HES2014 4 , the SIMBAD biblio

2014A&A...562A..40H - Astronomy and Astrophysics, volume 562A, 40-40 (2014/2-1)

HESS J1818-154, a new composite supernova remnant discovered in TeV gamma rays and X-rays.

HESS COLLABORATION, ABRAMOWSKI A., AHARONIAN F., AIT BENKHALI F., AKHPERJANIAN A.G., ANGUENER E., ANTON G., BALENDERAN S., BALZER A., BARNACKA A., BECHERINI Y., BECKER TJUS J., BERNLOEHR K., BIRSIN E., BISSALDI E., BITEAU J., BOETTCHER M., BOISSON C., BOLMONT J., BORDAS P., BRUCKER J., BRUN F., BRUN P., BULIK T., CARRIGAN S., CASANOVA S., CERRUTI M., CHADWICK P.M., CHALME-CALVET R., CHAVES R.C.G., CHEESEBROUGH A., CHRETIEN M., COLAFRANCESCO S., COLOGNA G., CONRAD J., COUTURIER C., CUI Y., DALTON M., DANIEL M.K., DAVIDS I.D., DEGRANGE B., DEIL C., DEWILT P., DICKINSON H.J., DJANNATI-ATAIE A., DOMAINKO W., DRURY L.O'C., DUBUS G., DUTSON K., DYKS J., DYRDA M., EDWARDS T., EGBERTS K., EGER P., ESPIGAT P., FARNIER C., FEGAN S., FEINSTEIN F., FERNANDES M.V., FERNANDEZ D., FIASSON A., FONTAINE G., FOERSTER A., FUESSLING M., GAJDUS M., GALLANT Y.A., GARRIGOUX T., GIAVITTO G., GIEBELS B., GLICENSTEIN J.F., GRONDIN M.-H., GRUDZINSKA M., HAEFFNER S., HAHN J., HARRIS J., HEINZELMANN G., HENRI G., HERMANN G., HERVET O., HILLERT A., HINTON J.A., HOFMANN W., HOFVERBERG P., HOLLER M., HORNS D., JACHOLKOWSKA A., JAHN C., JAMROZY M., JANIAK M., JANKOWSKY F., JUNG I., KASTENDIECK M.A., KATARZYNSKI K., KATZ U., KAUFMANN S., KHELIFI B., KIEFFER M., KLEPSER S., KLOCHKOV D., KLUZNIAK W., KNEISKE T., KOLITZUS D., KOMIN NU., KOSACK K., KRAKAU S., KRAYZEL F., KRUEGER P.P., LAFFON H., LAMANNA G., LEFAUCHEUR J., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LENNARZ D., LOHSE T., LOPATIN A., LU C.-C., MARANDON V., MARCOWITH A., MARX R., MAURIN G., MAXTED N., MAYER M., McCOMB T.J.L., MEHAULT J., MEINTJES P.J., MENZLER U., MEYER M., MODERSKI R., MOHAMED M., MOULIN E., MURACH T., NAUMANN C.L., DE NAUROIS M., NIEMIEC J., NOLAN S.J., OAKES L., OHM S., DE ONA WILHELMI E., OPITZ B., OSTROWSKI M., OYA I., PANTER M., PARSONS R.D., PAZ ARRIBAS M., PEKEUR N.W., PELLETIER G., PEREZ J., PETRUCCI P.-O., PEYAUD B., PITA S., POON H., PUEHLHOFER G., PUNCH M., QUIRRENBACH A., RAAB S., RAUE M., REIMER A., REIMER O., RENAUD M., DE LOS REYES R., RIEGER F., ROB L., ROMOLI C., ROSIER-LEES S., ROWELL G., RUDAK B., RULTEN C.B., SAHAKIAN V., SANCHEZ D.A., SANTANGELO A., SCHLICKEISER R., SCHUESSLER F., SCHULZ A., SCHWANKE U., SCHWARZBURG S., SCHWEMMER S., SOL H., SPENGLER G., SPIES F., STAWARZ L., STEENKAMP R., STEGMANN C., STINZING F., STYCZ K., SUSHCH I., SZOSTEK A., TAVERNET J.-P., TAVERNIER T., TAYLOR A.M., TERRIER R., TLUCZYKONT M., TRICHARD C., VALERIUS K., VAN ELDIK C., VAN SOELEN B., VASILEIADIS G., VENTER C., VIANA A., VINCENT P., VOELK H.J., VOLPE F., VORSTER M., VUILLAUME T., WAGNER S.J., WAGNER P., WARD M., WEIDINGER M., WEITZEL Q., WHITE R., WIERZCHOLSKA A., WILLMANN P., WOERNLEIN A., WOUTERS D., ZABALZA V., ZACHARIAS M., ZAJCZYK A., ZDZIARSKI A.A., ZECH A. and ZECHLIN H.-S.

Abstract (from CDS):

Composite supernova remnants (SNRs) constitute a small subclass of the remnants of massive stellar explosions where non-thermal radiation is observed from both the expanding shell-like shock front and from a pulsar wind nebula (PWN) located inside of the SNR. These systems represent a unique evolutionary phase of SNRs where observations in the radio, X-ray, and γ-ray regimes allow the study of the co-evolution of both these energetic phenomena. In this article, we report results from observations of the shell-type SNR G 15.4+0.1 performed with the High Energy Stereoscopic System (H.E.S.S.) and XMM-Newton. A compact TeV γ-ray source, HESS J1818-154, located in the center and contained within the shell of G 15.4+0.1 is detected by H.E.S.S. and featurs a spectrum best represented by a power-law model with a spectral index of -2.3±0.3stat±0.2sys and an integral flux of F(>0.42TeV)=(0.9±0.3stat±0.2sys)x10–12/cm2/s. Furthermore, a recent observation with XMM-Newton reveals extended X-ray emission strongly peaked in the center of G 15.4+0.1. The X-ray source shows indications of an energy-dependent morphology featuring a compact core at energies above 4 keV and more extended emission that fills the entire region within the SNR at lower energies. Together, the X-ray and VHE γ-ray emission provide strong evidence of a PWN located inside the shell of G 15.4+0.1 and this SNR can therefore be classified as a composite based on these observations. The radio, X-ray, and γ-ray emission from the PWN is compatible with a one-zone leptonic model that requires a low average magnetic field inside the emission region. An unambiguous counterpart to the putative pulsar, which is thought to power the PWN, has been detected neither in radio nor in X-ray observations of G 15.4+0.1.

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Journal keyword(s): X-rays: individuals: G15.4+0.1 - gamma rays: general - methods: observational - supernovae: individual: HESS J1818-154 - X-rays: general

Nomenclature: Fig. 4, Table 1: HES2014 N (Nos 1-5).

Simbad objects: 14

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