A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7

F. A. Aharonian; A. G. Akhperjanian; A. R. Bazer-Bachi; M. Beilicke; W. Benbow; D. Berge; K. Bernlöhr; C. Boisson; O. Bolz; V. Borrel; I. Braun; F. Breitling; A. M. Brown; P. M. Chadwick; L. M. Chounet; R. Cornils; L. Costamante; B. Degrange; H. J. Dickinson; A. Djannati-Ataï; L. O C Drury; G. Dubus; D. Emmanoulopoulos; P. Espigat; F. Feinstein; G. Fontaine; Y. Fuchs; S. Funk; Y. A. Gallant; B. Giebels; S. Gillessen; J. F. Glicenstein; P. Goret; C. Hadjichristidis; M. Hauser; G. Heinzelmann; G. Henri; G. Hermann; J. A. Hinton; W. Hofmann; M. Holleran; D. Horns; A. Jacholkowska; O. C. de Jager; B. Khélifi; N. Komin; A. Konopelko; I. J. Latham; R. le Gallou; A. Lemière; M. Lemoine-Goumard; N. Leroy; T. Lohse; J. M. Martin; O. Martineau-Huynh; A. Marcowith; C. Masterson; T. J L McComb; M. de Naurois; S. J. Nolan; A. Noutsos; K. J. Orford; J. L. Osborne; M. Ouchrif; M. Panter; G. Pelletier; S. Pita; G. Pühlhofer; M. Punch; B. C. Raubenheimer; M. Raue; J. Raux; S. M. Rayner; A. Reimer; O. Reimer; J. Ripken; L. Rob; L. Rolland; G. Rowell; V. Sahakian; L. Saugé; S. Schlenker; R. Schlickeiser; C. Schuster; U. Schwanke; M. Siewert; H. Sol; D. Spangler; R. Steenkamp; C. Stegmann; J. P. Tavernet; R. Terrier; C. G. Théoret; M. Tluczykont; G. Vasileiadis; C. Venter; P. Vincent; H. J. Völk; S. J. Wagner

doi:10.1051/0004-6361:200500180

A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7

F. A. Aharonian, A. G. Akhperjanian, A. R. Bazer-Bachi, M. Beilicke, W. Benbow, D. Berge, K. Bernlöhr, C. Boisson, O. Bolz, V. Borrel, I. Braun, F. Breitling, A. M. Brown, P. M. Chadwick, L. M. Chounet, R. Cornils, L. Costamante, B. Degrange, H. J. Dickinson, A. Djannati-AtaïL. O C Drury, G. Dubus, D. Emmanoulopoulos, P. Espigat, F. Feinstein, G. Fontaine, Y. Fuchs, S. Funk, Y. A. Gallant, B. Giebels, S. Gillessen, J. F. Glicenstein, P. Goret, C. Hadjichristidis, M. Hauser, G. Heinzelmann, G. Henri, G. Hermann, J. A. Hinton, W. Hofmann, M. Holleran, D. Horns, A. Jacholkowska, O. C. de Jager, B. Khélifi, N. Komin, A. Konopelko, I. J. Latham, R. le Gallou, A. Lemière, M. Lemoine-Goumard, N. Leroy, T. Lohse, J. M. Martin, O. Martineau-Huynh, A. Marcowith, C. Masterson, T. J L McComb, M. de Naurois, S. J. Nolan, A. Noutsos, K. J. Orford, J. L. Osborne, M. Ouchrif, M. Panter, G. Pelletier, S. Pita, G. Pühlhofer, M. Punch, B. C. Raubenheimer, M. Raue, J. Raux, S. M. Rayner, A. Reimer, O. Reimer, J. Ripken, L. Rob, L. Rolland, G. Rowell, V. Sahakian, L. Saugé, S. Schlenker, R. Schlickeiser, C. Schuster, U. Schwanke, M. Siewert, H. Sol, D. Spangler, R. Steenkamp, C. Stegmann, J. P. Tavernet, R. Terrier, C. G. Théoret, M. Tluczykont, G. Vasileiadis, C. Venter, P. Vincent, H. J. Völk, S. J. Wagner

Physics and Astronomy (Twin Cities)

