Chandra and HESS observations of the supernova remnant CTB 37B

Aharonian, F.; Akhperjanian, A. G.; Almeida, U. Barres de; Bazer‐Bachi, A. R.; Behera, B.; Beilicke, M.; Benbow, W.; Bernlöhr, K.; Boisson, C.; Borrel, V.; Braun, I.; Brion, E.; Brucker, J.; Bühler, R.; Bulik, T.; Büsching, I.; Boutelier, T.; Carrigan, S.; Chadwick, P. M.; Chaves, R. C. G.; Chounet, L.‐M.; Clapson, A. C.; Coignet, G.; Cornils, R.; Costamante, L.; Dalton, M.; Degrange, B.; Dickinson, H. J.; Djannati‐Ataï, A.; Domainko, W.; Drury, L. O’c.; Dubois, F.; Dubus, G.; Dyks, J.; Egberts, K.; Emmanoulopoulos, D.; Espigat, P.; Farnier, C.; Feinstein, F.; Fiaßon, A.; ̈orster, A. F; Fontaine, G.; Funk, S.; Füßling, M.; Gabici, S.; Gallant, Y. A.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Hadjichristidis, C.; Hauser, D.; Hauser, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Holleran, M.; Hoppe, S.; Horns, D.; Jachołkowska, A.; Jager, O. C. de; Jung, I.; Katarzyński, K.; Kaufmann, S.; Kendziorra, E.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Keogh, D.; Komin, Nu.; Kosack, K.; Lamanna, G.; Latham, I. J.; Lemoine‐Goumard, M.; Lenain, J.‐P.; Löhse, T.; Martin, Jean‐Michel; Martineau‐Huynh, O.; Marcowith, A.; Masterson, C.; Maurin, D.; McComb, T. J. L.; Moderski, R.; Moulin, Emmanuel; Naumann-Godó, M.; Naurois, M. de; Nedbal, D.; Nekrassov, D.; Nolan, S. J.; Ohm, S.; Olive, J.-P.; Oña-Wilhelmi, E.; Orford, K. J.; Osborne, J. L.; Ostrowski, M.; Panter, M.; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raubenheimer, Britt; Raue, M.; Rayner, S. M.; Renaud, M.; Rieger, F.; Reimer, O.; Ripken, J.; Rob, L.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Ruppel, J.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schröder, R.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Skilton, J. L.; Sol, H.; Spangler, D.; Stawarz,; Steenkamp, R.; Stegmann, C.; Superina, G.; Tam, P. H. T.; Tavernet, J.‐P.; Terrier, R.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Vialle, J. P.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Wagner, S. J.; Ward, M. J.; Zdziarski, A. A.; Zech, A.

doi:10.1051/0004-6361:200809655

Cited by 40 publications

(43 citation statements)

References 27 publications

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“…It is interesting to note that the GeV spectrum appears to have a peak near 10 GeV. The spectrum of the diffuse thermal X-ray emission implies a low density of ∼1 cm −3 and an age of ∼5000 years (Aharonian et al 2008b), which are consistent with a pre-shock electron density of 0.4±0.1 cm −3 estimated by Nakamura et al (2009) with a non-equilibrium collisional ionization model for Suzaku and Chandra observations. The distance to CTB 37B has been estimated to be 10.2±3.5 kpc by Caswell et al (1975), »8 kpc by Green (2009) and a large value of ∼13.2 kpc by Tian & Leahy (2012).…”

Section: Ctb 37bsupporting

confidence: 79%

Evolution of High-Energy Particle Distribution in Mature Shell-Type Supernova Remnants

Zeng

Xin

Liu

et al. 2017

ApJ

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Multi-wavelength observations of mature supernova remnants (SNRs), especially with recent advances in γ-ray astronomy, make it possible to constrain energy distribution of energetic particles within these remnants. In consideration of the SNR origin of Galactic cosmic rays and physics related to particle acceleration and radiative processes, we use a simple one-zone model to fit the nonthermal emission spectra of three shell-type SNRs located within 2°on the sky: RX J1713.7−3946, CTB 37B, and CTB 37A. Although radio images of these three sources all show a shell (or half-shell) structure, their radio, X-ray, and γ-ray spectra are quite different, offering an ideal case to explore evolution of energetic particle distribution in SNRs. Our spectral fitting shows that (1) the particle distribution becomes harder with aging of these SNRs, implying a continuous acceleration process, and the particle distributions of CTB 37A and CTB 37B in the GeV range are harder than the hardest distribution that can be produced at a shock via the linear diffusive shock particle acceleration process, so spatial transport may play a role; (2) the energy loss timescale of electrons at the high-energy cutoff due to synchrotron radiation appears to be always a bit (within a factor of a few) shorter than the age of the corresponding remnant, which also requires continuous particle acceleration; (3) double power-law distributions are needed to fit the spectra of CTB 37B and CTB 37A, which may be attributed to shock interaction with molecular clouds.

