LMT/AzTEC observations of Vega
Article
Article Title | LMT/AzTEC observations of Vega |
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ERA Journal ID | 1074 |
Article Category | Article |
Authors | Marshall, J P, Chavez-Dagostino, M, Sanchez-Arguelles, D, Matra, L, Del Burgo, C, Kemper, F, Bertone, E, Dent, W R F, Vega, O, Wilson, G, Gómez-Ruiz, A and Montaña, A |
Journal Title | Monthly Notices of the Royal Astronomical Society |
Journal Citation | 514 (3), pp. 3815-3820 |
Number of Pages | 6 |
Year | 2022 |
Publisher | Oxford University Press |
Place of Publication | United Kingdom |
ISSN | 0035-8711 |
1365-2966 | |
Digital Object Identifier (DOI) | https://doi.org/10.1093/mnras/stac1510 |
Web Address (URL) | https://academic.oup.com/mnras/article/514/3/3815/6603855 |
Abstract | Vega is the prototypical debris disc system. Its architecture has been extensively studied at optical to millimetre wavelengths, revealing a near face-on, broad, and smooth disc with multiple distinct components. Recent millimetre-wavelength observations from ALMA spatially resolved the inner edge of the outer, cold planetesimal belt from the star for the first time. Here we present early science imaging observations of the Vega system with the AzTEC instrument on the 32-m LMT, tracing extended emission from the disc out to 150 au from the star. We compare the observations to three models of the planetesimal belt architecture to better determine the profile of the outer belt. A comparison of these potential architectures for the disc does not significantly differentiate between them with the modelling results being similar in many respects to the previous ALMA analysis, but differing in the slope of the outer region of the disc. The measured flux densities are consistent between the LMT (single dish) and ALMA (interferometric) observations after accounting for the differences in wavelength of observation. The LMT observations suggest the outer slope of the planetesimal belt is steeper than was suggested in the ALMA analysis. This would be consistent with the interferometric observations being mostly blind to structure at the disc outer edges, but the overall low signal to noise of the LMT observations does not definitively resolve the structure of the outer planetesimal belt. |
Keywords | stars; HD 172167; individual |
Public Notes | This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2022 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. |
Byline Affiliations | Centre for Astrophysics |
Academia Sinica Institute of Astronomy and Astrophysics, Taiwan | |
National Institute of Astrophysics Optics and Electronics, Mexico | |
National Council of Humanities Science and Technology, Mexico | |
University of Dublin, Ireland | |
Institute of Space Sciences, Spain | |
Catalan Institution for Research and Advanced Studies (ICREA), Spain | |
Institute of Space Studies of Catalonia (IEEC), Spain | |
ALMA Santiago Central Offices (ALMA SCO), Chile | |
University of Massachusetts, United States |
https://research.usq.edu.au/item/z026v/lmt-aztec-observations-of-vega
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