Nonthermal X‐Ray Emission from the Shell‐Type Supernova Remnant G347.3−0.5

Slane, Patrick; Gaensler, B. M.; Dame, T. M.; Hughes, John P.; Plucinsky, Paul P.; Green, Anne

doi:10.1086/307893

Cited by 280 publications

(440 citation statements)

References 42 publications

Supporting

Mentioning

400

Contrasting

Order By: Relevance

“…G347.3À0.5 (RX J1713.7À3946) was first discovered in the ROSAT (Röntgensatellit) All-Sky Survey by Pfeffermann & Aschenbach (1996). Later, ASCA (Advanced Satellite for Cosmology and Astrophysics) observations revealed that the X-ray emission from the remnant is predominantly nonthermal (Koyama et al 1997;Slane et al 1999). The remnant is $1 in diameter and appears to be of a shell-type morphology with the brightest emission in the western region (we use equatorial coordinates to identify directions in the sky throughout this paper).…”

Section: Introductionmentioning

confidence: 99%

“…Originally, Pfeffermann & Aschenbach (1996) adopted a distance to the SNR of $1 kpc based on the estimate of the column density derived from the spectral analysis of the ASCA data (see also Koyama et al 1997). Later, the possible association of a molecular cloud (later referred to as ''cloud A'') was used to derive a distance of 6:3 AE 0:4 kpc from observations of the 2.6 mm CO (J ¼ 1 0) line emission at 9 0 resolution by Slane et al (1999). In their discussion, these authors argued that an enhanced value of the CO (J ¼ 2 1)/(J ¼ 1 0) line ratio in cloud A indicates the physical interaction with the SNR shock (see also Butt et al 2001).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

Moriguchi

Tamura

Tawara

et al. 2005

ApJ

108

134

View full text Add to dashboard Cite

The supernova remnant G347.3À0.5 (J1713.7À3946) is known as one of the unique SNRs that emit TeV -rays, as well as nonthermal X-rays. We present a detailed study of molecular gas toward this SNR obtained with the 4 m millimeter and submillimeter telescope NANTEN at an angular resolution of 2A6. This study has revealed that several intensity peaks and the overall distribution of the molecular gas with radial velocities from À12 to À3 km s À1 show a remarkably good correlation with the X-ray features, strongly supporting the recently derived kinematic distance around 1 kpc, as opposed to the 6 kpc previously claimed. In addition, we show that absorption of X-rays is caused by local molecular gas at softer X-ray bands. Subsequent measurements of the submillimeter J ¼ 3 2 transition of CO made with the ASTE 10 m and CSO 10.4 m submillimeter telescopes toward three of the molecular intensity peaks have revealed higher excitation conditions, most likely higher temperatures above $30 K , in contrast to the typical gas temperature, 10 K, in low-mass dark clouds. This temperature rise is most likely caused by enhanced heating by the high-energy events in the SNR, where possible mechanisms include heating by X-rays, -rays, and/or cosmic-ray protons, although we admit that additional radiative heating by young protostars embedded may be working as well. In one of the CO peaks, we have confirmed the presence of broad molecular wings of $20 km s À1 velocity extent in the CO J ¼ 3 2 transition. Two alternative interpretations for the wings are presented; one is shock acceleration by the blast wave, and the other is molecular outflow driven by an embedded protostar. The SNR evolution is well explained as the free expansion phase based on the distance of 1 kpc. The molecular data set should be valuable for making a further detailed comparison with the -ray and X-ray distributions in order to examine the cosmic-ray acceleration quantitatively. Subject headingg s: cosmic rays -ISM: individual (SNR J1713.37À3946) -ISM: kinematics and dynamicssupernova remnants

show abstract

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

Moriguchi

Tamura

Tawara

et al. 2005

ApJ

108

134

View full text Add to dashboard Cite

show abstract

“…RXJ1713.7−3946 (also known as a radio SNR G347.3 −0.5; Slane et al 1999), one of the brightest VHE gamma-ray sources ever detected (Muraishi et al 2000;Enomoto et al 2002;Aharonian et al 2004Aharonian et al , 2006Aharonian et al , 2007a, is an ideal target to study these unresolved mysteries. The distance and age of RXJ1713.7−3946 are estimated to be 0.9-1.3kpc and ∼1600yr, respectively (Fukui et al 2003;Moriguchi et al 2005), which is consistent with its connection with the guest star AD393 (e.g., Wang et al 1997).…”

