HESS upper limits for Kepler's supernova remnant

F. Aharonian; A. G. Akhperjanian; U. Barres De Almeida; A. R. Bazer-Bachi; B. Behera; M. Beilicke; W. Benbow; D. Berge; K. Bernlöhr; C. Boisson; O. Bolz; V. Borrel; I. Braun; E. Brion; J. Brucker; R. Bühler; T. Bulik; I. Büsching; T. Boutelier; S. Carrigan; P. M. Chadwick; L. M. Chounet; A. C. Clapson; G. Coignet; R. Cornils; L. Costamante; M. Dalton; B. Degrange; H. J. Dickinson; A. Djannati-Ataï; W. Domainko; L. O.C. Drury; F. Dubois; G. Dubus; J. Dyks; K. Egberts; D. Emmanoulopoulos; P. Espigat; C. Farnier; F. Feinstein; A. Fiasson; A. Förster; G. Fontaine; M. Füßling; Y. A. Gallant; B. Giebels; J. F. Glicenstein; B. Glück; P. Goret; C. Hadjichristidis; D. Hauser; M. Hauser; G. Heinzelmann; G. Henri; G. Hermann; J. A. Hinton; A. Hoffmann; W. Hofmann; M. Holleran; S. Hoppe; D. Horns; A. Jacholkowska; O. C. De Jager; I. Jung; K. Katarzyński; E. Kendziorra; M. Kerschhaggl; B. Khélifi; D. Keogh; Nu Komin; K. Kosack; G. Lamanna; I. J. Latham; M. Lemoine-Goumard; J. P. Lenain; T. Lohse; J. M. Martin; O. Martineau-Huynh; A. Marcowith; C. Masterson; D. Maurin; T. J.L. McComb; R. Moderski; E. Moulin; M. Naumann-Godo; M. De Naurois; D. Nedbal; D. Nekrassov; S. J. Nolan; S. Ohm; J. P. Olive; E. De Oña Wilhelmi; K. J. Orford; J. L. Osborne; M. Ostrowski; M. Panter; G. Pedaletti; G. Pelletier; P. O. Petrucci; S. Pita; G. Pühlhofer; M. Punch; A. Quirrenbach; B. C. Raubenheimer; M. Raue; S. M. Rayner; M. Renaud; J. Ripken; L. Rob; S. Rosier-Lees; G. Rowell; B. Rudak; J. Ruppel; V. Sahakian; A. Santangelo; R. Schlickeiser; F. M. Schöck; R. Schröder; U. Schwanke; S. Schwarzburg; S. Schwemmer; A. Shalchi; H. Sol; D. Spangler; Stawarz; R. Steenkamp; C. Stegmann; G. Superina; P. H. Tam; J. P. Tavernet; R. Terrier; C. Van Eldik; G. Vasileiadis; C. Venter; J. P. Vialle; P. Vincent; M. Vivier; H. J. Völk; F. Volpe; S. J. Wagner; M. Ward; A. A. Zdziarski; A. Zech

doi:10.1051/0004-6361:200809401

HESS upper limits for Kepler's supernova remnant

F. Aharonian
, A. G. Akhperjanian
, U. Barres De Almeida
, A. R. Bazer-Bachi
, B. Behera
, M. Beilicke
, W. Benbow
, D. Berge
, K. Bernlöhr
, C. Boisson
, O. Bolz
, V. Borrel
, I. Braun
, E. Brion
, J. Brucker
, R. Bühler
, T. Bulik
, I. Büsching
, T. Boutelier
, S. Carrigan

