Thermal methanol observations of the outflow from the G31.41+0.31 hot molecular core

E. Araya, P. Hofner, Stanley Eugene Kurtz Smith, L. Olmi, H. Linz

Resultado de la investigación: Contribución a una revistaArtículo

19 Citas (Scopus)

Resumen

The G31.41+0.31 region hosts one of the most prominent hot molecular cores known. Coincident with the hot molecular core is an outflow whose orientation has been controversial. We report VLA-C observations of thermal methanol (7 0 -6 1 A + , 44 GHz) toward the position of the G31.41+0.31 hot molecular core. Our goals are to clarify the orientation of the outflow and to study the properties of a molecular outflow from a very young region of massive star formation. We confirm that the outflow is indeed associated with the hot molecular core. Our observations strongly suggest that the outflow is oriented in the northeast-southwest direction. The outflow is massive (≳ 15 M⊙), with a dynamical time of the order of ∼4 × 10 3 yr, and has a wide-angle bipolar morphology.

Idioma originalInglés
Páginas (desde-hasta)420-426
Número de páginas7
PublicaciónAstrophysical Journal
Volumen675
N.º1
DOI
EstadoPublicada - 1 mar 2008

Huella dactilar

methanol
outflow
methyl alcohol
massive stars
star formation

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Araya, E. ; Hofner, P. ; Kurtz Smith, Stanley Eugene ; Olmi, L. ; Linz, H. / Thermal methanol observations of the outflow from the G31.41+0.31 hot molecular core. En: Astrophysical Journal. 2008 ; Vol. 675, N.º 1. pp. 420-426.
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abstract = "The G31.41+0.31 region hosts one of the most prominent hot molecular cores known. Coincident with the hot molecular core is an outflow whose orientation has been controversial. We report VLA-C observations of thermal methanol (7 0 -6 1 A + , 44 GHz) toward the position of the G31.41+0.31 hot molecular core. Our goals are to clarify the orientation of the outflow and to study the properties of a molecular outflow from a very young region of massive star formation. We confirm that the outflow is indeed associated with the hot molecular core. Our observations strongly suggest that the outflow is oriented in the northeast-southwest direction. The outflow is massive (≳ 15 M⊙), with a dynamical time of the order of ∼4 × 10 3 yr, and has a wide-angle bipolar morphology.",
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Thermal methanol observations of the outflow from the G31.41+0.31 hot molecular core. / Araya, E.; Hofner, P.; Kurtz Smith, Stanley Eugene; Olmi, L.; Linz, H.

En: Astrophysical Journal, Vol. 675, N.º 1, 01.03.2008, p. 420-426.

Resultado de la investigación: Contribución a una revistaArtículo

TY - JOUR

T1 - Thermal methanol observations of the outflow from the G31.41+0.31 hot molecular core

AU - Araya, E.

AU - Hofner, P.

AU - Kurtz Smith, Stanley Eugene

AU - Olmi, L.

AU - Linz, H.

PY - 2008/3/1

Y1 - 2008/3/1

N2 - The G31.41+0.31 region hosts one of the most prominent hot molecular cores known. Coincident with the hot molecular core is an outflow whose orientation has been controversial. We report VLA-C observations of thermal methanol (7 0 -6 1 A + , 44 GHz) toward the position of the G31.41+0.31 hot molecular core. Our goals are to clarify the orientation of the outflow and to study the properties of a molecular outflow from a very young region of massive star formation. We confirm that the outflow is indeed associated with the hot molecular core. Our observations strongly suggest that the outflow is oriented in the northeast-southwest direction. The outflow is massive (≳ 15 M⊙), with a dynamical time of the order of ∼4 × 10 3 yr, and has a wide-angle bipolar morphology.

AB - The G31.41+0.31 region hosts one of the most prominent hot molecular cores known. Coincident with the hot molecular core is an outflow whose orientation has been controversial. We report VLA-C observations of thermal methanol (7 0 -6 1 A + , 44 GHz) toward the position of the G31.41+0.31 hot molecular core. Our goals are to clarify the orientation of the outflow and to study the properties of a molecular outflow from a very young region of massive star formation. We confirm that the outflow is indeed associated with the hot molecular core. Our observations strongly suggest that the outflow is oriented in the northeast-southwest direction. The outflow is massive (≳ 15 M⊙), with a dynamical time of the order of ∼4 × 10 3 yr, and has a wide-angle bipolar morphology.

KW - H II regions

KW - ISM: clouds

KW - ISM: molecules

KW - Radio lines: ISM

UR - http://www.scopus.com/inward/record.url?scp=40249117405&partnerID=8YFLogxK

U2 - 10.1086/527284

DO - 10.1086/527284

M3 - Artículo

AN - SCOPUS:40249117405

VL - 675

SP - 420

EP - 426

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -