The morphology of the Milky Way - I. Reconstructing CO maps from simulations in fixed potentials (dataset)
Arm_Maps.tar.gz (62.53Mb) Arm_Simulations_05pa_N2.tar.gz (6.451Gb) Arm_Simulations_10pa_N2.tar.gz (5.624Gb) Arm_Simulations_10pa_N4.tar.gz (6.450Gb) Arm_Simulations_12pa_N2.tar.gz (5.628Gb) Arm_Simulations_12pa_N4.tar.gz (6.027Gb) Arm_Simulations_15pa_N2.tar.gz (5.630Gb) Arm_Simulations_15pa_N4.tar.gz (6.473Gb) Arm_Simulations_20pa_N4.tar.gz (6.036Gb) Arm_Simulations_CGx2.tar.gz (2.572Gb) Arm_Simulations_PM_N2.tar.gz (1.732Gb) Bar_Maps.tar.gz (15.51Mb) Bar_Simulations_LM.tar.gz (5.590Gb) Bar_Simulations_WD.tar.gz (6.479Gb) Bar_Simulations_WDr2.tar.gz (6.485Gb) Mix_Maps.tar.gz (106.5Mb) WD_B50ps_A20ps_2N10pa.tar.gz (8.613Gb) WD_B50ps_A20ps_2N12pa.tar.gz (8.613Gb) WD_B50ps_A20ps_2N15pa.tar.gz (8.620Gb) WD_B50ps_A20ps_4N10pa.tar.gz (8.546Gb) WD_B50ps_A20ps_4N12pa.tar.gz (8.567Gb) WD_B50ps_A20ps_4N15pa.tar.gz (8.574Gb) WDr2_B60ps_A15ps_2N10pa.tar.gz (8.580Gb) WDr2_B60ps_A15ps_2N12pa.tar.gz (8.584Gb) WDr2_B60ps_A15ps_2N15pa.tar.gz (8.582Gb) WDr2_B60ps_A20ps_2N10pa.tar.gz (8.638Gb) WDr2_B60ps_A20ps_2N12pa.tar.gz (8.634Gb) WDr2_B60ps_A20ps_2N15pa.tar.gz (8.630Gb) WDr2_B60ps_A20ps_4N10pa.tar.gz (8.592Gb) WDr2_B60ps_A20ps_4N12pa.tar.gz (8.600Gb) WDr2_B60ps_A20ps_4N15pa.tar.gz (8.608Gb)Show MoreShow Less
Price, Daniel J.
Acreman, David M.
Pettitt, Alex R.
University of Exeter
Please contact Alex Pettitt at email@example.com before using this data.
Datasets 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.
Alex Pettitt is supported by an STFC-funded post-graduate studentship.
Science and Technology Facilities Council
The 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.