P. M. Chadwick, L. M. Chounet, A. C. Clapson, G. Coignet, R. Cornils, L. Costamante, M. Dalton, B. Degrange, H. J. Dickinson, A. Djannati-Ataï, W. Domainko, L. O.C. Drury, F. Dubois, G. Dubus, J. Dyks, K. Egberts, D. Emmanoulopoulos, P. Espigat, C. Farnier, F. Feinstein, A. Fiasson, A. Förster, G. Fontaine, M. Füßling, Y. A. Gallant, B. Giebels, J. F. Glicenstein, B. Glück, P. Goret, C. Hadjichristidis, D. Hauser, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, A. Hoffmann, W. Hofmann, M. Holleran, S. Hoppe, D. Horns, A. Jacholkowska, O. C. De Jager, I. Jung, K. Katarzyński, E. Kendziorra, M. Kerschhaggl, B. Khélifi, D. Keogh, Nu Komin, K. Kosack, G. Lamanna, I. J. Latham, M. Lemoine-Goumard, J. P. Lenain, T. Lohse, J. M. Martin, O. Martineau-Huynh, A. Marcowith, C. Masterson, D. Maurin, T. J.L. McComb, R. Moderski, E. Moulin, M. Naumann-Godo, M. De Naurois, D. Nedbal, D. Nekrassov, S. J. Nolan, S. Ohm, J. P. Olive, E. De Oña Wilhelmi, K. J. Orford, J. L. Osborne, M. Ostrowski, M. Panter, G. Pedaletti, G. Pelletier, P. O. Petrucci, S. Pita, G. Pühlhofer, M. Punch, A. Quirrenbach, B. C. Raubenheimer, M. Raue, S. M. Rayner, M. Renaud, J. Ripken, L. Rob, S. Rosier-Lees, G. Rowell, B. Rudak, J. Ruppel, V. Sahakian, A. Santangelo, R. Schlickeiser, F. M. Schöck, R. Schröder, U. Schwanke, S. Schwarzburg, S. Schwemmer, A. Shalchi, H. Sol, D. Spangler, Stawarz, R. Steenkamp, C. Stegmann, G. Superina, P. H. Tam, J. P. Tavernet, R. Terrier, C. Van Eldik, G. Vasileiadis, C. Venter, J. P. Vialle, P. Vincent, M. Vivier, H. J. Völk, F. Volpe, S. J. Wagner, M. Ward, A. A. Zdziarski, A. Zech

Max-Planck-Institut für Kernphysik
Dublin Institute for Advanced Studies
Yerevan Physics Institute
Durham University
CAPES Foundation
Centre national de la recherche scientifique
Landessternwarte Heidelberg
Universität Hamburg
European Organization for Nuclear Research
Institut für Physik
Humboldt-Universität zu Berlin
LUTH - Laboratoire de l'Univers et de ses Theories
Universite Paris-Saclay
Physikalisches Institut
Friedrich-Alexander University (FAU) Erlangen-Nürnberg and Universitätsklinikum Erlangen
Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
Unit for Space Physics
North-West University
Université Paris-Sud
European Associated Laboratory for Gamma-Ray Astronomy
Astroparticule and Cosmol APC
Laboratoire Univers et Particules de Montpellier
School of Physics and Astronomy
University of Leeds
Institut für Astronomie und Astrophysik
University of Tübingen
Toruń Centre for Astronomy
Nicolaus Copernicus University
UMR 5797
Universités Paris VI and VII
Charles University
Obserwatorium Astronomiczne
Jagiellonian University
University of Adelaide
Institut für Theoretische Physik
Ruhr-University Bochum
University of Namibia

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

29 Citations (Scopus)

Abstract

Aims. Observations of Kepler's supernova remnant (G4.5+6.8) with the HESS telescope array in 2004 and 2005 with a total live time of 13 h are presented.Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays.Results. No evidence for a very high energy (VHE: $]]>100 GeV) gamma-ray signal from the direction of the remnant is found. An upper limit (99% confidence level) on the energy flux in the range of is obtained.Conclusions. In the context of an existing theoretical model for the remnant, the lack of a detectable gamma-ray flux implies a distance of at least . A corresponding upper limit for the density of the ambient matter of is derived. With this distance limit, and assuming a spectral index , the total energy in accelerated protons is limited to . In the synchrotron/inverse Compton framework, extrapolating the power law measured by RXTE between and down in energy, the predicted gamma-ray flux from inverse Compton scattering is below the measured upper limit for magnetic field values greater than .

