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91 results for “Milky way”
Validation of the Bond et. al. (2010) SDSS-derived kinematic models for the Milky Way's disk and halo stars with Gaia Data Release 3 proper motion and radial velocity data
<p>We validate the Bond et. al. (2010) kinematic models for the Milky Way's disk and halo stars with Gaia Data Release 3 data. Bond et al. constructed models for stellar velocity distributions using stellar radial velocities measured by the Sloan Digital Sky Survey (SDSS) and stellar proper motions derived from SDSS and the Palomar Observatory Sky Survey astrometric measurements. These models describe velocity distributions as functions of position in the Galaxy, with separate models for disk and halo stars that were labeled using SDSS photometric and spectroscopic metallicity measurements. We find that the Bond et al. model predictions are in good agreement with recent measurements of stellar radial velocities and proper motions by the Gaia survey. In particular, the model accurately predicts the skewed non-Gaussian distribution of rotational velocity for disk stars and its vertical gradient, as well as the dispersions for all three velocity components. Additionally, the spatial invariance of velocity ellipsoid for halo stars when expressed in spherical coordinates is also confirmed by Gaia data at galacto-centric radial distances of up to 15 kpc.</p>
The data for a catalog of newly discovered close binary open clusters in the Milky Way from Gaia DR3
<p>The database for a catalog of newly discovered close binary open clusters in the Milky Way from Gaia DR3.</p> <p>It corresponds to the study of Zhongmu Li, Zhanpeng Zhu in 2024, which was submitted to AJ. When one use these data, please cite to that work. </p> <p>The database contains four parts, i.e., a parameter file and four directories. They are explained as follows.</p> <p>The file of ''data_tableI.csv'' gives the spatial positions and parallaxs of 13 newly discovered close binary open clusters (CBOCs).</p> <p>There are 11 columns in this file. The colums are for Name1, RA1, DEC1, Parallax1, Rtidal1, Name2, RA2, DEC2, Parallax2, Rtidal2 respectively. </p> <p>They correspond to the contents of a manuscript that was submitted to AJ.</p> <p>The file of ''data_tableII.csv'' contains the data of the fundamental parameters of 13 newly discovered CBOCs, together with their astrometric information. PBOC means primordial binary open cluster member. Distance modulus, color excess, age, and metal abundance of the clusters were obtained by fitting Parsec isochrones and Powerful CMD code. Proper motion data for the clusters were provided by HR23.</p> <p>Columns 3-14 show the basic parameters (distance modulus, color excess, age, and metal abundance) and errors of the cluster. Columns 15-16 are the proper motion data for the clusters. Column 17 is the number of member stars of the cluster.</p> <p>The file of ''data_tableIII.csv'' contains the data of Parameters for checking gravitationally bound and unbound cluster pairs. The subscripts 1 and 2 indicate the first and second sub-clusters respectively. Rroche is the Roche radius. RV 1, RV 2 and ΔRV denote the radial velocities of two member clusters and their difference. Porb and Vorb denote orbital period and orbital velocity.</p> <p>There are 13 columns in this file. The colums are for Name1, Name2, d12, r1, r2, Rroche, Mass1, Mass2, Porb, RV1, RV2, ΔRV, Vorb respectively. </p> <p>The file of ''memeber_allp.txt'' gives the list of member stars of 13 pairs of clusters. Data provided by HR23.</p> <p>If you have any problems with using these data, send an email to zhongmuli@126.com.</p>
On the detection of stellar wakes in the Milky Way: a deep learning approach
<p>The machine learning dataset used in the work of "On the detection of stellar wakes in the Milky Way: a deep learning approach". The .tar contains .h5 files for four different subhalo target masses such that each file is generated from a unique simulation seed. Each file contains data from a single simulation run and is comprised of 100 samples which are generated by sampling 1% of all star particles from a particular simulation snapshot. Prior to sampling particles, we split the simulation box into three equal slices in the Z-coordinate and bin the data onto the X-Y plane with 32 bins on each axis. Each sample is then characterised by a 2D histogram of shape (32, 32, 12) with the last dimension containing the training features which are the overdensity, mean X-Y velocity, X-Y velocity dispersion and divergence in X-Y for the three Z-slices.</p>
Milky Way Sensor: Device Validation for Infiltrated Tissues
ClinicalTrials.gov study NCT07311733. IPD Sharing: Not stated. Countries: 1. Publications: 0.
Milky Way Sensor Motion Validation
ClinicalTrials.gov study NCT07228416. IPD Sharing: Not stated. Countries: 0. Publications: 0.