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Abstract

We report on a possible association of the recently discovered very high-energy γ-ray source HESS J1825-137 with the pulsar wind nebula (commonly referred to as G 18.0-0.7) of the 2.1 × 10 ⁴ year old Vela-like pulsar PSR B1823-13. HESS J1825-137 was detected with a significance of 8.1σ in the Galactic Plane survey conducted with the HESS instrument in 2004. The centroid position of HESS J1825-137 is offset by 11′ south of the pulsar position. XMM-Newton observations have revealed X-ray synchrotron emission of an asymmetric pulsar wind nebula extending to the south of the pulsar. We argue that the observed morphology and TeV spectral index suggest that HESS J1825-137 and G 18.0-0.7 may be associated: the lifetime of TeV emitting electrons is expected to be longer compared to the XMM-Newton X-ray emitting electrons, resulting in electrons from earlier epochs (when the spin-down power was larger) contributing to the present TeV flux. These electrons are expected to be synchrotron cooled, which explains the observed photon index of ∼2.4, and the longer lifetime of TeV emitting electrons naturally explains why the TeV nebula is larger than the X-ray size. Finally, supernova remnant expansion into an inhomogeneous medium is expected to create reverse shocks interacting at different times with the pulsar wind nebula, resulting in the offset X-ray and TeV γ-ray morphology.

Original language	English (US)
Pages (from-to)	L25-L29
Journal	Astronomy and Astrophysics
Volume	442
Issue number	3
DOIs	https://doi.org/10.1051/0004-6361:200500180
State	Published - Nov 2005

Keywords

Gamma-rays: observations
ISM: individual objects: PSR B1823-13, HESS J1825-137, G 18.0-0.7
ISM: plerions

Publisher link

10.1051/0004-6361:200500180

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Aharonian, F. A., Akhperjanian, A. G., Bazer-Bachi, A. R., Beilicke, M., Benbow, W., Berge, D., Bernlöhr, K., Boisson, C., Bolz, O., Borrel, V., Braun, I., Breitling, F., Brown, A. M., Chadwick, P. M., Chounet, L. M., Cornils, R., Costamante, L., Degrange, B., Dickinson, H. J., ... Wagner, S. J. (2005). A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7. Astronomy and Astrophysics, 442(3), L25-L29. https://doi.org/10.1051/0004-6361:200500180

Aharonian, FA, Akhperjanian, AG, Bazer-Bachi, AR, Beilicke, M, Benbow, W, Berge, D, Bernlöhr, K, Boisson, C, Bolz, O, Borrel, V, Braun, I, Breitling, F, Brown, AM, Chadwick, PM, Chounet, LM, Cornils, R, Costamante, L, Degrange, B, Dickinson, HJ, Djannati-Ataï, A, Drury, LOC, Dubus, G, Emmanoulopoulos, D, Espigat, P, Feinstein, F, Fontaine, G, Fuchs, Y, Funk, S, Gallant, YA, Giebels, B, Gillessen, S, Glicenstein, JF, Goret, P, Hadjichristidis, C, Hauser, M, Heinzelmann, G, Henri, G, Hermann, G, Hinton, JA, Hofmann, W, Holleran, M, Horns, D, Jacholkowska, A, de Jager, OC, Khélifi, B, Komin, N, Konopelko, A, Latham, IJ, le Gallou, R, Lemière, A, Lemoine-Goumard, M, Leroy, N, Lohse, T, Martin, JM, Martineau-Huynh, O, Marcowith, A, Masterson, C, McComb, TJL, de Naurois, M, Nolan, SJ, Noutsos, A, Orford, KJ, Osborne, JL, Ouchrif, M, Panter, M, Pelletier, G, Pita, S, Pühlhofer, G, Punch, M, Raubenheimer, BC, Raue, M, Raux, J, Rayner, SM, Reimer, A, Reimer, O, Ripken, J, Rob, L, Rolland, L, Rowell, G, Sahakian, V, Saugé, L, Schlenker, S, Schlickeiser, R, Schuster, C, Schwanke, U, Siewert, M, Sol, H, Spangler, D, Steenkamp, R, Stegmann, C, Tavernet, JP, Terrier, R, Théoret, CG, Tluczykont, M, Vasileiadis, G, Venter, C, Vincent, P, Völk, HJ & Wagner, SJ 2005, 'A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7', Astronomy and Astrophysics, vol. 442, no. 3, pp. L25-L29. https://doi.org/10.1051/0004-6361:200500180