Original language	English
Pages (from-to)	219-223
Number of pages	5
Journal	Astronomy and Astrophysics
Volume	488
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361:200809401
Publication status	Published - 1 Jan 2008
Externally published	Yes

Keywords

Gamma rays: observations
ISM: individual objects: Kepler's SNR, SN1604, G4.5+6.8
ISM: supernova remnants

Access to Document

10.1051/0004-6361:200809401

Cite this

Aharonian, F., Akhperjanian, A. G., Barres De Almeida, U., Bazer-Bachi, A. R., Behera, B., Beilicke, M., Benbow, W., Berge, D., Bernlöhr, K., Boisson, C., Bolz, O., Borrel, V., Braun, I., Brion, E., Brucker, J., Bühler, R., Bulik, T., Büsching, I., Boutelier, T., ... Zech, A. (2008). HESS upper limits for Kepler's supernova remnant. Astronomy and Astrophysics, 488(1), 219-223. https://doi.org/10.1051/0004-6361:200809401

@article{61d76d3065d945a69bd20589569703e3,

title = "HESS upper limits for Kepler's supernova remnant",

abstract = "Aims. Observations of Kepler's supernova remnant (G4.5+6.8) with the HESS telescope array in 2004 and 2005 with a total live time of 13 h are presented.Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays.Results. No evidence for a very high energy (VHE: \$]]>100 GeV) gamma-ray signal from the direction of the remnant is found. An upper limit (99\% confidence level) on the energy flux in the range of is obtained.Conclusions. In the context of an existing theoretical model for the remnant, the lack of a detectable gamma-ray flux implies a distance of at least . A corresponding upper limit for the density of the ambient matter of is derived. With this distance limit, and assuming a spectral index , the total energy in accelerated protons is limited to . In the synchrotron/inverse Compton framework, extrapolating the power law measured by RXTE between and down in energy, the predicted gamma-ray flux from inverse Compton scattering is below the measured upper limit for magnetic field values greater than .",

keywords = "Gamma rays: observations, ISM: individual objects: Kepler's SNR, SN1604, G4.5+6.8, ISM: supernova remnants",

