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21 results for “APOGEE”
Data Associated with Chemical Cartography with APOGEE: Two-process Parameters and Residual Abundances for 288,789 Stars from Data Release 17
<p>Stellar abundance measurements are subject to systematic errors that induce extra scatter and artificial correlations in elemental abundance patterns. We derive empirical calibration offsets to remove systematic trends with surface gravity log(g) in 17 elemental abundances of 288,789 evolved stars from the SDSS APOGEE survey. We fit these corrected abundances as the sum of a prompt process tracing core-collapse supernovae and a delayed process tracing Type Ia supernovae, thus recasting each star's measurements into the amplitudes A_cc and A_Ia and the element-by-element residuals from this two-parameter fit. Here we present the log(g)-calibrated abundances, fit parameters, process amplitudes, and element-by-element abundance residuals of 288,789 stars (310,427 spectra) in APOGEE DR17 that accompany <a href="https://arxiv.org/abs/2403.08067" target="_blank" rel="noopener">the paper</a>.</p> <p>calibration_values_final.dat contains all derived calibration offsets, including the grids of log(g) calibration offsets and zero-point offsets for two-process model analysis. The first five rows of this catalog are reproduced in Table 2 of the paper.</p> <p>logg_calib_example.ipynb is a Jupyter notebook containing Python code to load calibration_values_final.dat, extract the log(g) calibration offsets for specific element, and apply calibration offsets to 10 sample stars.</p> <p>2process_residual_abund_catalog_final.fits is the catalog of 310,427 APOGEE DR17 spectra (288,789 unique stars) containing calibrated abundances, two-process fit parameters, and abundance residuals. A full listing of columns in this catalog is given in Table 5 of the paper.</p> <p>catalog_examples.ipynb is a Jupyter notebook containing Python code to load 2process_residual_abund_catalog_final.fits, cross match with other catalogs (using AstroNN and the APOGEE DR17 Globular Cluster Value-Added Catalog as examples), and make some example plots utilizing the cross-matched data.</p>
Observation logs for APOGEE-1
<p>These files are the observation logs for the SDSS-III/APOGEE survey. The provide information on when different locations on the sky were observed and for how long. They are to be used with the code at https://github.com/jobovy/apogee for determining the APOGEE selection function (the fraction of potential targets observed as in different parts of the sky).</p>
DETERMINING AGES OF APOGEE GIANTS WITH KNOWN DISTANCES - Full PDFs
<p>Supplementary data to Feuillet+ (2016, ApJ, arXiv:1511.04088):</p> <p>Using the APOGEE survey instrument and the NMSU 1m telescope, we observe a sample of bright, nearby, red giant stars with known distances measured by Hipparcos. By applying Bayesian analysis and hierarchical modeling, we determine individual stellar ages and the star formation histories of single alpha-abundance subsamples. The probability distribution functions (PDFs) and modeled star formation histories (SFHs) of all stars analyzed in this paper.</p> <p>Data included: APOGEE/2MASS ID, the age values for PDFs in log(age), the isochrone matching likelihood function as given in Equation 4 of paper, the age PDF of a Bayesian analysis using a flat SFH (Section 4.3), the hierarchically modeled SFH using an alpha-abundance dependent Gaussian+uniform model (Section 4.6), and the age PDF of an empirical Bayesian analysis using the hierarchically modeled SFH (Section 4.6). Individual ages of stars in the paper are taken as the mean of the age PDF, however, most PDFs are non-Gaussian, which introduces complicated errors into the selection of a single age.</p>
The APO-K2 Catalog. I. ~7,500 Red Giants with Fundamental Stellar Parameters from APOGEE DR17 Spectroscopy and K2-GAP Asteroseismology
<p><strong>Abstract: </strong>We present a catalog of fundamental stellar properties for ~7,500 evolved stars, including stellar radii and masses, determined from the combination of spectroscopic observations from the Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey IV (SDSS), and asteroseismology from K2. The resulting APO-K2 catalog provides spectroscopically derived temperatures and metallicities, asteroseismic global parameters, evolutionary states, and asteroseismically-derived masses and radii. Additionally, we include kinematic information from <em>Gaia</em>. We investigate the multi-dimensional space of abundance, stellar mass, and velocity with an eye toward applications in Galactic archaeology. The APO-K2 sample has a large population of low metallicity stars (~288 at [M/H] ≤ -1), and their asteroseismic masses are larger than astrophysical estimates. We argue that this may reflect offsets in the adopted fundamental temperature scale for metal-poor stars rather than metallicity-dependent issues with interpreting asteroseismic data. We characterize the kinematic properties of the population as a function of α-enhancement and position in the disk and identify those stars in the sample that are candidate components of the <em>Gaia-Enceladus</em> merger. Importantly, we characterize the selection function for the APO-K2 sample as a function of metallicity, radius, mass, νmax, color, and magnitude referencing Galactic simulations and target selection criteria to enable robust statistical inferences with the catalog.