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

A. Abramowski; F. Aharonian; F. Ait Benkhali; A. G. Akhperjanian; E. O. Angüner; M. Backes; S. Balenderan; A. Balzer; A. Barnacka; Y. Becherini; J. Becker Tjus; D. Berge; S. Bernhard; K. Bernlöhr; E. Birsin; J. Biteau; M. Böttcher; C. Boisson; J. Bolmont; P. Bordas; J. Bregeon; F. Brun; P. Brun; M. Bryan; T. Bulik; S. Carrigan; S. Casanova; P. M. Chadwick; N. Chakraborty; R. Chalme-Calvet; R. C G Chaves; M. Chrétien; S. Colafrancesco; G. Cologna; J. Conrad; C. Couturier; Y. Cui; I. D. Davids; B. Degrange; C. Deil; P. Dewilt; A. Djannati-Ataï; W. Domainko; A. Donath; L. O. Drury; G. Dubus; K. Dutson; J. Dyks; M. Dyrda; T. Edwards; K. Egberts; P. Eger; P. Espigat; C. Farnier; S. Fegan; F. Feinstein; M. V. Fernandes; D. Fernandez; A. Fiasson; G. Fontaine; A. Förster; M. Füßling; S. Gabici; M. Gajdus; Y. A. Gallant; T. Garrigoux; G. Giavitto; B. Giebels; J. F. Glicenstein; D. Gottschall; M. H. Grondin; M. Grudzińska; D. Hadasch; S. Häffner; J. Hahn; J. Harris; G. Heinzelmann; G. Henri; G. Hermann; O. Hervet; A. Hillert; J. A. Hinton; W. Hofmann; P. Hofverberg; M. Holler; D. Horns; A. Ivascenko; A. Jacholkowska; C. Jahn; M. Jamrozy; M. Janiak; F. Jankowsky; I. Jung-Richardt; M. A. Kastendieck; K. Katarzyński; U. Katz; S. Kaufmann; B. Khélifi; M. Kieffer; S. Klepser; D. Klochkov; W. Kluźniak; D. Kolitzus; Nu Komin; K. Kosack; S. Krakau; F. Krayzel; P. P. Krüger; H. Laffon; G. Lamanna; J. Lefaucheur; V. Lefranc; A. Lemière; M. Lemoine-Goumard; J. P. Lenain; T. Lohse; A. Lopatin; C. C. Lu; V. Marandon; A. Marcowith; R. Marx; G. Maurin; N. Maxted; M. Mayer; T. J L McComb; J. Méhault; P. J. Meintjes; U. Menzler; M. Meyer; A. M W Mitchell; R. Moderski; M. Mohamed; K. Morå; E. Moulin; T. Murach; M. De Naurois; J. Niemiec; S. J. Nolan; L. Oakes; H. Odaka; S. Ohm; B. Opitz; M. Ostrowski; I. Oya; M. Panter; R. D. Parsons; M. Paz Arribas; N. W. Pekeur; G. Pelletier; P. O. Petrucci; B. Peyaud; S. Pita; H. Poon; G. Pühlhofer; M. Punch; A. Quirrenbach; S. Raab; I. Reichardt; A. Reimer; O. Reimer; M. Renaud; R. De Los Reyes; F. Rieger; C. Romoli; S. Rosier-Lees; G. Rowell; B. Rudak; C. B. Rulten; V. Sahakian; D. Salek; D. A. Sanchez; A. Santangelo; R. Schlickeiser; F. Schüssler; A. Schulz; U. Schwanke; S. Schwarzburg; S. Schwemmer; H. Sol; F. Spanier; G. Spengler; F. Spies; [No Value] Stawarz; R. Steenkamp; C. Stegmann; F. Stinzing; K. Stycz; I. Sushch; J. P. Tavernet; T. Tavernier; A. M. Taylor; R. Terrier; M. Tluczykont; C. Trichard; K. Valerius; C. Van Eldik; B. Van Soelen; G. Vasileiadis; J. Veh; C. Venter; A. Viana; P. Vincent; J. Vink; H. J. Völk; F. Volpe; M. Vorster; T. Vuillaume; S. J. Wagner; P. Wagner; R. M. Wagner; M. Ward; M. Weidinger; Q. Weitzel; R. White; A. Wierzcholska; P. Willmann; A. Wörnlein; D. Wouters; R. Yang; V. Zabalza; D. Zaborov; M. Zacharias; A. A. Zdziarski; A. Zech; H. S. Zechlin

