2015A&A...575A..81H

Query : 2015A&A...575A..81H

2015A&A...575A..81H - Astronomy and Astrophysics, volume 575A81-81 (2015/3-1)

H.E.S.S. reveals a lack of TeV emission from the supernova remnant Puppis A.

HESS COLLABORATION, ABRAMOWSKI A., AHARONIAN F., AIT BENKHALI F., AKHPERJANIAN A.G., ANGUENER E.O., BACKES M., BALENDERAN S., BALZER A., BARNACKA A., BECHERINI Y., BECKER TJUS J., BERGE D., BERNHARD S., BERNLOEHR K., BIRSIN E., BITEAU J., BOETTCHER M., BOISSON C., BOLMONT J., BORDAS P., BREGEON J., BRUN F., BRUN P., BRYAN M., BULIK T., CARRIGAN S., CASANOVA S., CHADWICK P.M., CHAKRABORTY N., CHALME-CALVET R., CHAVES R.C.G., CHRETIEN M., COLAFRANCESCO S., COLOGNA G., CONRAD J., COUTURIER C., CUI Y., DAVIDS I.D., DEGRANGE B., DEIL C., DEWILT P., DJANNATI-ATAIE A., DOMAINKO W., DONATH A., 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., GABICI S., GAJDUS M., GALLANT Y.A., GARRIGOUX T., GIAVITTO G., GIEBELS B., GLICENSTEIN J.F., GOTTSCHALL D., GRONDIN M.-H., GRUDZINSKA M., HADASCH D., 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., IVASCENKO A., JACHOLKOWSKA A., JAHN C., JAMROZY M., JANIAK M., JANKOWSKY F., JUNG-RICHARDT I., KASTENDIECK M.A., KATARZYNSKI K., KATZ U., KAUFMANN S., KHELIFI B., KIEFFER M., KLEPSER S., KLOCHKOV D., KLUZNIAK W., KOLITZUS D., KOMIN NU., KOSACK K., KRAKAU S., KRAYZEL F., KRUEGER P.P., LAFFON H., LAMANNA G., LEFAUCHEUR J., LEFRANC V., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., 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., MITCHELL A.M.W., MODERSKI R., MOHAMED M., MORA K., MOULIN E., MURACH T., DE NAUROIS M., NIEMIEC J., NOLAN S.J., OAKES L., ODAKA H., OHM S., OPITZ B., OSTROWSKI M., OYA I., PANTER M., PARSONS R.D., PAZ ARRIBAS M., PEKEUR N.W., PELLETIER G., PETRUCCI P.-O., PEYAUD B., PITA S., POON H., PUEHLHOFER G., PUNCH M., QUIRRENBACH A., RAAB S., REICHARDT I., REIMER A., REIMER O., RENAUD M., DE LOS REYES R., RIEGER F., ROMOLI C., ROSIER-LEES S., ROWELL G., RUDAK B., RULTEN C.B., SAHAKIAN V., SALEK D., SANCHEZ D.A., SANTANGELO A., SCHLICKEISER R., SCHUESSLER F., SCHULZ A., SCHWANKE U., SCHWARZBURG S., SCHWEMMER S., SOL H., SPANIER F., SPENGLER G., SPIES F., STAWARZ L., STEENKAMP R., STEGMANN C., STINZING F., STYCZ K., SUSHCH I., TAVERNET J.-P., TAVERNIER T., TAYLOR A.M., TERRIER R., TLUCZYKONT M., TRICHARD C., VALERIUS K., VAN ELDIK C., VAN SOELEN B., VASILEIADIS G., VEH J., VENTER C., VIANA A., VINCENT P., VINK J., VOELK H.J., VOLPE F., VORSTER M., VUILLAUME T., WAGNER S.J., WAGNER P., WAGNER R.M., WARD M., WEIDINGER M., WEITZEL Q., WHITE R., WIERZCHOLSKA A., WILLMANN P., WOERNLEIN A., WOUTERS D., YANG R., ZABALZA V., ZABOROV D., ZACHARIAS M., ZDZIARSKI A.A., ZECH A. and ZECHLIN H.-S.

Abstract (from CDS):

object{Puppis A} is an interesting ∼4kyr-old supernova remnant (SNR) that shows strong evidence of interaction between the forward shock and a molecular cloud. It has been studied in detail from radio frequencies to high-energy (HE, 0.1-100GeV) γ-rays. An analysis of the Fermi-LAT data has shown extended HE γ-ray emission with a 0.2-100GeV spectrum exhibiting no significant deviation from a power law, unlike most of the GeV-emitting SNRs known to be interacting with molecular clouds. This makes it a promising target for imaging atmospheric Cherenkov telescopes (IACTs) to probe the γ-ray emission above 100GeV. Very-high-energy (VHE, E ≥0.1TeV) γ-ray emission from Puppis A has been, for the first time, searched for with the High Energy Stereoscopic System (H.E.S.S.). Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the direction and energy of the incident γ-rays in order to produce sky images and source spectra. The profile likelihood method is applied to find constraints on the existence of a potential break or cutoff in the photon spectrum. The analysis of the H.E.S.S. data does not reveal any significant emission towards Puppis A. The derived upper limits on the differential photon flux imply that its broadband γ-ray spectrum must exhibit a spectral break or cutoff. By combining Fermi-LAT and H.E.S.S. measurements, the 99% confidence-level upper limits on such a cutoff are found to be 450 and 280GeV, assuming a power law with a simple exponential and a sub-exponential cutoff, respectively. It is concluded that none of the standard limitations (age, size, radiative losses) on the particle acceleration mechanism, assumed to be continuing at present, can explain the lack of VHE signal. The scenario in which particle acceleration has ceased some time ago is considered as an alternative explanation. The HE/VHE spectrum of Puppis A could then exhibit a break of non-radiative origin (as observed in several other interacting SNRs, albeit at somewhat higher energies), owing to the interaction with dense and neutral material, in particular towards the NE region.

Abstract Copyright: ∼

Journal keyword(s): gamma rays: ISM - ISM: individual objects: Puppis A - radiation mechanisms: non-thermal - cosmic rays - acceleration of particles

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 - 2026 		#notes
1 SNR G180.0-01.7 SNR 05 39 00.000 +27 50 00.00           ~ 294 2
2 IC 443 SNR 06 17 00.0000000 +22 34 11.998901           ~ 1314 1
3 NAME Pup A SNR 08 24 07 -42 59.8           ~ 636 1
4 NAME Vela X Psr 08 33 08.880 -45 11 24.36           ~ 302 1
5 SNR G349.7+00.2 SNR 17 18 10.160 -37 18 53.80           ~ 196 0
6 SNR G006.4-00.1 SNR 18 00 31.2011719 -23 25 48.001099           ~ 782 1
7 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 1034 2
8 W 49b SNR 19 11 09.5 +09 06 21           ~ 500 1
9 SNR G049.1-00.1 SNR 19 23 19.300 +14 09 21.00           ~ 309 0
10 SNR G089.0+04.7 SNR 20 45.0 +50 35           ~ 237 0
11 NAME Cyg Loop SNR 20 51.0 +30 40           ~ 964 0
12 NAME Vela Field reg ~ ~           ~ 200 0

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