</p> <p><strong>Included Files:</strong></p> <ul> <li>The publicly available APO-K2 catalog, the is provided in the publication.</li> <li>The APO-K2 catalog without truncation to any numbers. </li> <li>The selection function relative density tables for the mass-radius parameter space. </li> <li>The selection function relative density tables for the metallicity-mass parameter space. </li> <li>The selection function relative density tables for the magnitude-color parameter space. </li> <li>The selection function relative density tables for the ν<sub>max</sub>-mag parameter space. </li> </ul>
APOGEE LSFs for DR12
<p>These files are the APOGEE LSF for it's Data Release 12 (DR12) as (a) an average of a combination of 6 fibers (apogee-lsf-dr12-combo.fits) and (b) an average of all fibers. The LSF is computed at pixel offsets x= numpy.linspace(-7.,7.,43) and at pixel centers subdivided in 3. For use with https://github.com/jobovy/apogee.</p>
APOGEE DR13 matched to Gaia DR1
<p><strong>APOGEE DR13</strong></p> <p>from Jessica Birky.</p> <p>Documentation https://arxiv.org/pdf/1608.02013.pdf</p> <p> </p> <p>the download link for the catalog of all of the APOGEE sources:</p> <p>https://data.sdss.org/sas/dr13/apogee/spectro/redux/r6/allStar-l30e.2.fits</p> <p> </p> <p>In addition, Jessica's list of specific M star sources with their RA and DEC values `APOGEE_Mstars.csv`</p> <p> </p> <p>crossmatch with Gaia DR1 TGAS by M. Fouesneau provided in</p> <p>`xmatch_TGAS_allStar-l30e.2.fits` median angular matched distances 0.08 arcsec.</p> <p>`xmatch_TGAS_APOGEE_Mstars.csv` median angular matched distances 0.073 arcsec.</p> <p> </p> <p>crossmatch with Gaia DR1 (all) by M. Fouesneau provided in</p> <p>`xmatch_DR1_allStar-l30e.2.fits` median angular matched distances 0.12 arcsec.</p> <p>`xmatch_DR1_APOGEE_Mstars.csv` median angular matched distances 0.108 arcsec.</p>
Spectro-photometric distances and self-calibrated abundances for Apogee DR16 RGB stars within the Milky Way disk
<p>The data file contains 48,853 RGB stars from Apogee DR16 within the Milky Way disk, for which we determine spectro-photometric parallax estimates (as described in Hogg et al. 2019, AJ, 158, 147), as well as self-calibrated stellar element abundances. The data set is described in detail and analyzed in Eilers et al. 2022 (arXiv: 2112.03295).</p>
Data for lodubay/galactic-dtd: Multi-Zone Galactic Chemical Evolution Model Outputs and APOGEE Sample
<p>Data for <a href="github.com/lodubay/galactic-dtd">lodubay/galactic-dtd</a>, a project exploring different models for the Type Ia supernova delay-time distribution (DTD) in multi-zone galactic chemical evolution models with the <a href="github.com/giganano/VICE">VICE</a> package. This dataset contains two files: <code>multizone.tar.gz</code> is a compressed archive of all 33 multi-zone outputs (combinations of 8 DTDs x 4 star formation histories, plus one with an alternate stellar migration scheme), and <code>sample.csv</code> contains chemical abundance data from the <a href="https://www.sdss4.org/surveys/apogee/">APOGEE survey</a> (data release 17) and stellar ages from <a href="https://ui.adsabs.harvard.edu/abs/2023MNRAS.tmp.1191L">Leung et al. (2023)</a>. This project is made reproducible with <code>showyourwork</code>, which will automatically download and extract all data from this deposit when it builds the article.</p> <p>This version contains a minor update to the APOGEE sample file.</p>
Dataset: Apogee Enterprises, Inc. (APOG) Stock Performance
This dataset provides historical stock market performance data for specific companies. It enables users to analyze and understand the past trends and fluctuations in stock prices over time. This information can be utilized for various purposes such as investment analysis, financial research, and market trend forecasting.
Dataset: Apogee Enterprises, Inc. (APOG) Stock Performance
This dataset provides historical stock market performance data for specific companies. It enables users to analyze and understand the past trends and fluctuations in stock prices over time. This information can be utilized for various purposes such as investment analysis, financial research, and market trend forecasting.
Dataset: Apogee Therapeutics, Inc. (APGE) Stock Performance
This dataset provides historical stock market performance data for specific companies. It enables users to analyze and understand the past trends and fluctuations in stock prices over time. This information can be utilized for various purposes such as investment analysis, financial research, and market trend forecasting.
