J/A+A/612/A3 HESS Galactic supernova remnants (Hess+, 2018)
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., Zywucka N.
<Astron. Astrophys., 612, A3 (2018)>
=2018A&A...612A...3H 2018A&A...612A...3H (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Supernova remnants ; Milky Way
Keywords: gamma rays: general - ISM: supernova remnants
Abstract:
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.
Description:
In this study, we selected only data of high quality using the
criteria described in Aharonian et al. (2006A&A...457..899A 2006A&A...457..899A) and the
quality cut on atmospheric transparency conditions developed by Hahn
et al. (2014, Astropart. Phys., 54, 25). The observation live time of
the analysed regions, corrected by the H.E.S.S. γ-ray
acceptance, spans a range from ∼10min to ∼80h with a median value of
14.5h. The majority of data ( ∼80%) have been recorded at average
zenith angles smaller than 40°. Table A.1 lists the analysed
source sample and the corrected observation live time, the averaged
zenith angle for the observations of each source, and the closest
H.E.S.S. source.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 102 108 Results overview
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See also:
http://www.physics.umanitoba.ca/snr/SNRcat : SNRCat Home Page
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Source Source designation (GLLL.l+B.b)
12- 17 F6.2 deg GLON Galactic longitude
19- 23 F5.2 deg GLAT Galactic latitude
25- 28 F4.2 deg RON Radius of the circular analysis regions
30- 36 A7 --- Type SNR morphology type (1)
38- 42 F5.2 kpc Dist ? Distance (2)
46- 49 F4.1 h LTime Corrected observation live time
54- 57 F4.1 deg Avzenith Averaged zenith angle
62- 75 A14 --- CDetec Closest HESS source detected
76 A1 --- --- [/]
77- 80 F4.1 deg Sep ? Angular distance of closest HESS source
81- 85 F5.1 10-13cm-2/s Ful Upper limit on the integrated flux in
the (1,10)TeV interval
87- 90 F4.1 --- signi Significance (sigma)
92- 96 F5.1 10+41W Wpxnul ?=- Upper limit on the product of proton
energy content above 10TeV and ambient
density, (Wpxn)ul[>10TeV]
98-102 F5.1 10+38W Weul ?=- Upper limit on the total energy content
in electrons, Wule[>10TeV]
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Note (1): The SNR morphology type is indicated by S for shell-type and
C for mixed morphology SNRs. The type of the latter is indicated as thermal
(t), plerionic (p), or both (t&p). If molecular cloud interaction is probable
or certain (information taken from SNRcat, Ferrand & Safi-Harb,
2012AdSpR..49.1313F 2012AdSpR..49.1313F), this is indicated by an asterisk.
For sources with an observational live time ≲1h, instrumental effects can
impact the result and should be used with care.
Note (2): Distance assumptions correspond to the arithmetic mean of the density
range limits reported in SNRcat (Ferrand & Safi-Harb, 2012AdSpR..49.1313F 2012AdSpR..49.1313F).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 12-Jun-2018