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7 results for “Stellar streams”
Supplementary data to "GD-1 STELLAR STREAM AND COCOON IN THE DESI EARLY DATA RELEASE"
<p>Supplementary material to DESI's publication "GD-1 STELLAR STREAM AND COCOON IN THE DESI EARLY DATA RELEASE" to comply with the data management plan. Data associated with revised version of paper submitted to The Astrophysical Journal. Directory contains data points for all figures with file names indicating the figure to which the data corresponds as well as a FITS file for Table 4. Data for 13 figures and one table (46 FITS files) included in .zip directory</p>
Data for section 3.2 of Stellar Population Properties in the Stellar Streams Around SPRC047
<p>Supplementary (input and output) data for Section 3.2 ("<em>Measurement Uncertainties in the Deconvolved Image</em>") of the paper "<em>Stellar Population Properties in the Stellar Streams Around SPRC047</em>", accepted for publication in ApJ and available in <a href="https://arxiv.org/abs/2312.05358" target="_blank" rel="noopener">arXiv:2312.05358.</a> The source code for this project is publicly available <a href="https://gitlab.com/makhlaghi/sprc047-stream-clumps-photometry" target="_blank" rel="noopener">on Gitlab</a> and is archived on<a href="https://archive.softwareheritage.org/swh:1:dir:882514891cdcfc08261409352437bc6b8a836b8b;origin=https://gitlab.com/makhlaghi/sprc047-stream-clumps-photometry;visit=swh:1:snp:11cb02c374d7856028c57fb7312b60531f1be2e6;anchor=swh:1:rev:5d81b833931e58732627c06998c2488e6d2a8fb7" target="_blank" rel="noopener"> SoftwareHeritage</a> for longevity.</p> <p>A brief description of the contents in this repository are given below. Note that because the AWMLE deconvolution code is not yet publicly released, the second two files below are necessary (they are used by the reproducible Makefile of this section <a href="https://gitlab.com/makhlaghi/sprc047-stream-clumps-photometry" target="_blank" rel="noopener">on Gitlab</a>).</p> <ul> <li><a href="../records/10397812/files/sprc047_3.6um-bck.fits?download=1">sprc047_3.6um-bck.fits</a>: Spitzer image of SPRC047.</li> <li><a href="../records/10397812/files/deconvolved-it75.fits?download=1">deconvolved-it75.fits</a>: The deconvolved Spitzer image.</li> <li><a href="../records/10397812/files/deconvolved-simulated.tar.gz?download=1">deconvolved-simulated.tar.gz</a>: 100 realizations of random noise over a point-like source used to estimate the error of the deconvolved measurements.</li> </ul>
Simulation data for the article "Revisiting a disky origin for the faint branch of the Sagittarius stellar stream"
<p>This archive contains the data shared in the context of the "Revisiting a disky origin for the faint branch of the Sagittarius stellar stream" (Oria et al. 2022) article. It allows one to run the simulation of the Sgr dwarf falling into the joint potential of the MW and the LMC, based on the model of Vasiliev et al. (2021), and extended with our faint branch particles. Furthermore, plots and videos complementary to those shown in the article are shared here as well.</p> <p><strong>best_model_y_axis_rotation</strong></p> <p>contains data pertaining to our best model, put forward in the article: plots of the evolution of our faint branch particles for every snapshot of the simulation and its corresponding video, initial conditions, trajectory of the progenitor, final snapshot with many coordinates and kinematics. </p> <p><strong>other_model_x_axis_rotation</strong></p> <p>contains the same data as before for our other model mentioned in the article</p> <p><strong>potentials_triax</strong></p> <p>contains the evolving MW+LMC potential files as shared by Vasiliev et al. (2021), under DOI 10.5281/zenodo.4300977 necessary to run the simulation</p> <p><strong>scripts</strong></p> <p>contains scripts to create the initial conditions (with Agama) and run the simulation (with Gyrfalcon)</p>
oceanus: Populations of stellar streams in deforming MW--LMC systems - I
