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14 results for “galaxies: dwarf”
Supplementary Material for A Global Analysis of Dark Matter Signals from 27 Dwarf Spheroidal Galaxies using 11 Years of Fermi-LAT Observations
<p><strong>Description of the Supplementary Data</strong></p> <p>This record contains tabulated Bayesian and frequentist exclusion limits, profile likelihood maps and posterior probability maps for the publication S. Hoof, A. Geringer-Sameth, and R. Trotta, “<i>A Global Analysis of Dark Matter Signals from 27 Dwarf Spheroidal Galaxies using 11 Years of Fermi-LAT Observations</i>,” <a href="https://doi.org/10.1088/1475-7516/2020/02/012">JCAP 02 (2020) 012</a> (also available on the <a href="https://arxiv.org/abs/1812.06986">arXiv</a>). The dwarf spheroidal galaxies considered in this work are (in alphabetical order): Aquarius II, Boötes I, Canes Venatici I, Canes Venatici II, Carina, Carina II, Coma Berenices, Draco, Draco II, Fornax, Grus I, Hercules, Horologium I, Leo I, Leo II, Leo IV, Leo V, Pegasus III, Pisces II, Reticulum II, Sculptor, Segue 1, Sextans, Tucana II, Ursa Major I, Ursa Major II, and Ursa Minor.</p> <p>This record consists of the following files, which correspond to the limits presented Figures 9 and 10 of the paper. The files can be downloaded individually or obtained by downloading and unpacking the <code>record_2612268.zip</code>. In what follows,<code><strong>[CHANNEL]</strong></code> refers to the annihilation channel used, i.e. <i>e<sup>+</sup> e<sup>-</sup></i>, <i>μ<sup>+</sup> μ<sup>-</sup></i>, <i>τ<sup>+</sup> τ<sup>-</sup></i>, <i>b b̄</i>, <i>c c̄</i>, <i>t t̄</i>, <i>g g</i>, <i>W<sup>+</sup> W<sup>-</sup></i>, and <i>Z Z</i>. We also provide a simple plotting script for <code>Python</code>, named <code>plotting_script.py</code>, which provides basic plotting routines for all files.</p> <ul> <li>One-dimensional limits on <i><σ v></i>. The files <code>oneD_frequentist_limits_<strong>[CHANNEL]</strong>_channel.txt</code> contain the frequentist limits (at 95% confidence level, 1 degree of freedom) given the value of the WIMP mass <i>m<sub>χ</sub></i> tabulated there. The files <code>oneD_Bayesian_limits_<strong>[CHANNEL]</strong>_channel.txt</code> contain the Bayesian limit (95% credibility conditioned on the mass <i>m<sub>χ</sub></i> tabulated there).</li> <li>Two-dimensional grid of profile likelihood values. The files <code>twoD_profile_likelihood_map_<strong>[CHANNEL]</strong>_channel.txt</code> contain the natural logarithm of the profile likelihood w.r.t. the global best-fit likelihood value for that channel together with the corresponding values of <i>m<sub>χ</sub></i> and <i><σ v></i>. Note that for obtaining the limits in Fig. 10, which are conditioned on the WIMP mass, one needs to rescale the profile likelihood values with the maximum profile likelihood for a given WIMP mass.</li> <li>Two-dimensional grid of posterior probabilities for each combination of <i>m<sub>χ</sub></i> and <i><σ v></i>. The files <code>twoD_posterior_probability_map_<strong>[CHANNEL]</strong>_channel.txt</code> contain probabilities (obtained using a log-uniform prior on <i><σ v></i>) together with the corresponding values of <i>m<sub>χ</sub></i> and <i><σ v></i>. The tabulated values of <i>m<sub>χ</sub></i> and <i><σ v></i> correspond to the centres of the respective bins in <i>m<sub>χ</sub></i> and <i><σ v></i> and the posterior probability contained in them (the total posterior probability sums to 1).</li> </ul> <p>Please contact the authors if you require different data or have any questions regarding this data set.</p>
Science ready spectra and their best-fitting models described in the research paper ``Internal dynamics and stellar content of nine ultra-diffuse galaxies in the Coma cluster prove their evolutionary link with dwarf early-type galaxies'' by Chilingarian et al.
