A morphological study of the supernova remnant RX J0852.0-4622 (Vela Jr.)

Nigel I. Maxted; M. D. Filipovic; H. Sano; G. E. Allen; T. G. Pannuti; G. P. Rowell; A. Grech; Q. Roper; G. F. Wong; T. J. Galvin; Y. Fukui; J. D. Collier; E. J. Crawford; K. Grieve; A. D. Horta; P. Manojlovic; A. O'Brien

doi:10.3847/1538-4357/aae082

A morphological study of the supernova remnant RX J0852.0-4622 (Vela Jr.)

Nigel I. Maxted, M. D. Filipovic, H. Sano, G. E. Allen, T. G. Pannuti, G. P. Rowell, A. Grech, Q. Roper, G. F. Wong, T. J. Galvin, Y. Fukui, J. D. Collier, E. J. Crawford, K. Grieve, A. D. Horta, P. Manojlovic, A. O'Brien

Western Sydney University

Research output: Contribution to journal › Article › peer-review

13 Citations (Scopus)

Abstract

We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (also known as Vela Jr., Vela Z, and G266.2-1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela SNR causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio-continuum emission can be characterized by a two-dimensional shell with a radius of 0 degrees.90 +/- 0 degrees.01 (or 11.8 +/- 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 degrees.08 +/- 0 degrees.01,-46 degrees.34 +/- 0 degrees.01) (or R.A. = 8(h)52(m)19(s).2, decl. = -46 degrees 20'24 ''.0, J2000), consistent with X-ray and gamma-ray emission. Although [O III] emission features are generally associated with the Vela SNR, one particular [ O III] emission feature, which we denote as "the Vela Claw," morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Toward the northwestern edge of RX J0852.0-4622, we find a flattening of the radio spectral index toward another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and interstellar medium gas.

Original language	English
Article number	76
Number of pages	9
Journal	Astrophysical Journal
Volume	866
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/aae082
Publication status	Published - 2018

Keywords

gamma rays
particle acceleration
radio continuum
supernova remnants

Access to Document

10.3847/1538-4357/aae082

Cite this

Maxted, N. I., Filipovic, M. D., Sano, H., Allen, G. E., Pannuti, T. G., Rowell, G. P., Grech, A., Roper, Q., Wong, G. F., Galvin, T. J., Fukui, Y., Collier, J. D., Crawford, E. J., Grieve, K., Horta, A. D., Manojlovic, P., & O'Brien, A. (2018). A morphological study of the supernova remnant RX J0852.0-4622 (Vela Jr.). Astrophysical Journal, 866(2), Article 76. https://doi.org/10.3847/1538-4357/aae082

@article{06c82694c834483fb1f60a4bc5d1cde3,

title = "A morphological study of the supernova remnant RX J0852.0-4622 (Vela Jr.)",

abstract = "We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (also known as Vela Jr., Vela Z, and G266.2-1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela SNR causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio-continuum emission can be characterized by a two-dimensional shell with a radius of 0 degrees.90 +/- 0 degrees.01 (or 11.8 +/- 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 degrees.08 +/- 0 degrees.01,-46 degrees.34 +/- 0 degrees.01) (or R.A. = 8(h)52(m)19(s).2, decl. = -46 degrees 20'24 ''.0, J2000), consistent with X-ray and gamma-ray emission. Although [O III] emission features are generally associated with the Vela SNR, one particular [ O III] emission feature, which we denote as {"}the Vela Claw,{"} morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Toward the northwestern edge of RX J0852.0-4622, we find a flattening of the radio spectral index toward another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and interstellar medium gas.",

keywords = "gamma rays, particle acceleration, radio continuum, supernova remnants",

author = "Maxted, {Nigel I.} and Filipovic, {M. D.} and H. Sano and Allen, {G. E.} and Pannuti, {T. G.} and Rowell, {G. P.} and A. Grech and Q. Roper and Wong, {G. F.} and Galvin, {T. J.} and Y. Fukui and Collier, {J. D.} and Crawford, {E. J.} and K. Grieve and Horta, {A. D.} and P. Manojlovic and A. O'Brien",

year = "2018",

doi = "10.3847/1538-4357/aae082",

language = "English",

volume = "866",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing",

number = "2",

}

TY - JOUR

T1 - A morphological study of the supernova remnant RX J0852.0-4622 (Vela Jr.)

AU - Maxted, Nigel I.

AU - Filipovic, M. D.

AU - Sano, H.

AU - Allen, G. E.

AU - Pannuti, T. G.

AU - Rowell, G. P.

AU - Grech, A.

AU - Roper, Q.

AU - Wong, G. F.

AU - Galvin, T. J.

AU - Fukui, Y.

AU - Collier, J. D.

AU - Crawford, E. J.

AU - Grieve, K.

AU - Horta, A. D.

AU - Manojlovic, P.

AU - O'Brien, A.

PY - 2018

Y1 - 2018

N2 - We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (also known as Vela Jr., Vela Z, and G266.2-1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela SNR causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio-continuum emission can be characterized by a two-dimensional shell with a radius of 0 degrees.90 +/- 0 degrees.01 (or 11.8 +/- 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 degrees.08 +/- 0 degrees.01,-46 degrees.34 +/- 0 degrees.01) (or R.A. = 8(h)52(m)19(s).2, decl. = -46 degrees 20'24 ''.0, J2000), consistent with X-ray and gamma-ray emission. Although [O III] emission features are generally associated with the Vela SNR, one particular [ O III] emission feature, which we denote as "the Vela Claw," morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Toward the northwestern edge of RX J0852.0-4622, we find a flattening of the radio spectral index toward another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and interstellar medium gas.

AB - We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0-4622 (also known as Vela Jr., Vela Z, and G266.2-1.2). RX J0852.0-4622 is coincident with the edge of the larger Vela SNR causing confusion in the attribution of some filamentary structures to either RX J0852.0-4622 or its larger sibling. We find that the RX J0852.0-4622 radio-continuum emission can be characterized by a two-dimensional shell with a radius of 0 degrees.90 +/- 0 degrees.01 (or 11.8 +/- 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133 degrees.08 +/- 0 degrees.01,-46 degrees.34 +/- 0 degrees.01) (or R.A. = 8(h)52(m)19(s).2, decl. = -46 degrees 20'24 ''.0, J2000), consistent with X-ray and gamma-ray emission. Although [O III] emission features are generally associated with the Vela SNR, one particular [ O III] emission feature, which we denote as "the Vela Claw," morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0-4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0-4622. Toward the northwestern edge of RX J0852.0-4622, we find a flattening of the radio spectral index toward another molecular clump also thought to be associated with RX J0852.0-4622. It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0-4622 shock and interstellar medium gas.

KW - gamma rays

KW - particle acceleration

KW - radio continuum

KW - supernova remnants

UR - http://handle.westernsydney.edu.au:8081/1959.7/uws:49351

U2 - 10.3847/1538-4357/aae082

DO - 10.3847/1538-4357/aae082

M3 - Article

SN - 0004-637X

VL - 866

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 76

ER -

A morphological study of the supernova remnant RX J0852.0-4622 (Vela Jr.)

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Cite this