2018A&A...612A...3H


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.22CET09:45:55

2018A&A...612A...3H - Astronomy and Astrophysics, volume 612A, 3-3 (2018/4-1)

Population study of Galactic supernova remnants at very high γ-ray energies with H.E.S.S.

HESS COLLABORATION, ABDALLA H., ABRAMOWSKI A., AHARONIAN F., AIT BENKHALI F., ANGUNER E.O., ARAKAWA M., ARRIETA M., AUBERT P., BACKES M., BALZER A., BARNARD M., BECHERINI Y., BECKER TJUS J., BERGE D., BERNHARD S., BERNLOHR K., BLACKWELL R., BOTTCHER M., BOISSON C., BOLMONT J., BONNEFOY S., BORDAS P., BREGEON J., BRUN F., BRUN P., BRYAN M., BUCHELE M., BULIK T., CAPASSO M., CAROFF S., CAROSI A., CASANOVA S., CERRUTI M., CHAKRABORTY N., CHAVES R.C.G., CHEN A., CHEVALIER J., COLAFRANCESCO S., CONDON B., CONRAD J., DAVIDS I.D., DECOCK J., DEIL C., DEVIN J., DEWILT P., DIRSON L., DJANNATI-ATAI A., DONATH A., DRURY L.O., DUTSON K., DYKS J., EDWARDS T., EGBERTS K., EMERY G., ERNENWEIN J.-P., ESCHBACH S., FARNIER C., FEGAN S., FERNANDES M.V., FERNANDEZ D., FIASSON A., FONTAINE G., FUNK S., FUSSLING M., GABICI S., GALLANT Y.A., GARRIGOUX T., GATE F., GIAVITTO G., GIEBELS B., GLAWION D., GLICENSTEIN J.F., GOTTSCHALL D., GRONDIN M.-H., HAHN J., HAUPT M., HAWKES J., HEINZELMANN G., HENRI G., HERMANN G., HINTON J.A., HOFMANN W., HOISCHEN C., HOLCH T.L., HOLLER M., HORNS D., IVASCENKO A., IWASAKI H., JACHOLKOWSKA A., JAMROZY M., JANKOWSKY D., JANKOWSKY F., JINGO M., JOUVIN L., JUNG-RICHARDT I., KASTENDIECK M.A., KATARZYNSKI K., KATSURAGAWA M., KATZ U., KERSZBERG D., KHANGULYAN D., KHELIFI B., KING J., KLEPSER S., KLOCHKOV D., KLUZNIAK W., KOMIN N., KOSACK K., KRAKAU S., KRAUS M., KRUGER P.P., LAFFON H., LAMANNA G., LAU J., LEES J.-P., LEFAUCHEUR J., LEMIERE A., LEMOINE-GOUMARD M., LENAIN J.-P., LESER E., LOHSE T., LORENTZ M., LIU R., LOPEZ-COTO R., LYPOVA I., MALYSHEV D., MARANDON V., MARCOWITH A., MARIAUD C., MARX R., MAURIN G., MAXTED N., MAYER M., MEINTJES P.J., MEYER M., MITCHELL A.M.W., MODERSKI R., MOHAMED M., MOHRMANN L., MORA K., MOULIN E., MURACH T., NAKASHIMA S., DE NAUROIS M., NDIYAVALA H., NIEDERWANGER F., NIEMIEC J., OAKES L., O'BRIEN P., ODAKA H., OHM S., OSTROWSKI M., OYA I., PADOVANI M., PANTER M., PARSONS R.D., PEKEUR N.W., PELLETIER G., PERENNES C., PETRUCCI P.-O., PEYAUD B., PIEL Q., PITA S., POIREAU V., POON H., PROKHOROV D., PROKOPH H., PUHLHOFER G., PUNCH M., QUIRRENBACH A., RAAB S., RAUTH R., REIMER A., REIMER O., RENAUD M., DE LOS REYES R., RIEGER F., RINCHIUSO L., ROMOLI C., ROWELL G., RUDAK B., RULTEN C.B., SAFI-HARB S., SAHAKIAN V., SAITO S., SANCHEZ D.A., SANTANGELO A., SASAKI M., SCHLICKEISER R., SCHUSSLER F., SCHULZ A., SCHWANKE U., SCHWEMMER S., SEGLAR-ARROYO M., SETTIMO M., SEYFFERT A.S., SHAFI N., SHILON I., SHININGAYAMWE K., SIMONI R., SOL H., SPANIER F., SPIR-JACOB M., STAWARZ L., STEENKAMP R., STEGMANN C., STEPPA C., SUSHCH I., TAKAHASHI T., TAVERNET J.-P., TAVERNIER T., TAYLOR A.M., TERRIER R., TIBALDO L., TIZIANI D., TLUCZYKONT M., TRICHARD C., TSIROU M., TSUJI N., TUFFS R., UCHIYAMA Y., VAN DER WALT D.J., VAN ELDIK C., VAN RENSBURG C., VAN SOELEN B., VASILEIADIS G., VEH J., VENTER C., VIANA A., VINCENT P., VINK J., VOISIN F., VOLK H.J., VUILLAUME T., WADIASINGH Z., WAGNER S.J., WAGNER P., WAGNER R.M., WHITE R., WIERZCHOLSKA A., WILLMANN P., WORNLEIN A., WOUTERS D., YANG R., ZABOROV D., ZACHARIAS M., ZANIN R., ZDZIARSKI A.A., ZECH A., ZEFI F., ZIEGLER A., ZORN J. and ZYWUCKA N.