doi:10.1051/0004-6361/201424805

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

A. Abramowski, F. Aharonian, F. Ait Benkhali, A. G. Akhperjanian, E. O. Angüner, M. Backes, S. Balenderan, A. Balzer, A. Barnacka, Y. Becherini, J. Becker Tjus, D. Berge, S. Bernhard, K. Bernlöhr, E. Birsin, J. Biteau, M. Böttcher, C. Boisson, J. Bolmont, P. BordasJ. Bregeon, F. Brun, P. Brun, M. Bryan, T. Bulik, S. Carrigan, S. Casanova, P. M. Chadwick, N. Chakraborty, R. Chalme-Calvet, R. C G Chaves, M. Chrétien, S. Colafrancesco, G. Cologna, J. Conrad, C. Couturier, Y. Cui, I. D. Davids, B. Degrange, C. Deil, P. Dewilt, A. Djannati-Ataï, W. Domainko, A. Donath, L. O. Drury, G. Dubus, K. Dutson, J. Dyks, M. Dyrda, T. Edwards, K. Egberts, P. Eger, P. Espigat, C. Farnier, S. Fegan, F. Feinstein, M. V. Fernandes, D. Fernandez, A. Fiasson, G. Fontaine, A. Förster, M. Füßling, S. Gabici, M. Gajdus, Y. A. Gallant, T. Garrigoux, G. Giavitto, B. Giebels, J. F. Glicenstein, D. Gottschall, M. H. Grondin, M. Grudzińska, D. Hadasch, S. Häffner, J. Hahn, J. Harris, G. Heinzelmann, G. Henri, G. Hermann, O. Hervet, A. Hillert, J. A. Hinton, W. Hofmann, P. Hofverberg, M. Holler, D. Horns, A. Ivascenko, A. Jacholkowska, C. Jahn, M. Jamrozy, M. Janiak, F. Jankowsky, I. Jung-Richardt, M. A. Kastendieck, K. Katarzyński, U. Katz, S. Kaufmann, B. Khélifi, M. Kieffer, S. Klepser, D. Klochkov, W. Kluźniak, D. Kolitzus, Nu Komin, K. Kosack, S. Krakau, F. Krayzel, P. P. Krüger, H. Laffon, G. Lamanna, J. Lefaucheur, V. Lefranc, A. Lemière, M. Lemoine-Goumard, J. P. Lenain, T. Lohse, A. Lopatin, C. C. Lu, V. Marandon, A. Marcowith, R. Marx, G. Maurin, N. Maxted, M. Mayer, T. J L McComb, J. Méhault, P. J. Meintjes, U. Menzler, M. Meyer, A. M W Mitchell, R. Moderski, M. Mohamed, K. Morå, E. Moulin, T. Murach, M. De Naurois, J. Niemiec, S. J. Nolan, L. Oakes, H. Odaka, S. Ohm, B. Opitz, M. Ostrowski, I. Oya, M. Panter, R. D. Parsons, M. Paz Arribas, N. W. Pekeur, G. Pelletier, P. O. Petrucci, B. Peyaud, S. Pita, H. Poon, G. Pühlhofer, M. Punch, A. Quirrenbach, S. Raab, I. Reichardt, A. Reimer, O. Reimer, M. Renaud, R. De Los Reyes, F. Rieger, C. Romoli, S. Rosier-Lees, G. Rowell, B. Rudak, C. B. Rulten, V. Sahakian, D. Salek, D. A. Sanchez, A. Santangelo, R. Schlickeiser, F. Schüssler, A. Schulz, U. Schwanke, S. Schwarzburg, S. Schwemmer, H. Sol, F. Spanier, G. Spengler, F. Spies, [No Value] Stawarz, R. Steenkamp, C. Stegmann, F. Stinzing, K. Stycz, I. Sushch, J. P. Tavernet, T. Tavernier, A. M. Taylor, R. Terrier, M. Tluczykont, C. Trichard, K. Valerius, C. Van Eldik, B. Van Soelen, G. Vasileiadis, J. Veh, C. Venter, A. Viana, P. Vincent, J. Vink, H. J. Völk, F. Volpe, M. Vorster, T. Vuillaume, S. J. Wagner, P. Wagner, R. M. Wagner, M. Ward, M. Weidinger, Q. Weitzel, R. White, A. Wierzcholska, P. Willmann, A. Wörnlein, D. Wouters, R. Yang, V. Zabalza, D. Zaborov, M. Zacharias, A. A. Zdziarski, A. Zech, H. S. Zechlin

