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Class I methanol masers in low-mass star formation regions

Published online by Cambridge University Press:  24 July 2012

S. V. Kalenskii ,
V. I. Slysh ,
L. E. B. Johansson ,
P. Bergman ,
S. Kurtz ,
P. Hofner  and
C. M. Walmsley
S. V. Kalenskii
Affiliation:
Astro Space Center, Lebedev Physical Institute, 84/32 Profsoyuznaya st., Moscow, 117997, Russia email: [email protected]
V. I. Slysh
Affiliation:
Astro Space Center, Lebedev Physical Institute, 84/32 Profsoyuznaya st., Moscow, 117997, Russia email: [email protected]
L. E. B. Johansson
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden email: [email protected]
P. Bergman
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden email: [email protected]
S. Kurtz
Affiliation:
Centro de Radioastronomía y Astrofísica, Universidad Nacional Autonoma de México (Morelia, Michoacán, México) email: [email protected]
P. Hofner
Affiliation:
Physics Department, New Mexico Tech., 801 Leroy Pl., Socorro, NM 87801, and National Radio Astronomy Observatory, Socorro, NM 87801, USA email: [email protected]
C. M. Walmsley
Affiliation:
Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 1-50125 Firenze, Italy email: [email protected]
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Abstract

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Four Class I maser sources were detected at 44, 84, and 95 GHz toward chemically rich outflows in the regions of low-mass star formation NGC 1333I4A, NGC 1333I2A, HH25, and L1157. One more maser was found at 36 GHz toward a similar outflow, NGC 2023. Flux densities of the newly detected masers are no more than 18 Jy, being much lower than those of strong masers in regions of high-mass star formation. The brightness temperatures of the strongest peaks in NGC 1333I4A, HH25, and L1157 at 44 GHz are higher than 2000 K, whereas that of the peak in NGC 1333I2A is only 176 K. However, a rotational diagram analysis showed that the latter source is also a maser. The main properties of the newly detected masers are similar to those of Class I methanol masers in regions of massive star formation. The former masers are likely to be an extension of the latter maser population toward low luminosities of both the masers and the corresponding YSOs.

Keywords

masersISM: jets and outflowsISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 161 - 165
Copyright
Copyright © International Astronomical Union 2012

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