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Observing substructure in circumstellar discs around massive young stellar objects

Jankovic, Marija R.; Haworth, Thomas J.; Ilee, John D.; Forgan, Duncan H.; Cyganowski, Claudia J.; Walsh, Catherine; Brogan, Crystal L.; Hunter, Todd R.; Mohanty, Subhanjoy


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  <identifier identifierType="DOI">10.5281/zenodo.1408072</identifier>
  <creators>
    <creator>
      <creatorName>Jankovic, Marija R.</creatorName>
      <givenName>Marija R.</givenName>
      <familyName>Jankovic</familyName>
    </creator>
    <creator>
      <creatorName>Haworth, Thomas J.</creatorName>
      <givenName>Thomas J.</givenName>
      <familyName>Haworth</familyName>
    </creator>
    <creator>
      <creatorName>Ilee, John D.</creatorName>
      <givenName>John D.</givenName>
      <familyName>Ilee</familyName>
    </creator>
    <creator>
      <creatorName>Forgan, Duncan H.</creatorName>
      <givenName>Duncan H.</givenName>
      <familyName>Forgan</familyName>
    </creator>
    <creator>
      <creatorName>Cyganowski, Claudia J.</creatorName>
      <givenName>Claudia J.</givenName>
      <familyName>Cyganowski</familyName>
    </creator>
    <creator>
      <creatorName>Walsh, Catherine</creatorName>
      <givenName>Catherine</givenName>
      <familyName>Walsh</familyName>
    </creator>
    <creator>
      <creatorName>Brogan, Crystal L.</creatorName>
      <givenName>Crystal L.</givenName>
      <familyName>Brogan</familyName>
    </creator>
    <creator>
      <creatorName>Hunter, Todd R.</creatorName>
      <givenName>Todd R.</givenName>
      <familyName>Hunter</familyName>
    </creator>
    <creator>
      <creatorName>Mohanty, Subhanjoy</creatorName>
      <givenName>Subhanjoy</givenName>
      <familyName>Mohanty</familyName>
    </creator>
  </creators>
  <titles>
    <title>Observing substructure in circumstellar discs around massive young stellar objects</title>
  </titles>
  <publisher>Zenodo</publisher>
  <publicationYear>2018</publicationYear>
  <subjects>
    <subject>stars: massive</subject>
    <subject>(stars:) circumstellar matter</subject>
    <subject>stars: formation</subject>
    <subject>radiative transfer</subject>
    <subject>accretion, accretion discs</subject>
  </subjects>
  <dates>
    <date dateType="Issued">2018-11-06</date>
  </dates>
  <resourceType resourceTypeGeneral="Dataset"/>
  <alternateIdentifiers>
    <alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/1408072</alternateIdentifier>
  </alternateIdentifiers>
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    <relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.1408071</relatedIdentifier>
  </relatedIdentifiers>
  <rightsList>
    <rights rightsURI="http://creativecommons.org/licenses/by/4.0/legalcode">Creative Commons Attribution 4.0 International</rights>
    <rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
  </rightsList>
  <descriptions>
    <description descriptionType="Abstract">&lt;p&gt;Synthetic dust continuum and molecular line Atacama Large Millimetre Array (ALMA) observations of massive, self-gravitating disc models surrounding massive young stellar objects are presented here. Semi-analytic models of self-gravitating discs with spiral density waves and clumps/fragments are combined with radiative transfer models, and synthetic observations are produced using CASA software. Models presented here have different disc masses, distances, inclinations, thermal structures, dust distributions, number and orientation of spirals and fragments.&lt;br&gt;
&amp;nbsp;&amp;nbsp; &amp;nbsp;&amp;nbsp;&amp;nbsp; &amp;nbsp;&amp;nbsp;&amp;nbsp; &amp;nbsp;&lt;br&gt;
Data is in the FITS format, with filenames starting either with &amp;#39;line&amp;#39; (synthetic molecular line datacube) or &amp;#39;cont&amp;#39; (synthetic continuum images), and each filename contains the model ID. Tables of model IDs and model parameters are given in files models_table_spiral.dat and models_table_spiral_fragments.dat for models without and with fragments, respectively. Starting from a fiducial disc model, model parameters were varied one by one, with the exception of disc inclination which is separately set in each model.&lt;br&gt;
&amp;nbsp;&amp;nbsp; &amp;nbsp;&amp;nbsp;&amp;nbsp; &amp;nbsp;&amp;nbsp;&amp;nbsp; &amp;nbsp;&lt;br&gt;
For details about the model parameters, detailed presentation of methods, proposed substructure-enhancing filtering methods, discussion and predictions for the upcoming ALMA observations, see Jankovic et al. 2018 (accepted for publication in MNRAS, arxiv.org/abs/1810.11398).&lt;/p&gt;

&lt;p&gt;&amp;nbsp;&lt;/p&gt;</description>
  </descriptions>
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