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42 results for “Red Giants”
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>
Reflectance and emission spectra of Earth-like planets orbiting red giant stars
<p>Spectra of red giant stellar hosts and reflectance/emission planetary spectra as described in Kozakis & Kaltenegger (2020). File names and content are explained in 0readme.txt. Please email theakozakis@gmail.com with any questions.</p> <p> </p>
Figure 2. Neodendrina carnelia igen. et isp. n in Large dendrinids meet giant clam: the bioerosion trace fossil Neodendrina carnelia igen. et isp. n. in a Tridacna shell from Pleistocene-Holocene coral reef deposits, Red Sea, Egypt
Figure 2. Neodendrina carnelia igen. et isp. n. on the inner side of a Tridacna maxima bivalve shell from the Pleistocene–Holocene coral reef deposits in the Marsa Alam area, Red Sea, Egypt. (a) Inner side of valve (left; prior to sectioning) with hundreds of N. carnelia specimens, and outer surface (right) intensely bioeroded by the sponge boring Entobia isp. (b) Section of the valve (MB.W 5640) with the holotype (centre) and the paratypes (all other specimens) in various ichnogenetic stages. (c) Close-up of the holotype trace. (d–e) Respective micro-CT scan of the holotype in plan and angular views as seen from inside the substrate.
Figure 1 in Large dendrinids meet giant clam: the bioerosion trace fossil Neodendrina carnelia igen. et isp. n. in a Tridacna shell from Pleistocene-Holocene coral reef deposits, Red Sea, Egypt
Figure 1. The Pleistocene raised coral reef limestones exposed at the type locality of Neodendrina carnelia igen. et isp. n. just south of the Carnelia Beach Resort, located between El Quseir and Marsa Alam, exhibiting scleractinian corals as primary reef builders (a) and giant clams Tridacna spp. weathering from the carbonate–siliciclastic rocks (b) that mix with Holocene and modern Tridacna valves, forming a highly time-averaged assemblage (c).
Figure 4. Neodendrina carnelia igen. et isp. n in Large dendrinids meet giant clam: the bioerosion trace fossil Neodendrina carnelia igen. et isp. n. in a Tridacna shell from Pleistocene-Holocene coral reef deposits, Red Sea, Egypt
Figure 4. Neodendrina carnelia igen. et isp. n. on the outer surface of a large recent Tridacna squamosa valve from Nosy-BØ, northern Madagascar (ZMB/Mol 102671). (a) Shell surface with various encrusters as well as bioerosion traces. (b) Close-up of a cluster of N. carnelia. (c) A large specimen with distinct pitted arrays developed in most of the branches.
Figure 3 in Large dendrinids meet giant clam: the bioerosion trace fossil Neodendrina carnelia igen. et isp. n. in a Tridacna shell from Pleistocene-Holocene coral reef deposits, Red Sea, Egypt
Figure 3. SEM images (BSE detector) of Neodendrina carnelia igen. et isp. n. of the inner side of a Tridacna maxima bivalve shell from the Pleistocene–Holocene coral reef deposits in the Marsa Alam area, Red Sea, Egypt. (a–c) Overview and close-ups of the holotype. (d–e) Overview and close-up of an early ichnogenetic stage. (f–g) Overview and close-up of a specimen with authigenic gypsum crystals, calcite spar, and clay minerals within the boring as well as on the host's shell surface. (h) Different morphologies possibly developed in the trace, comprising deep open canals (1), isolated deep pits (2), shallow open canals (3), pits in shallow canals (4) and discontinuities (5). (i) Cross section of a trace showing deep (1) and shallow (2) open canals. (j–k) Overview and detail of an epoxy resin cast of a specimen, illustrating the smooth surface texture and the high degree of microbioerosion in the surrounding (partly mechanically removed to gain a view of the dendrinid).
