Discovery of 35 New Supernova Remnants in the Inner Galaxy

Brogan, C. L.; Gelfand, Joseph D.; Gaensler, B. M.; Kassim, N. E.; Lazio, T. Joseph W.

doi:10.1086/501500

Cited by 180 publications

(305 citation statements)

References 17 publications

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“…We also note the presence of two additional SNRs in the region : G018.1−0.1 and G018.6−0.2 (Brogan et al 2006) as shown in Fig. 1.…”

Section: Introductionmentioning

confidence: 58%

“…1). Such an overlap could result from the interaction of multi-TeV cosmic-rays with molecular clouds, and thus raises the possibility of cosmic-ray acceleration in the vicinity, notably from HESS J1825-137's progenitor SNR.We also note the presence of two additional SNRs in the region : G018.1−0.1 and G018.6−0.2 (Brogan et al 2006) as shown in Fig. 1.…”

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confidence: 64%

“…If this PWN produces the HESS J1826−130 emission, the adjacent molecular gas at v lsr = 60 − 80 km/s may explain the TeV morphology and would suggest a PWN distance d = 4.6 kpc (near) or d = 11.4 kpc (far). SNR G018.2−0.1 and SNR G018.6−0.2 (see Brogan et al 2006 andGreen 2014) are also positioned close to HESS J1826−130. Their small angular diameters however and their offset position makes the two SNRs unlikely to be associated with HESS J1826−130.…”

Section: Discussionmentioning

confidence: 88%

“…HESS excess counts image (> 100 GeV) towards HESS J1825−137 overlaid by the CO(1-0) integrated intensity contour (40,60,80, 100 K km/s) between v lsr = 40 − 60 km/s from Dame, Hartmann & Thaddeus (2001) as revealed by Lemiere, Terrier & DjannatiAtaï (2006). The white circles represent the different SNRs detected (Brogan et al 2006). P1 indicates the pulsar PSR J1826-1334's location while P2 shows the position of PSR J1826-1256.…”

Section: Carbon Monosulfide Cs(1-0) and Isotopologuesmentioning

confidence: 99%

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ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

Voisin¹,

Rowell²,

Burton³

et al. 2016

Mon. Not. R. Astron. Soc.

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HESS J1825−137 is a pulsar wind nebula (PWN) whose TeV emission extends across ∼ 1 deg. Its large asymmetric shape indicates that its progenitor supernova interacted with a molecular cloud located in the north of the PWN as detected by previous CO Galactic survey (e.g Lemiere, Terrier & Djannati-Ataï 2006).Here we provide a detailed picture of the ISM towards the region north of HESS J1825−137, with the analysis of the dense molecular gas from our 7mm and 12mm Mopra survey and the more diffuse molecular gas from the Nanten CO(1-0) and GRS 13 CO(1-0) surveys. Our focus is the possible association between HESS J1825−137 and the unidentified TeV source to the north, HESS J1826−130. We report several dense molecular regions whose kinematic distance matched the dispersion measured distance of the pulsar. Among them, the dense molecular gas located at (RA, Dec)=(18.421h,−13.282 • ) shows enhanced turbulence and we suggest that the velocity structure in this region may be explained by a cloud-cloud collision scenario.Furthermore, the presence of a Hα rim may be the first evidence of the progenitor SNR of the pulsar PSR J1826-1334 as the distance between the Hα rim and the TeV source matched with the predicted SNR radius R SNR ∼ 120 pc.From our ISM study, we identify a few plausible origins of the HESS J1826−130 emission, including the progenitor SNR of PSR J1826−1334 and the PWN G018.5−0.4 powered by PSR J1826−1256. A deeper TeV study however, is required to fully identify the origin of this mysterious TeV source.Key words: molecular data -pulsars: individual: PSR J1826−1334 -ISM: cloudscosmic-rays -gamma-rays: ISM. INTRODUCTIONHESS J1825−137 is one of the brightest and most extensive pulsar wind nebulae (PWNe) detected in TeV γ-rays (Aharonian et al. 2006). It is powered by the high spin-down power (ĖSD = 2.8 × 10 36 erg/s) pulsar PSR J1826−1334 with a dispersion measure distance of 3.9±0.4 kpc and characteristic age τc ∼ 20 kyr.PWNe represent a significant fraction of the Galactic TeV γ-ray source population. They convert a varying fraction of their pulsars' spin down energyĖSD into high energy E-mail:fabien.voisin@adelaide.edu.au (AVR); fabien.voisin@adelaide.edu.au (ANO) electrons. The electron flow is temporally randomized and re-accelerated at a termination shock resulting from pressure from the surrounding interstellar medium (ISM). InverseCompton (IC) up-scattering of soft photons then leads to TeV γ-rays, and associated synchrotron radio to X-ray emission.The morphology of PWNe can be heavily influenced by the ISM. The interaction of the progenitor supernova shock with adjacent molecular clouds can lead to a reverse shock propagating back into the PWN (Blondin, Chevalier & Frierson 2001), giving rise to an asymmetry in the radio, X-ray and γ-ray emission that can trail away from the pulsar along the pulsar-molecular cloud axis.HESS J1825−137 is an excellent example of this situa- Lemiere, Terrier & Djannati-Ataï (2006), with the bulk of the TeV γ-ray extending up to a degree south of the pulsar. In...

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“…We also note the presence of two additional SNRs in the region : G018.1−0.1 and G018.6−0.2 (Brogan et al 2006) as shown in Fig. 1.…”

Section: Introductionmentioning

confidence: 58%

mentioning

confidence: 64%

Section: Discussionmentioning

confidence: 88%

Section: Carbon Monosulfide Cs(1-0) and Isotopologuesmentioning

confidence: 99%

See 2 more Smart Citations

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

Voisin¹,

Rowell²,

Burton³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…However, new radiocontinuum surveys of the galactic plane (Helfand et al 2006;Brogan et al 2006) have recently identified a host of (candidate) SNR in the inner galaxy and surveys searching for signposts of interaction in the 1720 MHz transition of OH have been conducted by Hewitt & Yusef-Zadeh (2009).…”

Section: Introductionmentioning

confidence: 99%

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

Liszt

2009

A&A

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Results. Although broad CO lines characteristic of shocked gas were not seen in this kinematically complex region, a bright (14 K), new, marginally-resolved ±9 km s −1 outflow source G5.638+0.233 and a comparably bright rim of CO emission were found at/around the periphery of SNR G5.55+0.12. Most of the periphery of SNR G5.71-0.08 is surrounded by a bright rim of CO emission. CO emission at the 7 km s −1 velocity of a 1720 OH maser spot near SNR G5.70-0.12 is very bright, 19 K, but gas at −21 km s −1 is widespread over the region and CO emission is rather weak toward the OH maser spots at this velocity north of G5.4-1.2. Other very bright CO lines in the region are associated with H II regions, i.e. 27 K toward W28A2 = G5.89-0.39 and 15 K toward an MSX-IR source at l = 5.9 o , b = −0.13 o which is probably the exciting agent of a separate, classical HII region just north of W28A2.

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Supernova Remnants and Cosmic Rays: Non-thermal Radiation

Vink

2020

Astronomy and Astrophysics Library

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Discovery of 35 New Supernova Remnants in the Inner Galaxy

Cited by 180 publications

References 17 publications

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

ISM gas studies towards the TeV PWN HESS J1825−137 and northern region

CO $\mathsf{J}=\mathsf{1}{-}0$ observations of gas near the galactic supernova remnants G5.4-1.2, G5.55+0.32 and G5.71-0.08

Supernova Remnants and Cosmic Rays: Non-thermal Radiation

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