author = "F. Aharonian and Akhperjanian, \{A. G.\} and \{Barres De Almeida\}, U. and Bazer-Bachi, \{A. R.\} and B. Behera and M. Beilicke and W. Benbow and D. Berge and K. Bernl{\"o}hr and C. Boisson and O. Bolz and V. Borrel and I. Braun and E. Brion and J. Brucker and R. B{\"u}hler and T. Bulik and I. B{\"u}sching and T. Boutelier and S. Carrigan and Chadwick, \{P. M.\} and Chounet, \{L. M.\} and Clapson, \{A. C.\} and G. Coignet and R. Cornils and L. Costamante and M. Dalton and B. Degrange and Dickinson, \{H. J.\} and A. Djannati-Ata{\"i} and W. Domainko and Drury, \{L. O.C.\} and F. Dubois and G. Dubus and J. Dyks and K. Egberts and D. Emmanoulopoulos and P. Espigat and C. Farnier and F. Feinstein and A. Fiasson and A. F{\"o}rster and G. Fontaine and M. F{\"u}{\ss}ling and Gallant, \{Y. A.\} and B. Giebels and Glicenstein, \{J. F.\} and B. Gl{\"u}ck and P. Goret and C. Hadjichristidis and D. Hauser and M. Hauser and G. Heinzelmann and G. Henri and G. Hermann and Hinton, \{J. A.\} and A. Hoffmann and W. Hofmann and M. Holleran and S. Hoppe and D. Horns and A. Jacholkowska and \{De Jager\}, \{O. C.\} and I. Jung and K. Katarzy{\'n}ski and E. Kendziorra and M. Kerschhaggl and B. Kh{\'e}lifi and D. Keogh and Nu Komin and K. Kosack and G. Lamanna and Latham, \{I. J.\} and M. Lemoine-Goumard and Lenain, \{J. P.\} and T. Lohse and Martin, \{J. M.\} and O. Martineau-Huynh and A. Marcowith and C. Masterson and D. Maurin and McComb, \{T. J.L.\} and R. Moderski and E. Moulin and M. Naumann-Godo and \{De Naurois\}, M. and D. Nedbal and D. Nekrassov and Nolan, \{S. J.\} and S. Ohm and Olive, \{J. P.\} and \{De O{\~n}a Wilhelmi\}, E. and Orford, \{K. J.\} and Osborne, \{J. L.\} and M. Ostrowski and M. Panter and G. Pedaletti and G. Pelletier and Petrucci, \{P. O.\} and S. Pita and G. P{\"u}hlhofer and M. Punch and A. Quirrenbach and Raubenheimer, \{B. C.\} and M. Raue and Rayner, \{S. M.\} and M. Renaud and J. Ripken and L. Rob and S. Rosier-Lees and G. Rowell and B. Rudak and J. Ruppel and V. Sahakian and A. Santangelo and R. Schlickeiser and Sch{\"o}ck, \{F. M.\} and R. Schr{\"o}der and U. Schwanke and S. Schwarzburg and S. Schwemmer and A. Shalchi and H. Sol and D. Spangler and Stawarz and R. Steenkamp and C. Stegmann and G. Superina and Tam, \{P. H.\} and Tavernet, \{J. P.\} and R. Terrier and \{Van Eldik\}, C. and G. Vasileiadis and C. Venter and Vialle, \{J. P.\} and P. Vincent and M. Vivier and V{\"o}lk, \{H. J.\} and F. Volpe and Wagner, \{S. J.\} and M. Ward and Zdziarski, \{A. A.\} and A. Zech",

year = "2008",

month = jan,

day = "1",

doi = "10.1051/0004-6361:200809401",

language = "English",

volume = "488",

pages = "219--223",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "1",

}

Aharonian, F, Akhperjanian, AG, Barres De Almeida, U, Bazer-Bachi, AR, Behera, B, Beilicke, M, Benbow, W, Berge, D, Bernlöhr, K, Boisson, C, Bolz, O, Borrel, V, Braun, I, Brion, E, Brucker, J, Bühler, R, Bulik, T, Büsching, I, Boutelier, T, Carrigan, S, Chadwick, PM, Chounet, LM, Clapson, AC, Coignet, G, Cornils, R, Costamante, L, Dalton, M, Degrange, B, Dickinson, HJ, Djannati-Ataï, A, Domainko, W, Drury, LOC, Dubois, F, Dubus, G, Dyks, J, Egberts, K, Emmanoulopoulos, D, Espigat, P, Farnier, C, Feinstein, F, Fiasson, A, Förster, A, Fontaine, G, Füßling, M, Gallant, YA, Giebels, B, Glicenstein, JF, Glück, B, Goret, P, Hadjichristidis, C, Hauser, D, Hauser, M, Heinzelmann, G, Henri, G, Hermann, G, Hinton, JA, Hoffmann, A, Hofmann, W, Holleran, M, Hoppe, S, Horns, D, Jacholkowska, A, De Jager, OC, Jung, I, Katarzyński, K, Kendziorra, E, Kerschhaggl, M, Khélifi, B, Keogh, D, Komin, N, Kosack, K, Lamanna, G, Latham, IJ, Lemoine-Goumard, M, Lenain, JP, Lohse, T, Martin, JM, Martineau-Huynh, O, Marcowith, A, Masterson, C, Maurin, D, McComb, TJL, Moderski, R, Moulin, E, Naumann-Godo, M, De Naurois, M, Nedbal, D, Nekrassov, D, Nolan, SJ, Ohm, S, Olive, JP, De Oña Wilhelmi, E, Orford, KJ, Osborne, JL, Ostrowski, M, Panter, M, Pedaletti, G, Pelletier, G, Petrucci, PO, Pita, S, Pühlhofer, G, Punch, M, Quirrenbach, A, Raubenheimer, BC, Raue, M, Rayner, SM, Renaud, M, Ripken, J, Rob, L, Rosier-Lees, S, Rowell, G, Rudak, B, Ruppel, J, Sahakian, V, Santangelo, A, Schlickeiser, R, Schöck, FM, Schröder, R, Schwanke, U, Schwarzburg, S, Schwemmer, S, Shalchi, A, Sol, H, Spangler, D, Stawarz, Steenkamp, R, Stegmann, C, Superina, G, Tam, PH, Tavernet, JP, Terrier, R, Van Eldik, C, Vasileiadis, G, Venter, C, Vialle, JP, Vincent, P, Vivier, M, Völk, HJ, Volpe, F, Wagner, SJ, Ward, M, Zdziarski, AA & Zech, A 2008, 'HESS upper limits for Kepler's supernova remnant', Astronomy and Astrophysics, vol. 488, no. 1, pp. 219-223. https://doi.org/10.1051/0004-6361:200809401

