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36 results for “star clusters”
The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds
<p>Supplemental material to 'The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds'. This includes, for each star in the sample: a plot of the observed spectrum overlaid with best fitting models and fitness diagrams for all free parameters. Furthermore we include data (the normalised spectra used in the analysis, and best fitting models) and a basic reproduction package. </p>
MESA Inlists for: Barium Surface Abundances of Blue Straggler Stars in the Open Clusters NGC 7789 and M67
<p>These are the MESA v15140 inlists and Python script associated with the models presented in Nine et al. (2024). The files are as follows:</p> <p>inlist, inlist_start_header, inlist_to_end_core_h_burn_header, inlist_to_start_he_core_flash_header, inlist_to_end_core_he_burn_header, inlist_to_end_agb_header, inlist_to_wd_header: Pointer files to tell MESA which inlists to read for control, kappa, and PGStar commands.</p> <p>inlist_start, inlist_to_end_core_h_burn, inlist_to_start_he_core_flash, inlist_to_end_core_he_burn, inlist_to_end_agb, inlist_to_wd: MESA inlist files with control, kappa, and PGStar commands for each stage.</p> <p>turnoff_masses.py: a Python script that takes in the file inlist_start_base and rewrites it to create a starting model with the mass of a turnoff star in NGC 7789 (1.8 solar masses), NGC 6819 (1.5 solar masses), M67 (1.3 solar masses), and NGC 188 (1.1 solar masses). This starting model is then used in the following inlists to create AGB star models with these masses.</p> <p>inlist_start_base: The base starting inlist that turnoff_masses.py reads in and alters to create inlist_start.</p>
Properties of intermediate- to high-mass stars in the young cluster M17 Characterizing the (pre-)Zero Age Main Sequence
<p>Data and extra figures of the paper "Properties of intermediate- to high-mass stars in the young cluster M17 -- Characterizing the (pre-)Zero Age Main Sequence" by Frank Backs. Published in Astronomy and Astrophysics.</p> <p>The observed data and the fitted models are included. The fitting algorithm Kiwi-GA is available on Github: https://github.com/sarahbrands/Kiwi-GA</p> <p>Additional figures are available. These figures give an overview of the best fit models for each line like Fig. 1 in the paper. </p>
Online material to publication "Exploring the dynamical evolution of Cepheid multiplicity in star clusters and its implications for B-star multiplicity at birth"
<p>The description of the movie can be found in the file movie_description.pdf.</p> <p>The full paper can be found here: https://ui.adsabs.harvard.edu/abs/2024arXiv240907530D/abstract</p>
Dataset for Runaway and Hypervelocity Stars from Compact Object Encounters in Globular Clusters
<p>The dataset used for Cabrera & Rodriguez 2023. If building from the showyourwork-enabled GitHub, the file can be directly unzipped into the <code>src/data</code> folder.</p> <p>The top-level contains folders for <code>CMC</code> model- and Milky Way globular cluster-delineated data (<code>cmc</code> and <code>mwgcs</code>, respectively), and some auxiliary files, including the composite catalogs. Within the two folders are subfolders for each of the <code>CMC</code> models and MWGCs. The <code>CMC</code> model folders contain some of the output files from the <code>CMC Cluster Catalog</code> <a href="https://ui.adsabs.harvard.edu/abs/2020ApJS..247...48K">(Kremer+20</a>) (used in this project to examine GC evolution), and also two files <code>output_N-10.txt</code> (which has data for all <code>Fewbody</code> realizations for the model) and <code>output_N-10_ejections.txt</code> (which has data for all ejections from the model). The columns in the former file are regrettably not labeled, but correspond to the