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Multi-scale observational study of G45.804-0.355 star-forming region

Published online by Cambridge University Press:  07 February 2024

M. Seidu Open the ORCID record for M. Seidu [Opens in a new window] ,
J. O. Chibueze Open the ORCID record for J. O. Chibueze [Opens in a new window] ,
G. A. Fuller ,
A. Avison  and
N. A Frimpong
M. Seidu*
Affiliation:
Centre for Space Research, North-West University, Potchefstroom, 2520, South Africa.
J. O. Chibueze
Affiliation:
Centre for Space Research, North-West University, Potchefstroom, 2520, South Africa. Department of Mathematical Sciences, University of South Africa, Roodepoort, 1709, South Africa Department of Physics and Astronomy, University of Nigeria, Nsukka, 410001, Nigeria
G. A. Fuller
Affiliation:
Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, School of Natural Science, The University of Manchester, Manchester, M13 9PL, UK I. Physikalisches Institut, University of Cologne, Zülpicher Str. 77, 50937 Köln, Germany
A. Avison
Affiliation:
Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, School of Natural Science, The University of Manchester, Manchester, M13 9PL, UK SKA Observatory, Jodrell Bank, Lower Withington, Macclesfield, SK11 9FT
N. A Frimpong
Affiliation:
Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, School of Natural Science, The University of Manchester, Manchester, M13 9PL, UK Ghana Space Science and Technology Institute, Ghana Atomic Energy Commission, LG80, Ghana
*
email: [email protected]
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Abstract

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This is a multi-wavelength study to examine the G45.804-0.355 massive star-forming region (SFR) and its environs. Using MeerKAT with angular resolution (θ) of 8″ at 1.28 GHz, we identify for the first time, a faint radio continuum emission core in G45.804-0.355. At 1.3 mm, ALMA observations (θ∼0″ 7) resolved the core into multiple dust continuum condensations including MM1 which was found to be the primary massive dust dense core in the region (mass Mc∼ 54.3M⊙). The dust continuum shows an arm-like extended emission within which other dense cores are situated. The velocity gradient of the MM1 core indicates that the source is associated with a rotation gas motion. The red- and blue-shifted lobes overlap at the position of MM1. The compact morphology of the 4.5 μm IR emission, the presence of spiral arms and overlapping of the red- and blue-shifted lobes suggest a face-on geometry of G45.80-40.355.

Keywords

stars: formation(ISM:) HII regionsISM: jets and outflowsISM: kinematics and dynamicsISM: individual (AGAL045.804–00.356)instrumentation: interferometers
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. 235 - 237
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

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