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title = "A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7",

abstract = "We report on a possible association of the recently discovered very high-energy γ-ray source HESS J1825-137 with the pulsar wind nebula (commonly referred to as G 18.0-0.7) of the 2.1 × 10 4 year old Vela-like pulsar PSR B1823-13. HESS J1825-137 was detected with a significance of 8.1σ in the Galactic Plane survey conducted with the HESS instrument in 2004. The centroid position of HESS J1825-137 is offset by 11′ south of the pulsar position. XMM-Newton observations have revealed X-ray synchrotron emission of an asymmetric pulsar wind nebula extending to the south of the pulsar. We argue that the observed morphology and TeV spectral index suggest that HESS J1825-137 and G 18.0-0.7 may be associated: the lifetime of TeV emitting electrons is expected to be longer compared to the XMM-Newton X-ray emitting electrons, resulting in electrons from earlier epochs (when the spin-down power was larger) contributing to the present TeV flux. These electrons are expected to be synchrotron cooled, which explains the observed photon index of ∼2.4, and the longer lifetime of TeV emitting electrons naturally explains why the TeV nebula is larger than the X-ray size. Finally, supernova remnant expansion into an inhomogeneous medium is expected to create reverse shocks interacting at different times with the pulsar wind nebula, resulting in the offset X-ray and TeV γ-ray morphology.",

keywords = "Gamma-rays: observations, ISM: individual objects: PSR B1823-13, HESS J1825-137, G 18.0-0.7, ISM: plerions",

author = "Aharonian, {F. A.} and Akhperjanian, {A. G.} and Bazer-Bachi, {A. R.} 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 F. Breitling and Brown, {A. M.} and Chadwick, {P. M.} and Chounet, {L. M.} and R. Cornils and L. Costamante and B. Degrange and Dickinson, {H. J.} and A. Djannati-Ata{\"i} and Drury, {L. O C} and G. Dubus and D. Emmanoulopoulos and P. Espigat and F. Feinstein and G. Fontaine and Y. Fuchs and S. Funk and Gallant, {Y. A.} and B. Giebels and S. Gillessen and Glicenstein, {J. F.} and P. Goret and C. Hadjichristidis and M. Hauser and G. Heinzelmann and G. Henri and G. Hermann and Hinton, {J. A.} and W. Hofmann and M. Holleran and D. Horns and A. Jacholkowska and {de Jager}, {O. C.} and B. Kh{\'e}lifi and N. Komin and A. Konopelko and Latham, {I. J.} and {le Gallou}, R. and A. Lemi{\`e}re and M. Lemoine-Goumard and N. Leroy and T. Lohse and Martin, {J. M.} and O. Martineau-Huynh and A. Marcowith and C. Masterson and McComb, {T. J L} and {de Naurois}, M. and Nolan, {S. J.} and A. Noutsos and Orford, {K. J.} and Osborne, {J. L.} and M. Ouchrif and M. Panter and G. Pelletier and S. Pita and G. P{\"u}hlhofer and M. Punch and Raubenheimer, {B. C.} and M. Raue and J. Raux and Rayner, {S. M.} and A. Reimer and O. Reimer and J. Ripken and L. Rob and L. Rolland and G. Rowell and V. Sahakian and L. Saug{\'e} and S. Schlenker and R. Schlickeiser and C. Schuster and U. Schwanke and M. Siewert and H. Sol and D. Spangler and R. Steenkamp and C. Stegmann and Tavernet, {J. P.} and R. Terrier and Th{\'e}oret, {C. G.} and M. Tluczykont and G. Vasileiadis and C. Venter and P. Vincent and V{\"o}lk, {H. J.} and Wagner, {S. J.}",

year = "2005",

month = nov,

doi = "10.1051/0004-6361:200500180",

language = "English (US)",

volume = "442",

pages = "L25--L29",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "3",

}

TY - JOUR

T1 - A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7

AU - Aharonian, F. A.

AU - Akhperjanian, A. G.

AU - Bazer-Bachi, A. R.

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 - Breitling, F.

AU - Brown, A. M.

AU - Chadwick, P. M.

AU - Chounet, L. M.

AU - Cornils, R.

AU - Costamante, L.

AU - Degrange, B.

AU - Dickinson, H. J.

AU - Djannati-Ataï, A.

AU - Drury, L. O C

AU - Dubus, G.

AU - Emmanoulopoulos, D.

AU - Espigat, P.

AU - Feinstein, F.

AU - Fontaine, G.

AU - Fuchs, Y.

AU - Funk, S.

AU - Gallant, Y. A.

AU - Giebels, B.

AU - Gillessen, S.

AU - Glicenstein, J. F.

AU - Goret, P.

AU - Hadjichristidis, C.

AU - Hauser, M.

AU - Heinzelmann, G.

AU - Henri, G.

AU - Hermann, G.

AU - Hinton, J. A.

AU - Hofmann, W.

AU - Holleran, M.

AU - Horns, D.

AU - Jacholkowska, A.

AU - de Jager, O. C.

AU - Khélifi, B.

AU - Komin, N.

AU - Konopelko, A.

AU - Latham, I. J.

AU - le Gallou, R.

AU - Lemière, A.

AU - Lemoine-Goumard, M.

AU - Leroy, N.

