Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>Using deep machine learning we show that the internal velocities of galaxies can be retrieved from optical images trained using 4596 systems observed with the SDSS-MaNGA survey. Using only <jats:italic>i</jats:italic>-band images we show that the velocity dispersions and the rotational velocities of galaxies can be measured to an accuracy of 29 km s<jats:sup>−1</jats:sup> and 69 km s<jats:sup>−1</jats:sup> respectively, close to the resolution limit of the spectroscopic data. This shows that galaxy structures in the optical holds important information concerning the internal properties of galaxies, and that the internal kinematics of galaxies are quantitatively reflected in their stellar light distributions.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The Dark Energy Spectroscopic Instrument (DESI) will execute a nearly magnitude-limited survey of low redshift galaxies (0.05 ≤ <jats:italic>z</jats:italic> ≤ 0.4, median <jats:italic>z</jats:italic> ≈ 0.2). Clustering analyses of this Bright Galaxy Survey (BGS) will yield the most precise measurements to date of baryon acoustic oscillations and redshift-space distortions at low redshift. DESI BGS will comprise two target classes: (i) BRIGHT (<jats:italic>r</jats:italic> &lt; 19.5 mag), and (ii) FAINT (19.5 &lt; <jats:italic>r</jats:italic> &lt; 20 mag). Here we present a summary of the star-galaxy separation, and different photometric and geometrical masks, used in BGS to reduce the number of spurious targets. The selection results in a total density of ∼800 objects deg<jats:sup>−2</jats:sup> for the BRIGHT and ∼600 objects deg<jats:sup>−2</jats:sup> for the FAINT selections. A full characterization of the BGS selection can be found in Ruiz-Macias et al.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The DESI Milky Way Survey (MWS) will observe ≥8 million stars between 16 &lt; <jats:italic>r</jats:italic> &lt; 19 mag, supplemented by observations of brighter targets under poor observing conditions. The survey will permit an accurate determination of stellar kinematics and population gradients, characterize diffuse substructure in the thick disk and stellar halo, enable the discovery of extremely metal-poor stars and other rare stellar types, and improve constraints on the Galaxy’s 3D dark matter distribution from halo star kinematics. MWS will also enable a detailed characterization of the stellar populations within 100 pc of the Sun, including a complete census of white dwarfs. The target catalog from the preliminary selection described here is public (Available at <jats:ext-link xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="uri" xlink:href="https://data.desi.lbl.gov/public/ets/target/catalogs/" xlink:type="simple">https://data.desi.lbl.gov/public/ets/target/catalogs/</jats:ext-link> and detailed at  <jats:ext-link xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="uri" xlink:href="https://desidatamodel.readthedocs.io" xlink:type="simple">https://desidatamodel.readthedocs.io</jats:ext-link>).</jats:p>