Probing the local environment of the supernova remnant HESS J1731−347 with CO and CS observations

Maxted, N.; Burton, M. G.; Braiding, Catherine; Rowell, G.; Sano, Hidetoshi; Voisin, F.; Capasso, M.; Pühlhofer, G.; Fukui, Y.

doi:10.1093/mnras/stx2727

Cited by 24 publications

(26 citation statements)

References 75 publications

(123 reference statements)

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“…In our model it represents the entire space other than the MC-clumps -MC-core and MC-J1729. (Maxted et al 2018), and the TeV image by Abramowski et al (2011) is shown in green contours. The color bar represents the scale of CO line intensity with a unit of K km s −1 .…”

Section: Resultsmentioning

confidence: 99%

“…These features can be seen clearer in Fig. 2 of Maxted et al (2018), due to a different scale of color bar used in their CO map.…”

Section: Nearby Molecular Cloudsmentioning

confidence: 96%

“…5, one can obtain the column density of the MC near the SNR. Our model adopts a 12 CO emission integrated from −5 km/s to −25 km/s (the giant MC at 3.2 kpc, Maxted et al 2018) and a CO-to-H 2 mass conversion factor of 1.8 × 10 20 cm −2 K −1 km −1 s (Dame et al 2001). When compared with the previous 12 CO observations on HESS J1731-347 with the CfA survey (Abramowski et al 2011, Cui et al 2016, the 12 CO observations with Mopra have much higher angular resolution and deliver a slightly lower column density (∼ 95%) at MC-core region.…”

Section: Nearby Molecular Cloudsmentioning

confidence: 99%

“…The CO studies together with the X-ray studies by Abramowski et al (2011), Doroshenko et al (2017), Maxted et al (2018) have suggested a giant MC of the Scutum-Crux arm (∼3.2 kpc) to be located right in front of the western part of the SNR, and this giant MC could have already been encountered by the SNR (Doroshenko et al 2017, Maxted et al 2018). This distance of 3.2 kpc is also supported by the NS modeling work by Klochkov et al (2013Klochkov et al ( , 2015.…”

Section: Introductionmentioning

confidence: 96%

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Is the SNR HESS J1731-347 Colliding with Molecular Clouds?

Cui

Yang

et al. 2019

ApJ

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The supernova remnant (SNR) HESS J1731-347 is a young SNR which displays a non-thermal X-ray and TeV shell structure. A molecular cloud at a distance of ∼3.2 kpc is spatially coincident with the western part of the SNR, and it is likely hit by the SNR. The X-ray emission from this part of the shell is much lower than from the rest of the SNR. Moreover, a compact GeV emission region coincident with the cloud has been detected with a soft spectrum. These observations seem to imply a shock-cloud collision scenario at this area, where the stalled shock can no longer accelerate super-TeV electrons or maintain strong magnetic turbulence downstream, while the GeV cosmic rays (CRs) are released through this stalled shock. To test this hypothesis, we have performed a detailed Fermi-LAT reanalysis of the HESS J1731-347 region with over 9 years of data. Two distinct GeV components are found, one displaying a soft spectrum is from the compact GeV emission region, the other one displaying a hard spectrum is from the rest of the SNR (excluding the cloud region). A hadronic model involving a shock-cloud collision scenario is built to explain the γ-ray emission from this area. It consists of three CR sources: run-away super-TeV CRs that have escaped from the fast shock, leaked GeV CRs from the stalled shock, and the local CR sea. The X-ray and γ-ray emission of the SNR excluding the shock-cloud interaction region is explained in a one-zone leptonic model. Our shock-cloud collision model explains the GeV-TeV observations from the clouds around HESS J1731-347, i.e. a cloud in contact with the SNR and a distant cloud in spatial coincidence to the TeV source HESS J1729-345. We find however that the leaked GeV CRs from the shock-cloud collision do not necessarily dominate the GeV emission from the clouds, due to a comparable contribution from the local CR sea.

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Section: Resultsmentioning

confidence: 99%

“…These features can be seen clearer in Fig. 2 of Maxted et al (2018), due to a different scale of color bar used in their CO map.…”

Section: Nearby Molecular Cloudsmentioning

confidence: 96%

Section: Nearby Molecular Cloudsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

See 2 more Smart Citations

Is the SNR HESS J1731-347 Colliding with Molecular Clouds?

Cui

Yang

et al. 2019

ApJ

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“…However, evidence for a dominant hadronic component for HESS J1731−347 only exists for the 5.2-6 kpc distance solution, as opposed to the 3.2 kpc solution favoured by theCui et al (2016) model and explicitly derived inMaxted et al (2018a) …”

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confidence: 85%

A Supernova Remnant Counterpart for HESS J1832−085

Maxted¹,

Filipović²,

Hurley‐Walker³

et al. 2019

ApJ

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We examine the new Galactic supernova remnant (SNR) candidate, G23.11+0.18, as seen by the Murchison Widefield Array (MWA) radio telescope. We describe the morphology of the candidate and find a spectral index of −0.63±0.05 in the 70-170 MHz domain. A coincident TeV gamma-ray detection in High-Energy Stereoscopic System (HESS) data supports the SNR nature of G23.11+0.18 and suggests that G23.11+0.18 is accelerating particles beyond TeV energies, thus making this object a promising new cosmic ray hadron source candidate. The remnant cannot be seen in current optical, infrared and X-ray data-sets. We do find, however, a dip in CO-traced molecular gas at a line-of-sight velocity of ∼85 km s −1 , suggesting the existence of a G23.11+0.18 progenitor wind-blown bubble. Furthermore, the discovery of molecular gas clumps at a neighbouring velocity towards HESS J1832−085 adheres to the notion that a hadronic gamma-ray production mechanism is plausible towards the north of the remnant. Based on these morphological arguments, we propose an interstellar medium association for G23.11+0.18 at a kinematic distance of 4.6±0.8 kpc.

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The Mopra Southern Galactic Plane CO Survey—Data Release 3

Braiding

Wong

Maxted

et al. 2018

Publ. Astron. Soc. Aust.

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We present observations of fifty square degrees of the Mopra carbon monoxide (CO) survey of the Southern Galactic Plane, covering Galactic longitudes l = 300-350 • and latitudes |b| ≤ 0.5 • . These data have been taken at 0.6 arcminute spatial resolution and 0.1 km s −1 spectral resolution, providing an unprecedented view of the molecular clouds and gas of the Southern Galactic Plane in the 109-115 GHz J = 1-0 transitions of 12 CO, 13 CO, C 18 O and C 17 O.We present a series of velocity-integrated maps, spectra and position-velocity plots that illustrate Galactic arm structures and trace masses on the order of ∼10 6 M per square degree; and include a preliminary catalogue of C 18 O clumps located between l = 330-340 • . Together with information about the noise statistics of the survey these data can be retrieved from the Mopra CO website, the PASA data store and the Harvard Dataverse.

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Probing the local environment of the supernova remnant HESS J1731−347 with CO and CS observations

Cited by 24 publications

References 75 publications

Is the SNR HESS J1731-347 Colliding with Molecular Clouds?

Is the SNR HESS J1731-347 Colliding with Molecular Clouds?

A Supernova Remnant Counterpart for HESS J1832−085

The Mopra Southern Galactic Plane CO Survey—Data Release 3

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