2020/08/31 by Yuping Tang, Q. Daniel Wang, Grant W. Wilson +21
Physics and Astronomy · #Amplitude #Angular resolution (graph drawing) #Astronomy #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics #Deconvolution #Galaxies: Formation, Evolution, Phenomena #Galaxy #Millimeter #Optics #Photometry (optics) #Physics #Spectral energy distribution #Spectral index #Spectral line #Stars #Telescope #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stab1191
Accepted for publication by MNRAS
arxiv created 2021/04/22 · openalex publication_date 2021/04/26 · arxiv updated 2021/05/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT We present a large-scale survey of the central molecular zone (CMZ) of our Galaxy, as well as a monitoring program of Sgr A*, with the AzTEC/Large Millimeter Telescope in the 1.1 mm continuum. Our 1.1 mm map covers the main body of the CMZ over a field of 1.6 × 1.1 deg2 with an angular resolution of 10.5 arcsec and a depth of 15 mJy beam−1. To account for the intensity loss due to the background removal process, we combine this map with lower resolution CSO/Bolocam and Planck/HFI data to produce an effective full intensity 1.1 mm continuum map. With this map and existing Herschel surveys, we have carried out a comprehensive analysis of the spectral energy distribution of dust in the CMZ. A key component of this analysis is the implementation of a model-based deconvolution approach, incorporating the Point Spread Functions (PSFs) of the different instruments, and hence recovering a significant amount of spatial information on angular scales larger than 10.5 arcsec. The monitoring of Sgr A* was carried out as part of a worldwide, multiwavelength campaign when the so-called G2 object was undergoing the pericentre passage around the massive black hole. Our preliminary results include (1) high-resolution maps of column density, temperature and dust spectral index across the CMZ; (2) a 1.1 mm light curve of Sgr A* showing an outburst of 140 \rm per cent maximum amplitude on 2014 May 9th May, 2014 but otherwise only stochastic variations of 10 \rm per cent and no systematic long-term change, consistent with other observations.