Skip to main content Accessibility help
×
Home
Hostname: page-component-564cf476b6-pxp6n Total loading time: 0.265 Render date: 2021-06-21T22:42:32.993Z Has data issue: true Feature Flags: { "shouldUseShareProductTool": true, "shouldUseHypothesis": true, "isUnsiloEnabled": true, "metricsAbstractViews": false, "figures": true, "newCiteModal": false, "newCitedByModal": true, "newEcommerce": true }

Class I methanol masers in low-mass star formation regions

Published online by Cambridge University Press:  24 July 2012

S. V. Kalenskii
Affiliation:
Astro Space Center, Lebedev Physical Institute, 84/32 Profsoyuznaya st., Moscow, 117997, Russia email: kalensky@asc.rssi.ru
V. I. Slysh
Affiliation:
Astro Space Center, Lebedev Physical Institute, 84/32 Profsoyuznaya st., Moscow, 117997, Russia email: kalensky@asc.rssi.ru
L. E. B. Johansson
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden email: pbergman@chalmers.se
P. Bergman
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, 439 92 Onsala, Sweden email: pbergman@chalmers.se
S. Kurtz
Affiliation:
Centro de Radioastronomía y Astrofísica, Universidad Nacional Autonoma de México (Morelia, Michoacán, México) email: s.kurtz@crya.unam.mx
P. Hofner
Affiliation:
Physics Department, New Mexico Tech., 801 Leroy Pl., Socorro, NM 87801, and National Radio Astronomy Observatory, Socorro, NM 87801, USA email: hofner_p@yahoo.com
C. M. Walmsley
Affiliation:
Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 1-50125 Firenze, Italy email: walmsley@arcetri.astro.it
Rights & Permissions[Opens in a new window]

Abstract

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.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

References

Bachiller, R., Codella, C., Colomer, F., Liechti, S., & Walmsley, C. M. 1998, A&A, 335, 266Google Scholar
Bae, J.-H., Kim, K.-T., Youn, S.-Y., Kim, W.-J., Byun, D.-Y., Kang, H., & Oh, C. S., 2011, ApJS 196, 21CrossRefGoogle Scholar
Benedettini, M., Viti, S., Codella, C., Bachiller, R., Gueth, F., Beltran, M. T., Dutrey, A., & Guilloteau, S. 2007, Mon. Not. R. Astron. Soc., 381, 1127CrossRefGoogle Scholar
Chen, X., Ellingsen, S. P., & Shen, Z.-Q. 2009, Mon. Not. R. Astron. Soc., 396, 1603CrossRefGoogle Scholar
Gibb, A. & Davis, C. J. 1998, Mon. Not. R. Astron. Soc., 298, 644CrossRefGoogle Scholar
Kalenskii, S. V., Promyslov, V. G., Slysh, V. I., Bergman, P., & Winnberg, A. 2006, Astron. Rep., 50, 289CrossRefGoogle Scholar
Kalenskii, S. V., Johansson, L. E. B., Bergman, P., Kurtz, S., Hofner, P., Walmsley, C. M., & Slysh, V. I., 2010, Mon. Not. R. Astron. Soc., 405, 613Google Scholar
Kalenskii, S. V., Kurtz, S., Slysh, V. I., Hofner, P., Walmsley, C. M., Johansson, L. E. B., & Bergman, P. 2010, Astron. Rep., 54, 932CrossRefGoogle Scholar
Plambeck, R. L. & Menten, K. M. 1990, ApJ, 364, 555CrossRefGoogle Scholar
Pratap, P., Shute, P. A., Keane, T. C., Battersby, C., & Sterling, S. 2008, AJ, 135, 1718CrossRefGoogle Scholar
Sobolev, A. M., Wallin, B. K., & Watson, W. D. 1998, ApJ, 498, 763CrossRefGoogle Scholar
Zhou, S. 1996, in van Dishoeck, E. F., ed, Proc. IAU Symp. 178, Molecules in Astrophysics: Probes and Processes, Kluwer, Dordrecht, p. 195Google Scholar
Viti, S., Codella, C., Benedettini, M., & Bachiller, R. 2004, Mon. Not. R. Astron. Soc., 350, 1029CrossRefGoogle Scholar
You have Access

Send article to Kindle

To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

Find out more about the Kindle Personal Document Service.

Class I methanol masers in low-mass star formation regions
Available formats
×

Send article to Dropbox

To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

Class I methanol masers in low-mass star formation regions
Available formats
×

Send article to Google Drive

To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

Class I methanol masers in low-mass star formation regions
Available formats
×
×

Reply to: Submit a response

Please enter your response.

Your details

Please enter a valid email address.

Conflicting interests

Do you have any conflicting interests? *