Cavity of Molecular Gas Associated With Supernova Remnant 3c 397

Jiang, Bin; Chen, Yang; Wang, Junzhi; Su, Yang; Zhou, Xin; Safi‐Harb, Samar; DeLaney, Tracey

doi:10.1088/0004-637x/712/2/1147

Cited by 132 publications

(156 citation statements)

References 113 publications

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“…Although core-collapsed SNe are naturally associated with molecular cloud environments (see e.g. Jiang et al 2010, and reference therein), a SN Ia type origin cannot be excluded for Kes 69, since it has never been found to contain a compact remnant. According to the models of SN Ia nucleosynthesis developed by Maeda et al (2010), the yield of 48 Ti can exceed 10 −3 M in SN Ia ejecta.…”

Section: Interpretation As Ejecta Fragmentsmentioning

confidence: 99%

A population of isolated hard X-ray sources near the supernova remnant Kes 69

Bocchino¹,

Bykov²,

Chen³

et al. 2012

A&A

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Recent X-ray observations of the supernova remnant (SNR) IC 443 interacting with molecular clouds detected a new population of hard X-ray sources related to the remnant itself, which has been proposed to be fast ejecta fragments propagating within the dense environment. Encouraged by these studies, we obtained a deep XMM-Newton observation of the SNR Kes 69, which also shows signs of a shock-cloud interaction. We report on the detection of 18 hard X-ray sources in the field of Kes 69, which is a number sognificantly higher than expected for the Galactic source population in the field. The sources are spatially correlated with CO emission from the cloud in the remnant environment. The spectra of 3 of the 18 sources can be described as hard power-laws with photon indices smaller than two plus line emission associated with K-shell transitions. We discuss the two most promising scenarios for the interpretation of the sources, namely fast ejecta fragments (as in IC 443) and cataclysmic variables. While most of the observational evidence is consistent with the former interpretation, we cannot rule out the latter.

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Section: Interpretation As Ejecta Fragmentsmentioning

confidence: 99%

A population of isolated hard X-ray sources near the supernova remnant Kes 69

Bocchino¹,

Bykov²,

Chen³

et al. 2012

A&A

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“…The maximum value of R I CO(3−2) /I CO(2−1) is 1.6 in the molecular arc, which is higher than that in the previous measurement of individual Galactic MCs. A high value of R I CO(3−2) /I CO(2−1) has been proposed to be suggested as a signature of the SNR-MC interaction system (Jiang et al 2010;Xu et al 2011a). Together, these observations strongly indicate that the MCs are interacting with G59.5+0.1.…”

Section: Snr G595+01 and Mcsmentioning

confidence: 85%

“…These associations are established by the detection of OH 1720 MHz masers, the broad emission lines, the large ratio of 12 CO J = 2−1 to J = 1−0 integrated line intensity, γ-ray emission from MCs toward SNR, as well as the morphological relation between SNR and MCs, and so on (Frail et al 1996;Green et al 1997;Hartmann & Burton 1997;Seta et al 1998;Wilner et al 1998;Huang & Thaddeus 1986;Byun et al 2006;Hewitt & Yusef-Zadeh 2009). Jiang et al (2010) summarized the criteria of the SNR-MCs association. In addition, some results from numerical simulation speculated that star formation can be triggered by the SNR-MC interaction (Melioli et al 2006;Leao et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The open cluster NGC 6823 and possible triggered star formation associated with SNR G59.5+0.1

Xu¹,

Wang²

2012

A&A

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Aims. We investigate the environment in the vicinity of the supernova remnant (SNR) G59.5+0.1 and identify all the young stellar objects (YSOs) around the SNR, to derive the physical properties, obtain insight into the star-formation history, and determine whether SNR G59.5+0.1 can trigger star formation in this region. Methods. We perform the submillimeter/millimeter observations in CO lines toward the southeast of SNR G59.5+0.1 with the KOSMA 3 m Telescope. High values of the integrated CO line-intensity ratio R I CO(3−2) /I CO(2−1) is identified as one good signature of the SNR-MC (molecular cloud) interacting system. To investigate the impact of SNR G59.5+0.1 on the process of star formation, we use GLIMPSE I catalog to select YSOs (including Class I and Class II sources).Results. The CO emission forming an arc-like shape and mid-infrared 8.28 μm emission are coincident with SNR G59.5+0.1, which has a total mass of 1.1×10 4 M and fully covers the open cluster NGC 6823. Three molecular clumps are identified in the CO molecular arc, each clump tracing the broad-line wing emission, indicating that there are three outflows in motion. The integrated CO line intensity ratio (R I CO(3−2) /I CO(2−1) ) for the whole molecular arc is between 0.48 and 1.57. The maximum value is 1.57, which is much higher than previous measurements of individual Galactic MCs. The CO molecular arc has a line-intensity ratio gradient. The SNR G59.5+0.1 is in adiabatic expansion phase. The age of the SNR is 8.6 × 10 4 yr. Based on the GLIMPSE I catalog, we select 625 YSOs candidates (including 176 Class I sources and 449 Class II sources). The timescales for Class 0, Class I and Class II sources are ≤10 4 yr, ∼10 5 yr, and ∼10 6 yr, respectively. The number of YSOs are significantly enhanced in the interacting regions, indicating the presence of some recently formed stars.

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“…Such a spectrum can be interpreted as the emission from accelerated particles at the SNR shock, the cutoff being due to either escape of the highest energy particles or limitation of the acceleration because of the SNR age or radiative losses (for leptons) (Aharonian et al 2007). On the other hand, γ-ray broken power-law spectra with E br,γ ∼ 1−20 GeV have been observed in several SNRs known to be interacting with MCs (see Jiang et al 2010, and references therein), such as W28 (Aharonian et al 2008;Abdo et al 2010a), W51C Aleksić et al 2012), W49B (Abdo et al 2010c;Brun et al 2011), IC 443 (Acciari et al 2009Ackermann et al 2013) or W41 (Aharonian et al 2006b;Castro et al 2013). The CR spectral shape (broken power-law and exponential cutoff power-law) underlying this γ-ray spectrum will be investigated in the following sections in view of the γ-ray emission scenarios.…”

Section: Combined Analysismentioning

confidence: 99%

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

Abramowski¹,

Aharonian²,

Benkhali³

et al. 2015

A&A

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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 ∼10 34 erg s −1 above the same energy threshold, and a steep photon index Γ VHE = 2.8 ± 0.27 stat ± 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 +0.13 −0.31 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 +70 −30 GeV, 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 +1.6 −0.55 (respectively 0.35 +0.75 −0.21 ) 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 × 10 51 erg cm −3 .

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Cavity of Molecular Gas Associated With Supernova Remnant 3c 397

Cited by 132 publications

References 113 publications

A population of isolated hard X-ray sources near the supernova remnant Kes 69

A population of isolated hard X-ray sources near the supernova remnant Kes 69

The open cluster NGC 6823 and possible triggered star formation associated with SNR G59.5+0.1

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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