Abstract (from CDS):

Shell-type supernova remnants (SNRs) are considered prime candidates for the acceleration of Galactic cosmic rays (CRs) up to the knee of the CR spectrum at E~=3x1015eV. Our Milky Way galaxy hosts more than 350 SNRs discovered at radio wavelengths and at high energies, of which 220 fall into the H.E.S.S. Galactic Plane Survey (HGPS) region. Of those, only 50 SNRs are coincident with a H.E.S.S source and in 8 cases the very high-energy (VHE) emission is firmly identified as an SNR. The H.E.S.S. GPS provides us with a legacy for SNR population study in VHE γ-rays and we use this rich data set to extract VHE flux upper limits from all undetected SNRs. Overall, the derived flux upper limits are not in contradiction with the canonical CR paradigm. Assuming this paradigm holds true, we can constrain typical ambient density values around shell-type SNRs to n≤7cm–3 and electron-to-proton energy fractions above 10TeV to εep≤5x10–3. Furthermore, comparisons of VHE with radio luminosities in non-interacting SNRs reveal a behaviour that is in agreement with the theory of magnetic field amplification at shell-type SNRs.

Abstract Copyright: © ESO 2018

Journal keyword(s): gamma rays: general - ISM: supernova remnants

VizieR on-line data: <Available at CDS (J/A+A/612/A3): tablea1.dat>

Simbad objects: 127

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Number of rows : 127

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 SN 1572A SN* 00 25 21.5 +64 08 27           B8 1047 1
2 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5489 4
3 NAME Vela Jr SN SNR 08 52.0 -46 20           ~ 389 2
4 SNR G038.7-01.3 SNR 09 06 40.50 +04 28 18.8           ~ 9 0
5 SNR G272.2-03.2 SNR 09 06 50 -52 07.0           ~ 56 0
6 SNR G279.0+01.1 SNR 09 57.7 -53 15           ~ 23 0
7 SNR G286.5-01.2 Rad 10 35.7 -59 42           ~ 15 1
8 NAME MSH 11-61A SNR 10 59 25.36 -61 18 42.6           ~ 151 0
9 SNR G289.7-00.3 SNR 11 01.2 -60 18           ~ 13 0
10 SNR G291.0-00.1 SNR 11 11 54 -60 38.0           ~ 83 0
11 SNR G292.0+01.8 SNR 11 24 59 -59 19.1           ~ 280 1
12 SNR G293.8+00.6 SNR 11 35 00 -60 54.0           ~ 31 0
13 SNR G294.1-00.0 SNR 11 36.2 -61 38           ~ 10 0
14 SNR G296.1-00.5 SNR 11 51 10 -62 34.0           ~ 44 0
15 GAL 296.59-00.98 SN? 11 54 51.0 -63 08 54           ~ 13 0
16 SNR G296.8-00.3 SNR 11 58 30 -62 35.0           ~ 47 0
17 SNR G298.6-00.0 SNR 12 13 41.000 -62 37 00.00           ~ 33 0
18 SNR G299.2-02.9 SNR 12 15 13 -65 30.0           ~ 42 0
19 SNR G299.6-00.5 SNR 12 21.7 -63 09           ~ 12 0
20 SNR G301.4-01.0 SNR 12 37.9 -63 49           ~ 12 0
21 SNR G302.3+00.7 SNR 12 45.9 -62 08           ~ 27 0
22 SNR G306.3-00.9 SNR 13 21 50.9 -63 33 50           ~ 11 0
23 SNR G308.1-00.7 SNR 13 37.6 -63 04           ~ 12 0
24 SNR G308.3-01.4 SNR 13 41 30 -63 44.0           ~ 12 0
25 SNR G308.8-00.1 SNR 13 42 30 -62 23.0           ~ 37 1
26 SNR G309.2-00.6 SNR 13 46.5 -62 54           ~ 54 0
27 SNR G309.8+00.0 SNR 13 50 30.000 -62 05 00.00           ~ 38 0
