SIMBAD references

2005A&A...435L..17A - Astronomy and Astrophysics, volume 435L17-20 (2005/5-3)

Discovery of extended VHE gamma-ray emission from the asymmetric pulsar wind nebula in MSH 15-52 with HESS.

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., BRAUN I., 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., EMMANOULOPOULOS D., ESPIGAT P., FEINSTEIN F., FLEURY P., FONTAINE G., FUCHS Y., FUNK S., GALLANT Y.A., GIEBELS B., GILLESSEN S., GLICENSTEIN J.F., 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., KHELIFI B., KOMIN N., KONOPELKO A., LATHAM I.J., LE GALLOU R., LEMIERE A., LEMOINE-GOUMARD M., LEROY N., LOHSE T., MARTINEAU-HUYNH O., 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., SAHAKIAN V., SAUGE L., SCHLENKER S., SCHLICKEISER R., SCHUSTER C., SCHWANKE U., SIEWERT M., SOL H., STEENKAMP R., STEGMANN C., TAVERNET J.-P., TERRIER R., THEORET C.G., TLUCZYKONT M., VASILEIADIS G., VENTER C., VINCENT P., VOELK H.J. and WAGNER S.J.

Abstract (from CDS):

The Supernova Remnant MSH 15-52 has been observed in very high energy (VHE) γ-rays using the HESS 4-telescope array located in Namibia. A γ-ray signal is detected at the 25 sigma level during an exposure of 22.1h live time. The image reveals an elliptically shaped emission region around the pulsar PSRB1509-58, with semi-major axis ∼6' in the NW-SE direction and semi-minor axis ∼2'. This morphology coincides with the diffuse pulsar wind nebula as observed at X-ray energies by ROSAT. The overall energy spectrum from 280GeV up to 40TeV can be fitted by a power law with photon index Γ=2.27±0.03stat±0.20syst. The detected emission can be plausibly explained by inverse Compton scattering of accelerated relativistic electrons with soft photons.

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Journal keyword(s): gamma-rays: observations - ISM: supernova remnants - pulsar wind nebula - ISM: individual objects: PSR B1509-58 - ISM: individual objects: G320.4-1.2

Simbad objects: 3

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