING I., BOUTELIER T., CHADWICK P.M., CHARBONNIER A., CHAVES R.C.G., CHEESEBROUGH A., CONRAD J., CHOUNET L.-M., CLAPSON A.C., COIGNET G., DALTON M., DANIEL M.K., DAVIDS I.D., DEGRANGE B., DEIL C., DICKINSON H.J., DJANNATI-ATAIE A., DOMAINKO W., DRURY L.O'C., DUBOIS F., DUBUS G., DYKS J., DYRDA M., EGBERTS K., EGER P., ESPIGAT P., FALLON L., FARNIER C., FEGAN S., FEINSTEIN F., FIASSON A., FOERSTER A., FONTAINE G., FUESSLING M., GABICI S., GALLANT Y.A., GERARD L., GERBIG D., GIEBELS B., GLICENSTEIN J.F., GLUECK B., GORET P., GOERING D., HAUSER M., HEINZ S., HEINZELMANN G., HENRI G., HERMANN G., HINTON J.A., HOFFMANN A., HOFMANN W., HOFVERBERG P., HOLLERAN M., HOPPE S., HORNS D., JACHOLKOWSKA A., DE JAGER O.C., JAHN C., JUNG I., KATARZYNSKI K., KATZ U., KAUFMANN S., KERSCHHAGGL M., KHANGULYAN D., KHELIFI B., KEOGH D., KLOCHKOV D., KLUZNIAK W., KNEISKE T., KOMIN N., KOSACK K., KOSSAKOWSKI R., LAMANNA G., LENAIN J.-P., LOHSE T., MARANDON V., MARCOWITH A., MASBOU J., MAURIN D., McCOMB T.J.L., MEDINA M.C., MEHAULT J., MODERSKI R., MOULIN E., NAUMANN-GODO M., DE NAUROIS M., NEDBAL D., NEKRASSOV D., NICHOLAS B., NIEMIEC J., NOLAN S.J., OHM S., OLIVE J.-F., DE ONA WILHELMI E., ORFORD K.J., OSTROWSKI M., PANTER M., PAZ ARRIBAS M., PEDALETTI G., PELLETIER G., PETRUCCI P.-O., PITA S., PUEHLHOFER G., PUNCH M., QUIRRENBACH A., RAUBENHEIMER B.C., RAUE M., RAYNER S.M., REIMER O., RENAUD M., DE LOS REYES R., RIEGER F., RIPKEN J., ROB L., ROSIER-LEES S., ROWELL G., RUDAK B., RULTEN C.B., RUPPEL J., RYDE F., SAHAKIAN V., SANTANGELO A., SCHLICKEISER R., SCHOECK F.M., SCHOENWALD A., SCHWANKE U., SCHWARZBURG S., SCHWEMMER S., SHALCHI A., SUSHCH I., SIKORA M., SKILTON J.L., SOL H., STAWARZ L., STEENKAMP R., STEGMANN C., STINZING F., SUPERINA G., SZOSTEK A., TAM P.H., TAVERNET J.-P., TERRIER R., TIBOLLA O., TLUCZYKONT M., VAN ELDIK C., VASILEIADIS G., VENTER C., VENTER L., VIALLE J.P., VINCENT P., VIVIER M., VOELK H.J., VOLPE F., VOROBIOV S., WAGNER S.J., WARD M., ZDZIARSKI A.A. and ZECH A.

Abstract (from CDS):

High energy particles reside in the relativistic jets of microquasars, making them possible sources of very high energy radiation (VHE, >100GeV). Detecting this emission would provide a new handle on jet physics. Observations of the microquasar GRS 1915+105 with the HESS telescope array were undertaken in 2004-2008 to search for VHE emission. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays. There is no evidence for a VHE gamma-ray signal either from the direction of the microquasar or its vicinity. An upper limit of 6.1x10–13ph/cm2/s (99.9% confidence level) is set on the photon flux above 410GeV, equivalent to a VHE luminosity of ∼1034erg/s at 11kpc. The VHE to X-ray luminosity ratio in GRS 1915+105 is at least four orders of magnitude lower than the ratio observed in gamma-ray binaries. The VHE radiative efficiency of the compact jet is less than 0.01% based on its estimated total power of 1038erg/s. Particle acceleration in GRS 1915+105 is not efficient at high energies and/or the magnetic field is too strong. It is also possible that VHE gamma-rays are produced by GRS 1915+105, but the emission is highly time-dependent.

Abstract Copyright:

Journal keyword(s): X-rays: binaries - X-rays: individual: GRS 1915+105 - gamma rays: observations

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 LS I +61 303 HXB 02 40 31.6641883136 +61 13 45.591138110 11.27 11.61 10.75 10.19 9.55 B0Ve 775 2
2 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4866 1
3 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5705 4
4 CPD-63 2495 HXB 13 02 47.6541729594 -63 50 08.625922862 10.34 10.72 9.98 10.03   O9.5Ve 689 1
5 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1056 0
6 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 626 0
7 V* V479 Sct HXB 18 26 15.0561532140 -14 50 54.249464136 12.02 12.23 11.27 11.04   ON6V((f))z 504 2
8 ARGO J1912+1026 gam 19 12 +10.1           ~ 32 0
9 IRAS 19124+1106 IR 19 14 45 +11 12.1           ~ 22 0
10 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2347 0
11 IRAS 19132+1035 Y*O 19 15 38.97768 +10 41 14.4276           ~ 43 0
12 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3984 0

    Equat.    Gal    SGal    Ecl

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