VRO 42.05.01 - One supernova remnant or two

Landecker, T. L.; Pineault, S.; Routledge, D.; Vaneldik, J. F.

doi:10.1086/183885

Cited by 24 publications

(25 citation statements)

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“…For VRO42.05.01, only the compact sources' flux density corrections are needed at 38, 83, 610 and 2700 MHz. We note that Landecker et al (1982) believe that the flux density at 2700 MHz from Willis (1973) is overestimated. Thus we obtain a new flux density value from the Effelsberg 2695 MHz image: 4.6 ± 0.2 Jy and use this instead.…”

Section: Integrated Flux Densities and Spectral Indicesmentioning

confidence: 74%

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Radio spectral index study of the SNRs OA184 and VRO42.05.01

Leahy¹,

2005

A&A

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Section: Integrated Flux Densities and Spectral Indicesmentioning

confidence: 74%

“…VRO42.05.01 has an unusual shape with a northeastern shell intersected by a much larger bowl-shaped wing in the southwest (Landecker et al 1982). The shell has a radius of 25 pc, for a distance of 5 kpc, and the SNR is currently in its isothermal stage (Pineault et al 1987).…”

Section: Introductionmentioning

confidence: 99%

Radio spectral index study of the SNRs OA184 and VRO42.05.01

Leahy¹,

2005

A&A

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“…A 1.4 GHz image of SNR G166.0+04.3 (VRO 42.05.01; Landecker et al 1982 ;Pineault, Landecker, & Routledge 1987) is shown in Figure 3, revealing a striking resemblance between this SNR and G350.0-02.0. G166.0+04.3 is also composed of three separate regions, whose relative shape, size and orientation are similar to those in G350.0-02.0.…”

Section: G3500-020mentioning

confidence: 99%

The Nature of Bilateral Supernova Remnants

Gaensler¹

1998

ApJ

114

113

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We present high-resolution radio images at 1.4 GHz of two Galactic supernova remnants (SNRs), G003.8-00.3 (formerly G003.7-00.2) and G350.0-02.0 (formerly G350.0-01.8). Although the two objects are very different in appearance, in both cases the radio emission shows a clear bilateral (or "barrel") morphology for which the axis is parallel to the Galactic Plane.The majority of Galactic SNRs have now been observed at high resolution, and one can define a clear bilateral subset of the population. We consider a sample of 17 such SNRs, and find a highly significant tendency for the bilateral axes of these SNRs to be aligned with the Galactic Plane. We interpret this as indicating that "extrinsic" effects dominate the morphology of such remnants. Specifically, we argue that the Galactic magnetic field causes these SNRs to appear bilateral, either directly, in the form of magnetic field compression and/or quasi-perpendicular acceleration of electrons in the supernova shock, or more likely indirectly, by pre-processing the interstellar medium to produce density stratifications extended along the Plane.

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“…1). It has been studied in the X-rays (Burrows & Guo 1994;Guo & Burrows 1997;Bocchino et al 2009;Matsumura et al 2017), in the optical (van den Bergh et al 1973;Fesen et al 1985;Boumis et al 2016), in the radio continuum (Landecker et al 1982;Pineault et al 1985;Leahy & Tian 2005;Arias et al 2019), and in H I (Landecker et al 1989). It has also been detected in GeV γ-rays (Araya 2013), although this detec- Labelled are the regions referred to throughout the text as 'shell' (the small semicircle) and 'wing' (the large triangle).…”

Section: Introductionmentioning

confidence: 99%

The environment of supernova remnant VRO 42.05.01 as probed with IRAM 30m molecular line observations

Arias

Domček

Zhou

et al. 2019

A&A

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Context. The environment of supernova remnants (SNRs) is a key factor in their evolution, particularly at later stages of their existence. Mixed-morphology (MM) SNRs have a peculiar centre-filled X-ray shape that remains enigmatic. It is often assumed that they evolve in very dense environments, and that the X-ray morphology is due to interactions between the SNRs and their surroundings. Aims. We aim to determine whether VRO 42.05.01 is embedded in, and interacting with, a dense molecular environment. We also aim to understand the multi-wavelength emission from the environment of this SNR, and whether the interstellar material can be responsible for the the MM nature of the source, and for its strange radio and optical shape. Methods. We used the IRAM telescope in Pico Veleta, Spain, to search for signs of interaction between the SNR and neighbouring molecular clouds. We observed a region of 26 × 14 towards the west of VRO 42.05.01 and a region of 8 × 4 towards the north of the remnant in the 12 CO J = 1 − 0, 13 CO J = 1 − 0, and 12 CO J = 2 − 1 transitions with the EMIR receiver. We made maps of the properties of the observed molecular clouds (peak temperatures, central velocities, velocity dispersions), as well as maps of column density along the line of sight, and ratio of the 12 CO J = 2 − 1 to 12 CO J = 1 − 0 transitions. We also analyse archival optical, infrared, and radio spectroscopic data for other hints on the nature of the medium. Results. We do not find conclusive physical proof that the SNR is interacting with the few, clumpy molecular clouds that surround it in the region of our observations, although there is some suggestion of such interaction (in a region outside our map) from infrared emission. We find that there is a velocity gradient in one of the molecular clouds that is consistent with a stellar wind blown by a 12−14 M progenitor star. We reassess the literature distance to VRO 42.05.01, and propose that it has a local standard of rest velocity of −6 km s −1 , and that it is located 1.0 ± 0.4 kpc away (the earlier distance value was 4.5 ± 1.5 kpc). We find that a dust sheet intersects VRO 42.05.01 and is possibly related to its double shell-shaped morphology.

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VRO 42.05.01 - One supernova remnant or two

Cited by 24 publications

References 0 publications

Radio spectral index study of the SNRs OA184 and VRO42.05.01

Radio spectral index study of the SNRs OA184 and VRO42.05.01

The Nature of Bilateral Supernova Remnants

The environment of supernova remnant VRO 42.05.01 as probed with IRAM 30m molecular line observations

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