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Water Maser Zeeman Splitting in the Ionized Jet IRAS 19035+0641 A

Published online by Cambridge University Press:  07 February 2024

Tatiana M. Rodríguez Open the ORCID record for Tatiana M. Rodríguez [Opens in a new window] ,
Emmanuel Momjian ,
Peter Hofner ,
Anuj P. Sarma  and
Esteban D. Araya
Tatiana M. Rodríguez*
Affiliation:
New Mexico Tech, 801 Leroy Pl., Socorro, NM 87801, USA.
Emmanuel Momjian
Affiliation:
National Radio Astronomy Observatory, P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801, USA.
Peter Hofner
Affiliation:
New Mexico Tech, 801 Leroy Pl., Socorro, NM 87801, USA. National Radio Astronomy Observatory, P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801, USA.
Anuj P. Sarma
Affiliation:
Physics and Astrophysics Department, DePaul University, 2219 N. Kenmore Ave., Chicago, IL 60614, USA.
Esteban D. Araya
Affiliation:
New Mexico Tech, 801 Leroy Pl., Socorro, NM 87801, USA. Physics Department, Western Illinois University, 1 University Circle, Macomb, IL 61455, USA.
*
email: [email protected]
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Abstract

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A key ingredient in the earliest evolutionary phase of high-mass (M>8 M⊙) star formation (HMSF) is the presence of a jet/outflow system. To study its role in HMSF, we have carried out high resolution (0.1″) VLA K-band (18-26.5 GHz) observations toward IRAS 19035+0641 A, identified as a high-mass protostellar jet candidate based on previous cm continuum data. Our observations resolve the continuum emission into an elongated structure in the NE-SW direction, confirming that the K-band continuum arises from an ionized jet. Furthermore, we detected several 22.2 GHz H2O maser spots aligned in a direction consistent with the jet axis. Zeeman splitting was detected in the strongest maser spot. In this paper, we present our results and discuss the implications of our findings.

Keywords

Radio jetsWater masersMassive starsMagnetic fields
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. 232 - 234
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Araya, E. D., Hofner, P., Kurtz, S., Bronfman, L., DeDeo, S. 2005, ApJS, 157, 279.10.1086/427187CrossRefGoogle Scholar
Crutcher, R. M. 1999, ApJ, 520, 706.10.1086/307483CrossRefGoogle Scholar
Rosero, V., Hofner, P., Claussen, M., Kurtz, S., Cesaroni, R. et al. 2016, ApJS, 227, 25.10.3847/1538-4365/227/2/25CrossRefGoogle Scholar
Sarma, A. P., Troland, T. H., Crutcher, R. M., Roberts, D. A. 2002, ApJ, 580, 928. 10.1086/343799CrossRefGoogle Scholar