{"dcterms:modified":"2025-04-01","dcterms:creator":"Harvard Dataverse","@type":"ore:ResourceMap","schema:additionalType":"Dataverse OREMap Format v1.0.1","dvcore:generatedBy":{"@type":"schema:SoftwareApplication","schema:name":"Dataverse","schema:version":"6.6 build 1829-192cdc4","schema:url":"https://github.com/iqss/dataverse"},"@id":"https://dataverse.harvard.edu/api/datasets/export?exporter=OAI_ORE&persistentId=https://doi.org/10.7910/DVN/40C44C","ore:describes":{"citation:datasetContact":{"citation:datasetContactName":"Green, Gregory","citation:datasetContactAffiliation":"Harvard Astronomy","citation:datasetContactEmail":"gregorymgreen@gmai.com"},"citation:dsDescription":{"citation:dsDescriptionValue":"A three-dimensional map of dust reddening, covering the three quarters of the sky surveyed by the Pan-STARRS 1 (PS1) survey. We use PS1 and 2MASS optical and near-infrared photometry to infer distances and reddenings to ~800 million stars. These stars trace the reddening along different lines of sight, allowing us to build up a map of reddening in 3D.

\r\n\r\nThe map is structured as a set of sightlines, each of which contains multiple samples of the cumulative dust reddening as a function of distance. Each sightline is identified by a HEALPix nside parameter and nested pixel index. Within each sightline, cumulative reddening is given at discrete distances, spaced evenly in distance modulus. For each pixel, we provide multiple samples from the posterior on dust reddening.

\r\n\r\nQuality assurance information is given for each pixel, including:
\r\n\r\n
\r\n\r\nNote that the reddening is given in units of \"SFD-like\" E(B-V). They are meant to be comparable E(B-V), as reported by Schlegel, Finkbeiner & Davis (1998). In order to convert to extinction in different passbands, use the coefficients in Table 6 of Schlafly & Finkbeiner (2011).

\r\n\r\nThe 3D map is described in more detail in Green et al. (2015), and tools for accessing the map are provided at argonaut.skymaps.info.","citation:dsDescriptionDate":"2015-06-26"},"publication":{"publicationIDType":"doi","publicationIDNumber":"10.1088/0004-637X/810/1/25","publicationURL":"http://adsabs.harvard.edu/abs/2015arXiv150701005G"},"author":{"citation:authorName":"Green, Gregory","citation:authorAffiliation":"Harvard Astronomy","authorIdentifierScheme":"ORCID","authorIdentifier":"orcid.org/0000-0001-5417-2260"},"subject":"Astronomy and Astrophysics","title":"3D Dust map from Green et al. (2015)","citation:depositor":"Green, Gregory","dateOfDeposit":"2015-06-26","@id":"https://doi.org/10.7910/DVN/40C44C","@type":["ore:Aggregation","schema:Dataset"],"schema:version":"2.2","schema:name":"3D Dust map from Green et al. (2015)","schema:dateModified":"Wed Dec 09 15:29:08 UTC 2015","schema:datePublished":"2015-06-28","schema:creativeWorkStatus":"RELEASED","schema:license":"http://creativecommons.org/publicdomain/zero/1.0","dvcore:fileTermsOfAccess":{"dvcore:fileRequestAccess":false},"schema:includedInDataCatalog":"Harvard Dataverse","schema:isPartOf":{"schema:name":"Bayestar Dataverse","@id":"https://dataverse.harvard.edu/dataverse/bayestar","schema:description":"3D maps of reddening due to interstellar dust, created by the program \"Bayestar,\" by Gregory Green, Mario Jurić, Edward Schlafly and Douglas Finkbeiner.","schema:isPartOf":{"schema:name":"Interstellar Medium in 3D Dataverse","@id":"https://dataverse.harvard.edu/dataverse/ism3d","schema:description":"Data pertaining to the three-dimensional structure of the interstellar medium of the Milky Way Galaxy.","schema:isPartOf":{"schema:name":"Harvard Dataverse","@id":"https://dataverse.harvard.edu/dataverse/harvard","schema:description":"

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