TY - JOUR

T1 - HESS upper limits for Kepler's supernova remnant

AU - Aharonian, F.

AU - Akhperjanian, A. G.

AU - Barres De Almeida, U.

AU - Bazer-Bachi, A. R.

AU - Behera, B.

AU - Beilicke, M.

AU - Benbow, W.

AU - Berge, D.

AU - Bernlöhr, K.

AU - Boisson, C.

AU - Bolz, O.

AU - Borrel, V.

AU - Braun, I.

AU - Brion, E.

AU - Brucker, J.

AU - Bühler, R.

AU - Bulik, T.

AU - Büsching, I.

AU - Boutelier, T.

AU - Carrigan, S.

AU - Chadwick, P. M.

AU - Chounet, L. M.

AU - Clapson, A. C.

AU - Coignet, G.

AU - Cornils, R.

AU - Costamante, L.

AU - Dalton, M.

AU - Degrange, B.

AU - Dickinson, H. J.

AU - Djannati-Ataï, A.

AU - Domainko, W.

AU - Drury, L. O.C.

AU - Dubois, F.

AU - Dubus, G.

AU - Dyks, J.

AU - Egberts, K.

AU - Emmanoulopoulos, D.

AU - Espigat, P.

AU - Farnier, C.

AU - Feinstein, F.

AU - Fiasson, A.

AU - Förster, A.

AU - Fontaine, G.

AU - Füßling, M.

AU - Gallant, Y. A.

AU - Giebels, B.

AU - Glicenstein, J. F.

AU - Glück, B.

AU - Goret, P.

AU - Hadjichristidis, C.

AU - Hauser, D.

AU - Hauser, M.

AU - Heinzelmann, G.

AU - Henri, G.

AU - Hermann, G.

AU - Hinton, J. A.

AU - Hoffmann, A.

AU - Hofmann, W.

AU - Holleran, M.

AU - Hoppe, S.

AU - Horns, D.

AU - Jacholkowska, A.

AU - De Jager, O. C.

AU - Jung, I.

AU - Katarzyński, K.

AU - Kendziorra, E.

AU - Kerschhaggl, M.

AU - Khélifi, B.

AU - Keogh, D.

AU - Komin, Nu

AU - Kosack, K.

AU - Lamanna, G.

AU - Latham, I. J.

AU - Lemoine-Goumard, M.

AU - Lenain, J. P.

AU - Lohse, T.

AU - Martin, J. M.

AU - Martineau-Huynh, O.

AU - Marcowith, A.

AU - Masterson, C.

AU - Maurin, D.

AU - McComb, T. J.L.

AU - Moderski, R.

AU - Moulin, E.

AU - Naumann-Godo, M.

AU - De Naurois, M.

AU - Nedbal, D.

AU - Nekrassov, D.

AU - Nolan, S. J.

