Poster Open Access

# Large Aperture Camera for the Simons Observatory

Dicker, Simon; Simons Observatory collaboration

### DataCite XML Export

<?xml version='1.0' encoding='utf-8'?>
<identifier identifierType="DOI">10.5281/zenodo.1158852</identifier>
<creators>
<creator>
<creatorName>Dicker, Simon</creatorName>
<givenName>Simon</givenName>
<familyName>Dicker</familyName>
<affiliation>University of Pennsylvania, USA</affiliation>
</creator>
<creator>
<creatorName>Simons Observatory collaboration</creatorName>
</creator>
</creators>
<titles>
<title>Large Aperture Camera for the Simons Observatory</title>
</titles>
<publisher>Zenodo</publisher>
<publicationYear>2018</publicationYear>
<dates>
<date dateType="Issued">2018-01-25</date>
</dates>
<resourceType resourceTypeGeneral="Text">Poster</resourceType>
<alternateIdentifiers>
<alternateIdentifier alternateIdentifierType="url">https://zenodo.org/record/1158852</alternateIdentifier>
</alternateIdentifiers>
<relatedIdentifiers>
<relatedIdentifier relatedIdentifierType="DOI" relationType="IsVersionOf">10.5281/zenodo.1158851</relatedIdentifier>
<relatedIdentifier relatedIdentifierType="URL" relationType="IsPartOf">https://zenodo.org/communities/atlast2018</relatedIdentifier>
</relatedIdentifiers>
<rightsList>
<rights rightsURI="info:eu-repo/semantics/openAccess">Open Access</rights>
</rightsList>
<descriptions>
<description descriptionType="Abstract">The Simon's observatory will consist of one large 6m telescope and three or more smaller telescopes working together with a goal of measuring the polarization in the Cosmic Microwave Background on angular scales as small as ~1' to larger than 1 degree and at a sensitivity far greater than has ever been reached before.  To reach these sensitivities, needed for our science goals, we require over 90000 background limited TES detectors on the large telescope - hence a very large field-of-view.  The telescope design we have selected is a copy of the CCAT-prime telescope, a Crossed Dragone with extra aspheric terms to increase the diffraction limited field-of-view.  At the secondary focus will be a ~2.5m diameter cryostat containing re-imaging silicon optics which can correct remaining aberrations (mostly astigmatism) at the edge of the field of view and allow this part of the focal plane to be used at higher frequencies.  This poster will contain an outline of our optical designs and take a brief look at how they could be scaled to a larger telescope.</description>
</descriptions>
</resource>

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