The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview. (arXiv:1812.04040v1 [astro-ph.SR])

The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview. (arXiv:1812.04040v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_S/0/1/0/all/0/1">Sean M. Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_J/0/1/0/all/0/1">Jane Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_L/0/1/0/all/0/1">Laura M. P&#xe9;rez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isella_A/0/1/0/all/0/1">Andrea Isella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dullemond_C/0/1/0/all/0/1">Cornelis P. Dullemond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kurtovic_N/0/1/0/all/0/1">Nicol&#xe1;s T. Kurtovic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guzman_V/0/1/0/all/0/1">Viviana V. Guzm&#xe1;n</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">John M. Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilner_D/0/1/0/all/0/1">David J. Wilner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">Shangjia Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_Z/0/1/0/all/0/1">Zhaohuan Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birnstiel_T/0/1/0/all/0/1">Tilman Birnstiel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">Xue-Ning Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benisty_M/0/1/0/all/0/1">Myriam Benisty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_A/0/1/0/all/0/1">A. Meredith Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oberg_K/0/1/0/all/0/1">Karin I. &#xd6;berg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_L/0/1/0/all/0/1">Luca Ricci</a>

We introduce the Disk Substructures at High Angular Resolution Project
(DSHARP), one of the initial Large Programs conducted with the Atacama Large
Millimeter/submillimeter Array (ALMA). The primary goal of DSHARP is to find
and characterize substructures in the spatial distributions of solid particles
for a sample of 20 nearby protoplanetary disks, using very high resolution
(0.035 arcsec, or 5 au FWHM) observations of their 240 GHz (1.25 mm) continuum
emission. These data provide a first homogeneous look at the small-scale
features in disks that are directly relevant to the planet formation process,
quantifying their prevalence, morphologies, spatial scales, spacings, symmetry,
and amplitudes, for targets with a variety of disk and stellar host properties.
We find that these substructures are ubiquitous in this sample of large, bright
disks. They are most frequently manifested as concentric, narrow emission rings
and depleted gaps, although large-scale spiral patterns and small arc-shaped
azimuthal asymmetries are also present in some cases. These substructures are
found at a wide range of disk radii (from a few au to more than 100 au), are
usually compact ($<$10 au), and show a wide range of amplitudes (brightness contrasts). Here we discuss the motivation for the project, describe the survey design and the sample properties, detail the observations and data calibration, highlight some basic results, and provide a general overview of the key conclusions that are presented in more detail in a series of accompanying articles. The DSHARP data -- including visibilities, images, calibration scripts, and more -- are released for community use at https://almascience.org/alma-data/lp/DSHARP.

We introduce the Disk Substructures at High Angular Resolution Project
(DSHARP), one of the initial Large Programs conducted with the Atacama Large
Millimeter/submillimeter Array (ALMA). The primary goal of DSHARP is to find
and characterize substructures in the spatial distributions of solid particles
for a sample of 20 nearby protoplanetary disks, using very high resolution
(0.035 arcsec, or 5 au FWHM) observations of their 240 GHz (1.25 mm) continuum
emission. These data provide a first homogeneous look at the small-scale
features in disks that are directly relevant to the planet formation process,
quantifying their prevalence, morphologies, spatial scales, spacings, symmetry,
and amplitudes, for targets with a variety of disk and stellar host properties.
We find that these substructures are ubiquitous in this sample of large, bright
disks. They are most frequently manifested as concentric, narrow emission rings
and depleted gaps, although large-scale spiral patterns and small arc-shaped
azimuthal asymmetries are also present in some cases. These substructures are
found at a wide range of disk radii (from a few au to more than 100 au), are
usually compact ($<$10 au), and show a wide range of amplitudes (brightness
contrasts). Here we discuss the motivation for the project, describe the survey
design and the sample properties, detail the observations and data calibration,
highlight some basic results, and provide a general overview of the key
conclusions that are presented in more detail in a series of accompanying
articles. The DSHARP data — including visibilities, images, calibration
scripts, and more — are released for community use at
https://almascience.org/alma-data/lp/DSHARP.

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