Molecular gas in the Cartwheel Galaxy

We present the first detection of molecular gas in the Cartwheel, the prototype of a collisional ring galaxy formed in the head-on encounter of two galaxies. Until now, only very little atomic gas and no CO had been detected in the centre, where gas is theoretically expected to pile up. Using the Sw...

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Guardado en:
Detalles Bibliográficos
Publicado: 1998
Materias:
Galaxies: individual: AM 0035-33
Galaxies: individual: The Cartwheel
Galaxies: ISM
Radio lines: galaxies
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v340_n2_pL51_Horellou
http://hdl.handle.net/20.500.12110/paper_00046361_v340_n2_pL51_Horellou
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_00046361_v340_n2_pL51_Horellou
record_format dspace
spelling paper:paper_00046361_v340_n2_pL51_Horellou2023-06-08T14:27:23Z Molecular gas in the Cartwheel Galaxy Galaxies: individual: AM 0035-33 Galaxies: individual: The Cartwheel Galaxies: ISM Radio lines: galaxies We present the first detection of molecular gas in the Cartwheel, the prototype of a collisional ring galaxy formed in the head-on encounter of two galaxies. Until now, only very little atomic gas and no CO had been detected in the centre, where gas is theoretically expected to pile up. Using the Swedish ESO Submm Telescope, we detected both 12CO(1-0) and (2-1) line emission towards the central position. The line ratio and the line widths suggest that the CO(2-1) emission is sub-thermal and that the CO(1-0) emission arises within the central 22″ (13 kpc); it is probably associated with the inner ring and nucleus. We infer a mass of molecular gas (H2) of 1.5 to 6109 M⊙, which is significantly higher than the ∼ 108 M· of atomic gas within that region. The low excitation of the gas, whether it is due to a low temperature or a low density, is consistent with the weak star-forming activity observed in the centre of the Cartwheel. 1998 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v340_n2_pL51_Horellou http://hdl.handle.net/20.500.12110/paper_00046361_v340_n2_pL51_Horellou
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Galaxies: individual: AM 0035-33
Galaxies: individual: The Cartwheel
Galaxies: ISM
Radio lines: galaxies
spellingShingle Galaxies: individual: AM 0035-33
Galaxies: individual: The Cartwheel
Galaxies: ISM
Radio lines: galaxies
Molecular gas in the Cartwheel Galaxy
topic_facet Galaxies: individual: AM 0035-33
Galaxies: individual: The Cartwheel
Galaxies: ISM
Radio lines: galaxies
description We present the first detection of molecular gas in the Cartwheel, the prototype of a collisional ring galaxy formed in the head-on encounter of two galaxies. Until now, only very little atomic gas and no CO had been detected in the centre, where gas is theoretically expected to pile up. Using the Swedish ESO Submm Telescope, we detected both 12CO(1-0) and (2-1) line emission towards the central position. The line ratio and the line widths suggest that the CO(2-1) emission is sub-thermal and that the CO(1-0) emission arises within the central 22″ (13 kpc); it is probably associated with the inner ring and nucleus. We infer a mass of molecular gas (H2) of 1.5 to 6109 M⊙, which is significantly higher than the ∼ 108 M· of atomic gas within that region. The low excitation of the gas, whether it is due to a low temperature or a low density, is consistent with the weak star-forming activity observed in the centre of the Cartwheel.
title Molecular gas in the Cartwheel Galaxy
title_short Molecular gas in the Cartwheel Galaxy
title_full Molecular gas in the Cartwheel Galaxy
title_fullStr Molecular gas in the Cartwheel Galaxy
title_full_unstemmed Molecular gas in the Cartwheel Galaxy
title_sort molecular gas in the cartwheel galaxy
publishDate 1998
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v340_n2_pL51_Horellou
http://hdl.handle.net/20.500.12110/paper_00046361_v340_n2_pL51_Horellou
_version_ 1768543063483875328

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