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The Astrometric Animation of Water Masers toward the Mira Variable BX Cam. / Xu, Shuangjing; Imai, Hiroshi; Yun, Youngjoo et al.
In: Astrophysical Journal, Vol. 941, No. 2, 105, 01.12.2022.

Research output: Contribution to journal › Article › peer-review

Harvard

Xu, S, Imai, H, Yun, Y, Zhang, B, Rioja, MJ, Dodson, R, Cho, S, Kim, J, Cui, L, Sobolev, AM, Chibueze, JO, Kim, D, Amada, K, Nakashima, J, Orosz, G, Oyadomari, M, Oh, S, Yonekura, Y, Sun, Y, Mai, X, Zhang, J, Wen, S & Jung, T 2022, 'The Astrometric Animation of Water Masers toward the Mira Variable BX Cam', Astrophysical Journal, vol. 941, no. 2, 105. https://doi.org/10.3847/1538-4357/ac9599

APA

Xu, S., Imai, H., Yun, Y., Zhang, B., Rioja, M. J., Dodson, R., Cho, S., Kim, J., Cui, L., Sobolev, A. M., Chibueze, J. O., Kim, D., Amada, K., Nakashima, J., Orosz, G., Oyadomari, M., Oh, S., Yonekura, Y., Sun, Y., ... Jung, T. (2022). The Astrometric Animation of Water Masers toward the Mira Variable BX Cam. Astrophysical Journal, 941(2), [105]. https://doi.org/10.3847/1538-4357/ac9599

Vancouver

Xu S, Imai H, Yun Y, Zhang B, Rioja MJ, Dodson R et al. The Astrometric Animation of Water Masers toward the Mira Variable BX Cam. Astrophysical Journal. 2022 Dec 1;941(2):105. doi: 10.3847/1538-4357/ac9599

Author

Xu, Shuangjing ; Imai, Hiroshi ; Yun, Youngjoo et al. / The Astrometric Animation of Water Masers toward the Mira Variable BX Cam. In: Astrophysical Journal. 2022 ; Vol. 941, No. 2.

BibTeX

@article{b20ca30942bd4e4a9efab7329ca462d8,
title = "The Astrometric Animation of Water Masers toward the Mira Variable BX Cam",
abstract = "We report very long baseline interferometry (VLBI) monitoring observations of the 22 GHz water (H2O) masers around the Mira variable BX Cam, which were carried out as a part of the EAVN Synthesis of Stellar Maser Animations project. Data of 37 epochs in total were obtained from 2018 May to 2021 June with a time interval of 3-4 weeks, spanning approximately three stellar pulsation periods (P = ∼440 days). In particular, the dual-beam system equipped on the VERA stations was used to measure the kinematics and parallaxes of the H2O maser features. The measured parallax, π = 1.79 ± 0.08 mas, is consistent with Gaia EDR3 and previously measured VLBI parallaxes within a 1σ error level. The position of the central star was estimated, based on both the Gaia EDR3 data and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser distribution imaged with the Korean VLBI Network. The three-dimensional H2O maser kinematics indicates that the circumstellar envelope is expanding at a velocity of 13 ± 4 km s−1, while there are asymmetries in both the spatial and velocity distributions of the maser features. Furthermore, the H2O maser animation achieved by our dense monitoring program manifests the propagation of shock waves in the circumstellar envelope of BX Cam. {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society.",
author = "Shuangjing Xu and Hiroshi Imai and Youngjoo Yun and Bo Zhang and Rioja, {Mar{\'i}a J.} and Richard Dodson and Se-hyung Cho and Jaeheon Kim and Lang Cui and Sobolev, {Andrey M.} and Chibueze, {James O.} and Dong-jin Kim and Kei Amada and Jun-ichi Nakashima and Gabor Orosz and Miyako Oyadomari and Sejin Oh and Yoshinori Yonekura and Yan Sun and Xiaofeng Mai and Jingdong Zhang and Shiming Wen and Taehyun Jung",
note = "We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. We are grateful to all staff members in EAVN who helped to operate the array and to correlate the data. Particularly, the interferometer model (IM) files are provided by Mr. DongKyu Jung, and the delay recalculation tables are made by Dr. Takumi Nagayama and Dr. Kazuya Hachisuka. The KVN is a facility operated by the Korea Astronomy and Space Science Institute (KASI), and VERA is a facility operated by the National Astronomical Observatory of Japan (NAOJ) in collaboration with associated universities in Japan. The Tianma 65 m telescope is operated by Shanghai Astronomical Observatory (SHAO). The Nanshan 26 m telescope is operated by Xinjiang Astronomical Observatory (XAO). The Takahagi 32 m telescope is operated by NAOJ and Ibaraki University and partially supported by the Inter-university collaborative project “Japanese VLBI Network (JVN)” of NAOJ. H.I. and M.O. were supported by JSPS KAKENHI JP16H02167. L.C. is supported by the CAS “Light of West China” Program (grant No. 2021-XBQNXZ-005) and the National Natural Science Foundation of China (grant No. U2031212). A.M.S. was supported by the Russian Ministry of Science and Higher Education, No. FEUZ-2020-0030. B.Z. was supported by the National Natural Science Foundation of China (grant Nos. U2031212 and U1831136) and Shanghai Astronomical Observatory, Chinese Academy of Sciences (grant No. N2020-06-19-005).",
year = "2022",
month = dec,
day = "1",
doi = "10.3847/1538-4357/ac9599",
language = "English",
volume = "941",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing (IOP)",
number = "2",

}

RIS

TY - JOUR

T1 - The Astrometric Animation of Water Masers toward the Mira Variable BX Cam

AU - Xu, Shuangjing

AU - Imai, Hiroshi

AU - Yun, Youngjoo

AU - Zhang, Bo

AU - Rioja, María J.

