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dc.contributor.authorPrice, Daniel J.
dc.contributor.authorAcreman, David M.
dc.contributor.authorPettitt, Alex R.
dc.contributor.authorDobbs, Clare
dc.date.accessioned2014-06-20T08:25:00Z
dc.date.issued2014-06-19
dc.date.updated2014-06-19T21:50:08Z
dc.description.abstractDatasets for spiral, bar, and barred-spiral smoothed particle hydrodynamical simulations used in the paper Pettitt, Dobbs, Acreman & Price 2014. Also included are the integrated longitude-velocity maps created using a radiative transfer code.en_GB
dc.description.sponsorshipAlex Pettitt is supported by an STFC-funded post-graduate studentship.en_GB
dc.description.sponsorshipScience and Technology Facilities Councilen_GB
dc.identifier.urihttp://hdl.handle.net/10871/15057
dc.language.isoenen_GB
dc.publisherUniversity of Exeteren_GB
dc.relation.urlhttp://arxiv.org/abs/1406.4150en_GB
dc.relation.urlhttp://hdl.handle.net/10871/21920en_GB
dc.rightsPlease contact Alex Pettitt at a.r.pettitt@dunelm.org.uk before using this data.en_GB
dc.subjectGalaxyen_GB
dc.subjectMilky Wayen_GB
dc.subjectAstrophysicsen_GB
dc.titleThe morphology of the Milky Way - I. Reconstructing CO maps from simulations in fixed potentials (dataset)en_GB
dc.typeDataseten_GB
dc.date.available2014-06-20T08:25:00Z
dc.descriptionThe smoothed particle hydrodynamics binary dumps are grouped by type (arm, bar, mix) and labeled by parameters varied for each run. For arm models, N indicates the number of arms, pa the pitch angle (in degrees) and each zipped directory has different pattern speeds in different labelled directories (in units km/s/kpc). The CGx2 directory contains arm models with twice the normal strength, and the PM_N2 contains runs for a complex arm model (see paper for details). The bar models are organised by model type (WD, WDr2 and LM). The mixed simulations are labeled by: bar model, bar pattern speed, arm pattern speed, arm number, and finally pitch angle. The map directories are labelled similarly, but also contain a time stamp index (the last number of the directory) which gives the time in Myrs of the galaxy evolution divided by 2.12. The maps are then split into four separate FITS files, one for each galactic quadrant, and are of dimensions longitude x velocity x brightness temperature of CO (see FITS headers for more details). The smoothed particle hydrodynamics dumps can be viewed and converted to ascii format using the SPLASH software, http://users.monash.edu.au/~dprice/splash/, but other software is also available on the web. The FITS files can be opened with DS9, http://ds9.si.edu/site/Home.html, or GAIA, http://astro.dur.ac.uk/~pdraper/gaia/gaia.html, but various other software is also available.en_GB
dc.descriptionThe article associated with this dataset is available in ORE at: http://hdl.handle.net/10871/21920en_GB


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