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91 results for “Milky way”
13. Kepler 452b [Milky way Planets]
<p>13. Kepler 452b [Milky way Planets]</p> <p>In this video, visualization of Kepler 452b is carried out; various positions of Kepler 452b in the space</p>
11. Kepler 22b [Milky way Planets]
<p>11. Kepler 22b [Milky way Planets]</p> <p>In this video, visualization of Kepler 22b is carried out; various positions of Kepler 22b in the space</p>
10. K2-3d [Milky way Planets]
<p>10. K2-3d [Milky way Planets]</p> <p>In this video, visualization of K2-3d is carried out; various positions of K2-3d in the space</p>
09. HD40307g [Milky way Planets]
<p>09. HD40307g [Milky way Planets]</p> <p>In this video, visualization of HD40307g is carried out; various positions of HD40307g in the space</p>
06. Gliese 3293b [Milky way Planets]
<p>06. Gliese 3293b [Milky way Planets]</p> <p>In this video, visualization of Gliese 3293b is carried out; various positions of Gliese 3293b in the space</p>
05. Gliese 581g [Milky way Planets]
<p>05. Gliese 581g [Milkyway Planets]</p> <p>In this video, visualization of Gliese 581g is carried out; various positions of Gliese 581g in the space</p>
23. Kapteyn b [Milky way Planets]
<p>23. Kapteyn b [Milky way Planets]</p> <p>In this video, visualization of Kapteyn b is carried out; various positions of Kapteyn b in the space</p>
02. Sun, Venus [Milky way Planets]
<p>02. Sun, Venus [Milky way Planets]</p> <p>In this video, visualization of Sun and Venus is carried out; various positions of Sun and Venus in the space.</p>
25. Trappist-1e [Milky way Planets]
<p>25. Trappist-1e [Milky way Planets]</p> <p>In this video, visualization of Trappist-1e is carried out; various positions of Trappist-1e in the space</p>
19. Kepler 1229b [Milky way Planets]
<p>19. Kepler 1229b [Milky way Planets]</p> <p>In this video, visualization of Kepler 1229b is carried out; various positions of Kepler 1229b in the space</p>
20. Proxima Cetie [Milky way Planets]
<p>20. Proxima Cetie [Milky way Planets]</p> <p>In this video, visualization of Proxima Cetie is carried out; various positions of Proxima Cetie in the space</p>
Internal proper motion dispersion profiles for 37 Milky Way globular clusters extracted from Gaia EDR3
<p>Internal proper motion dispersion profiles, in the radial and tangential components, extracted from Gaia EDR3 data for 37 Milky Way globular clusters.</p> <p>Created for, and used for model fitting in, the submitted manuscript: "Multimass modelling of Milky Way globular clusters - I. Implications on their stellar initial mass function above 1 M$_{\odot}$". Details on the creation of this dataset are available within this article.</p>
Finding Stellar Streams in the Milky Way with CWoLa
<p>These datasets are designed to accompany the paper <em>Weakly-Supervised Anomaly Detection in the Milky Way </em>by M. Pettee, S. Thanvantri, B. Nachman, D. Shih, M. R. Buckley, and J. H. Collins (<a href="https://arxiv.org/abs/2305.03761">https://arxiv.org/abs/2305.03761</a>). They illustrate how the Classification Without Labels (CWoLa) technique can be applied in the search for localized anomalies -- in this case, cold stellar streams -- in the <em>Gaia </em>DR2 dataset. We consider both simulated stellar streams and the known stream GD-1. The codebase is located at <a href="https://github.com/hep-lbdl/GaiaCWoLa">https://github.com/hep-lbdl/GaiaCWoLa</a>. </p> <p>These datasets are all formatted as Pandas DataFrames, and can be loaded using `df = pd.read_hdf(file)`. Datasets ending in `*_cwola.h5*` indicate that CWoLa has been applied to the stars in that dataset. For this analysis, we consider circular "patches" of the sky of radius 15° from the Gaia DR2 dataset. </p> <p>Columns include: </p> <ul> <li>μ_δ: Proper motion (declination)</li> <li>μ_α: Proper motion (right ascension)</li> <li>δ: Declination</li> <li>α: Right ascension</li> <li>α_wrapped: Right ascension, wrapped such that all angles are > 0 </li> <li>b-r: Color</li> <li>g: Magnitude</li> <li>ϕ: Rotated & centered right ascension </li> <li>λ: Rotated & centered declination </li> <li>μ_ϕcosλ: Rotated & centered proper motion (right ascension) </li> <li>μ_λ: Rotated & centered proper motion (declination) </li> <li>stream: Boolean label (True if part of ground truth labeling for GD-1)</li> <li>patch_id: Index of the 21 patches of the GD-1 scan</li> <li>nn_score: CWoLa classifier score (0 = more background-like; 1 = more signal=like)</li> <li>5d_distance: For the potential GD-1 member candidates, the 5D Euclidean distance to the nearest labeled star</li> </ul> <p>Files include:</p> <ul> <li>gd1_1_patch.h5 <ul> <li>Example patch of GD-1</li> </ul> </li> <li>gd1_21_patches_cwola.h5 <ul> <li>Results from applying CWoLa to the 21 patches spanning GD-1 </li> </ul> </li> <li>promising_stars.h5 <ul> <li>A list of stars identified by CWoLa that do not belong to the labeled GD-1 stream catalogue, but are close in 5D Euclidean space to labeled stars. Ordered in descending order by CWoLa classifier score. </li> </ul> </li> <li>scan_bump_cwola.h5 <ul> <li>An example of how to apply CWoLa in a scan where the stream location is unknown</li> </ul> </li> <li>scan_no_bump_cwola.h5 <ul> <li>An example of how to apply CWoLa in a scan where the stream location is unknown</li> </ul> </li> <li>simulated_100_patches.h5 <ul> <li>Results from applying CWoLa to 100 simulated streams </li> </ul> </li> <li>simulated_patch.h5 <ul> <li>A full simulated stream </li> </ul> </li> <li>simulated_patch_cwola.h5 <ul> <li>Results from applying CWoLa to the example simulated stream</li> </ul> </li> </ul> <p>To recreate the full scan across GD-1, one would need to use the original 21 patches of Gaia DR2 located at <a href="https://doi.org/10.5281/zenodo.7897935">10.5281/zenodo.7897935</a> that were constructed for <a href="https://arxiv.org/abs/2104.12789">arXiv:2104.12789</a> [astro-ph.GA). GD-1 labels were derived from <a href="https://doi.org/10.5281/zenodo.1295543">10.5281/zenodo.1295543</a>. </p>
CSFD: The Corrected SFD Milky Way Dust Map
<p>This package contains the full-sky CSFD Galactic dust reddening E(B−V) map and associated data products described in <a href="https://arxiv.org/abs/2306.03926">Chiang 2023 (arXiv:2306.03926)</a>.</p> <p>This dust map improves upon the widely used <a href="https://ui.adsabs.harvard.edu/abs/1998ApJ...500..525S/abstract">Schlegel, Finkbeiner, & Davis (1998, SFD)</a> map by removing a tomographically reconstructed cosmic infrared background (CIB) component that contaminates the original SFD. This new dust map enables more accurate Galactic extinction corrections for extragalactic photometry. More information can be found on the <a href="https://idv.sinica.edu.tw/ykchiang/CSFD.html">project website</a>.</p>
Milky Way Satellites Shining Bright in Gravitational Waves: dataset release
<p>Data release relative to the analysis presented in:<br> Milky Way Satellites Shining Bright in Gravitational Waves (<a href="https://arxiv.org/abs/2002.10465">arxiv:2002.10465</a>)<br> Folders and subfolders are arranged by source properties</p> <ul> <li>Satellite name <ul> <li>Frequency <ul> <li>Component Masses <ul> <li>Inclination</li> </ul> </li> </ul> </li> </ul> </li> </ul> <p>as described in the paper.<br> Posterior samples, parameter estimation configuration files, sky localisation and SNR estimates are released.</p>
Strong chemical tagging with APOGEE: 21 candidate star clusters that have dissolved across the Milky Way disc
