Complex structure of the supernova remnant HB 3

Leahy, D. A.; Venkatesan, D.; Long, Knox S.; Naranan, S.

doi:10.1086/163285

Cited by 15 publications

(28 citation statements)

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“…The errors to the positions depend on signal-to-noise ratio. The continuum source G357.7+0.3 is a probable SNR (Reich & Fürst 1984;Leahy 1989;Gray 1994); the radio source is linearly polarized and has a steep spectral index, with a shell-like appearance and its associated X-ray emission. The structure of this unusual continuum source is noted for its nearly square-like morphology (Gray 1994).…”

Section: Resultsmentioning

confidence: 99%

Three New Supernova Remnant OH Masers Near the Galactic Center: Evidence for Large‐Scale Maser Emission from Supernova Remnants

Yusef‐Zadeh

Goss

Roberts

et al. 1999

ApJ

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A survey of the inner 8 • × 1 • of the Galactic plane toward the Galactic center has been carried out at the 1720 MHz transition of OH molecule using the VLA in its D configuration with a resolution of ≈70 ′′ × 45 ′′ . The detection of compact 1720 MHz OH masers associated with three supernova remnants G357.7+0.3, G1.13-0.1 (Sgr D) and G1.4-0.1 as well as new extended maser line emission from G357.7+0.3 and G357.7-0.1 (the Tornado Nebula) were then followed up by A-array observations with spectral and spatial resolutions of 0.3 kms −1 and ≈3 ′′ × 2 ′′ , respectively.The 1720 MHz OH maser line emission is considered to be a powerful shock diagnostic and is collisionally pumped by H 2 molecules at the site where C-type supernova shocks drive into adjacent molecular clouds. The new observations show clear evidence of extended features coincident with compact and bright masers, the best example of which is a coherent feature over a scale of about 20 pc surrounding the shell of the SNR G357.7+0.3. We argue that this remarkable feature is an OH maser and is physically associated with the remnant. This implies that the ambient molecular cloud is uniform in its density and temperature with restricted range of pumping conditions and survives the passage of a large-scale shock front.

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Section: Resultsmentioning

confidence: 99%

Three New Supernova Remnant OH Masers Near the Galactic Center: Evidence for Large‐Scale Maser Emission from Supernova Remnants

Yusef‐Zadeh

Goss

Roberts

et al. 1999

ApJ

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“…It is bordered to the west by HB3, a very large, evolved supernova remnant (SNR), which is clearly seen in the ROSAT All-Sky Survey image and was observed with Einstein (Leahy et al 1985). Radio studies (Routledge et al 1991) suggest that the SNR shock has not yet reached the W3 H II regions, but it is influencing the distribution of CO in the W3 molecular cloud.…”

Section: W3mentioning

confidence: 98%

Parsec-scale X-ray flows in high-mass star-forming regions

Townsley¹,

Feigelson²,

Montmerle³

et al. 2005

Proc. IAU

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Abstract. The Chandra X-ray Observatory is providing remarkable new views of massive starforming regions, revealing all stages in the life cycle of high-mass stars and their effects on their surroundings. We present a Chandra tour of several high-mass star-forming regions, highlighting physical processes that characterize the life of a cluster of high-mass stars, from deeply-embedded cores too young to have established an HII region to superbubbles so large that they shape our views of galaxies. Along the way we see that X-ray observations reveal hundreds of stellar sources powering great HII region complexes, suffused by both hard and soft diffuse X-ray structures caused by fast O-star winds thermalized in wind-wind collisions or by termination shocks against the surrounding media. Finally, we examine the effects of the deaths of high-mass stars that remained close to their birthplaces, exploding as supernovae within the superbubbles that these clusters created. We present new X-ray results on W51 IRS2E and 30 Doradus and we introduce new data on Trumpler 14 in Carina and the W3 HII region complexes W3 Main and W3(OH).

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“…The evolved supernova remnant (SNR) HB3 (G132.7+1.3; Landecker et al 1987), as one of the largest galactic SNRs currently known, has been previously observed by Caswell (1967) and Landecker et al (1987) in the radio continuum, by Leahy et al (1985) in X-rays, by Routledge et al (1991) in the HI-line, by Fesen et al (1995) in Hα, and by Koralesky et al (1998) in hydroxy1 (OH). Its known basic physical features are 60×80 pc in size based on a distance of 2 kpc (Routledge 1991).…”

Section: Introductionmentioning

confidence: 95%

Radio spectral index variations of the SNR HB3

Tian

Leahy

2005

A&A

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Abstract. We present images of the SNR HB3 at both 408 MHz and 1420 MHz from the Canadian Galactic Plane Survey mainly based on data from the Synthesis Telescope of the Dominion Radio Astrophysical Observatory. We reproduce the 100 m-Effelsberg HB3 image at 2695 MHz at large scale, and find that there exists a background emission gradient across the HB3 area. Based on our analysis of background emission and the boundary between W3 and HB3, we give HB3's flux density as 68.6 ± 11.5 Jy at 408 MHz and 44.8 ± 12.0 Jy at 1420 MHz, after subtracting flux from compact sources within HB3. The integrated flux-density-based spectral index between 408 MHz and 1420 MHz is 0.34 ± 0.15. The averaged T-T plot spectral index using all subareas is 0.36. Our measurement values are less than a previously published value of 0.6. The 408-1420 MHz spectral index varies spatially in HB3 in the range 0.1 to 0.7. We investigate the data used by previous authors, and consider more data at 232 MHz, 3650 MHz and 3900 MHz which are not included in previous calculations. There is evidence for two spectral indices for HB3 in the radio band, i.e., 0.63 (38-610 MHz) and 0.32 (408-3900 MHz). This is consistent with the spatial variations: the low frequency data mainly reflects the steeper indices and the high frequency data mainly reflects the flatter indices.

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Complex structure of the supernova remnant HB 3

Cited by 15 publications

References 0 publications

Three New Supernova Remnant OH Masers Near the Galactic Center: Evidence for Large‐Scale Maser Emission from Supernova Remnants

Three New Supernova Remnant OH Masers Near the Galactic Center: Evidence for Large‐Scale Maser Emission from Supernova Remnants

Parsec-scale X-ray flows in high-mass star-forming regions

Radio spectral index variations of the SNR HB3

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