Physics and Astronomy (Twin Cities)

Research output: Contribution to journal › Article › peer-review

14 Scopus citations

Abstract

Context. Puppis A is an interesting ∼4 kyr-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..100 GeV) γ-rays. An analysis of the Fermi-LAT data has shown extended HE γ-ray emission with a 0.2-100 GeV 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 100 GeV.

Aims. Very-high-energy (VHE, E ≥ 0.1 TeV) γ-ray emission from Puppis A has been, for the first time, searched for with the High Energy Stereoscopic System (H.E.S.S.).

Methods. 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.

Results. 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 280 GeV, 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.

Original language	English (US)
Article number	A81
Journal	Astronomy and Astrophysics
Volume	575
DOIs	https://doi.org/10.1051/0004-6361/201424805
State	Published - Mar 1 2015

Bibliographical note

Publisher Copyright:
© 2015 ESO.

Keywords

Acceleration of particles
Cosmic rays
Gamma rays: ISM
ISM: individual objects: Puppis A
Radiation mechanisms: non-thermal

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Abramowski, A., Aharonian, F., Ait Benkhali, F., Akhperjanian, A. G., Angüner, E. O., Backes, M., Balenderan, S., Balzer, A., Barnacka, A., Becherini, Y., Becker Tjus, J., Berge, D., Bernhard, S., Bernlöhr, K., Birsin, E., Biteau, J., Böttcher, M., Boisson, C., Bolmont, J., ... Zechlin, H. S. (2015). H.E.S.S. reveals a lack of TeV emission from the supernova remnant Puppis A. Astronomy and Astrophysics, 575, Article A81. https://doi.org/10.1051/0004-6361/201424805

