Cold neutral gas associated with the Gum nebula

Based on HI maps covering the 3 600 square degrees area delimited by 230° ≤ l ≤ 290°, -30° ≤ b ≤ 30°, we investigated the neutral hydrogen distribution in the Gum nebula and its environments. The main result is the appearence of a huge disk of neutral gas at a kinematical distance compatible with th...

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Guardado en:
Detalles Bibliográficos
Publicado: 1997
Materias:
ISM: bubbles
ISM: individual objects: Gum nebula
ISM: supernova remnants
Radio lines: ISM
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03650138_v123_n1_p31_Reynoso
http://hdl.handle.net/20.500.12110/paper_03650138_v123_n1_p31_Reynoso
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_03650138_v123_n1_p31_Reynoso
record_format dspace
spelling paper:paper_03650138_v123_n1_p31_Reynoso2023-06-08T15:35:38Z Cold neutral gas associated with the Gum nebula ISM: bubbles ISM: individual objects: Gum nebula ISM: supernova remnants Radio lines: ISM Based on HI maps covering the 3 600 square degrees area delimited by 230° ≤ l ≤ 290°, -30° ≤ b ≤ 30°, we investigated the neutral hydrogen distribution in the Gum nebula and its environments. The main result is the appearence of a huge disk of neutral gas at a kinematical distance compatible with that of the nebula, and whose angular dimensions coincide with the optical image of the Gum nebula. The disk, roughly centered at l ≃ 262°, b ≃ -3°, is located at ∼ 500 pc and has a radius of ∼ 150 pc. We propose that this HI disk is the neutral gas component of the optical nebula, hence becoming the first time in which a structure with the dimensions of the optical nebula is detected in other wavelengths. We analyze the fitting of observations with different theoretical models and conclude that the most plausible interpretation is that the Gum nebula is a supershell produced by the action of repeated SN explosions, where the explosions may have originated in the aged association Vela OB2. In this context, the thick HI shell shown by Dubner et al. (1992) near (266°, -2.5°) and the Vela SNR are the debris of two of the several outbursts which started in the region about 6 10 6 years ago. The southern boundary is distorted due to the presence of a ∼ 28° radius shell, which appears to be an interstellar bubble driven by the stellar winds of the O-type star HD 49798. 1997 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03650138_v123_n1_p31_Reynoso http://hdl.handle.net/20.500.12110/paper_03650138_v123_n1_p31_Reynoso
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: bubbles
ISM: individual objects: Gum nebula
ISM: supernova remnants
Radio lines: ISM
spellingShingle ISM: bubbles
ISM: individual objects: Gum nebula
ISM: supernova remnants
Radio lines: ISM
Cold neutral gas associated with the Gum nebula
topic_facet ISM: bubbles
ISM: individual objects: Gum nebula
ISM: supernova remnants
Radio lines: ISM
description Based on HI maps covering the 3 600 square degrees area delimited by 230° ≤ l ≤ 290°, -30° ≤ b ≤ 30°, we investigated the neutral hydrogen distribution in the Gum nebula and its environments. The main result is the appearence of a huge disk of neutral gas at a kinematical distance compatible with that of the nebula, and whose angular dimensions coincide with the optical image of the Gum nebula. The disk, roughly centered at l ≃ 262°, b ≃ -3°, is located at ∼ 500 pc and has a radius of ∼ 150 pc. We propose that this HI disk is the neutral gas component of the optical nebula, hence becoming the first time in which a structure with the dimensions of the optical nebula is detected in other wavelengths. We analyze the fitting of observations with different theoretical models and conclude that the most plausible interpretation is that the Gum nebula is a supershell produced by the action of repeated SN explosions, where the explosions may have originated in the aged association Vela OB2. In this context, the thick HI shell shown by Dubner et al. (1992) near (266°, -2.5°) and the Vela SNR are the debris of two of the several outbursts which started in the region about 6 10 6 years ago. The southern boundary is distorted due to the presence of a ∼ 28° radius shell, which appears to be an interstellar bubble driven by the stellar winds of the O-type star HD 49798.
title Cold neutral gas associated with the Gum nebula
title_short Cold neutral gas associated with the Gum nebula
title_full Cold neutral gas associated with the Gum nebula
title_fullStr Cold neutral gas associated with the Gum nebula
title_full_unstemmed Cold neutral gas associated with the Gum nebula
title_sort cold neutral gas associated with the gum nebula
publishDate 1997
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_03650138_v123_n1_p31_Reynoso
http://hdl.handle.net/20.500.12110/paper_03650138_v123_n1_p31_Reynoso
_version_ 1768543848893513728

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