SiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43A

We report here the first mapping of SiO v = 1 J  = 5 → 4 maser emission toward the “water fountain” source W 43A in order to explore the central stellar system driving the collimated, bipolar, fast jet. The maser source has a systemic line-of-sight velocity consistent with that of CO J  = 2 → 1 emis...

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Main Authors: Hiroshi Imai, Takeshi Hoshino, Daniel Tafoya, José F. Gómez, Jun-ichi Nakashima, Gabor Orosz
Format: Article
Language:English
Published: IOP Publishing 2025-01-01
Series:The Astrophysical Journal
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Online Access:https://doi.org/10.3847/1538-4357/adde4e
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author Hiroshi Imai
Takeshi Hoshino
Daniel Tafoya
José F. Gómez
Jun-ichi Nakashima
Gabor Orosz
author_facet Hiroshi Imai
Takeshi Hoshino
Daniel Tafoya
José F. Gómez
Jun-ichi Nakashima
Gabor Orosz
author_sort Hiroshi Imai
collection DOAJ
description We report here the first mapping of SiO v = 1 J  = 5 → 4 maser emission toward the “water fountain” source W 43A in order to explore the central stellar system driving the collimated, bipolar, fast jet. The maser source has a systemic line-of-sight velocity consistent with that of CO J  = 2 → 1 emission tracing the jet within ∼2 km s ^−1 but a velocity gradient opposite that of the jet. The dynamical center of the maser source is located within ∼10 mas (or ∼20 au) of the brightness peak of the central 1.3 mm continuum emission. The spatiokinematic properties of the SiO J  = 5 → 4 and J  = 1 → 0 masers suggest that they are associated with the root of a slow (10 km s ^−1 < V _outflow  << 100 km s ^−1 ) outflow with a large opening angle, and the central stellar system is contained within the inner maser region (∼20 au) during a possible common-envelope evolution.
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institution OA Journals
issn 1538-4357
language English
publishDate 2025-01-01
publisher IOP Publishing
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series The Astrophysical Journal
spelling doaj-art-71a11b6074644c1fab09ef5d1310e3562025-08-20T02:37:25ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01987211410.3847/1538-4357/adde4eSiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43AHiroshi Imai0https://orcid.org/0000-0002-0880-0091Takeshi Hoshino1Daniel Tafoya2https://orcid.org/0000-0002-2149-2660José F. Gómez3https://orcid.org/0000-0002-7065-542XJun-ichi Nakashima4https://orcid.org/0000-0003-3324-9462Gabor Orosz5https://orcid.org/0000-0002-5526-990XAmanogawa Galaxy Astronomy Research Center, Graduate School of Science and Engineering, Kagoshima University , 1-12-35 Korimoto, Kagoshima 890-0065, Japan ; hiroimai@km.kagoshima-u.ac.jp; Center for General Education, Institute for Comprehensive Education, Kagoshima University , 1-12-30 Korimoto, Kagoshima 890-0065, JapanFaculty of Science, Kagoshima University , 1-12-35 Korimoto, Kagoshima 890-0065, JapanDepartment of Space, Earth and Environment, Chalmers University of Technology , Onsala Space Observatory, 439 92 Onsala, SwedenInstituto de Astrofísica de Andalucía , CSIC, Glorieta de la Astronomía s/n, E-18008 Granada, SpainSchool of Physics and Astronomy, Sun Yat-sen University , Tang Jia Wan, Zhuhai 519082, People’s Republic of China; CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area, 67 Sun Yat-Sen University , 2 Duxue Road, Zhuhai 519082, Guangdong Province, People’s Republic of ChinaJoint Institute for VLBI ERIC , Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The NetherlandsWe report here the first mapping of SiO v = 1 J  = 5 → 4 maser emission toward the “water fountain” source W 43A in order to explore the central stellar system driving the collimated, bipolar, fast jet. The maser source has a systemic line-of-sight velocity consistent with that of CO J  = 2 → 1 emission tracing the jet within ∼2 km s ^−1 but a velocity gradient opposite that of the jet. The dynamical center of the maser source is located within ∼10 mas (or ∼20 au) of the brightness peak of the central 1.3 mm continuum emission. The spatiokinematic properties of the SiO J  = 5 → 4 and J  = 1 → 0 masers suggest that they are associated with the root of a slow (10 km s ^−1 < V _outflow  << 100 km s ^−1 ) outflow with a large opening angle, and the central stellar system is contained within the inner maser region (∼20 au) during a possible common-envelope evolution.https://doi.org/10.3847/1538-4357/adde4eCircumstellar masersStellar jetsStellar mass lossCommon envelope evolution
spellingShingle Hiroshi Imai
Takeshi Hoshino
Daniel Tafoya
José F. Gómez
Jun-ichi Nakashima
Gabor Orosz
SiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43A
The Astrophysical Journal
Circumstellar masers
Stellar jets
Stellar mass loss
Common envelope evolution
title SiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43A
title_full SiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43A
title_fullStr SiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43A
title_full_unstemmed SiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43A
title_short SiO v = 1 J = 5 → 4 Maser Emission from the Root of the “Water Fountain” Source W 43A
title_sort sio v 1 j 5 4 maser emission from the root of the water fountain source w 43a
topic Circumstellar masers
Stellar jets
Stellar mass loss
Common envelope evolution
url https://doi.org/10.3847/1538-4357/adde4e
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