<p>Two files containing the chemically tagged abundances derived by astroNN from the Apache Point Observatory Galactic Evolution Experiment. The chemical tagging procedure is described in <a href="https://arxiv.org/abs/2004.04263">https://arxiv.org/abs/2004.04263</a>. DBSCAN_labels_APOGEE_DR16.npy contains only members of groups with more than 15 members and silhouette coefficients greater than 0. DBSCAN_labels_APOGEE_DR16_all.npy contains labels for all stars in the quality controlled data set. The data are packaged as a numpy structured array. Most of the columns are described at <a href="https://data.sdss.org/datamodel/files/APOGEE_ASTRONN/apogee_astronn.html">https://data.sdss.org/datamodel/files/APOGEE_ASTRONN/apogee_astronn.html</a>. There are two additional columns: CLUSTER_ID, and SILHOUETTE_COEFF, which are respectively the label and silhouette coefficient for each star.</p>
Catalogue of stars in Milky Way Dwarf Spheroidal Galaxies from Gaia EDR3
<p>Pace, Erkal, and Li 2022. </p> <p>Summary Table (including fits, csv, and npy file formats)</p> <p>(1) Catalogs</p> <p>(2) Diagnostic Plot Figures</p> <p>(3) Comparison Plot Figures</p> <p>v2 changes:</p> <ul> <li>The input velocity of Tucana V had the incorrect sign and has been corrected. All orbit models and values that depended on the velocity have been updated. </li> <li>the column "rhalf_sph_physical_mcmc_error" had the same values for each galaxy.</li> <li>The error columns (ep/em) for the following columns have been updated: average_density, m_l, mhalf, density_ratio. The errors are now the difference between the 16/84 confidence interval and the 50 confidence interval which follows the format of the rest of the summary file. </li> </ul> <p>v3 changes:</p> <ul> <li>The correlation errors between pmra, pmdec where incorrectly computed (named edr3_pmra_pmdec_error and edr3_gauss_pmra_pmdec_error in the catalogs here) and have been fixed. Only the summary files have been updated. </li> </ul>
Simulation data for the article "On the Effect of the Large Magellanic Cloud on the Orbital Poles of Milky Way Satellite Galaxies"
<p>This archive contains the data shared in the context of the "On the Effect of the Large Magellanic Cloud on the Orbital Poles of Milky Way Satellite Galaxies" article.</p> <p>In particular, it contains the initial conditions and final snapshots of our N-body simulation.</p>
age metallicity data for simulated Milky Way mass galaxy from the NIHAO-UHD suite
<p>pickle file containing ages and metallicities of stellar particles from the galaxy g2.79e12 from the NIHAO-UHD simulation suite</p>
Milky Way phase spiral animations
<h3>Animations of the Gaia phase spiral in the Milky Way disc</h3> <p>This record contains three animations showing the number density of stars in the Milky Way disc in the Z-V_Z phase plane in a range of azimuthal angles.</p> <p>Stars in the Z-V_Z phase plane in the Milky Way disc form a spiral pattern, a phase spiral, and the orientation of this spiral depends on the location in the Galaxy of the stars. </p> <p>The animations show the phase spiral in a moving 5 degree range going from 210 degrees to 150 degrees in Galactic azimuth, showing an apparent rotation of approximately 90 degrees. The stars are located in the outer part of the MW disc, selected by vertical angular momentum, L_Z. The ranges of angular momentum are 2000-2200, 2200-2400, and 2400-2600 kpc km / s for the low, medium, and high angular momentum animations respectively. The phase spiral pattern is clearest by far in the medium range.</p> <p>The Sun lays at an azimuthal angle of 180 degrees in this system, and the azimuthal angle is decreasing in the direction of Galactic rotation.</p>
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