The Southern Galactic Plane Survey: H
                    <scp>i</scp>
                    Observations and Analysis

McClure-Griffiths, N. M.; Dickey, John M.; Gaensler, B. M.; Green, Anne; Haverkorn, M.; Strasser, S.

doi:10.1086/430114

Cited by 347 publications

(341 citation statements)

References 22 publications

(32 reference statements)

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“…In order to complete the picture of the gas distribution towards HESS J1826−130, we made use of SGPS data with ∆v = 0.8 km/s and Trms=1.4 K/channel (McClure-Griffiths et al 2005) to search for diffuse atomic gas.…”

Section: Hi Analysismentioning

confidence: 99%

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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Section: Hi Analysismentioning

confidence: 99%

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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“…BYW acknowledges funding from NSF grant # AST-0507244. Figure 1 was produced using data from the Southern Galactic Plane Survey (McClure-Griffiths et al 2005).…”

Section: Acknowledgementsmentioning

confidence: 99%

The interstellar medium towards the Ara OB1 region

Henderson

Welsh

Hearnshaw

2008

Astrophys Space Sci

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We present high resolution (R ∼ 4 km s −1 ) absorption measurements of the interstellar NaI and CaII lines measured towards 14 early-type stars of distance 123 pc-1650 pc, located in the direction of the Ara OB1 stellar cluster. The line profiles can broadly be split into four distinct groupings of absorption component velocity, and we have attempted to identify an origin and distance to each of these interstellar features. For gas with absorption covering the velocity range −10 km s −1 < V helio < +10 km s −1 , we can identify the absorbing medium with local gas belonging to the Lupus-Norma interstellar cavity located between 100 and 485 pc in this galactic direction. Gas with velocities spanning the range −20 km s −1 < V helio < +20 km s −1 is detected towards stars with distances of 570-800 pc. We identify a wide-spread interstellar feature at V helio ∼ −15 km s −1 with the expanding HI shell called GSH 337+00−05, which is now placed at a distance of ∼ 530 pc.Gas with velocities in the range −45 km s −1 < V helio < −25 km s −1 is only detected towards stars with distances > 1 kpc, which places this absorbing gas at a similar distance to that of the Ara OB1 stellar cluster. The similarity between the radial velocity of the stellar cluster and that of the absorbing gas suggests that the cluster stars may be presently embedded within, and traveling through, this interstellar cloud complex. Absorption at velocities < −50 km s −1 is seen towards only two stars, HD 154873 and HD 150958, both of which have distances > 1300 pc. Although the NaI/CaII for this component is consistent with the presence of interstellar shocks, we believe that it is unlikely that this highly negative velocity gas is physically associated with the Ara OB1 cluster itself, and its origin may be linked to the more distant (and larger) Sco OB1 cluster.

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“…The Southern Galactic Plane Survey (SGPS) is a survey in the neutral hydrogen line and full-polarization continuum at 1.4 GHz, obtained with the Australia Telescope Compact Array (ATCA) and Parkes 64m single dish (McClure-Griffiths et al 2005). (However, the data presented here are solely from the ATCA.)…”

Section: The Southern Galactic Plane Surveymentioning

confidence: 99%

“…For a detailed description of the continuum part of the SGPS discussed here see Haverkorn et al (2006); the neutral hydrogen part is described in McClure-Griffiths et al (2005).…”

Section: The Southern Galactic Plane Surveymentioning

confidence: 99%

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Magnetic fields in the Southern Galactic Plane Survey

et al. 2006

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The Southern Galactic Plane Survey (SGPS) is a 1.4 GHz radio polarization and HI survey in a large part of the inner Galactic plane at a resolution of about an arcmin. Depolarization and Faraday rotation of polarized radiation from diffuse Galactic synchrotron emission, pulsars, and extragalactic sources can be used to infer information about the strength and structure of the Galactic magnetic field. Here, we discuss science results of the polarization data from the SGPS. We show from statistical analysis of rotation measures of polarized extragalactic sources that fluctuations in the magneto-ionized medium of the spiral arms are probably mainly caused by HII regions, while the rotation measure fluctuations in the interarm regions may be connected to the interstellar turbulent cascade. Furthermore, the variations of rotation measure with Galactic longitude enable modeling of the large-scale component of the Galactic magnetic field, including determination of the number and location of magnetic field reversals. Finally, the SGPS is an excellent way to study subparsec-scale structure in the ionized ISM by way of depolarization studies in HII regions.Comment: to appear in proceedings for the conference "The Origin and Evolution of Cosmic Magnetic Fields", eds R. Beck, G. Brunetti, L. Feretti, and B. Gaensle

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The Southern Galactic Plane Survey: H i Observations and Analysis

Cited by 347 publications

References 22 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

The interstellar medium towards the Ara OB1 region

Magnetic fields in the Southern Galactic Plane Survey

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