<p>Science ready spectra of nine ultra-diffuse galaxies in the Coma cluster collected with the Binospec multi-object spectrograph and their best-fitting PEGASE.HR templates obtained using the NBursts full spectrum fitting code. These spectra were presented in the paper ``Internal dynamics and stellar content of nine ultra-diffuse galaxies in the Coma cluster prove their evolutionary link with dwarf early-type galaxies'' by Chilingarian et al. accepted for publication in the Astrophysical Journal on Sep/3/2019 (arXiv:1901.05489).</p> <p>Each spectrum is presented as a binary FITS table, which contains a spectrum (wavelength, flux, uncertainties), best-fitting template, best-fitting parameters (radial velocity, age, metallicity), and a pixel mask used in the fitting procedure. For six galaxies there are two files provided: (i) one-dimensional optimally extracted integrated spectrum and (ii) two dimensional spectrum for spatially resolved radial velocity information. For the remaining three galaxies, only spatially resolved spectra are provided.</p>
Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo
<p>m2fs_HiRes_catalog_public.fits: public catalog of measurements derived from spectroscopic observations of individual targets with the Magellan/M2FS spectrograph in HiRes configuration</p> <p>m2fs_MedRes_catalog_public.fits: public catalog of measurements derived from spectroscopic observations of individual targets with the Magellen/M2FS spectrograph in MedRes configuration</p> <p>hecto_catalog_public.fits: public catalog of measurements derived from spectroscopic observations of individual targets with the MMT/Hectochelle spectrograph</p> <p>fits_files.tar.gz: Supplementary data products, including all sky-subtracted spectra from individual targets and best-fitting model spectra.</p> <p>template_spectra.tar.gz: synthetic template spectra (columns are wavelength in air (Angstroms), normalized flux)</p>
MCMC chains for distance and structural parameters of Pisces A&B dwarf galaxies
<p>These are Markov Chain Monte Carlo chains for Hubble Space Telescope observations of the dwarf galaxies Pisces A&B. More details on how they are derived will be provided in a forthcoming ApJ paper.</p>
Simulations of the NGC-5466 tidal stream in a Galactic-like potential, with and without dwarf galaxies included
<p>A mock stream of NGC-5466 simulated with the particle-spray code `galpy.df.streamspraydf`, which is an implementation of the Fardal et al 2015 mock stream generation method. The current position and velocity of the progenitor globular cluster is from Vasiliev et al 2019. The progenitor's orbit is back-integrated 5 Gyr in a `galpy.potential.MWPotential2014` potential then forward integrated, forming the tidal tails. The file with the name 'dwarfgalaxy' includes the effects of dwarf galaxies on the stream. For more information see (and cite) <a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.2437E/abstract">https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.2437E</a>.</p>
Stellar Density Profiles of Dwarf Spheroidal Galaxies - Posterior Distributions
<p>This archive contains samples from the posterior distributions of our 3-plummer, 1-plummer, 3-steeper and 1-steeper fits for 40 dwarf spheroidal galaxies as described in "Stellar Density Profiles of Dwarf Spheroidal Galaxies" (<a href="https://arxiv.org/abs/1910.10134">https://arxiv.org/abs/1910.10134</a>)</p>
Reproduction package for the paper "A LOFAR sample of luminous compact sources coincident with nearby dwarf galaxies"
<p>Scripts to reproduce analyses from Vohl et al. 2023, A&A.</p>
The Binary Fraction of Stars in Dwarf Galaxies: The Cases of Draco and Ursa Minor
<p>supplementary data products, including all sky-subtracted spectra from individual targets, as well as random draws from posterior PDFs for model parameters (see enclosed README file)</p>