APOGEE-Kepler Catalog SDSS Internal Version
<p>This represents the publication of the SDSS internal version of the APOGEE-Kepler Catalog (v.7.4.0, August 2024), previous versions of which have been available to SDSS-IV collaboration members on the internal wiki page https://trac.sdss.org/wiki/APOGEE2/APOKASC/Catalog and have been used for a variety of projects. It has been designed to include all stars in the Kepler field which had APOGEE spectra at the end of SDSS-IV (DR17) and as such is not limited to giants or seismic oscillators. For giant oscillators, this catalog contains a subset of the information available in all of the tables available with the journal edition of the APOKASC-3 catalog (Pinsonneault et al., 2024), as well as some additional information including matches to external datasets that may be of interest. This table also contains some historical information, previous versions of some values, and so forth that were used for comparison and validation. The header_APOKASC_cat_v7.4.0.txt file contains a list of the available columns as well as some descriptions of where the values are from. These values represent effort from a variety of people including those involved in the APOKASC collaboration as well as related individual efforts and anyone using this data is strongly encouraged to cite the original published version. In all cases where the values in this file and the values in the journal disagree, the journal values should be viewed as the correct version of record. The fits and ascii versions of the APOKASC catalog are the same, and both are provided for ease of use. </p>
UniDAM results for APOGEE dr16
<p>UniDAM results for APOGEE dr16 + Gaia dr2 parallax + 2MASS/AllWISE photometry.</p> <p>Parallax offset of 0.052 mas is used for Gaia parallaxes</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>
Corrected DR12 APOGEE linelist
<p>This is a corrected version of the DR12 APOGEE linelist for high-resolution, H-band spectroscopy of cool stars. The linelist is in air wavelengths in Turbospectrum format (http://www.pages-perso-bertrand-plez.univ-montp2.fr/). This linelist was provided by Matthew Shetrone, using the same methodology as in APOGEE DR12 (see http://arxiv.org/abs/1502.04080), but correcting the total-flux vs. center-of-disk bug in the APOGEE DR12 line list.</p>
Data for "Improving Radial Velocities by Marginalizing over Stars and Sky: Achieving 30 m/s RV Precision for APOGEE in the Plate Era"
<p>Data products associated with the paper "Improving Radial Velocities by Marginalizing over Stars and Sky: Achieving 30 m/s RV Precision for APOGEE in the Plate-Era" are made publicly available including data and code to reproduce all figures.</p>
APOGEE-TESS Verification
<p>This dataset contains stars from NASA's TESS mission and APOGEE to test TESS's calibration comparatively to the Kepler scale. Link to publication: </p> <p>Arxiv:</p> <p><a href="https://arxiv.org/abs/2307.13853">https://arxiv.org/abs/2307.13853</a></p> <p>RNAAS:</p> <p><a href="https://iopscience.iop.org/article/10.3847/2515-5172/ace7af">https://iopscience.iop.org/article/10.3847/2515-5172/ace7af</a></p>
APOGEE likely binaries with estimated companion masses
<p>This Zenodo has an assortment of data files related to <strong><a href="https://iopscience.iop.org/article/10.3847/2515-5172/ad5964" target="_blank" rel="noopener">Schochet, Tayar & Andrews (2024) "A Lack of Mass-Gap Compact Object Binaries in APOGEE"</a></strong> which sought to identify binary systems with a single stellar component that may be host to a "mass-gap" black hole/neutron star companion. These files utilize data from the Sloan Digital Sky Survey IV's (<a href="https://ui.adsabs.harvard.edu/abs/2017AJ....154...28B/abstract" target="_blank" rel="noopener">Blanton et al. 2017</a>) Apache Point Galactic Evolution Experiment (<a href="https://ui.adsabs.harvard.edu/abs/2017AJ....154...94M/abstract">Majewski et al. 2017</a>) Data Release 17 (<a href="https://ui.adsabs.harvard.edu/abs/2022ApJS..259...35A/abstract" target="_blank" rel="noopener">Abdurro'uf et al. 2022</a>), including stellar abundances from the ASPCAP pipeline (<a href="http://adsabs.harvard.edu/abs/2016AJ....151..144G" target="_blank" rel="noopener">Garcia Perez et al. 2016</a>) and with spectra reduced using the Doppler (<a href="http://adsabs.harvard.edu/abs/2015AJ....150..173N">Nidever et al. 2015</a>). Radius values used in the catalog come from Gaia + SED fitting (<a href="https://iopscience.iop.org/article/10.3847/1538-4365/acabc8" target="_blank" rel="noopener">Yu et al. 2023</a>). </p> <p>In this repository you will find:</p> <p><strong>Files</strong></p> <ul> <li>APOGEE_likely_binaries.csv: datafile contains basic information and IDs for the 4751 likely binary objects from our data reductions (2MASS ID, SNR, nvisits, vsini, vscatter, teff, log(g), M/H and errors for the final 3 stellar parameters).