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Volume-limited radio survey of ultracool dwarfs

Antonova, A. and Hallinan, G. and Doyle, J. G. and Yu, S. and Kuznetsov, A. and Metodieva, Y. and Golden, A. and Cruz, K. L. (2013) Volume-limited radio survey of ultracool dwarfs. Astronomy and Astrophysics, 549 . Art. No. A131. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20140205-143458443

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Abstract

Aims. We aim to increase the sample of ultracool dwarfs studied in the radio domain to allow a more statistically significant understanding of the physical conditions associated with these magnetically active objects. Methods. We conducted a volume-limited survey at 4.9 GHz of 32 nearby ultracool dwarfs with spectral types covering the range M7–T8. A statistical analysis was performed on the combined data from the present survey and previous radio observations of ultracool dwarfs. Results. Whilst no radio emission was detected from any of the targets, significant upper limits were placed on the radio luminosities that are below the luminosities of previously detected ultracool dwarfs. Combining our results with those from the literature gives a detection rate for dwarfs in the spectral range M7–L3.5 of ~9%. In comparison, only one dwarf later than L3.5 is detected in 53 observations. We report the observed detection rate as a function of spectral type and the number distribution of the dwarfs as a function of spectral type and rotation velocity. Conclusions. The radio observations to date point to a drop in the detection rate toward the ultracool dwarfs. However, the emission levels of detected ultracool dwarfs are comparable to those of earlier type active M dwarfs, which may imply that a mildly relativistic electron beam or a strong magnetic field can exist in ultracool dwarfs. Fast rotation may be a sufficient condition to produce magnetic fields strengths of several hundred Gauss to several kilo Gauss, as suggested by the data for the active ultracool dwarfs with known rotation rates. A possible reason for the non-detection of radio emission from some dwarfs is that maybe the centrifugal acceleration mechanism in these dwarfs is weak (due to a low rotation rate) and thus cannot provide the necessary density and/or energy of accelerated electrons. An alternative explanation could be long-term variability, as is the case for several ultracool dwarfs whose radio emission varies considerably over long periods with emission levels dropping below the detection limit in some instances.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1212.3464arXivDiscussion Paper
http://dx.doi.org/10.1051/0004-6361/201118583 DOIArticle
http://www.aanda.org/articles/aa/abs/2013/01/aa18583-11/aa18583-11.htmlPublisherArticle
ORCID:
AuthorORCID
Hallinan, G.0000-0002-7083-4049
Golden, A.0000-0002-8599-2031
Cruz, K. L.0000-0002-1821-0650
Additional Information:© 2013 ESO. Article published by EDP Sciences. Received 5 December 2011; Accepted 19 November 2012. Published online 15 January 2013. We gratefully acknowledge funding for this project by the Bulgarian National Science Fund (contract No DDVU02/40/2010). Research at Armagh Observatory is grant-aided by the N. Ireland Department of Culture, Arts and Leisure. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. AKU, SYU & JGD thank the Leverhulme Trust for their support of this project.
Funders:
Funding AgencyGrant Number
Bulgarian National Science FundDDVU02/40/2010
Northern Ireland Department of Culture, Arts and Leisure (Northern Ireland)UNSPECIFIED
Leverhulme TrustUNSPECIFIED
Subject Keywords:stars: low-mass; brown dwarfs; radiation mechanisms: general; radio continuum: stars; masers
Record Number:CaltechAUTHORS:20140205-143458443
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20140205-143458443
Official Citation: Volume-limited radio survey of ultracool dwarfs A. Antonova, G. Hallinan, J. G. Doyle, S. Yu, A. Kuznetsov, Y. Metodieva, A. Golden, K. L. Cruz A&A 549 A131 (2013) DOI: 10.1051/0004-6361/201118583
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43678
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:03 Mar 2014 19:26
Last Modified:09 Mar 2020 13:18

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