Stellar Density Profiles of Dwarf Spheroidal Galaxies: Posterior Distributions
<p>This archive contains samples from the posterior distributions of our 3-plummer, 1-plummer, 3-steeper and 1-steeper fits for 38 dwarf spheroidal galaxies.</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>
Data for "HSTPROMO Internal Proper Motion Kinematics of Dwarf Spheroidal Galaxies: I. Velocity Anisotropy and Dark Matter Cusp Slope of Draco"
<p>DATA FOR:</p> <p>HSTPROMO Internal Proper Motion Kinematics of Dwarf Spheroidal Galaxies: I. Velocity Anisotropy and Dark Matter Cusp Slope of Draco</p> <p>THE PUBLIC FILES THAT ARE SHARED HERE ARE:</p> <p>1. DRACO_STARS: This file contains measured proper motions, uncertainties and respective instrumental magnitudes of stars with proper motion uncertainties smaller than Draco's intrinsic velocity dispersion. The detailed explanation of this dataset is given in Vitral et al. (2024, Section 2.3.5).<br>2. DRACO_BINS: This file corresponds to the data points in Figure 11 from Vitral et al. (2024), corresponding to 3D velocity dispersion profiles and respective line-of-sight rotation curve from Draco.<br>3. DRACO_LOS: This file contains the field "OBJ_ID" from the line-of-sight catalog from Walker et al. (2023) concerning the stars retained for internal mass-modeling in Vitral et al. (2024).</p> <p>Please read the "Notes" section of each file for further information.</p> <p>Please cite the following papers when using these catalogs:</p> <p>- Vitral et al. (2024), ApJ, DOI: <a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad571c" target="_blank" rel="noopener">10.3847/1538-4357/ad571c</a><br>- Walker et al. (2023), ApJS, 268, 19, DOI: <a href="https://doi.org/10.3847/1538-4365/acdd79">10.3847/1538-4365/acdd79</a></p>
A Multi-epoch Kinematic Study of the Remote Dwarf Spheroidal Galaxy Leo II
<p>supplementary data products, including all sky-subtracted spectra from individual targets, as well as random draws from posterior PDFs for model parameters (see enclosed README file)</p> <p> </p>
Dataset to Exploring X-ray Properties of Low Metallicity Dwarf Galaxies
<p>MCMC chains from the LW2-LX relation in Exploring X-ray Properties of Low Metallicity Dwarf Galaxies. In press at ApJ.</p>
Fornax Dwarf Galaxy XMM-Newton X-Ray Point Source Catalog
This table contains some of the results of a deep archive XMM-Newton observation of the Fornax spheroidal galaxy that the authors analyzed with the aim of fully characterizing the X-ray source population (in most of the cases likely to be background active galactic nuclei) detected towards the target. A cross-correlation with the available databases allowed them to find a source that may be associated with a variable star belonging to the galaxy. The authors also searched for X-ray sources in the vicinity of the Fornax globular clusters GC 3 and GC 4 and found two sources probably associated with the respective clusters. The deep X-ray observation was also suitable for the search for the intermediate-mass black hole (of mass ~ 10<sup>4</sup> solar masses) expected to be hosted in the center of the galaxy. In the case of Fornax, this search is extremely difficult since the galaxy centroid of gravity is poorly constrained because of the large asymmetry observed in the optical surface brightness. Since the authors cannot firmly establish the existence of an X-ray counterpart of the putative black hole, they put constraints only on the accretion parameters. In particular, they found that the corresponding upper limit on the accretion efficiency, with respect to the Eddington luminosity, is as low as a few 10<sup>-5</sup>. This table was created by the HEASARC in February 2013 based on an electronic version of Table 1 from the reference paper which was obtained from the A&A web site. This is a service provided by NASA HEASARC .
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