The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A90106%2F25%3A00646370" target="_blank" >RIV/67985815:90106/25:00646370 - isvavai.cz</a>
Result on the web
<a href="https://doi.org/10.3847/2041-8213/adb03c" target="_blank" >https://doi.org/10.3847/2041-8213/adb03c</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/2041-8213/adb03c" target="_blank" >10.3847/2041-8213/adb03c</a>
Alternative languages
Result language
angličtina
Original language name
The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Complete Size Distributions for the 100 Brightest Disks across Multiplicity and Spectral Energy Distribution Classes
Original language description
The size of a protoplanetary disk is a fundamental property, yet most remain unresolved, even in nearby star-forming regions (d similar to 140-200 pc). We present the complete continuum size distribution for the 105 brightest protoplanetary disks (M-dust greater than or similar to 2 M-circle plus) in the Ophiuchus cloud, obtained from ALMA Band 8 (410 GHz) observations at 0.'' 05 (7 au) to 0.'' 15 (21 au) resolution. This sample includes 54 Class II and 51 Class I and flat-spectrum sources, providing a comprehensive distribution across evolutionary stages. We measure the half-width at half-maximum and the radius encircling 68% of the flux (R-68%) for most nonbinary disks, yielding the largest flux-limited sample of resolved disks in any star-forming region. The distribution is log-normal with a median value of similar to 14 au and a logarithmic standard deviation sigma log=0.46 (factor of 2.9 in linear scale). Disks in close-binary systems (<200 au separation) have smaller radii, with a median value of similar to 5 au, indicating efficient radial drift as predicted by dust evolution models. The size distribution for young embedded objects (spectral energy distribution Class I and flat spectrum, age less than or similar to 1 Myr) is similar to that of Class II objects (age similar to a few Myr), implying that pressure bumps must be common at early disk stages to prevent millimeter-sized particle migration at astronomical unit scales.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
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Others
Publication year
2025
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal Letters
ISSN
2041-8205
e-ISSN
2041-8213
Volume of the periodical
981
Issue of the periodical within the volume
1
Country of publishing house
US - UNITED STATES
Number of pages
11
Pages from-to
L4
UT code for WoS article
001440394500001
EID of the result in the Scopus database
2-s2.0-86000147559