Cepheus a east: Unraveling the mysteries

Jennifer A. Goetz; J. L. Pipher; W. J. Forrest; Dan M. Watson; S. N. Raines; Charles E. Woodward; M. A. Greenhouse; H. A. Smith; V. A. Hughes; J. Fischer

doi:10.1086/306058

Cepheus a east: Unraveling the mysteries

Jennifer A. Goetz, J. L. Pipher, W. J. Forrest, Dan M. Watson, S. N. Raines, Charles E. Woodward, M. A. Greenhouse, H. A. Smith, V. A. Hughes, J. Fischer

Minnesota Institute for Astrophysics

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Abstract

New infrared images of Cep A East are presented that show two regions of shock-excited line emission from separate bipolar flows. We identify the dominant sources powering the outflows and argue that the results support a multiple outflow model (Narayanan & Walker) as opposed to a quadrupolar outflow scenario. The images include near-infrared broadband (k [2.158 μm], L″ [3.81 μm], and M' [4.67 μm]) and spectral line ([Fe II] emission line at 1.644 μm and H₂ 1-0 S[1] line at 2.122 μm) observations, as well as continuum emission, at 1.644 μm and 2.122 μm Considering our data and other results, we present a unified, self-consistent picture of the disk and shock structure. The northern emission region appears to be the result of the ablation of a dense molecular clump (coincident with HW 6) in the path of a diverting jet from YSO HW 2 and subsequent multiple bow shocks with prompt entrainment arising from the interaction of the jet with the molecular cloud Cep A-2. The southern line emission region near H W 7 resembles the " artillery shell " bow shocks found in Orion and is most likely a J-type shock caused by a jet from another YSO, possibly HW 3(d)ii.

Original language	English (US)
Pages (from-to)	359-374
Number of pages	16
Journal	Astrophysical Journal
Volume	504
Issue number	1 PART I
DOIs	https://doi.org/10.1086/306058
State	Published - 1998

Keywords

H II regions
ISM: individual (Cepheus A East)
ISM: molecules
Infrared: stars
Stars: formation
Stars: pre-main-sequence

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title = "Cepheus a east: Unraveling the mysteries",

abstract = "New infrared images of Cep A East are presented that show two regions of shock-excited line emission from separate bipolar flows. We identify the dominant sources powering the outflows and argue that the results support a multiple outflow model (Narayanan & Walker) as opposed to a quadrupolar outflow scenario. The images include near-infrared broadband (k [2.158 μm], L″ [3.81 μm], and M' [4.67 μm]) and spectral line ([Fe II] emission line at 1.644 μm and H2 1-0 S[1] line at 2.122 μm) observations, as well as continuum emission, at 1.644 μm and 2.122 μm Considering our data and other results, we present a unified, self-consistent picture of the disk and shock structure. The northern emission region appears to be the result of the ablation of a dense molecular clump (coincident with HW 6) in the path of a diverting jet from YSO HW 2 and subsequent multiple bow shocks with prompt entrainment arising from the interaction of the jet with the molecular cloud Cep A-2. The southern line emission region near H W 7 resembles the {"} artillery shell {"} bow shocks found in Orion and is most likely a J-type shock caused by a jet from another YSO, possibly HW 3(d)ii.",

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author = "Goetz, {Jennifer A.} and Pipher, {J. L.} and Forrest, {W. J.} and Watson, {Dan M.} and Raines, {S. N.} and Woodward, {Charles E.} and Greenhouse, {M. A.} and Smith, {H. A.} and Hughes, {V. A.} and J. Fischer",

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T2 - Unraveling the mysteries

AU - Goetz, Jennifer A.

AU - Pipher, J. L.

AU - Forrest, W. J.

AU - Watson, Dan M.

AU - Raines, S. N.

AU - Woodward, Charles E.

AU - Greenhouse, M. A.

AU - Smith, H. A.

AU - Hughes, V. A.

AU - Fischer, J.

PY - 1998

Y1 - 1998

N2 - New infrared images of Cep A East are presented that show two regions of shock-excited line emission from separate bipolar flows. We identify the dominant sources powering the outflows and argue that the results support a multiple outflow model (Narayanan & Walker) as opposed to a quadrupolar outflow scenario. The images include near-infrared broadband (k [2.158 μm], L″ [3.81 μm], and M' [4.67 μm]) and spectral line ([Fe II] emission line at 1.644 μm and H2 1-0 S[1] line at 2.122 μm) observations, as well as continuum emission, at 1.644 μm and 2.122 μm Considering our data and other results, we present a unified, self-consistent picture of the disk and shock structure. The northern emission region appears to be the result of the ablation of a dense molecular clump (coincident with HW 6) in the path of a diverting jet from YSO HW 2 and subsequent multiple bow shocks with prompt entrainment arising from the interaction of the jet with the molecular cloud Cep A-2. The southern line emission region near H W 7 resembles the " artillery shell " bow shocks found in Orion and is most likely a J-type shock caused by a jet from another YSO, possibly HW 3(d)ii.

AB - New infrared images of Cep A East are presented that show two regions of shock-excited line emission from separate bipolar flows. We identify the dominant sources powering the outflows and argue that the results support a multiple outflow model (Narayanan & Walker) as opposed to a quadrupolar outflow scenario. The images include near-infrared broadband (k [2.158 μm], L″ [3.81 μm], and M' [4.67 μm]) and spectral line ([Fe II] emission line at 1.644 μm and H2 1-0 S[1] line at 2.122 μm) observations, as well as continuum emission, at 1.644 μm and 2.122 μm Considering our data and other results, we present a unified, self-consistent picture of the disk and shock structure. The northern emission region appears to be the result of the ablation of a dense molecular clump (coincident with HW 6) in the path of a diverting jet from YSO HW 2 and subsequent multiple bow shocks with prompt entrainment arising from the interaction of the jet with the molecular cloud Cep A-2. The southern line emission region near H W 7 resembles the " artillery shell " bow shocks found in Orion and is most likely a J-type shock caused by a jet from another YSO, possibly HW 3(d)ii.

KW - H II regions

KW - ISM: individual (Cepheus A East)

KW - ISM: molecules

KW - Infrared: stars

KW - Stars: formation

KW - Stars: pre-main-sequence

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Cepheus a east: Unraveling the mysteries

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Keywords

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