J/A+A/662/A65 Kepler's supernova gamma-ray emissions (HESS Coll.+, 2022)
Evidence for gamma-ray emission from the remnant of Kepler's supernova based
on deep H.E.S.S. observations.
H.E.S.S. collaboration, Aharonian F., Ait Benkhali F., Anguener E.O.,
Ashkar H., Backes M., Barbosa Martins V., Batzofin R., Becherini Y.,
Berge D., Bernloehr K., Boettcher M., Boisson C., Bolmont J.,
de Bony de Lavergne M., Breuhaus M., Brose R., Brun F., Bulik T.,
Bylund T., Cangemi F., Caroff S., Casanova S., Cerruti M., Chand T.,
Chen A., Chibueze O., Cotter G., Cristofari P., Damascene Mbarubucyeye J.,
Devin J., Djannati-Atai A., Dmytriiev A., Egberts K., Einecke S.,
Ernenwein J.-P., Feijen K., Fiasson A., Fichet de Clairfontaine G.,
Fontaine G., Funk S., Gabici S., Gallant Y.A., Ghafourizadeh S.,
Giavitto G., Giunti L., Glawion D., Glicenstein J.F., Grondin M.-H.,
Hoerbe M., Hofmann W., Holch T.L., Holler M., Horns D., Huang Z.,
Jamrozy M., Joshi V., Jung-Richardt I., Kasai E., KatarzyNski K., Katz U.,
Khelifi B., Klu?niak W., Komin N., Kosack K., Kostunin D., Lemiere A.,
Lemoine-Goumard M., Lenain J.-P., Leuschner F., Lohse T., Luashvili A.,
Lypova I., Mackey J., Malyshev D., Marandon V., Marchegiani P.,
Marcowith A., Marti-Devesa G., Marx R., Maurin G., Meintjes P.J., Meyer M.,
Mitchell A., Moderski R., Mohrmann L., Montanari A., Moulin E., Muller J.,
Nakashima K., de Naurois M., Nayerhoda A., Niemiec J., Priyana Noel A.,
O'Brien P., Ohm S., Olivera-Nieto L., de Ona Wilhelmi E., Ostrowski M.,
Panny S., Panter M., Parsons R.D., Peron G., Poireau V., Prokhorov D.A.,
Puehlhofer G., Punch M., Quirrenbach A., Reichherzer P., Reimer A.,
Reimer O., Renaud M., Reville B., Rieger F., Rowell G., Rudak B.,
Rueda Ricarte H., Sahakian V., Sailer S., Salzmann H., Sanchez D.A.,
Santangelo A., Sasaki M., Schaefer J., Schuessler F., Schutte H.M.,
Schwanke U., Shapopi J.N.S., Simoni R., Sol H., Specovius A., Spencer S.,
Stawarz L., Steinmassl S., Steppa C., Sushch I., Takahashi T., Tanaka T.,
Taylor A.M., Terrier R., Tsirou M., Uchiyama Y., Unbehaun T., van Eldik C.,
Veh J., Vink J., Voelk H.J., Wagner S.J., Werner F., White R.,
Wierzcholska A., Wong Y.W., Yusafzai A., Zacharias M., Zargaryan D.,
Zdziarski A.A., Zech A., Zhu S.J., Zouari S., Zywucka N.
<Astron. Astrophys. 662, A65 (2022)>
=2022A&A...662A..65H 2022A&A...662A..65H (SIMBAD/NED BibCode)
ADC_Keywords: Supernova remnants ; Gamma rays
Keywords: gamma-rays: general - supernovae: individual: Kepler -
ISM: supernova remnants - radiation mechanisms: non-thermal
Abstract:
Observations with imaging atmospheric Cherenkov telescopes (IACTs)
have enhanced our knowledge of nearby supernova (SN) remnants with
ages younger than 500 yr by establishing Cassiopeia A and the remnant
of Tycho's SN as very-high-energy (VHE) γ-ray sources. The
remnant of Kepler's SN, which is the product of the most recent
naked-eye SN in our Galaxy, is comparable in age to the other two, but
is significantly more distant. If the γ-ray luminosities of the
remnants of Tycho's and Kepler's SNe are similar, then the latter
is expected to be one of the faintest γ-ray sources within reach
of the current generation IACT arrays. Here we report evidence at a
statistical level of 4.6σ for a VHE signal from the remnant of
Kepler's SN based on deep observations by the High Energy
Stereoscopic System (H.E.S.S.) with an exposure of 152h. The measured
integral flux above an energy of 226 GeV is ∼0.3% of the flux of the
Crab Nebula. The spectral energy distribution (SED) reveals a
γ-ray emitting component connecting the VHE emission observed
with H.E.S.S. to the emission observed at GeV energies with Fermi-LAT.
The overall SED is similar to that of the remnant of Tycho's SN,
possibly indicating the same nonthermal emission processes acting in
both these young remnants of thermonuclear SNe.
Description:
H.E.S.S. data points.
Objects:
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RA (2000) DE Designation(s)
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17 30 35.98 -21 28 56.2 Kepler's supernova = NAME Kepler SNR
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table.dat 32 4 H.E.S.S. data points shown in Figures 2a and 3
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Byte-by-byte Description of file: table.dat
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Bytes Format Units Label Explanations
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1- 10 E10.5 Hz Freq Frequency
12- 21 E10.5 mW/m2 E2*dN/dE Flux, E2*dN/dE (erg/cm2/s)
23- 32 E10.5 mW/m2 e_E2*dN/dE rms uncertainty on Flux (erg/cm2/s)
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Acknowledgements:
Dmitry Prokhorov, phdmitry(at)gmail.com
(End) Patricia Vannier [CDS] 25-Apr-2022