following parameters, many of which are direct <code>Fewbody</code> arguments:</p> <table align="center"> <thead> <tr> <th scope="col">#</th> <th scope="col">Parameter</th> <th scope="col">Description</th> <th scope="col">Units</th> </tr> </thead> <tbody> <tr> <td>1</td> <td>time</td> <td>Physical time of encounter in <code>CMC </code>model</td> <td>Myr</td> </tr> <tr> <td>2</td> <td>b</td> <td>Impact parameter</td> <td>a1</td> </tr> <tr> <td>3</td> <td>vinf</td> <td>Velocity of single object at infinity</td> <td>v_crit</td> </tr> <tr> <td>4</td> <td>a1</td> <td>Initial semi-major axis of binary</td> <td>AU</td> </tr> <tr> <td>5</td> <td>e1</td> <td>Initial binary eccentricity</td> <td>-</td> </tr> <tr> <td>6</td> <td>vesc</td> <td>Local escape velocity in <code>CMC </code>model</td> <td>km/s</td> </tr> <tr> <td>7</td> <td>m10</td> <td>Mass of first binary component</td> <td>Msun</td> </tr> <tr> <td>8</td> <td>m11</td> <td>Mass of second binary component</td> <td>Msun</td> </tr> <tr> <td>9</td> <td>m0</td> <td>Mass of single object</td> <td>Msun</td> </tr> <tr> <td>10</td> <td>r10</td> <td>Radius of first binary component</td> <td>Rsun</td> </tr> <tr> <td>11</td> <td>r11</td> <td>Radius of second binary component</td> <td>Rsun</td> </tr> <tr> <td>12</td> <td>r0</td> <td>Radius of single object</td> <td>Rsun</td> </tr> <tr> <td>13</td> <td>k10</td> <td>BSE k-type of first binary component</td> <td>-</td> </tr> <tr> <td>14</td> <td>k11</td> <td>BSE k-type of second binary component</td> <td>-</td> </tr> <tr> <td>15</td> <td>k0</td> <td>BSE k-type of single object</td> <td>-</td> </tr> <tr> <td>16</td> <td>s</td> <td>Random seed for <code>Fewbody</code></td> <td>-</td> </tr> <tr> <td>17</td> <td>type_i</td> <td> <p>Index classifying initial system (see below)</p> </td> <td>-</td> </tr> <tr> <td>18</td> <td>type_f</td> <td>Index classifying final system (see below)</td> <td>-</td> </tr> <tr> <td>19</td> <td>v_crit</td> <td>Critical velocity of encounter (<a href="https://ui.adsabs.harvard.edu/abs/2004MNRAS.352....1F/abstract">Fregeau+04</a>)</td> <td>km/s</td> </tr> <tr> <td>20</td> <td>a_fin</td> <td>Final semi-major axis of binary (0 if no binary is present)</td> <td>AU</td> </tr> <tr> <td>21</td> <td>e_fin</td> <td>Final binary eccentricity (identically 0 if no binary is present)</td> <td>-</td> </tr> <tr> <td>22</td> <td>Lx</td> <td>x-component of the initial angular momentum of the system</td> <td>code</td> </tr> <tr> <td>23</td> <td>Ly</td> <td>y-component of the initial angular momentum of the system</td> <td>code</td> </tr> <tr> <td>24</td> <td>Lz</td> <td>z-component of the initial angular momentum of the system</td> <td>code</td> </tr> <tr> <td>25</td> <td>Lbinx</td> <td>x-component of the angular momentum of the initial binary</td> <td>code</td> </tr> <tr> <td>26</td> <td>Lbiny</td> <td>y-component of the angular momentum of the initial binary</td> <td>code</td> </tr> <tr> <td>27</td> <td>Lbinz</td> <td>z-component of the angular momentum of the initial binary</td> <td>code</td> </tr> <tr> <td>28</td> <td>Ei</td> <td>Initial energy of the encounter</td> <td>code</td> </tr> <tr> <td>29</td> <td>DeltaEfrac</td> <td>Fractional change in energy by the time of termination</td> <td>-</td> </tr> <tr> <td>30/34/38</td> <td>vfin0/1/2</td> <td>Final velocity of the final top-level object with<code> Fewbody </code>index 0/1/2 (<a href="https://ui.adsabs.harvard.edu/abs/2004MNRAS.352....1F/abstract">Fregeau+04</a>)</td> <td>v_crit</td> </tr> <tr> <td>31/35/39</td> <td>kf0/1/2</td> <td>BSE k-type of the same</td> <td>-</td> </tr> <tr> <td>32/36/40</td> <td>Rmin0/1/2</td> <td>Minimum distance between this object and any other object during the encounter</td> <td>AU</td> </tr> <tr> <td>33/37/41</td> <td>Rmin_j0/1/2</td> <td><code>Fewbody </code>index of the other object at closest passage</td> <td>AU</td> </tr> </tbody> </table> <p>The