AU - Dodson, Richard

AU - Cho, Se-hyung

AU - Kim, Jaeheon

AU - Cui, Lang

AU - Sobolev, Andrey M.

AU - Chibueze, James O.

AU - Kim, Dong-jin

AU - Amada, Kei

AU - Nakashima, Jun-ichi

AU - Orosz, Gabor

AU - Oyadomari, Miyako

AU - Oh, Sejin

AU - Yonekura, Yoshinori

AU - Sun, Yan

AU - Mai, Xiaofeng

AU - Zhang, Jingdong

AU - Wen, Shiming

AU - Jung, Taehyun

N1 - We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research. We are grateful to all staff members in EAVN who helped to operate the array and to correlate the data. Particularly, the interferometer model (IM) files are provided by Mr. DongKyu Jung, and the delay recalculation tables are made by Dr. Takumi Nagayama and Dr. Kazuya Hachisuka. The KVN is a facility operated by the Korea Astronomy and Space Science Institute (KASI), and VERA is a facility operated by the National Astronomical Observatory of Japan (NAOJ) in collaboration with associated universities in Japan. The Tianma 65 m telescope is operated by Shanghai Astronomical Observatory (SHAO). The Nanshan 26 m telescope is operated by Xinjiang Astronomical Observatory (XAO). The Takahagi 32 m telescope is operated by NAOJ and Ibaraki University and partially supported by the Inter-university collaborative project “Japanese VLBI Network (JVN)” of NAOJ. H.I. and M.O. were supported by JSPS KAKENHI JP16H02167. L.C. is supported by the CAS “Light of West China” Program (grant No. 2021-XBQNXZ-005) and the National Natural Science Foundation of China (grant No. U2031212). A.M.S. was supported by the Russian Ministry of Science and Higher Education, No. FEUZ-2020-0030. B.Z. was supported by the National Natural Science Foundation of China (grant Nos. U2031212 and U1831136) and Shanghai Astronomical Observatory, Chinese Academy of Sciences (grant No. N2020-06-19-005).

PY - 2022/12/1

Y1 - 2022/12/1

N2 - We report very long baseline interferometry (VLBI) monitoring observations of the 22 GHz water (H2O) masers around the Mira variable BX Cam, which were carried out as a part of the EAVN Synthesis of Stellar Maser Animations project. Data of 37 epochs in total were obtained from 2018 May to 2021 June with a time interval of 3-4 weeks, spanning approximately three stellar pulsation periods (P = ∼440 days). In particular, the dual-beam system equipped on the VERA stations was used to measure the kinematics and parallaxes of the H2O maser features. The measured parallax, π = 1.79 ± 0.08 mas, is consistent with Gaia EDR3 and previously measured VLBI parallaxes within a 1σ error level. The position of the central star was estimated, based on both the Gaia EDR3 data and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser distribution imaged with the Korean VLBI Network. The three-dimensional H2O maser kinematics indicates that the circumstellar envelope is expanding at a velocity of 13 ± 4 km s−1, while there are asymmetries in both the spatial and velocity distributions of the maser features. Furthermore, the H2O maser animation achieved by our dense monitoring program manifests the propagation of shock waves in the circumstellar envelope of BX Cam. © 2022. The Author(s). Published by the American Astronomical Society.

AB - We report very long baseline interferometry (VLBI) monitoring observations of the 22 GHz water (H2O) masers around the Mira variable BX Cam, which were carried out as a part of the EAVN Synthesis of Stellar Maser Animations project. Data of 37 epochs in total were obtained from 2018 May to 2021 June with a time interval of 3-4 weeks, spanning approximately three stellar pulsation periods (P = ∼440 days). In particular, the dual-beam system equipped on the VERA stations was used to measure the kinematics and parallaxes of the H2O maser features. The measured parallax, π = 1.79 ± 0.08 mas, is consistent with Gaia EDR3 and previously measured VLBI parallaxes within a 1σ error level. The position of the central star was estimated, based on both the Gaia EDR3 data and the center position of the ring-like 43 GHz silicon-monoxide (SiO) maser distribution imaged with the Korean VLBI Network. The three-dimensional H2O maser kinematics indicates that the circumstellar envelope is expanding at a velocity of 13 ± 4 km s−1, while there are asymmetries in both the spatial and velocity distributions of the maser features. Furthermore, the H2O maser animation achieved by our dense monitoring program manifests the propagation of shock waves in the circumstellar envelope of BX Cam. © 2022. The Author(s). Published by the American Astronomical Society.

UR - http://www.scopus.com/inward/record.url?partnerID=8YFLogxK&scp=85144737533

UR - https://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcAuth=tsmetrics&SrcApp=tsm_test&DestApp=WOS_CPL&DestLinkType=FullRecord&KeyUT=000895911700001

U2 - 10.3847/1538-4357/ac9599

DO - 10.3847/1538-4357/ac9599

M3 - Article

VL - 941

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 105

ER -

ID: 33221878