AU - Lohse, T.

AU - Martin, J. M.

AU - Martineau-Huynh, O.

AU - Marcowith, A.

AU - Masterson, C.

AU - McComb, T. J L

AU - de Naurois, M.

AU - Nolan, S. J.

AU - Noutsos, A.

AU - Orford, K. J.

AU - Osborne, J. L.

AU - Ouchrif, M.

AU - Panter, M.

AU - Pelletier, G.

AU - Pita, S.

AU - Pühlhofer, G.

AU - Punch, M.

AU - Raubenheimer, B. C.

AU - Raue, M.

AU - Raux, J.

AU - Rayner, S. M.

AU - Reimer, A.

AU - Reimer, O.

AU - Ripken, J.

AU - Rob, L.

AU - Rolland, L.

AU - Rowell, G.

AU - Sahakian, V.

AU - Saugé, L.

AU - Schlenker, S.

AU - Schlickeiser, R.

AU - Schuster, C.

AU - Schwanke, U.

AU - Siewert, M.

AU - Sol, H.

AU - Spangler, D.

AU - Steenkamp, R.

AU - Stegmann, C.

AU - Tavernet, J. P.

AU - Terrier, R.

AU - Théoret, C. G.

AU - Tluczykont, M.

AU - Vasileiadis, G.

AU - Venter, C.

AU - Vincent, P.

AU - Völk, H. J.

AU - Wagner, S. J.

PY - 2005/11

Y1 - 2005/11

N2 - We report on a possible association of the recently discovered very high-energy γ-ray source HESS J1825-137 with the pulsar wind nebula (commonly referred to as G 18.0-0.7) of the 2.1 × 10 4 year old Vela-like pulsar PSR B1823-13. HESS J1825-137 was detected with a significance of 8.1σ in the Galactic Plane survey conducted with the HESS instrument in 2004. The centroid position of HESS J1825-137 is offset by 11′ south of the pulsar position. XMM-Newton observations have revealed X-ray synchrotron emission of an asymmetric pulsar wind nebula extending to the south of the pulsar. We argue that the observed morphology and TeV spectral index suggest that HESS J1825-137 and G 18.0-0.7 may be associated: the lifetime of TeV emitting electrons is expected to be longer compared to the XMM-Newton X-ray emitting electrons, resulting in electrons from earlier epochs (when the spin-down power was larger) contributing to the present TeV flux. These electrons are expected to be synchrotron cooled, which explains the observed photon index of ∼2.4, and the longer lifetime of TeV emitting electrons naturally explains why the TeV nebula is larger than the X-ray size. Finally, supernova remnant expansion into an inhomogeneous medium is expected to create reverse shocks interacting at different times with the pulsar wind nebula, resulting in the offset X-ray and TeV γ-ray morphology.

AB - We report on a possible association of the recently discovered very high-energy γ-ray source HESS J1825-137 with the pulsar wind nebula (commonly referred to as G 18.0-0.7) of the 2.1 × 10 4 year old Vela-like pulsar PSR B1823-13. HESS J1825-137 was detected with a significance of 8.1σ in the Galactic Plane survey conducted with the HESS instrument in 2004. The centroid position of HESS J1825-137 is offset by 11′ south of the pulsar position. XMM-Newton observations have revealed X-ray synchrotron emission of an asymmetric pulsar wind nebula extending to the south of the pulsar. We argue that the observed morphology and TeV spectral index suggest that HESS J1825-137 and G 18.0-0.7 may be associated: the lifetime of TeV emitting electrons is expected to be longer compared to the XMM-Newton X-ray emitting electrons, resulting in electrons from earlier epochs (when the spin-down power was larger) contributing to the present TeV flux. These electrons are expected to be synchrotron cooled, which explains the observed photon index of ∼2.4, and the longer lifetime of TeV emitting electrons naturally explains why the TeV nebula is larger than the X-ray size. Finally, supernova remnant expansion into an inhomogeneous medium is expected to create reverse shocks interacting at different times with the pulsar wind nebula, resulting in the offset X-ray and TeV γ-ray morphology.

KW - Gamma-rays: observations

KW - ISM: individual objects: PSR B1823-13, HESS J1825-137, G 18.0-0.7

KW - ISM: plerions

UR - http://www.scopus.com/inward/record.url?scp=27344446858&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=27344446858&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:200500180

DO - 10.1051/0004-6361:200500180

M3 - Article

AN - SCOPUS:27344446858

SN - 0004-6361

VL - 442

SP - L25-L29

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 3

ER -

A possible association of the new VHE γ-ray source HESS J1825-137 with the pulsar wind nebula G 18.0-0.7

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