28 SNR G310.6-00.3 SNR 13 58.0 -62 09           ~ 16 1
29 NAME Kes 20A Rad 13 59 44.9 -62 13 56           ~ 23 2
30 PSR J1400-6325 Psr 14 00 45.69 -63 25 42.6           ~ 23 1
31 SNR G311.5-00.3 Rad 14 05.6 -61 58           ~ 51 1
32 SNR G312.5-03.0 SNR 14 21.0 -64 12           ~ 11 0
33 NAME the Frying Pan SNR 14 38.4 -60 11           ~ 23 0
34 ESO 134-11 HII 14 40 29 -62 38.7           ~ 493 1
35 SNR G316.3-00.0 SNR 14 42 00.900 -59 58 59.00           ~ 49 0
36 SNR G317.3-00.2 SNR 14 49.7 -59 46           ~ 13 0
37 SNR G318.9+00.4 SNR 14 58.3 -58 28           ~ 14 0
38 NAME Lupus SN SNR 15 02 22.1 -42 05 49           SNIa 1183 1
39 SNR G321.9-00.3 SNR 15 20 39.000 -57 33 42.00           ~ 78 0
40 SNR G322.1+00.0 SR? 15 20 49 -57 10.0           ~ 3 0
41 SNR G322.5-00.1 SNR 15 23.4 -57 06           ~ 17 0
42 SNR G321.9-01.1 SNR 15 23.7 -58 13           ~ 13 0
43 SNR G323.5+00.1 SNR 15 28.7 -56 21           ~ 25 0
44 HESS J1534-571 gam 15 34 -57.1           ~ 7 0
45 SNR G327.4+01.0 SNR 15 46.8 -53 20           ~ 16 0
46 SNR G327.4+00.4 SNR 15 48 20 -53 49.0           ~ 79 0
47 SNR G327.2-00.1 SNR 15 50 55 -54 18.0           ~ 58 1
48 Kes 25 SNR 15 53 00.000 -56 10 00.00           ~ 112 0
49 SNR G330.2+01.0 SNR 16 01.1 -51 34           ~ 55 1
50 SNR G329.7+00.4 SNR 16 01.3 -52 18           ~ 12 0
51 SNR G337.2-00.7 Rad 16 39 15.0 -47 48 27           ~ 51 1
52 SNR G341.2+00.9 SNR 16 47.6 -43 47           ~ 23 1
53 SNR G342.1+00.9 SNR 16 50.7 -43 04           ~ 13 0
54 SNR G342.0-00.2 SNR 16 54.8 -43 53           ~ 27 0
55 SNR G341.9-00.3 SNR 16 55.0 -44 01           ~ 34 0
56 SNR G343.1-00.7 SNR 17 00.4 -43 14           ~ 12 0
57 SNR G347.3-00.5 SNR 17 12 27 -39 41.2           ~ 583 1
58 SNR G349.7+00.2 SNR 17 18 10.160 -37 18 53.80           ~ 159 0
59 SNR G356.2+04.5 SNR 17 19.0 -29 40           ~ 14 0
60 SNR G351.7+00.8 SNR 17 21.0 -35 27           ~ 18 0
61 SNR G350.1-00.3 SNR 17 21 06 -37 26.9           ~ 50 0
62 SNR G351.2+00.1 SNR 17 22 27 -36 11.0           ~ 31 0
63 SNR G358.0+03.8 SNR 17 26 00.000 -28 36 00.00           ~ 19 0
64 SNR G350.0-01.8 SNR 17 27 50 -38 32.0           ~ 42 0
65 SNR G351.9-00.9 Rad 17 28.9 -36 16           ~ 12 1
66 NAME Kepler SNR Rad 17 30 35.976 -21 28 56.23           SNIa 698 4
67 SNR G355.4+00.7 SNR 17 31 20.000 -32 26 00.00           ~ 11 0
68 SNR G353.6-00.7 SNR 17 31 55.0 -34 42 36           ~ 90 0
69 SNR G355.6+00.0 SNR 17 35 18 -32 37.0           ~ 20 0
70 SNR G354.8-00.8 SNR 17 36 00 -33 42.0           ~ 21 1
71 SNR G358.1+00.1 Rad 17 37 00 -29 59.0           ~ 8 1
72 SNR G356.3-00.3 SNR 17 37 56.000 -32 16 00.00           ~ 20 0
73 NAME the Square Nebula Rad 17 38.6 -30 44           ~ 42 1
74 SNR G353.9-02.0 SNR 17 38.9 -35 11           ~ 15 0
75 SNR G359.1+00.9 SNR 17 38 56.7 -29 08 25           G-KIII 39 0
76 NAME Tornado Nebula SNR 17 40 16.360 -30 58 18.87           ~ 135 0
77 SNR G356.3-01.5 SNR 17 42 35 -32 52.0           ~ 17 0
78 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11054 0