Milky Way Globular Clusters Catalog (December 2010 Version)
This is the Catalog of Parameters for Milky Way Globular Clusters (December 2010 Version) that was compiled by William E. Harris of McMaster University. This is the first update since 2003 and the biggest single revision since the original version of the catalog published in 1996. The list now contains a total of 157 objects classified as globular clusters. Major upgrades have been made especially to the cluster coordinates, metallicities, and structural profile parameters, and the list of parameters now also includes the central velocity dispersion. This table contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for over 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. When you cite it in your text, please use "Harris 1996 (2010 edition)". The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: <a href="http://physwww.mcmaster.ca/~harris/mwgc.ref">http://physwww.mcmaster.ca/~harris/mwgc.ref</a>. This table was originally ingested by the HEASARC circa 1995. It was last updated by the HEASARC in February 2014 based on an electronic version (dated December 2010) copied from the file <a href="http://physwww.mcmaster.ca/~harris/mwgc.dat">http://physwww.mcmaster.ca/~harris/mwgc.dat</a>. This is a service provided by NASA HEASARC .
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 .
Milky Way Project First Data Release IR Bubble Catalog
This table contains a new catalog of 5106 infrared bubbles created through visual classification via the online citizen science website 'The Milky Way Project' (MWP). Bubbles in the new catalog have been independently measured by at least five individuals, producing consensus parameters for their positions, radii, thicknesses, eccentricities and position angles. Citizen scientists - volunteers recruited online and taking part in this research - have independently rediscovered the locations of at least 86% of three widely used catalogs of bubbles and H II regions while finding an order of magnitude more objects. 29% of the bubbles in the Milky Way Project catalog lie on the rim of a larger bubble, or have smaller bubbles located within them, opening up the possibility of better statistical studies of triggered star formation. This online resource of the <a href="http://www.milkywayproject.org/">Milky Way Project</a> provides a crowd-sourced map of bubbles and arcs in the Milky Way, and will enable better statistical analysis of Galactic star formation sites. This table is the first data release of the MWP IR Bubble Catalog: the authors anticipate a future release of a second, refined catalog incorporating better data-reduction techniques. This table was created by the HEASARC in March 2013 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/424/2442">CDS Catalog J/MNRAS/424/2442</a> files mwplarge.dat and mwpsmall.dat. This is a service provided by NASA HEASARC .
Candidate Galaxies Behind the Milky Way
This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region. This database was created by the HEASARC in October 1999 based on a machine-readable version that was obtained from the CDS Data Center. This is a service provided by NASA HEASARC .
Milky Way Molecular Clouds from CO Measurements
This study presents a catalog of 8107 molecular clouds that covers the entire Galactic plane and includes 98% of the <sup>12</sup>CO emission observed within b +/- 5 deg. The catalog was produced using a hierarchical cluster identification method applied to the result of a Gaussian decomposition of the Dame+ (2001ApJ...547..792D) data. The total H<sub>2</sub> mass in the catalog is 1.2 x 10<sup>9</sup> M<sub>sun</sub>, in agreement with previous estimates. The authors find that 30% of the sight lines intersect only a single cloud, with another 25% intersecting only two clouds. The most probable cloud size is R~30pc. In contrast with the general idea, the authors find a rather large range of values of surface densities, Sigma = 2 to 300 M<sub>sun</sub>/pc<sup>2</sup>, and a systematic decrease with increasing Galactic radius, R<sub>gal</sub>. The cloud velocity dispersion and the normalization sigma<sub>0</sub> = sigma<sub>v</sub> / R<sup>1/2</sup> both decrease systematically with R<sub>gal</sub>. When studied over the whole Galactic disk, there is a large dispersion in the line width-size relation and a significantly better correlation between sigma<sub>v</sub> and SigmaR. The normalization of this correlation is constant to better than a factor of two for R<sub>gal</sub> < 20kpc. This relation is used to disentangle the ambiguity between near and far kinematic distances. The authors report a strong variation of the turbulent energy injection rate. In the outer Galaxy it may be maintained by accretion through the disk and/or onto the clouds, but neither source can drive the 100 times higher cloud-averaged injection rate in the inner Galaxy. The data set used in this catalog come from that of Dame+ (2001ApJ...547..792D). Those authors combined observations obtained over a period of 20 yr with two telescopes, one in the north (first located in New York City and then moved to Cambridge, Massachusetts) and one in the south (Cerro Tololo, Chile). These 1.2m telescopes have an angular resolution of ~8.5' at 115GHz, the frequency of the <sup>12</sup>CO 1-0 line. For the current study the authors used the data set covering the whole Galactic plane with +/- 5 deg in Galactic latitude. This table was created by the HEASARC in March 2019 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/834/57">CDS Catalog J/ApJ/834/57</a> file table1.dat. This is a service provided by NASA HEASARC .
Passo del Vestito & Milky Way
<u>Source</u>: Flickr <br><u>4DCity URL</u>: <a href="https://4dcity.org/imgupload/1656262227.2736.jpg">https://4dcity.org/imgupload/1656262227.2736.jpg</a> <br>
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