LMT/AzTEC observations of Vega

Article

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. 2022. "LMT/AzTEC observations of Vega." Monthly Notices of the Royal Astronomical Society. 514 (3), pp. 3815-3820. https://doi.org/10.1093/mnras/stac1510
Article Title

LMT/AzTEC observations of Vega

ERA Journal ID1074
Article CategoryArticle
AuthorsMarshall, 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 TitleMonthly Notices of the Royal Astronomical Society
Journal Citation514 (3), pp. 3815-3820
Number of Pages6
Year2022
PublisherOxford University Press
Place of PublicationUnited Kingdom
ISSN0035-8711
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.

Keywordsstars; 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 AffiliationsCentre 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
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