initial encounter classifying indices are as follows, where "C" denotes a compact object and "S" a star:</p> <table align="center"> <thead> <tr> <th scope="col">type_i</th> <th scope="col">Configuration</th> </tr> </thead> <tbody> <tr> <td>1</td> <td>(C,C)+S</td> </tr> <tr> <td>2</td> <td>(C,S)+C</td> </tr> <tr> <td>3</td> <td>(C,S)+S</td> </tr> <tr> <td>4</td> <td>(S,S)+C</td> </tr> </tbody> </table> <p>The final encounter classifying indices are as follows, using the initial <code>Fewbody </code>object indices to specify if objects end up in a binary ((a,b)) or if they merge (a:b) (note that <code>Fewbody</code> initializes all binary-single encounters in the <code>type_f=3</code> configuration, i.e. the object index 0 is assigned to the single):</p> <table align="center"> <thead> <tr> <th scope="col">type_f</th> <th scope="col">Configuration</th> </tr> </thead> <tbody> <tr> <td>0</td> <td>0+1+2 (Ionization)</td> </tr> <tr> <td>1</td> <td>(0,1)+2</td> </tr> <tr> <td>2</td> <td>(0,2)+1</td> </tr> <tr> <td>3</td> <td>0+(1,2)</td> </tr> <tr> <td>4</td> <td>0:1+2</td> </tr> <tr> <td>5</td> <td>0:2+1</td> </tr> <tr> <td>6</td> <td>1:2+0</td> </tr> <tr> <td>7</td> <td>0:1:2</td> </tr> <tr> <td>-2</td> <td>binary</td> </tr> <tr> <td>-3</td> <td>hierarchical triple</td> </tr> </tbody> </table> <p>The columns in <code>output_N-10_ejections.txt</code> are labeled, and use many of the same headers in the first table; the object indices for fields 30-41 are dropped because each row in this file corresponds to an escaper. The two additions are <code>mf</code> and <code>rf</code>, which indicate the mass and radius of the ejected object.</p> <p>Each of the <code>mwgcs</code> folders contain the FITS files described in Appendix B of the text. There are also <code>output_N-10_ejections.txt</code> files similar to the ones for the <code>CMC</code> models; the MWGC versions contain the additional fields below:</p> <table align="center"> <thead> <tr> <th scope="col">Parameter</th> <th scope="col">Description</th> <th scope="col">Units</th> </tr> </thead> <tbody> <tr> <td>vout</td> <td>Velocity of object at the time of ejection from the representative model</td> <td>km/s</td> </tr> <tr> <td>X/Y/Z</td> <td>Galactocentric X/Y/Z coordinate of object at the present day</td> <td>kpc</td> </tr> <tr> <td>U/V/W</td> <td>Galactocentric U/V/W velocity of object at the present day</td> <td>km/s</td> </tr> </tbody> </table> <p> </p>
Data from The Kinematics, Metallicities, and Orbits of Six Recently Discovered Galactic Star Clusters with Magellan/M2FS Spectroscopy
<p>Pace, Koposov, Walker et al 2023</p> <p>Catalog level data products from Magellan/M2FS and AAT/AAOmega spectroscopy (fits, npy formats) including membership information</p> <p>Summary table (Table 2) in machine readable formats (npy, fits, and csv formats)</p> <p>Updates (v2): The original M2FS sample had a bug in the application of the systematic errors. All errors have been corrected. The summary table has been updated accordingly. </p>
ALMA detection of CO rotational line emission in red supergiant stars of the massive young star cluster RSGC1
<p>Input files and data for the MESA simulations in the paper "ALMA detection of CO rotational line emission in red supergiant stars of the massive young star cluster RSGC1". Runs where performed with version r23.05.1 of the MESA code using the MESA SDK version x86_64-linux-22.6.1. Folder named "Decin" contains the simulation with the new mass loss rate described in the paper, while the folder named NdJ contains the input files for the simulation performed with the Nieuwenhuijzen & de Jager rates.</p>
A Cluster Randomised Trial of Community-led Distribution of HIV Self-tests in Rural Malawi (HIV Self-Testing Africa [STAR])
ClinicalTrials.gov study NCT03541382. IPD Sharing: YES. Countries: 1. Publications: 3.
