SIMBAD references

2010A&A...511A..52H - Astronomy and Astrophysics, volume 511A52-52 (2010/2-2)

PKS 2005-489 at VHE: four years of monitoring with HESS and simultaneous multi-wavelength observations.

HESS COLLABORATION, ACERO F., AHARONIAN F., AKHPERJANIAN A.G., ANTON G., BARRES DE ALMEIDA U., BAZER-BACHI A.R., BECHERINI Y., BEHERA B., BENBOW W., BERNLOEHR K., BOCHOW A., BOISSON C., BOLMONT J., BORREL V., BRUCKER J., BRUN F., BRUN P., BUEHLER R., BULIK T., BUESCHING I., BOUTELIER T., CHADWICK P.M., CHARBONNIER A., CHAVES R.C.G., CHEESEBROUGH A., CHOUNET L.-M., CLAPSON A.C., COIGNET G., COSTAMANTE L., 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., MARTINEAU-HUYNH O., 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., RENAUD M., RIEGER F., RIPKEN J., ROB L., ROSIER-LEES S., ROWELL G., RUDAK B., RULTEN C.B., RUPPEL J., SAHAKIAN V., SANTANGELO A., SCHLICKEISER R., SCHOECK F.M., SCHWANKE U., SCHWARZBURG S., SCHWEMMER S., SHALCHI A., 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., WAGNER S.J., WARD M., ZDZIARSKI A.A. and ZECH A.

Abstract (from CDS):

Our aim is to study the very high energy (VHE; E>100GeV) γ-ray emission from BLLac objects and the evolution in time of their broad-band spectral energy distribution (SED). VHE observations of the high-frequency peaked BLLac object PKS2005-489 were made with the High Energy Stereoscopic System (HESS) from 2004 through 2007. Three simultaneous multi-wavelength campaigns at lower energies were performed during the HESS data taking, consisting of several individual pointings with the XMM-Newton and RXTE satellites. A strong VHE signal, ∼17σ total, from PKS2005-489 was detected during the four years of HESS observations (90.3h live time). The integral flux above the average analysis threshold of 400GeV is ∼3% of the flux observed from the Crab Nebula and varies weakly on time scales from days to years. The average VHE spectrum measured from ∼300GeV to ∼5TeV is characterized by a power law with a photon index, Γ=3.20±0.16stat±0.10syst. At X-ray energies the flux is observed to vary by more than an order of magnitude between 2004 and 2005. Strong changes in the X-ray spectrum (ΔΓX≃0.7) are also observed, which appear to be mirrored in the VHE band. The SED of PKS2005-489, constructed for the first time with contemporaneous data on both humps, shows significant evolution. The large flux variations in the X-ray band, coupled with weak or no variations in the VHE band and a similar spectral behavior, suggest the emergence of a new, separate, harder emission component in September 2005.

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Journal keyword(s): galaxies: active - BL Lacertae objects: individual: PKS2005-489 - gamma rays: galaxies - X-rays: individual: PKS2005-489

Simbad objects: 3

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