H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud

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 C 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. Mora˚; 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:10.1051/0004-6361/201425070

H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud

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 C 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. Mora˚, 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

17 Scopus citations

Abstract

G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV < E < 100 GeV) γ-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E > 100 GeV) γ-ray emission coincident with this SNR with the High Energy Stereoscopic System (H.E.S.S.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F (E > 400 GeV) = (6.5 ± 1.1_stat ± 1.3_syst) × 10^-13 ph cm^-2 s^-1 corresponding to ∼0.7% of that of the Crab Nebula and to a luminosity of ∼10³⁴ erg s^-1 above the same energy threshold, and a steep photon index Γ_VHE = 2.8 ± 0.27stat ± 0.20_syst are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index Γ_HE = 2.2 ± 0.04_stat-0.31 ^+0.13 _sys. The combined γ-ray spectrum of G349.7+0.2 can be described by either a broken power-law (BPL) or a power-law with exponential (or sub-exponential) cutoff(PLC). In the former case, the photon break energy is found at E_br,γ = 55_-30 ⁺⁷⁰GeV, slightly higher than what is usually observed in the HE/VHE γ-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case, the exponential (respectively sub-exponential) cutoff energy is measured at E_cut,γ = 1.4_-0.55 ^+1.6 (respectively 0.35_-0.21 ^+0.75) TeV. A pion-decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the γ-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product of the average gas density and the total energy content of accelerated protons and nuclei amounts to n_H W_p ∼ 5 × 10⁵¹ erg cm^-3.

Original language	English (US)
Article number	A100
Journal	Astronomy and Astrophysics
Volume	574
DOIs	https://doi.org/10.1051/0004-6361/201425070
State	Published - Feb 1 2015

Bibliographical note

Funding Information:
Funded by contract ERC-StG-259391 from the European Community.

Funding Information:
The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment.

Publisher Copyright:
© ESO 2015.

Keywords

Gamma rays: General
ISM: clouds
ISM: supernova remnants

Publisher link

10.1051/0004-6361/201425070

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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. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud. Astronomy and Astrophysics, 574, Article A100. https://doi.org/10.1051/0004-6361/201425070

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, LOC, 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, Mora˚, 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. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud', Astronomy and Astrophysics, vol. 574, A100. https://doi.org/10.1051/0004-6361/201425070

@article{792b3674a8ac4b7bb412c7cabb5b4035,

title = "H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud",

abstract = "G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV < E < 100 GeV) γ-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E > 100 GeV) γ-ray emission coincident with this SNR with the High Energy Stereoscopic System (H.E.S.S.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F (E > 400 GeV) = (6.5 ± 1.1stat ± 1.3syst) × 10-13 ph cm-2 s-1 corresponding to ∼0.7% of that of the Crab Nebula and to a luminosity of ∼1034 erg s-1 above the same energy threshold, and a steep photon index ΓVHE = 2.8 ± 0.27stat ± 0.20syst are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index ΓHE = 2.2 ± 0.04stat-0.31 +0.13 sys. The combined γ-ray spectrum of G349.7+0.2 can be described by either a broken power-law (BPL) or a power-law with exponential (or sub-exponential) cutoff(PLC). In the former case, the photon break energy is found at Ebr,γ = 55-30 +70GeV, slightly higher than what is usually observed in the HE/VHE γ-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case, the exponential (respectively sub-exponential) cutoff energy is measured at Ecut,γ = 1.4-0.55 +1.6 (respectively 0.35-0.21 +0.75) TeV. A pion-decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the γ-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product of the average gas density and the total energy content of accelerated protons and nuclei amounts to nH Wp ∼ 5 × 1051 erg cm-3.",

keywords = "Gamma rays: General, ISM: clouds, ISM: supernova remnants",

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 C} 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. Mora˚ 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 = "Funding Information: Funded by contract ERC-StG-259391 from the European Community. Funding Information: The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment. Publisher Copyright: {\textcopyright} ESO 2015.",

year = "2015",

month = feb,

day = "1",

doi = "10.1051/0004-6361/201425070",

language = "English (US)",

volume = "574",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

TY - JOUR

T1 - H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud

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.

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N1 - Funding Information: Funded by contract ERC-StG-259391 from the European Community. Funding Information: The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the U.K. Science and Technology Facilities Council (STFC), the IPNP of the Charles University, the Czech Science Foundation, the Polish Ministry of Science and Higher Education, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment. Publisher Copyright: © ESO 2015.

PY - 2015/2/1

Y1 - 2015/2/1

N2 - G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV < E < 100 GeV) γ-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E > 100 GeV) γ-ray emission coincident with this SNR with the High Energy Stereoscopic System (H.E.S.S.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F (E > 400 GeV) = (6.5 ± 1.1stat ± 1.3syst) × 10-13 ph cm-2 s-1 corresponding to ∼0.7% of that of the Crab Nebula and to a luminosity of ∼1034 erg s-1 above the same energy threshold, and a steep photon index ΓVHE = 2.8 ± 0.27stat ± 0.20syst are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index ΓHE = 2.2 ± 0.04stat-0.31 +0.13 sys. The combined γ-ray spectrum of G349.7+0.2 can be described by either a broken power-law (BPL) or a power-law with exponential (or sub-exponential) cutoff(PLC). In the former case, the photon break energy is found at Ebr,γ = 55-30 +70GeV, slightly higher than what is usually observed in the HE/VHE γ-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case, the exponential (respectively sub-exponential) cutoff energy is measured at Ecut,γ = 1.4-0.55 +1.6 (respectively 0.35-0.21 +0.75) TeV. A pion-decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the γ-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product of the average gas density and the total energy content of accelerated protons and nuclei amounts to nH Wp ∼ 5 × 1051 erg cm-3.

AB - G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV < E < 100 GeV) γ-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E > 100 GeV) γ-ray emission coincident with this SNR with the High Energy Stereoscopic System (H.E.S.S.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F (E > 400 GeV) = (6.5 ± 1.1stat ± 1.3syst) × 10-13 ph cm-2 s-1 corresponding to ∼0.7% of that of the Crab Nebula and to a luminosity of ∼1034 erg s-1 above the same energy threshold, and a steep photon index ΓVHE = 2.8 ± 0.27stat ± 0.20syst are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index ΓHE = 2.2 ± 0.04stat-0.31 +0.13 sys. The combined γ-ray spectrum of G349.7+0.2 can be described by either a broken power-law (BPL) or a power-law with exponential (or sub-exponential) cutoff(PLC). In the former case, the photon break energy is found at Ebr,γ = 55-30 +70GeV, slightly higher than what is usually observed in the HE/VHE γ-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case, the exponential (respectively sub-exponential) cutoff energy is measured at Ecut,γ = 1.4-0.55 +1.6 (respectively 0.35-0.21 +0.75) TeV. A pion-decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the γ-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product of the average gas density and the total energy content of accelerated protons and nuclei amounts to nH Wp ∼ 5 × 1051 erg cm-3.

KW - Gamma rays: General

KW - ISM: clouds

KW - ISM: supernova remnants

UR - http://www.scopus.com/inward/record.url?scp=84961299965&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84961299965&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201425070

DO - 10.1051/0004-6361/201425070

M3 - Article

AN - SCOPUS:84961299965

SN - 0004-6361

VL - 574

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A100

ER -

H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud

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