Abramowski, A, Aharonian, F, Ait Benkhali, F, Akhperjanian, AG, Angüner, EO, Backes, M, Balenderan, S, Balzer, A, Barnacka, A, Becherini, Y, Becker Tjus, J, Berge, D, Bernhard, S, Bernlöhr, K, Birsin, E, Biteau, J, Böttcher, M, Boisson, C, Bolmont, J, Bordas, P, Bregeon, J, Brun, F, Brun, P, Bryan, M, Bulik, T, Carrigan, S, Casanova, S, Chadwick, PM, Chakraborty, N, Chalme-Calvet, R, Chaves, RCG, Chrétien, M, Colafrancesco, S, Cologna, G, Conrad, J, Couturier, C, Cui, Y, Davids, ID, Degrange, B, Deil, C, Dewilt, P, Djannati-Ataï, A, Domainko, W, Donath, A, Drury, LO, Dubus, G, Dutson, K, Dyks, J, Dyrda, M, Edwards, T, Egberts, K, Eger, P, Espigat, P, Farnier, C, Fegan, S, Feinstein, F, Fernandes, MV, Fernandez, D, Fiasson, A, Fontaine, G, Förster, A, Füßling, M, Gabici, S, Gajdus, M, Gallant, YA, Garrigoux, T, Giavitto, G, Giebels, B, Glicenstein, JF, Gottschall, D, Grondin, MH, Grudzińska, M, Hadasch, D, Häffner, S, Hahn, J, Harris, J, Heinzelmann, G, Henri, G, Hermann, G, Hervet, O, Hillert, A, Hinton, JA, Hofmann, W, Hofverberg, P, Holler, M, Horns, D, Ivascenko, A, Jacholkowska, A, Jahn, C, Jamrozy, M, Janiak, M, Jankowsky, F, Jung-Richardt, I, Kastendieck, MA, Katarzyński, K, Katz, U, Kaufmann, S, Khélifi, B, Kieffer, M, Klepser, S, Klochkov, D, Kluźniak, W, Kolitzus, D, Komin, N, Kosack, K, Krakau, S, Krayzel, F, Krüger, PP, Laffon, H, Lamanna, G, Lefaucheur, J, Lefranc, V, Lemière, A, Lemoine-Goumard, M, Lenain, JP, Lohse, T, Lopatin, A, Lu, CC, Marandon, V, Marcowith, A, Marx, R, Maurin, G, Maxted, N, Mayer, M, McComb, TJL, Méhault, J, Meintjes, PJ, Menzler, U, Meyer, M, Mitchell, AMW, Moderski, R, Mohamed, M, Morå, K, Moulin, E, Murach, T, De Naurois, M, Niemiec, J, Nolan, SJ, Oakes, L, Odaka, H, Ohm, S, Opitz, B, Ostrowski, M, Oya, I, Panter, M, Parsons, RD, Paz Arribas, M, Pekeur, NW, Pelletier, G, Petrucci, PO, Peyaud, B, Pita, S, Poon, H, Pühlhofer, 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, CB, Sahakian, V, Salek, D, Sanchez, DA, Santangelo, A, Schlickeiser, R, Schüssler, F, Schulz, A, Schwanke, U, Schwarzburg, S, Schwemmer, S, Sol, H, Spanier, F, Spengler, G, Spies, F, Stawarz, NV, Steenkamp, R, Stegmann, C, Stinzing, F, Stycz, K, Sushch, I, Tavernet, JP, Tavernier, T, Taylor, AM, 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, Völk, HJ, Volpe, F, Vorster, M, Vuillaume, T, Wagner, SJ, Wagner, P, Wagner, RM, Ward, M, Weidinger, M, Weitzel, Q, White, R, Wierzcholska, A, Willmann, P, Wörnlein, A, Wouters, D, Yang, R, Zabalza, V, Zaborov, D, Zacharias, M, Zdziarski, AA, Zech, A & Zechlin, HS 2015, 'H.E.S.S. reveals a lack of TeV emission from the supernova remnant Puppis A', Astronomy and Astrophysics, vol. 575, A81. https://doi.org/10.1051/0004-6361/201424805

@article{9ed8a07383c1464dac828502ed9f3625,

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

abstract = "Context. Puppis A is an interesting ∼4 kyr-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..100 GeV) γ-rays. An analysis of the Fermi-LAT data has shown extended HE γ-ray emission with a 0.2-100 GeV 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 100 GeV.Aims. Very-high-energy (VHE, E ≥ 0.1 TeV) γ-ray emission from Puppis A has been, for the first time, searched for with the High Energy Stereoscopic System (H.E.S.S.).Methods. 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.Results. 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 280 GeV, 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.",

keywords = "Acceleration of particles, Cosmic rays, Gamma rays: ISM, ISM: individual objects: Puppis A, Radiation mechanisms: non-thermal",