Section: Origin Of Gamma Rays From Snr Rxj17137−3946mentioning

confidence: 99%

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Acero¹,

Aloisio²,

Amans³

et al. 2017

ApJ

View full text Add to dashboard Cite

Citation for published item:e eroD pF nd eloisioD F nd em nsD tF nd em toD iF nd entonelliD vF eF nd er moD gF nd ermstrongD F nd erquerosD pF nd es noD uF nd eshleyD wF nd f kesD wF nd f l zsD gF nd f lzerD eF nd f m D eF nd f rkovD wF nd f rrioD tF eF nd fen owD F nd fernl¤ ohrD uF nd feshleyD F nd figongi riD gF nd fil ndD eF nd filinskyD eF nd fiss ldiD iF nd fite uD tF nd fl n hD yF nd fl siD F nd fl zekD tF nd foissonD gF nd fon nnoD qF nd fon rdiD eF nd fon volont D gF nd fonnoliD qF nd fr idingD gF nd fr uExogu¡ eD F nd fregeonD tF nd frownD eF wF nd fug evD F nd fulg relliD eF nd fulikD F nd furtonD wF nd furtovoiD eF nd fusettoD qF nd f¤ ott herD wF nd g meronD F nd g p l iD wF nd g proniD eF nd g r veoD F nd g rosiD F nd g s oneD iF nd gerrutiD wF nd gh tyD F nd ghenD eF nd ghenD F nd gherny kov D wF nd ghik w D wF nd ghudo D tF nd gohenE nugiD tF nd gol fr n es oD F nd gonfortiD F nd gontrer sD tF vF nd gost D eF nd gotterD qF nd govinoD F nd govoneD qF nd gum niD F nd gusum noD qF nd h9emm ndoD pF nd h9 rsoD hF nd h nielD wF nd h zziD pF nd he engelisD eF nd he ges reD qF nd he pr n oD eF nd he prond tD pF nd de qouvei h l inoD iF wF nd he visioD gF nd de los eyes vopezD F nd he vottoD fF nd de x uroisD wF nd he lm D pF nd hel ntoD wF nd helg doD gF nd dell olpeD hF nd hi qirol moD F nd hi qiulioD gF nd hi ierroD pF nd hi enereD vF nd horoD wF nd hourn uxD tF nd hum sD hF nd hw rk d sD F nd h¡ % zD gF nd i rD tF nd ig ertsD uF nd iine keD F nd ils¤ sserD hF nd is h hD F nd p l et Eqon lvesD hF nd p sol D qF nd pedorov D iF nd pern¡ ndezEf rr lD eF nd perr ndD qF nd pesquetD wF nd pi ndriniD iF nd pi ssonD eF nd pilipov¡ % D wF hF nd piorettiD F nd pontD vF nd pont ineD qF nd pr n oD pF tF nd goromin D vF preix s nd pujit D F nd pukuiD F nd punkD F nd p¤ orsterD eF nd q dol D eF nd v¡ opezD F q r i nd q r z r zykD wF nd qigliettoD xF nd qiord noD pF nd qiuli niD eF nd qli ensteinD tF nd qn tykD F nd qoldoniD F nd qr r zykD F nd qr i niD F nd qr h mD tF nd qr ndiD F nd qr notD tF nd qreenD eF tF nd qri0thsD F nd qunjiD F nd r ko y nD rF nd r r D F nd r ss nD F nd r y shid D wF nd rellerD wF nd reloD tF gF nd rintonD tF nd rn tykD fF nd ruetD tF nd ruettenD wF nd rumenskyD F fF nd russeinD wF nd r¤ or ndelD tF nd skenoD F nd sn d D F nd snomeD F nd snoueD F nd snoueD F nd snoueD F nd sok D uF nd soriD wF nd t quemierD tF nd t ne ekD F nd t nkowskyD hF nd tungD sF nd u retD F nd u t giriD rF nd uimeswengerD F nd uimur D F nd un¤ odlsederD tF nd uo hD fF nd uo otD tF nd uohriD uF nd uominD xF nd uonnoD F nd uos kD uF nd uoy m D F nd ur usD wF nd uu oD rF nd wezekD qF uuke nd uushid D tF nd lom r D xF v nd v likD uF nd v m nn D qF nd v ndtD rF nd v pingtonD tF nd v porteD F nd veeD F nd veesD tF nd vef u heurD tF nd ven inD tFE F nd vetoD qF nd vindforsD iF nd vohseD F nd vom rdiD F nd vongoD pF nd vopezD wF nd vu relliD pF nd vuqueEis mill D F vF nd v¡ opezEgotoD F nd w roneD wF gF nd w ierD qF nd w l gutiD qF nd w nd tD hF nd w nev D qF nd w ng noD F nd w r owithD eF nd w rt¡ %D tF nd w rt¡ %nezD wF nd ...

show abstract

“…Among the earliest identifications of X-ray synchrotron emitting supernova remnants were RX J1713.7-3946 (Koyama et al, 1997;Slane et al, 1999) and RX J0852.0-4622 (Slane et al, 2001), two supernova remnants that later turned out to be bright in TeV gamma-rays . Also the large diameter supernova remnant RCW 86 showed signs of non-thermal X-ray emission (Vink et al, 1997), which was later argued to be synchrotron radiation (Bamba et al, 2000;Borkowski et al, 2001).…”

Section: X-ray Observationsmentioning

confidence: 99%

Observational Signatures of Particle Acceleration in Supernova Remnants

Helder¹,

Vink²,

Bykov³

et al. 2012

Particle Acceleration in Cosmic Plasmas

View full text Add to dashboard Cite

We evaluate the current status of supernova remnants as the sources of Galactic cosmic rays. We summarize observations of supernova remnants, covering the whole electromagnetic spectrum and describe what these observations tell us about the acceleration processes by high Mach number shock fronts. We discuss the shock modification by cosmic rays, the shape and maximum energy of the cosmic-ray spectrum and the total energy budget of

show abstract

Nonthermal X‐Ray Emission from the Shell‐Type Supernova Remnant G347.3−0.5

Cited by 280 publications

References 42 publications

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

A Detailed Study of Molecular Clouds toward the TeV Gamma‐Ray Supernova Remnant G347.3−0.5

Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7−3946

Observational Signatures of Particle Acceleration in Supernova Remnants

Contact Info

Product

Resources

About