Some Observations of Shell-type Galactic Radio Sources

Hill, E. R.

doi:10.1071/ph670297

Cited by 15 publications

(12 citation statements)

References 2 publications

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“…The shell-like morphology of RCW 86 was first discovered in radio continuum observations (Mills et al 1961;Hill 1967). After half a century, such morphology has been confirmed at all wavelengths, including γ-rays.…”

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confidence: 95%

Interstellar gas and X-rays toward the Young supernova remnant RCW 86; pursuit of the origin of the thermal and non-thermal X-ray

Sano

Reynoso

Mitsuishi

et al. 2017

Journal of High Energy Astrophysics

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We have analyzed the atomic and molecular gas using the 21 cm Hi and 2.6/1.3 mm CO emissions toward the young supernova remnant (SNR) RCW 86 in order to identify the interstellar medium with which the shock waves of the SNR interact. We have found an Hi intensity depression in the velocity range between −46 and −28 km s −1 toward the SNR, suggesting a cavity in the interstellar medium. The Hi cavity coincides with the thermal and non-thermal emitting X-ray shell. The thermal X-rays are coincident with the edge of the Hi distribution, which indicates a strong density gradient, while the non-thermal X-rays are found toward the less dense, inner part of the Hi cavity. The most significant non-thermal X-rays are seen toward the southwestern part of the shell where the Hi gas traces the dense and cold component. We also identified CO clouds which are likely interacting with the SNR shock waves in the same velocity range as the Hi, although the CO clouds are distributed only in a limited part of the SNR shell. The most massive cloud is located in the southeastern part of the shell, showing detailed correspondence with the thermal X-rays. These CO clouds show an enhanced CO J = 2-1/1-0 intensity ratio, suggesting heating/compression by the shock front. We interpret that the shock-cloud interaction enhances non-thermal X-rays in the southwest and the thermal X-rays are emitted by the shock-heated gas of density 10-100 cm −3 . Moreover, we can clearly see an Hi envelope around the CO cloud, suggesting that the progenitor had a weaker wind than the massive progenitor of the core-collapse SNR RX J1713.7−3949. It seems likely that the progenitor of RCW 86 was a system consisting of a white dwarf and a low-mass star with low-velocity accretion winds.

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confidence: 95%

Interstellar gas and X-rays toward the Young supernova remnant RCW 86; pursuit of the origin of the thermal and non-thermal X-ray

Sano

Reynoso

Mitsuishi

et al. 2017

Journal of High Energy Astrophysics

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“…However, herein we use the designation RCW 86 to refer to the whole SNR, as is now common in the literature. Although the relation of the two knots and northern filaments to the remnant was noted as long ago as 1967 (Hill 1967), almost all optical studies of the remnant have concentrated on only the bright filaments in the southwest. Westerlund & Mathewson (1966) established that these optical filaments showed strong [S ii] λ6724 emission, a common characteristic of SNR filaments.…”

Section: Introductionmentioning

confidence: 99%

The discovery of Balmer-Filaments Encercling SNR RCW 86

Smith¹

1997

The Astronomical Journal

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We report the discovery of Balmer-dominated filaments along almost the complete periphery of the supernova remnant RCW 86 (also known as G 315.2-2.3 or MSH 14-63). Using the UM/CTIO Curtis Schmidt telescope, we obtained deep CCD images in the emission of Hα and [S ii], together with continuum images to remove stellar confusion. After continuum subtraction, we discovered a network of Hα filaments reaching almost completely around the remnant. Most of the newly identified filaments show no corresponding [S ii] emission, indicating that they belong to the peculiar "Balmer-dominated" class of filaments. Comparison of these Balmer filaments with existing radio and X-ray images of RCW 86 shows an overall similarity, although interesting differences are apparent upon detailed inspection. While further observations of these newly identified optical filaments may eventually provide more detailed information on the kinematics and distance to RCW 86, the distance currently remains uncertain. We argue that the shorter distance estimates of ∼1 kpc are still favored. Subject headings: supernova remnants: individual (RCW 86) -ISM: individual (RCW 86) -nebulae: individual (RCW 86) -shock waves -supernovae: individual (SN 185) 1 McLaughlin Fellow, University of Michigan.

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“…Optical emission from the nebula RCW 86 is associated with the remnant (Hill 1967;van den Bergh et al 1973), forming a partial shell (∼ 5 diameter) at the north-western end of the bright ridge of radio emission. An isolated optical filament (Hill 1967) is well-aligned with the northern part of the radio shell.…”

Section: Msca Sourcesmentioning

confidence: 99%

The MOST supernova remnant catalogue (MSC)

Whiteoak

Green

1996

Astron. Astrophys. Suppl. Ser.

297

441

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Abstract. -A catalogue of supernova remnants in the southern Galaxy within the area 245• ≤ l ≤ 355• , |b| ∼ < 1.5• has been produced from observations made at 0.843 GHz with a resolution of 43 using the Molonglo Observatory Synthesis Telescope (MOST). The catalogue, presented here, provides greyscale images and contour maps of known and newly-discovered remnants. The increased resolution and sensitivity of these observations has resulted in better statistics for southern remnants.

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Some Observations of Shell-type Galactic Radio Sources

Cited by 15 publications

References 2 publications

Interstellar gas and X-rays toward the Young supernova remnant RCW 86; pursuit of the origin of the thermal and non-thermal X-ray

Interstellar gas and X-rays toward the Young supernova remnant RCW 86; pursuit of the origin of the thermal and non-thermal X-ray

The discovery of Balmer-Filaments Encercling SNR RCW 86

The MOST supernova remnant catalogue (MSC)

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