author = "A. Abramowski and F. Aharonian and {Ait Benkhali}, F. and Akhperjanian, {A. G.} and Ang{\"u}ner, {E. O.} and M. Backes and S. Balenderan and A. Balzer and A. Barnacka and Y. Becherini and {Becker Tjus}, J. and D. Berge and S. Bernhard and K. Bernl{\"o}hr and E. Birsin and J. Biteau and M. B{\"o}ttcher and C. Boisson and J. Bolmont and P. Bordas and J. Bregeon and F. Brun and P. Brun and M. Bryan and T. Bulik and S. Carrigan and S. Casanova and Chadwick, {P. M.} and N. Chakraborty and R. Chalme-Calvet and Chaves, {R. C G} and M. Chr{\'e}tien and S. Colafrancesco and G. Cologna and J. Conrad and C. Couturier and Y. Cui and Davids, {I. D.} and B. Degrange and C. Deil and P. Dewilt and A. Djannati-Ata{\"i} and W. Domainko and A. Donath and Drury, {L. O.} and G. Dubus and K. Dutson and J. Dyks and M. Dyrda and T. Edwards and K. Egberts and P. Eger and P. Espigat and C. Farnier and S. Fegan and F. Feinstein and Fernandes, {M. V.} and D. Fernandez and A. Fiasson and G. Fontaine and A. F{\"o}rster and M. F{\"u}{\ss}ling and S. Gabici and M. Gajdus and Gallant, {Y. A.} and T. Garrigoux and G. Giavitto and B. Giebels and Glicenstein, {J. F.} and D. Gottschall and Grondin, {M. H.} and M. Grudzi{\'n}ska and D. Hadasch and S. H{\"a}ffner and J. Hahn and J. Harris and G. Heinzelmann and G. Henri and G. Hermann and O. Hervet and A. Hillert and Hinton, {J. A.} and W. Hofmann and P. Hofverberg and M. Holler and D. Horns and A. Ivascenko and A. Jacholkowska and C. Jahn and M. Jamrozy and M. Janiak and F. Jankowsky and I. Jung-Richardt and Kastendieck, {M. A.} and K. Katarzy{\'n}ski and U. Katz and S. Kaufmann and B. Kh{\'e}lifi and M. Kieffer and S. Klepser and D. Klochkov and W. Klu{\'z}niak and D. Kolitzus and Nu Komin and K. Kosack and S. Krakau and F. Krayzel and Kr{\"u}ger, {P. P.} and H. Laffon and G. Lamanna and J. Lefaucheur and V. Lefranc and A. Lemi{\`e}re and M. Lemoine-Goumard and Lenain, {J. P.} and T. Lohse and A. Lopatin and Lu, {C. C.} and V. Marandon and A. Marcowith and R. Marx and G. Maurin and N. Maxted and M. Mayer and McComb, {T. J L} and J. M{\'e}hault and Meintjes, {P. J.} and U. Menzler and M. Meyer and Mitchell, {A. M W} and R. Moderski and M. Mohamed and K. Mor{\aa} and E. Moulin and T. Murach and {De Naurois}, M. and J. Niemiec and Nolan, {S. J.} and L. Oakes and H. Odaka and S. Ohm and B. Opitz and M. Ostrowski and I. Oya and M. Panter and Parsons, {R. D.} and {Paz Arribas}, M. and Pekeur, {N. W.} and G. Pelletier and Petrucci, {P. O.} and B. Peyaud and S. Pita and H. Poon and G. P{\"u}hlhofer and M. Punch and A. Quirrenbach and S. Raab and I. Reichardt and A. Reimer and O. Reimer and M. Renaud and {De Los Reyes}, R. and F. Rieger and C. Romoli and S. Rosier-Lees and G. Rowell and B. Rudak and Rulten, {C. B.} and V. Sahakian and D. Salek and Sanchez, {D. A.} and A. Santangelo and R. Schlickeiser and F. Sch{\"u}ssler and A. Schulz and U. Schwanke and S. Schwarzburg and S. Schwemmer and H. Sol and F. Spanier and G. Spengler and F. Spies and Stawarz, {[No Value]} and R. Steenkamp and C. Stegmann and F. Stinzing and K. Stycz and I. Sushch and Tavernet, {J. P.} and T. Tavernier and Taylor, {A. M.} and R. Terrier and M. Tluczykont and C. Trichard and K. Valerius and {Van Eldik}, C. and {Van Soelen}, B. and G. Vasileiadis and J. Veh and C. Venter and A. Viana and P. Vincent and J. Vink and V{\"o}lk, {H. J.} and F. Volpe and M. Vorster and T. Vuillaume and Wagner, {S. J.} and P. Wagner and Wagner, {R. M.} and M. Ward and M. Weidinger and Q. Weitzel and R. White and A. Wierzcholska and P. Willmann and A. W{\"o}rnlein and D. Wouters and R. Yang and V. Zabalza and D. Zaborov and M. Zacharias and Zdziarski, {A. A.} and A. Zech and Zechlin, {H. S.}",

note = "Publisher Copyright: {\textcopyright} 2015 ESO.",

year = "2015",

month = mar,

day = "1",

doi = "10.1051/0004-6361/201424805",

language = "English (US)",

volume = "575",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

TY - JOUR

T1 - H.E.S.S. reveals a lack of TeV emission from the supernova remnant Puppis A

AU - Abramowski, A.

AU - Aharonian, F.

AU - Ait Benkhali, F.

AU - Akhperjanian, A. G.

