Hostname: page-component-78c5997874-g7gxr Total loading time: 0 Render date: 2024-11-14T17:29:26.931Z Has data issue: false hasContentIssue false
  • English
  • Français

Spatio-kinematics of water masers in the HMSFR NGC6334I before and during an accretion burst

Published online by Cambridge University Press:  07 February 2024

Jakobus M. Vorster Open the ORCID record for Jakobus M. Vorster [Opens in a new window] ,
James O. Chibueze Open the ORCID record for James O. Chibueze [Opens in a new window] ,
Tomoya Hirota Open the ORCID record for Tomoya Hirota [Opens in a new window]  and
Gordon C. MacLeod
Jakobus M. Vorster*
Affiliation:
University of Helsinki, Finland North-West University, South Africa,
James O. Chibueze
Affiliation:
North-West University, South Africa, Department of Mathematical Sciences, University of South Africa, Roodepoort, South Africa University of Nigeria, Nigeria
Tomoya Hirota
Affiliation:
National Astronomical Observatory of Japan, Japan SOKENDAI (The Graduate University for Advanced Studies), Japan
Gordon C. MacLeod
Affiliation:
The Open University of Tanzania, Tanzania SARAO Hartebeesthoek Astronomical Observatory, South Africa
*
email: jakobus.vorster@helsinki.fi
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In 2015, the high-mass star-forming region NGC6334I-MM1 underwent an accretion burst. Using VERA, we monitored 22 GHz water masers before and during the accretion burst to observe the changes in the maser spatial and velocity distributions in the region. The masers in CM2-W2 and MM1-W1 displayed variability that could be attributed to the accretion burst. The bright masers in CM2-W2 were found to better trace the shock structure as the epochs progressed. The mean 3D speeds derived from the proper motions were 50 km/s and 54 km/s for the pre-burst and burst epochs respectively. High-velocity proper motions were found at the southern edges of the N-S (∼80 km s−1) and NW-SE (∼150 km s−1) bipolar outflows. The precise mechanism of the flaring of the water masers due to the accretion burst has yet to be investigated.

Keywords

masersstars: formationISM: jets and outflows
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 258 - 260
Check for updates
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Brogan, C.L., Hunter, T.R., Cyganowski, C.J., et al. 2018, ApJ, 866, 87 10.3847/1538-4357/aae151CrossRefGoogle Scholar
Hunter, T.R., Brogan, C.L., MacLeod, G.C., et al. 2017, ApJ, 837, L29 10.3847/2041-8213/aa5d0eCrossRefGoogle Scholar
MacLeod, G.C., Smits, D.P., Goedhart, S., et al. 2018, MNRAS, 478, 1077 10.1093/mnras/sty996CrossRefGoogle Scholar
Hollenbach, D., Elitzur, M. and McKee, C.F. 2013, ApJ, 773, 70 10.1088/0004-637X/773/1/70CrossRefGoogle Scholar
Chibueze, J.O., MacLeod, G.C, Vorster, J.M., et al. 2021, ApJ, 908, 175 10.3847/1538-4357/abd474CrossRefGoogle Scholar
Supplementary material: PDF

Vorster et al. supplementary material

Vorster et al. supplementary material

Download Vorster et al. supplementary material(PDF)
PDF 3.5 MB