Volume 588, April 2016
|Number of page(s)||4|
|Published online||09 March 2016|
Two confirmed class I very low-mass objects in Taurus
1 Department of PhysicsHCM International University-VNU, Block 6, Linh Trung Ward, Thu Duc District, HCM city, Viet Nam
2 Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, 106 Taipei, Taiwan, ROC
3 Faculty of Physics and Engineering Physics, HCM University of Science-VNU, 227 Nguyen Van Cu Street, District 5, HCM city, Viet Nam
Received: 10 December 2015
Accepted: 10 February 2016
Context. [GKH94] 41 and IRAS 04191+1523B were previously identified to be proto-brown dwarf candidates in Taurus. [GKH94] 41 was classified to be a class I object. The dereddened spectral energy distribution of the source was later found to be suggestive of a class II object. IRAS 04191+1523B is a class I object that is the secondary component of a binary.
Aims. We determine the evolutionary stage of [GKH94] 41 and estimate the final masses of the two proto-brown dwarf candidates.
Methods. We used archive millimeter observations to produce continuum maps and collected data from the literature to construct the spectral energy distribution of the targets.
Results. Our continuum maps revealed that both [GKH94] 41 and IRAS 04191+1523B are surrounded by envelopes. This provides direct evidence that [GKH94] 41 is a class I object, not class II, as previously classified. For IRAS 04191+1523B, our continuum map spatially resolved the binary. Our estimated final masses are below 49-27+56 MJ and 75-26+40 MJ for [GKH94] 41 and IRAS 04191+1523B, respectively. This indicates that both sources will likely become brown dwarfs or very low-mass stars. Therefore, [GKH94] 41 and IRAS 04191+1523B are two new confirmed class I very low-mass objects. Their existence also supports the scenario that brown dwarfs have the same formation stages as low-mass stars.
Key words: brown dwarfs / stars: formation / stars: protostars / techniques: interferometric
© ESO, 2016
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