AU - Angüner, E. O.

AU - Backes, M.

AU - Balenderan, S.

AU - Balzer, A.

AU - Barnacka, A.

AU - Becherini, Y.

AU - Becker Tjus, J.

AU - Berge, D.

AU - Bernhard, S.

AU - Bernlöhr, K.

AU - Birsin, E.

AU - Biteau, J.

AU - Böttcher, M.

AU - Boisson, C.

AU - Bolmont, J.

AU - Bordas, P.

AU - Bregeon, J.

AU - Brun, F.

AU - Brun, P.

AU - Bryan, M.

AU - Bulik, T.

AU - Carrigan, S.

AU - Casanova, S.

AU - Chadwick, P. M.

AU - Chakraborty, N.

AU - Chalme-Calvet, R.

AU - Chaves, R. C G

AU - Chrétien, M.

AU - Colafrancesco, S.

AU - Cologna, G.

AU - Conrad, J.

AU - Couturier, C.

AU - Cui, Y.

AU - Davids, I. D.

AU - Degrange, B.

AU - Deil, C.

AU - Dewilt, P.

AU - Djannati-Ataï, A.

AU - Domainko, W.

AU - Donath, A.

AU - Drury, L. O.

AU - Dubus, G.

AU - Dutson, K.

AU - Dyks, J.

AU - Dyrda, M.

AU - Edwards, T.

AU - Egberts, K.

AU - Eger, P.

AU - Espigat, P.

AU - Farnier, C.

AU - Fegan, S.

AU - Feinstein, F.

AU - Fernandes, M. V.

AU - Fernandez, D.

AU - Fiasson, A.

AU - Fontaine, G.

AU - Förster, A.

AU - Füßling, M.

AU - Gabici, S.

AU - Gajdus, M.

AU - Gallant, Y. A.

AU - Garrigoux, T.

AU - Giavitto, G.

AU - Giebels, B.

AU - Glicenstein, J. F.

AU - Gottschall, D.

AU - Grondin, M. H.

AU - Grudzińska, M.

AU - Hadasch, D.

AU - Häffner, S.

AU - Hahn, J.

AU - Harris, J.

AU - Heinzelmann, G.

AU - Henri, G.

AU - Hermann, G.

AU - Hervet, O.

AU - Hillert, A.

AU - Hinton, J. A.

AU - Hofmann, W.

AU - Hofverberg, P.

AU - Holler, M.

AU - Horns, D.

AU - Ivascenko, A.

AU - Jacholkowska, A.

AU - Jahn, C.

AU - Jamrozy, M.

AU - Janiak, M.

AU - Jankowsky, F.

AU - Jung-Richardt, I.

AU - Kastendieck, M. A.

AU - Katarzyński, K.

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PY - 2015/3/1

Y1 - 2015/3/1

N2 - Context. Puppis A is an interesting ∼4 kyr-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..100 GeV) γ-rays. An analysis of the Fermi-LAT data has shown extended HE γ-ray emission with a 0.2-100 GeV 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 100 GeV.Aims. Very-high-energy (VHE, E ≥ 0.1 TeV) γ-ray emission from Puppis A has been, for the first time, searched for with the High Energy Stereoscopic System (H.E.S.S.).Methods. 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.Results. 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 280 GeV, 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.

AB - Context. Puppis A is an interesting ∼4 kyr-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..100 GeV) γ-rays. An analysis of the Fermi-LAT data has shown extended HE γ-ray emission with a 0.2-100 GeV 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 100 GeV.Aims. Very-high-energy (VHE, E ≥ 0.1 TeV) γ-ray emission from Puppis A has been, for the first time, searched for with the High Energy Stereoscopic System (H.E.S.S.).Methods. 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.Results. 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 280 GeV, 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.

KW - Acceleration of particles

KW - Cosmic rays

KW - Gamma rays: ISM

KW - ISM: individual objects: Puppis A

KW - Radiation mechanisms: non-thermal

UR - http://www.scopus.com/inward/record.url?scp=84924069211&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84924069211&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201424805

DO - 10.1051/0004-6361/201424805

M3 - Article

AN - SCOPUS:84924069211

SN - 0004-6361

VL - 575

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A81

ER -

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

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