</li> <li>For systems with a radius value from <a href="https://iopscience.iop.org/article/10.3847/1538-4365/acabc8" target="_blank" rel="noopener">Yu et al. 2023</a> (4288/4751), we also provide: <ul> <li>apogee_objects_with_kiauhoku_masses.csv: this file contains masses and ages from the four grids of kiauhoku (<a href="https://ui.adsabs.harvard.edu/abs/2020ApJ...888...43C/abstract" target="_blank" rel="noopener">Claytor et al. 2020</a>) which include models from MIST (MESA Isochrones and Stellar Tracks, <a href="https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C/abstract" target="_blank" rel="noopener">Choi et al. 2016</a> & <a href="https://ui.adsabs.harvard.edu/abs/2010ascl.soft10083P/abstract" target="_blank" rel="noopener">Paxton et al. 2010</a>), YREC (Yale Rotating stellar Evolution Code, <a href="https://ui.adsabs.harvard.edu/abs/2020arXiv201207957T/abstract" target="_blank" rel="noopener">Tayar et al. 2022</a> & <a href="https://ui.adsabs.harvard.edu/abs/1989ApJ...338..424P/abstract" target="_blank" rel="noopener">Pinsonneault et al. 1989</a>) Dart/DSEP (Dartmouth Stellar Evolution Program, <a href="https://ui.adsabs.harvard.edu/abs/2008ApJS..178...89D/abstract" target="_blank" rel="noopener">Dotter et al. 2008</a>), and GARSTEC/Gars (Garching Stellar Evolution Code, <a href="https://ui.adsabs.harvard.edu/abs/2013MNRAS.429.3645S/abstract" target="_blank" rel="noopener">Serenelli et al. 2013</a> & <a href="https://ui.adsabs.harvard.edu/abs/2008Ap%26SS.316...99W/abstract" target="_blank" rel="noopener">Weiss & Schlattl 2008</a>). These are in the final columns of the csv file, and other columns include Gaia IDs, APOGEE starflag and ASPCAP flags, and RA/Dec along with APOGEE Telescope and Field information for each target.</li> <li>estimated_companions.csv: this file contains estimated minimum companion masses from the tidal synchronization method (CO_mass_rsync) and Joker method (CO_mass_joker) used in<strong> </strong>Schochet et al., and velocity semi-amplitude, eccentricity, and period values from the Joker (K_joker, e_joker, P_joker; <a href="https://ui.adsabs.harvard.edu/abs/2017ApJ...837...20P/abstract">Price-Whelan et al. 2017</a>).</li> </ul> </li> </ul> <p> </p> <p><strong>Programs</strong></p> <ul> <li>spectra_replotter.ipynb: This program replots spectra from the APOGEE servers when given a 2MASS ID, Field, and the telescope (APO/LCO) used for a specific observed object. It will then print out an image of that object's spectra with the apVisit/asVisit <a href="https://data.sdss.org/datamodel/files/APOGEE_REDUX/APRED_VERS/visit/TELESCOPE/FIELD/PLATE_ID/MJD5/apVisit.html#hdu4" target="_blank" rel="noopener">files</a> (pre-RV-shift reduction) plotted above the apStar/asStar <a href="https://data.sdss.org/datamodel/files/APOGEE_REDUX/APRED_VERS/stars/TELESCOPE/FIELD/apStar.html#hdu9" target="_blank" rel="noopener">files</a> (post-RV-shift reduction) so that radial velocity shifts can be quickly identified by eye</li> </ul> <p> </p> <p> </p> <p><em>Notes</em></p> <p>estimated_companions.csv and apogee_objects_with_kiauhoku_masses.csv contain Fiber Dispersion in their data frames, as a reference to the observed trend that vscatter tends to be much lower for objects with 0 fiber dispersion, while objects with fiber dispersion > 0 show larger vscatters, in case there is future focus on investigating this phenomena </p> <p> </p> <p>Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss4.org.</p> <p>SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, Center for Astrophysics | Harvard & Smithsonian (CfA), the Chilean Participation Group, the French Participation Group, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.</p>
Apogee, A HeartWare HVAD Destination Product Surveillance Registry (PSR) Platform
ClinicalTrials.gov study NCT03697980. IPD Sharing: NO. Countries: 1. Publications: 0.
Apogee International
ClinicalTrials.gov study NCT04065997. IPD Sharing: Not stated. Countries: 17. Publications: 0.
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