The interstellar medium around the supernova remnant G320.4-1.2

Using the Australia Telescope Compact Array, we have carried out a survey of the H I emission in the direction of the barrel-shaped supernova remnant (SNR) G320.4-1.2 (MSH 15-52) and its associated young pulsar B1509-58. The angular resolution of the data is 4.′0 × 2.′7, and the rms noise is of orde...

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Detalles Bibliográficos
Publicado:	2002
Materias:	ISM: individual (G320.4-1.2, RCW 89) ISM: structure Pulsars: individual (B1509-58) supernova remnants
Acceso en línea:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v123_n11753_p337_Dubner http://hdl.handle.net/20.500.12110/paper_00046256_v123_n11753_p337_Dubner
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	paper:paper_00046256_v123_n11753_p337_Dubner
record_format	dspace
spelling	paper:paper_00046256_v123_n11753_p337_Dubner2023-06-08T14:27:13Z The interstellar medium around the supernova remnant G320.4-1.2 ISM: individual (G320.4-1.2, RCW 89) ISM: structure Pulsars: individual (B1509-58) supernova remnants Using the Australia Telescope Compact Array, we have carried out a survey of the H I emission in the direction of the barrel-shaped supernova remnant (SNR) G320.4-1.2 (MSH 15-52) and its associated young pulsar B1509-58. The angular resolution of the data is 4.′0 × 2.′7, and the rms noise is of order 30 mJy beam-1 (∼0.5 K). The H I observations indicate that the north-northwest radio limb has encountered a dense H I filament (density ∼12 cm-3) at the same LSR velocity as that of the SNR (VLSR ∼ -68 km s-1). This H I concentration would be responsible for the flattened shape of the northwestern lobe of G320.4-1.2 and for the formation of the radio-optical-X-ray nebula RCW 89. The emission associated with the bright knots in the interior of RCW 89 can be explained as arising from the interaction between the collimated relativistic outflow from the pulsar and the denser part of this H I filament (density ∼15 cm-3). The south-southeastern half of the SNR, on the other hand, seems to have rapidly expanded across a lower density environment (density ∼0.4 cm-3). The H I data also reveal an unusual H I feature aligned with a collimated outflow generated by the pulsar, suggestive of association with the SNR, The anomalous kinematical velocity of this feature (VLSR ∼ 15 km s-1), however, is difficult to explain. 2002 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v123_n11753_p337_Dubner http://hdl.handle.net/20.500.12110/paper_00046256_v123_n11753_p337_Dubner
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	ISM: individual (G320.4-1.2, RCW 89) ISM: structure Pulsars: individual (B1509-58) supernova remnants
spellingShingle	ISM: individual (G320.4-1.2, RCW 89) ISM: structure Pulsars: individual (B1509-58) supernova remnants The interstellar medium around the supernova remnant G320.4-1.2
topic_facet	ISM: individual (G320.4-1.2, RCW 89) ISM: structure Pulsars: individual (B1509-58) supernova remnants
description	Using the Australia Telescope Compact Array, we have carried out a survey of the H I emission in the direction of the barrel-shaped supernova remnant (SNR) G320.4-1.2 (MSH 15-52) and its associated young pulsar B1509-58. The angular resolution of the data is 4.′0 × 2.′7, and the rms noise is of order 30 mJy beam-1 (∼0.5 K). The H I observations indicate that the north-northwest radio limb has encountered a dense H I filament (density ∼12 cm-3) at the same LSR velocity as that of the SNR (VLSR ∼ -68 km s-1). This H I concentration would be responsible for the flattened shape of the northwestern lobe of G320.4-1.2 and for the formation of the radio-optical-X-ray nebula RCW 89. The emission associated with the bright knots in the interior of RCW 89 can be explained as arising from the interaction between the collimated relativistic outflow from the pulsar and the denser part of this H I filament (density ∼15 cm-3). The south-southeastern half of the SNR, on the other hand, seems to have rapidly expanded across a lower density environment (density ∼0.4 cm-3). The H I data also reveal an unusual H I feature aligned with a collimated outflow generated by the pulsar, suggestive of association with the SNR, The anomalous kinematical velocity of this feature (VLSR ∼ 15 km s-1), however, is difficult to explain.
title	The interstellar medium around the supernova remnant G320.4-1.2
title_short	The interstellar medium around the supernova remnant G320.4-1.2
title_full	The interstellar medium around the supernova remnant G320.4-1.2
title_fullStr	The interstellar medium around the supernova remnant G320.4-1.2
title_full_unstemmed	The interstellar medium around the supernova remnant G320.4-1.2
title_sort	interstellar medium around the supernova remnant g320.4-1.2
publishDate	2002
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046256_v123_n11753_p337_Dubner http://hdl.handle.net/20.500.12110/paper_00046256_v123_n11753_p337_Dubner
_version_	1768542915489955840

The interstellar medium around the supernova remnant G320.4-1.2

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