Interstellar gas towards CTB 37A and the TeV gamma-ray source HESS J1714-385

Maxted, N.; Rowell, G.; Dawson, B. R.; Burton, M. G.; Fukui, Y.; Walsh, A. J.; Kawamura, Akiko; Horachi, Hirotaka; Sano, Hidetoshi; Fukuda, Tatsuya

doi:10.1093/mnras/stt1159

Cited by 15 publications

(8 citation statements)

References 48 publications

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“…From velocity measurements of molecular clouds associated with the remnant, Reynoso & Mangum (2000) estimated the masses of individual clouds ranging froḿ 1.3 10 3  M and5.8 10 4 M e with H 2 densities between 150 cm −3 and 660 cm −3 assuming a distance of 11.3 kpc, which implies a size of the remnant close to 28 pc. Based on the CS(1-0) emission, Maxted et al (2013) obtained a density of 3 10 10 3 ( -) cm −3 and a mass of M 500 2300 ( -) ☉ , which is consistent with the estimation given by Reynoso & Mangum (2000). We will assume an effective density of 100 cm −3 for calculation of the γ-ray emission and a radius of 10 pc for estimation of the energy content in the magnetic field.…”

Section: Ctb 37asupporting

confidence: 82%

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 37asupporting

confidence: 82%

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

Zeng

Xin

Liu

et al. 2017

ApJ

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“…CTB 37A and G348.5−0.0 are both related to maser emission at about −65 and −22 km/s, respectively (Frail et al 1996). These systemic velocities for the two SNRs were confirmed by the detection of related CO(1-0) emission (Reynoso & Mangum 2000) and CO(2-1) and CS(1-0) emission (Maxted et al 2013) in the same velocity ranges. In the inner Galaxy, there is a distance ambiguity for negative radial velocities, but since we know that both SNRs are located beyond the tangent point, only the far distance is viable.…”

Section: Distance Estimatesupporting

confidence: 63%

X-ray and radio studies of SNR CTB 37B hosting the magnetar CXOU J171405.7−381031

Blumer

Safi‐Harb

Kothes

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a Chandra and XMM-Newton study of the supernova remnant (SNR) CTB 37B, along with archival radio observations. In radio wavelengths, the SNR CTB 37B is an incomplete shell showing bright emission from the eastern side while the Xray morphology shows diffuse emission from regions surrounding the magnetar CXOU J171405.7-381031. We used archival HI absorption measurements to constrain the distance to the remnant and obtain D = 9.8±1.5 kpc. The X-ray spectrum of the remnant is described by a thermal model in the 1-5 keV energy range, with a temperature of kT = 1.3±0.1 keV. The abundances from the spectral fits are consistent with being solar or sub-solar. A small region of diffuse emission is seen to the southern side of the remnant, best fitted by a nonthermal spectrum with an unusually hard photon index of Γ = 1.3±0.3. Assuming a distance of 9.8 kpc to the SNR, we infer a shock velocity of V s = 915±70 km s −1 and an explosion energy of E = (1.8±0.6)×10 50 ergs. The overall imaging and spectral properties of CTB 37B favor the interpretation of a young SNR ( 6200 yr old) propagating in a low-density medium, under the assumption of a Sedov evolutionary phase.

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“…This extended source is associated with the TeV emitting SNR CTB 37A (Aharonian et al 2008b, HESS J1714-385,) located at a distance of ∼ 13 kpc. The TeV emission is correlated with detected MCs (Maxted et al 2013) and could be associated with the non-thermal X-ray source CXOU J171419.8-383023. The detection of this SNR with Fermi-LAT in 2013 (Brandt et al 2013) in the GeV band is correlated with TeV and X-ray emissions, supporting the likely hypothesis of the presence of energised particles in the SNR shock with surrounding MCs.…”

Section: Supernova Remnantsmentioning

confidence: 67%

Second AGILE catalogue of gamma-ray sources

Bulgarelli

Fioretti

Parmiggiani

et al. 2019

A&A

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Aims. We present the second AGILE-GRID Catalog (2AGL) of γ-ray sources in the 100 MeV -10 GeV energy range. Methods. With respect to previous AGILE-GRID catalogs, the current 2AGL Catalog is based on the first 2.3 years of science data from the AGILE mission (the so called 'pointing mode') and incorporates more data and several analysis improvements, including better calibrations at the event reconstruction level, an updated model for the Galactic diffuse γ-ray emission, a refined procedure for point-like source detection, and the inclusion of a search for extended γ-ray sources.Results. The 2AGL Catalog includes 175 high-confidence sources (above 4σ significance) with their location regions and spectral properties, and a variability analysis with 4-day light curves for the most significant ones. Relying on the error region of each source position, including systematic uncertainties, 121 sources are considered as positionally associated with known couterparts at different wavelengths or detected by other γ-ray instruments. Among the identified or associated sources, 62 are Active Galactic Nuclei (AGNs) of the blazar class. Pulsars represent the largest Galactic source class, with 40 associated pulsars, 7 of them with detected pulsation; 8 Supernova Remnants and 4 high-mass X-ray binaries have also been identified. A substantial number of 2AGL sources are unidentified: for 54 sources no known counterpart is found at different wavelengths. Among these sources, we discuss a sub-class of 29 AGILE-GRID-only γ-ray sources that are not present in 1FGL, 2FGL or 3FGL catalogs; the remaining sources are unidentified in both 2AGL and 3FGL Catalogs. We also present an extension of the analysis of 2AGL sources detected in the 50 -100 MeV energy range.

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Interstellar gas towards CTB 37A and the TeV gamma-ray source HESS J1714-385

Cited by 15 publications

References 48 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

X-ray and radio studies of SNR CTB 37B hosting the magnetar CXOU J171405.7−381031

Second AGILE catalogue of gamma-ray sources

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