AU - Ohm, S.

AU - Olive, J. P.

AU - De Oña Wilhelmi, E.

AU - Orford, K. J.

AU - Osborne, J. L.

AU - Ostrowski, M.

AU - Panter, M.

AU - Pedaletti, G.

AU - Pelletier, G.

AU - Petrucci, P. O.

AU - Pita, S.

AU - Pühlhofer, G.

AU - Punch, M.

AU - Quirrenbach, A.

AU - Raubenheimer, B. C.

AU - Raue, M.

AU - Rayner, S. M.

AU - Renaud, M.

AU - Ripken, J.

AU - Rob, L.

AU - Rosier-Lees, S.

AU - Rowell, G.

AU - Rudak, B.

AU - Ruppel, J.

AU - Sahakian, V.

AU - Santangelo, A.

AU - Schlickeiser, R.

AU - Schöck, F. M.

AU - Schröder, R.

AU - Schwanke, U.

AU - Schwarzburg, S.

AU - Schwemmer, S.

AU - Shalchi, A.

AU - Sol, H.

AU - Spangler, D.

AU - Stawarz,

AU - Steenkamp, R.

AU - Stegmann, C.

AU - Superina, G.

AU - Tam, P. H.

AU - Tavernet, J. P.

AU - Terrier, R.

AU - Van Eldik, C.

AU - Vasileiadis, G.

AU - Venter, C.

AU - Vialle, J. P.

AU - Vincent, P.

AU - Vivier, M.

AU - Völk, H. J.

AU - Volpe, F.

AU - Wagner, S. J.

AU - Ward, M.

AU - Zdziarski, A. A.

AU - Zech, A.

PY - 2008/1/1

Y1 - 2008/1/1

N2 - Aims. Observations of Kepler's supernova remnant (G4.5+6.8) with the HESS telescope array in 2004 and 2005 with a total live time of 13 h are presented.Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays.Results. No evidence for a very high energy (VHE: $]]>100 GeV) gamma-ray signal from the direction of the remnant is found. An upper limit (99% confidence level) on the energy flux in the range of is obtained.Conclusions. In the context of an existing theoretical model for the remnant, the lack of a detectable gamma-ray flux implies a distance of at least . A corresponding upper limit for the density of the ambient matter of is derived. With this distance limit, and assuming a spectral index , the total energy in accelerated protons is limited to . In the synchrotron/inverse Compton framework, extrapolating the power law measured by RXTE between and down in energy, the predicted gamma-ray flux from inverse Compton scattering is below the measured upper limit for magnetic field values greater than .

AB - Aims. Observations of Kepler's supernova remnant (G4.5+6.8) with the HESS telescope array in 2004 and 2005 with a total live time of 13 h are presented.Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the energy and direction of the incident gamma rays.Results. No evidence for a very high energy (VHE: $]]>100 GeV) gamma-ray signal from the direction of the remnant is found. An upper limit (99% confidence level) on the energy flux in the range of is obtained.Conclusions. In the context of an existing theoretical model for the remnant, the lack of a detectable gamma-ray flux implies a distance of at least . A corresponding upper limit for the density of the ambient matter of is derived. With this distance limit, and assuming a spectral index , the total energy in accelerated protons is limited to . In the synchrotron/inverse Compton framework, extrapolating the power law measured by RXTE between and down in energy, the predicted gamma-ray flux from inverse Compton scattering is below the measured upper limit for magnetic field values greater than .

KW - Gamma rays: observations

KW - ISM: individual objects: Kepler's SNR, SN1604, G4.5+6.8

KW - ISM: supernova remnants

U2 - 10.1051/0004-6361:200809401

DO - 10.1051/0004-6361:200809401

M3 - Article

AN - SCOPUS:49749130020

SN - 0004-6361

VL - 488

SP - 219

EP - 223

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 1

ER -

HESS upper limits for Kepler's supernova remnant

Abstract

Keywords

Access to Document

Fingerprint

Cite this