Animation of MS evolution in young star clusters
<p>The video shows the evolution of binary and single stellar models from 1Myr to 100Myr. </p>
Pulsation-driven Mass Loss from Massive Stars behind Stellar Mergers in Metal-poor Dense Clusters
<p>MESA inlists, run_star_extras, and data associated with Nakauchi, Inayoshi, Omukai 2020. MESA version</p> <p>12115.</p>
Online material to paper "On the dynamical evolution of Cepheids in star clusters"
<p>The description of the movies can be found in the file movie_description.pdf.</p>
Effects of close binary evolution on the main-sequence morphology of young star clusters
<p>Star cluster animation to show their evolution in the Hertzsprung-Russell diagram.</p>
Milky Way Star Clusters Catalog
Although they are the main constituents of the Galactic disk population, for half of the open clusters in the Milky Way reported in the literature nothing is known except the raw position and an approximate size. The main goal of this study is to determine a full set of uniform spatial, structural, kinematic, and astrophysical parameters for as many known open clusters as possible. On the basis of stellar data from PPMXL and 2MASS, the authors used a dedicated data-processing pipeline to determine kinematic and photometric membership probabilities for stars in a cluster region. For an input list of 3,784 targets from the literature, they confirm that 3,006 are real objects, the vast majority of them are open clusters, but associations and globular clusters are also present. For each confirmed object, the authors determined the exact position of the cluster center, the apparent size, proper motion, distance, color excess, and age. For about 1,500 clusters, these basic astrophysical parameters have been determined for the first time. For the bulk of the clusters the authors also derived the tidal radii. In addition, they estimated average radial velocities for more than 30% of the confirmed clusters. The present sample (called MWSC) reaches both the central parts of the Milky Way and its outer regions. It is almost complete up to 1.8 kpc from the Sun and also covers the neighboring spiral arms. However, for a small subset of the oldest open clusters (ages more than ~ 1 Gyr), the authors found some evidence of incompleteness within about 1 kpc from the Sun. This table contains the list of 3,006 Milky Way stellar clusters (MWSC) found in the 2MAst (2MASS with Astrometry) catalog presented in Paper II of this series (these clusters have source numbers below 4000), together with an additional 139 new open clusters (these clusters have source numbers between 5000 and 6000) found by the authors at high Galactic latitudes (|b_II_| > 18.5 degrees) which were presented in Paper III of the series, and an additional 63 new open clusters (these clusters have source numbers between 4000 and 5000) which were presented in Paper IV of the series. The target list in Paper II from which the 3,006 open clusters was contained was compiled on the basis of present-day lists of open, globular and candidate clusters. The list of new high-latitude open clusters in Paper III was obtained from a target list of 714 density enhancements found using the 2MASS Catalog. The list of new open clusters in Paper IV was obtained from an initial list of 692 compact cluster candidates which were found by the authors by conducting an almost global search of the sky (they excluded the portions of the sky with |b_II_| < 5 degrees) in the PPMXL and the UCAC4 proper-motion catalogs. For confirmed clusters, the authors determined a homogeneous set of astrophysical parameters such as membership, angular radii of the main morphological parts, mean cluster proper motions, distances, reddenings, ages, tidal parameters, and sometimes radial velocities. This table was created by the HEASARC in February 2014 based on the list of open clusters given in <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/558/A53">CDS Catalog J/A+A/558/A53</a> files catalog.dat and notes.dat. It was updated in September 2014 with 139 additional star clusters from <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/568/A51">CDS Catalog J/A+A/568/A51</a> files catalog.dat and notes.dat. It was further updated in October 2015 with 63 additional star clusters from <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/581/A39">CDS Catalog J/A+A/581/A39</a> files catalog.dat and notes.dat. Note that this table does not include the information on candidates which turned out not to be open clusters which was also contained in these catalogs. This is a service provided by NASA HEASARC .
Star Formation in Nearby Clouds (SFiNCs) Probable Cluster Members Catalog
