Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/118042
Title: The evolution of the H2O maser emission in the accretion burst source G358.93-0.03
Authors: Bayandina, O. S.
Brogan, C. L.
Burns, R. A.
Caratti o Garatti, A.
Chibueze, J. O.
Van Den Heever, S. P.
Kurtz, S. E.
MacLeod, G. C.
Moscadelli, L.
Sobolev, A. M.
Sugiyama, K.
Valâtts, I. E.
Yonekura, Y.
Issue Date: 2022
Publisher: EDP Sciences
Citation: The evolution of the H2O maser emission in the accretion burst source G358.93-0.03 / O. S. Bayandina, C. L. Brogan, R. A. Burns et al. // Astronomy and Astrophysics. — 2022. — Vol. 664. — A44.
Abstract: Context. The massive young stellar object (MYSO) G358.93-0.03-MM1 showed an extraordinary near-infrared- to (sub-)millimetredark and far-infrared-loud accretion burst, which is closely associated with flares of several class II methanol maser transitions, and, later, a 22 GHz water maser flare. Aims. Water maser flares provide an invaluable insight into ejection events associated with accretion bursts. Although the short timescale of the 22 GHz water maser flare made it impossible to carry out a very long baseline interferometry observation, we could track it with the Karl G. Jansky Very Large Array (VLA). Methods. The evolution of the spatial structure of the 22 GHz water masers and their association with the continuum sources in the region is studied with the VLA during two epochs, pre- and post-H2O maser flare. Results. A drastic change in the distribution of the water masers is revealed: in contrast to the four maser groups detected during epoch I, only two newly formed clusters are detected during epoch II. The 22 GHz water masers associated with the bursting source MM1 changed in morphology and emission velocity extent. Conclusions. Clear evidence of the influence of the accretion burst on the ejection from G358.93-0.03-MM1 is presented. The accretion event has also potentially affected a region with a radius of ∼200 (∼13 500AU at 6.75 kpc), suppressing water masers associated with other point sources in this region. © O. S. Bayandina et al. 2022.
Keywords: MASERS
STARS: EVOLUTION
STARS: FORMATION
STARS: INDIVIDUAL: G358.93-0.03
STARS: JETS
STARS: MASSIVE
INFRARED DEVICES
STARS
MASER EMISSIONS
STAR: EVOLUTION
STAR: INDIVIDUAL: G358.93-0.03
STARS FORMATION
STARS: INDIVIDUAL: PROXIMA CENTAURI
STARS: JETS
STARS: MASSIVE
VERY LARGE ARRAYS
WATER MASERS
YOUNG STELLAR OBJECTS
MASERS
URI: http://hdl.handle.net/10995/118042
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85135734965
ISSN: 46361
DOI: 10.1051/0004-6361/202244089
metadata.dc.description.sponsorship: Japan Society for the Promotion of Science, KAKEN: JP21H00032, JP21H01120, JP24340034; Ministry of Education and Science of the Russian Federation, Minobrnauka: 075-15-2020-780; National Astronomical Observatory of Japan, NAOJ
Acknowledgements. The Ibaraki 6.7-GHz Methanol Maser Monitor (iMet) program is partially supported by the Inter-university collaborative project “Japanese VLBI Network (JVN)” of NAOJ and JSPS KAKENHI Grant Numbers JP24340034, JP21H01120, and JP21H00032 (YY). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.00768.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. In addition, publications from NA authors must include the standard NRAO acknowledgement: The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. A.M.S. acknowledges support by the Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780. A.C.G. acknowledges support by PRIN-INAF-MAIN-STREAM 2017 “Protoplanetary disks seen through the eyes of new-generation instruments” and by PRIN-INAF 2019 “Spectroscopically tracing the disk dispersal evolution (STRADE)”.
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