AzTEC Survey of the Central Molecular Zone: Data Reduction, Analysis, and Preliminary Results. (arXiv:2008.12351v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tang_Y/0/1/0/all/0/1">Yuping Tang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Q/0/1/0/all/0/1">Q. Daniel Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilson_G/0/1/0/all/0/1">Grant W. Wilson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heyer_M/0/1/0/all/0/1">Mark H. Heyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutermuth_R/0/1/0/all/0/1">Robert A. Gutermuth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schloerb_P/0/1/0/all/0/1">Peter Schloerb</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yun_M/0/1/0/all/0/1">Min S. Yun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bally_J/0/1/0/all/0/1">John Bally</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loinard_L/0/1/0/all/0/1">Laurent Loinard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Silich_S/0/1/0/all/0/1">Sergiy Silich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chavez_M/0/1/0/all/0/1">Miguel Chávez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haggard_D/0/1/0/all/0/1">Daryl Haggard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montana_A/0/1/0/all/0/1">Alfredo Montaña</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Arguelles_D/0/1/0/all/0/1">David Sánchez-Argüelles</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zeballos_M/0/1/0/all/0/1">Milagros Zeballos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zavala_J/0/1/0/all/0/1">Jorge A. Zavala</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leon_Tavares_J/0/1/0/all/0/1">Jonathan León-Tavares</a>
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 (LMT) in the 1.1 mm continuum. Our 1.1 mm map covers the
main body of the CMZ over a field of $1.6 times 1.1$ deg$^2$ with an angular
resolution of $10.5”$ and a depth of 15 mJy/beam. To account for the intensity
loss due to the background removal process, we combine this map with lower
resolution CSO/Bolocam and textit{Planck}/HFI data to produce an effective
full intensity 1.1 mm continuum map. With this map and existing
textit{Herschel} surveys, we have carried out a comprehensive analysis of the
spectral energy distribution (SED) 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 $10.5”$. The monitoring of Sgr A* was carried out as part
of a worldwide, multi-wavelength campaign when the so-called G2 object was
undergoing the pericenter passage around the massive black hole (MBH). 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 $140%$ maximum amplitude on 9th May, 2014 but
otherwise only stochastic variations of $10%$ and no systematic long-term
change, consistent with other observations.
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 (LMT) in the 1.1 mm continuum. Our 1.1 mm map covers the
main body of the CMZ over a field of $1.6 times 1.1$ deg$^2$ with an angular
resolution of $10.5”$ and a depth of 15 mJy/beam. To account for the intensity
loss due to the background removal process, we combine this map with lower
resolution CSO/Bolocam and textit{Planck}/HFI data to produce an effective
full intensity 1.1 mm continuum map. With this map and existing
textit{Herschel} surveys, we have carried out a comprehensive analysis of the
spectral energy distribution (SED) 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 $10.5”$. The monitoring of Sgr A* was carried out as part
of a worldwide, multi-wavelength campaign when the so-called G2 object was
undergoing the pericenter passage around the massive black hole (MBH). 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 $140%$ maximum amplitude on 9th May, 2014 but
otherwise only stochastic variations of $10%$ and no systematic long-term
change, consistent with other observations.
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