The Star Formation in Nearby Clouds (SFiNCs) project is aimed at providing a detailed study of the young stellar populations and of star cluster formation in the nearby 22 star-forming regions (SFRs) for comparison with the authors' earlier MYStIX survey of richer, more distant clusters. As a foundation for the SFiNCs science studies, in the reference paper homogeneous data analyses of the Chandra X-ray and Spitzer mid-infrared (MIR) archival SFiNCs data are described, and the resulting catalogs of over 15,300 X-ray and over 1,630,000 mid-infrared point sources are presented. On the basis of their X-ray/infrared properties and spatial distributions, nearly 8500 point sources have been identified as probable young stellar members of the SFiNCs regions. Compared to the existing X-ray/mid-infrared publications, the SFiNCs member list increases the census of YSO members by 6%-200% for individual SFRs and by 40% for the merged sample of all 22 SFiNCs SFRs. Sixty-five X-ray observations of the 22 SFiNCs SFRs made with the imaging array on the Advanced CCD Imaging Spectrometer (ACIS) were extracted from the Chandra archive (spanning from 2000 January to 2015 April). See Tables 1 and 2 of the reference paper for the list of SFRs and the log of Chandra ACIS observations, respectively. The final Chandra-ACIS catalog for the 22 SFiNCs SFRs comprises 15,364 X-ray sources (presented in Tables 3 and 4 and section 3.2 of the reference paper, and available as the HEASARC table, SFINCSXRAY). To obtain MIR photometry for X-ray objects and to identify and measure MIR photometry for additional non-Chandra disky stars that were missed in previous studies of the SFiNCs regions (typically faint YSOs), the authors have reduced the archived Spitzer-IRAC data by homogeneously applying the MYStIX-based Spitzer-IRAC data reduction methods of Kuhn et al. (2013, ApJS, 209, 29) to the 423 Astronomical Object Request (AORs) data sets for the 22 SFiNCs SFRs (listed in Table 5 of the reference paper). As in MYStIX, the SFiNCs IRAC source catalog retains all point sources with the photometric signal-to-noise ratio > 5 in both [3.6] and [4.5] um channels. This catalog covers the 22 SFiNCs SFRs and their vicinities on the sky and comprises 1,638,654 IRAC sources with available photometric measurements for 100%, 100%, 29%, and 23% of these sources in the 3.6, 4.5, 5.8, and 8.0um bands, respectively (see table 6 and section 3.4 of the reference paper). Source position cross-correlations between the SFiNCs Chandra X-ray source catalog and an IR catalog, either the "cut-out" IRAC or 2MASS, were made using the steps described in section 3.5 of the reference paper. Using the ensemble of X-ray and infrared data that they have obtained, the authors selected probable YSOs in the 22 SFRs using selection criteria described in section 4.1 of the reference paper. Tables 7 and 8 of the reference paper provide the list of 8,492 SFiNCs probable cluster members (SPCMs: but see below for a caveat on this number) and their main IR and X-ray properties (see section 4 of the reference paper). This present HEASARC table comprises the contents of these two tables. A fuller list of the X-ray properties of the X-ray-detected SPCMs is available in the HEASARC's SFINCSXRAY table (q.v.). This table was created by the HEASARC in September 2017 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/229/28">CDS Catalog J/ApJS/229/28</a> files table7.dat (the IR photometry of the SFiNCs probable cluster members) and table8.dat (the main X-ray and other properties of the SFiNCs probable cluster members). This is a service provided by NASA HEASARC .
HLA Star Clusters ConeSearch
All MAST catalog holdings are available via a ConeSearch endpoint. A high-level science product was produced cataloging star clusters within the HLA:compact star cluster catalogs are presented for 20 nearby, star-forming galaxies using observations from the Advanced Catalog for Surveys (ACS) and source lists generated by the Hubble Legacy Archive. Results based on these cluster catalogs are published in the paper "The Luminosity Function of Star Clusters in 20 Star-Forming Galaxies Based on Hubble Legacy Archive Photometry" Whitmore, AJ 147:78. A typical cluster luminosity function can be approximated by a power-law, with an average value for the index of -2.37 and rms scatter = 0.18. The uniform database provided by these HLA catalogs results in a small scatter (0.5 magnitude) in the correlation between the magnitude of the brightest cluster (M_brightest) and Log of the number of clusters brighter than M_I = -9 (Log N). More information on the catalog is available at https://archive.stsci.edu/prepds/hlastarclusters/.All available missions are listed at http://archive.stsci.edu/vo/mast_services.html.
Multiple RHB Populations in Globular Clusters - AstroSat NUV Photometry of Modelled Stars
<p>This deposition consists of two datasets:</p> <ol> <li>RHBI.txt</li> <li>RHBII.txt</li> </ol> <p>These datasets contain the AstroSat UVIT photometry of 18 red horizontal branch (RHB) stars from the globular cluster NGC 2808, which were selected for modelling in the study titled ''Multiple RHB Populations in Globular Clusters''. Each dataset contains the photometry of 9 stars (in 6 near-UV filters) belonging to one of the two RHB groups (RHBI and RHBII) present in NGC 2808. </p> <p>Each dataset contains the following columns:</p> <p>ID - The number/name of the source.</p> <p>XC, YC - Image coordinates </p> <p>RA, Dec - Right Ascension and Declination of the source in J2000 epoch.</p> <p>NF6, NF5, NF3, NF2, NF1 - Photometric magnitude (in ABmag) of source in the filters N279N, N263M, N245M, N219M and N242W respectively. </p> <p>ERRF6, ERRNF5, ERRNF3, ERRNF2, ERRNF1 - Error in photometric magnitude (in ABmag) of source in the filters N279N, N263M, N245M, N219M and N242W respectively. </p> <p> </p>
ScienceDex guides
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.