<p>We publish o<em>ceanus,</em> the t = 0 Gyr simulation snapshots of all 16,384 streams in each MW--LMC potential used in<em> </em>Brooks, R. A. N et al. (2024)<em>.</em> The first part of the archived data includes:</p> <ul> <li><strong>rigid-mw-woutmotion-nolmc.hdf5</strong> - dataset for the stream population generated in the "Rigid MW without motion (no LMC)" potential.</li> <li><strong>rigid-mw-wmotion-nolmc.hdf5</strong> - dataset for the stream population generated in the "Rigid MW + motion (no LMC)" potential.</li> <li><strong>rigidmono-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Rigid Monopole & LMC" potential.</li> <li><strong>evolmono-wlmc.hdf5</strong> - dataset for the stream population generated in the "Evolving Monopole & LMC" potential.</li> </ul> <p>Each stream contains 20,000 particles with 3-D Galactocentric positions and velocities, plus progenitor information on its initial conditions, mass and scale radius. We do not include summary statistic values. The functions to calculate stream summary statistics will be shared upon reasonable request. This dataset can be used to explore the effect of the LMC and the MW halo response on MW streams.</p> <p>The basis function expansion MW--LMC potentials can be found and installed using instruction at:<em> </em><a href="https://github.com/sophialilleengen/mwlmc" target="_blank" rel="noopener">https://github.com/sophialilleengen/mwlmc</a>.</p>
oceanus: Populations of stellar streams in deforming MW--LMC systems - II
<p>We publish o<em>ceanus,</em> the t = 0 Gyr simulation snapshots of all 16,384 streams in each MW--LMC potential used in Brooks, R. A. N et al. (2024)<em>.</em> The second part of the archived data includes:</p> <ul> <li><strong>monodipole-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Monopole + Dipole & LMC" potential.</li> <li><strong>monoquad-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Monopole + Quadrupole & LMC" potential.</li> <li><strong>monodipolequad-wlmc.hdf5 </strong>- dataset for the stream population generated in the "Monopole + Dipole + Quadrupole & LMC" potential.</li> <li><strong>fullexp-nolmc.hdf5 </strong>- dataset for the stream population generated in the "ull Expansion & LMC" potential.</li> <li><strong>fullexp-wlmc.hdf5 </strong>- dataset for the stream population generated in the "ull Expansion (no LMC)" potential.</li> </ul> <p>Each stream contains 20,000 particles with 3-D Galactocentric positions and velocities, plus progenitor information on its initial conditions, mass and scale radius. We do not include summary statistic values. The functions to calculate stream summary statistics will be shared upon reasonable request. This dataset can be used to explore the effect of the LMC and the MW halo response on MW streams.</p> <p>The basis function expansion MW--LMC potentials can be found and installed using instruction at: <a href="https://github.com/sophialilleengen/mwlmc" target="_blank" rel="noopener">https://github.com/sophialilleengen/mwlmc</a>.</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>
Stellar Stream Models in the presence of the Milky Way and LMC
<p>These files include simulated stream models from Shipp et al. 2021 (https://ui.adsabs.harvard.edu/abs/2021arXiv210713004S/abstract).</p> <p>These streams are simulated using a modified Lagrange Cloud Stripping technique developed in Gibbons 2014, in a McMillan 2017 Milky Way potential, and with an LMC modeled as a Hernquist profile, with details described in Shipp et al. 2021. These are best-fit models resulting from fits to data from the Southern Stellar Stream Spectroscopic Survey (S5), Gaia, and the Dark Energy Survey (DES).</p> <p>The columns, as listed in the file headers, are ra and dec (deg), stream coordinates phi1 and phi2 (deg), proper motion in ra and dec (mas/yr, without reflex correction), radial velocity (km/s), Heliocentric distance (kpc), and stream positions and velocities in standard Galactocentric cartesian coordinates, x, y, z (kpc), vx, vy, vz (km/s).</p> <p>Please cite <a href="https://ui.adsabs.harvard.edu/abs/2021arXiv210713004S/abstract">Shipp et al. 2021</a> if you make use of this data.</p>
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