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Section: Ctb 37bsupporting

confidence: 79%

Evolution of High-Energy Particle Distribution in Mature Shell-Type Supernova Remnants

Zeng

Xin

Liu

et al. 2017

ApJ

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“…About half of them have been firmly identified as supernova remnants (SNRs) and pulsar wind nebulae (PWNe). However, there is still a significant fraction of VHE sources that has not been identified due to the lack of counterparts in the radio/X-ray or GeV γ-ray band (Aharonian et al 2005(Aharonian et al , 2008a. Therefore, searching for the counterparts of these unidentified VHE sources in longer wavelength bands is very helpful to identify and classify them.…”

Section: Introductionmentioning

confidence: 99%

HESS J1427−608: AN UNUSUAL HARD, UNBROKEN Γ-Ray SPECTRUM IN a VERY WIDE ENERGY RANGE

Guo

Xin

Liao

et al. 2017

ApJ

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We report the detection of a GeV γ-ray source which is spatially overlapping and thus very likely associated with the unidentified very-high-energy (VHE) γ-ray source HESS J1427-608 with the Pass 8 data recorded by the Fermi Large Area Telescope. The photon spectrum of this source is best described by a power-law with an index of 1.85 ± 0.17 in the energy range of 3 − 500 GeV, and the measured flux connects smoothly with that of HESS J1427-608 at a few hundred GeV. This source shows no significant extension and time variation. The broadband GeV-TeV emission over four decades of energies can be well fitted by a single power-law function with an index of 2.0, without obvious indication of spectral cutoff toward high energies. Such a result implies that HESS J1427-608 may be a PeV particle accelerator. We discuss possible nature of HESS J1427-608 according to the multi-wavelength spectral fittings. Given the relatively large errors, either a leptonic or a hadronic model can explain the multi-wavelength data from radio to VHE γ-rays. The inferred magnetic field strength is a few µG, which is smaller than typical values of supernova remnants (SNRs), and is consistent with some pulsar wind nebulae (PWNe). On the other hand, the flat γ-ray spectrum is slightly different from typical PWNe but similar to that of some known SNRs.

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“…The importance of a broadband approach using multiwavelength observations for understanding the γ-ray emission processes has been firmly demonstrated over the course of the last few years. Good examples of this class of studies performed especially in the radio and X-rays bands are those presented by Aharonian et al (2008), H.E.S.S. Collaboration et al (2011), Gotthelf et al (2014), on the γ-ray sources named HESS J1713−381 (linked to the supernova remnant (SNR) CTB 37B), HESS J1731−347 (in SNR G353.6−0.7), and HESS J1640−465 (in PSR J1640−4631, SNR G338.3−0.0), respectively.…”

Section: Introductionmentioning

confidence: 99%

Unveiling the origin of HESS J1809−193

Castelletti

Giacani

Petriella

2016

A&A

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Aims. The main goal of this paper is to provide new insights on the origin of the observable flux of γ rays from HESS J1809−193 using new high-quality observations in the radio domain. Methods. We used the Expanded Very Large Array (now known as the Karl G. Jansky Very large Array, JVLA) to produce a deep full-synthesis imaging at 1.4 GHz of the vicinity of PSR J1809−1917. These data were used in conjunction with 12 CO observations from the James Clerk Maxwell Telescope in the transition line J = 3−2 and atomic hydrogen data from the Southern Galactic Plane Survey to investigate the properties of the interstellar medium in the direction of the source HESS J1809−193. Results. The new radio continuum image, obtained with a synthesized beam of 8 × 4 and a sensitivity of 0.17 mJy beam −1 , reveals with unprecedented detail all the intensity structures in the field. No radio counterpart to the observed X-ray emission supposed to be a pulsar wind nebula powered by PSR J1809−1917 is seen in the new JVLA image. We discovered a system of molecular clouds on the edge of the supernova remnant (SNR) G11.0−0.0 shock front, which is positionally coincident with the brightest part of the TeV source HESS J1809−193. We determine, on the basis of kinematic and morphological evidences, a physical link of the SNR with the clouds for which we estimated a total (molecular plus atomic) mass of ∼3 × 10 3 M and a total proton density in the range 2-3 × 10 3 cm −3 . Conclusions. We propose as the most likely origin of the very high-energy γ-ray radiation from HESS J1809−193 a hadronic mechanism through collisions of ions accelerated at the SNR G11.0−0.0 shock with the molecular matter in the vicinity of the remnant.

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Chandra and HESS observations of the supernova remnant CTB 37B

Cited by 40 publications

References 27 publications

Evolution of High-Energy Particle Distribution in Mature Shell-Type Supernova Remnants

Evolution of High-Energy Particle Distribution in Mature Shell-Type Supernova Remnants

HESS J1427−608: AN UNUSUAL HARD, UNBROKEN Γ-Ray SPECTRUM IN a VERY WIDE ENERGY RANGE

Unveiling the origin of HESS J1809−193

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