79 SNR G355.9-02.5 Rad 17 45.9 -33 43           ~ 39 1
80 SNR G005.9+03.1 SNR 17 47.3 -22 16           ~ 21 0
81 SNR G001.9+00.3 SNR 17 48 46.10 -27 09 50.9           ~ 151 1
82 SNR G003.8+00.3 SNR 17 52 55 -25 28.0           ~ 16 0
83 SNR G003.7-00.2 SNR 17 55 26 -25 50.0           ~ 21 0
84 SNR G006.1+00.5 Rad 17 57.5 -23 25           ~ 13 1
85 SNR G007.2+00.2 SNR 18 01.1 -22 38           ~ 12 0
86 SNR G006.4-00.1 SNR 18 01 22.7 -23 17 20           ~ 631 1
87 NAME Duck Redux Rad 18 02 10.000 -24 54 00.00           ~ 168 3
88 SNR G009.8+00.6 SNR 18 05.1 -20 14           ~ 37 0
89 SNR G005.2-02.6 Rad 18 07.5 -25 45           ~ 18 1
90 SNR G007.5-01.7 SNR 18 09 -23.3           ~ 6 0
91 SNR G012.2+00.3 SNR 18 11.3 -18 10           ~ 12 0
92 SNR G011.2-01.1 SNR 18 14.0 -19 46           ~ 56 1
93 SNR G014.1-00.1 SNR 18 15.9 -16 34           ~ 12 0
94 SNR G014.3+00.1 SNR 18 16.0 -16 27           ~ 14 0
95 SNR G007.7-03.7 SNR 18 17 25 -24 04.0           ~ 39 0
96 SNR G015.9+00.2 SNR 18 18 52 -15 02.0           ~ 75 0
97 SNR G013.3-01.3 SNR 18 19 34 -18 00.0           ~ 18 0
98 SNR G016.0-00.5 SNR 18 21.9 -15 14           ~ 12 0
99 SNR G015.1-01.6 SNR 18 24.0 -16 34           ~ 21 0
100 SNR G018.8+00.3 SNR 18 24.0 -12 23           ~ 91 0
101 SNR G019.1+00.2 SNR 18 24.9 -12 07           ~ 12 0
102 SNR G020.4+00.1 SNR 18 27.8 -11 00           ~ 18 0
103 SNR G018.9-01.1 SNR 18 29.8 -12 58           ~ 50 0
104 SNR G021.0-00.4 SNR 18 31.2 -10 47           ~ 12 0
105 4C -01.46 Rad 18 43 51.33 -01 29 15.5           ~ 40 2
106 SNR G025.1-02.3 SNR 18 45 10 -08 00.0           ~ 9 0
107 SNR G036.6+02.6 SNR 18 48.8 +04 26           ~ 21 0
108 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 798 2
109 HESS J1857+026 gam 18 57 11.0 +02 40 00           ~ 34 0
110 HESS J1858+020 gam 18 58 20.0 +02 05 24           ~ 33 0
111 SNR G036.6-00.7 Rad 19 00.6 +02 56           ~ 35 1
112 SNR G039.2-00.3 SNR 19 04 04.50 +05 27 12.0           ~ 167 1
113 SNR G043.9+01.6 SNR 19 05.8 +10 30           ~ 27 0
114 SNR G042.8+00.6 SNR 19 07 41.80 +09 07 17.0           ~ 115 1
115 W 49b SNR 19 11 09.000 +09 06 24.00           ~ 384 1
116 SNR G046.8-00.3 SNR 19 18 10 +12 09.0           ~ 61 0
117 SNR G055.0+00.3 SNR 19 32.0 +19 50           ~ 20 0
118 SNR G054.4-00.3 SNR 19 33 22.5 +18 58 34           ~ 84 0
119 SNR G057.2+00.8 SNR 19 35.0 +21 57           ~ 45 0
120 SNR G053.6-02.2 SNR 19 38.8 +17 14           ~ 133 0
121 SNR G059.5+00.1 SNR 19 42.6 +23 35           ~ 20 0
122 SNR G064.5+00.9 SNR 19 50 25 +28 16.0           ~ 7 0
123 SNR G068.8+02.6 SNR 19 52 55 +32 54.2           ~ 327 1
124 SNR G067.7+01.8 SNR 19 54.5 +31 29           ~ 31 0
125 SNR G065.1+00.6 SNR 19 54.7 +28 35           ~ 41 0
126 SNR G069.7+01.0 SNR 20 02.7 +32 43           ~ 32 0
127 NAME Cas A SNR 23 23 24.000 +58 48 54.00           ~ 2339 1

    Equat.    Gal    SGal    Ecl

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2019.11.22-09:45:55

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