Datasets for Ash et al. (2024): Testing the Breakdown of the Asteroseismic Scaling Relations in Luminous Red Giants
<p>Datasets used for the high-alpha sequence and cluster analysis in Ash et al. (2024) which explores the efficacy of the asteroseismic scaling relations with a focus on the luminous giant regime. These datasets are a subset of the APOKASC3 dataset, which is publiclly available (Pinsonneault et al. (2024)). The data selection methods to genrate these data subsets are available in Ash et al. (2024). The high-alpha sequence and open cluster datasets are used to compare seismic masses computed with various methods to seismic-independent masses. <a href="https://zenodo.org/api/records/14008022/draft/files/NGC6791_APO_giants+rc_GaiaDR3_membership.txt/content" target="_blank" rel="noopener noreferrer">NGC6791_APO_giants+rc_GaiaDR3_membership.txt</a> and <a href="https://zenodo.org/api/records/14008022/draft/files/NGC6819_APO_giants+rc_GaiaDR3_membership.txt/content" target="_blank" rel="noopener noreferrer">NGC6819_APO_giants+rc_GaiaDR3_membership.txt</a> contains asteroseismic data for red clump and red giant branch stars in the open clusters NGC6791 and NGC6819. The <a href="https://zenodo.org/api/records/14008022/draft/files/high_alp_sequence.txt/content" target="_blank" rel="noopener noreferrer">high_alp_sequence.txt</a> file contains asteroseismic data, including the several methods to compute seismic masses, for Milky Way high-alpha sequence stars. </p> <p> </p> <p>APOKASC 3 paper may be found at: https://arxiv.org/abs/2410.00102</p> <p> </p> <p> </p> <p> </p>
Age-resolved chemistry of red giants in the solar neighbourhood
<p>In our associated paper we find age-abundance trends for individual elements using a sample of solar-neighborhood stars observed with the SDSS-APOGEE instrument. Here we publish the likelihood functions from a Bayesian isochrone matching to determine the most probable age.</p>
Data for: Tip of the Red Giant Branch Distances with JWST. II. I−band Measurements in a Sample of Hosts of 10 SN Ia Match HST Cepheids
<p>Data for: "Tip of the Red Giant Branch Distances with JWST. II. I−band Measurements in a Sample of Hosts of 10 SN Ia Match HST Cepheids". The photometry provided is after DOLPHOT quality cuts, foreground extinction corrections, and spatial cuts.</p>
Figure 3 in Morphometric structure and allometry profiles of the giant red shrimp Aristaeomorpha foliacea (Risso, 1827) in the eastern Mediterranean
Figure 3. Relationship between carapace length and other measurements (mm) (logarithmic plots) of females of Aristaeomorpha foliacea (Risso, 1827) (data pooled for all the sampling periods).
Figure 2 in Morphometric structure and allometry profiles of the giant red shrimp Aristaeomorpha foliacea (Risso, 1827) in the eastern Mediterranean
Figure 2. Morphometric measurements taken on Aristaeomorpha foliacea (Risso, 1827). CL, carapace length; T, telson; U, uropodal exopodite; S, scaphocerite; P, third pereiopod; R, rostrum; ABD, abdomen.
Figure 1 in Morphometric structure and allometry profiles of the giant red shrimp Aristaeomorpha foliacea (Risso, 1827) in the eastern Mediterranean
Figure 1. Map of the sampling area and the depth range of the sampling stations of Aristaeomorpha foliacea (Risso, 1827) in the Greek Ionian Sea.
Figure 4 in Morphometric structure and allometry profiles of the giant red shrimp Aristaeomorpha foliacea (Risso, 1827) in the eastern Mediterranean
Figure 4. Relationship between carapace length and other measurements (mm) (logarithmic plots) of males of Aristaeomorpha foliacea (Risso, 1827) (data pooled for all the sampling periods).
MESA histories for "Characterizing Observed Extra Mixing Trends in Red Giants using the Reduced Density Ratio from Thermohaline Models"
<p>This repository provides MESA history files for each of the stellar models in the publication "Characterizing Observed Extra Mixing Trends in Red Giants using the Reduced Density Ratio from Thermohaline Models". The MESA version used was stable release version 21.12.21. Runs are organized into tarballs according to the thermohaline mixing prescription used:</p> <ul> <li>BGS13 = Brown, Garaud, Stellmach 2013</li> <li>Kipp1e-1 = Kippenhahn with alpha_th = 0.1</li> <li>Kipp2 = Kippenhahn with alpha_th = 2</li> <li>Kipp7e2 = Kippenhahn with alpha_th = 700</li> </ul> <p>and are additionally grouped according to the stellar mass (M = 0.9, 1.1, 1.3, 1.5, 1.7 in units of Msol). Within each tarball is a number of run directories which contain a LOGS/history.data file from the MESA run. The subdirectories in the tarball contain runs at various metallicities; conversion between Z (MESA input) and [Fe/H] (paper reported value) are found in Table 2 of the manuscript.<br> <br> Inlists and information for recreating these MESA simulations can be found online at the paper's github repository: <a href="https://github.com/afraser3/Empirical-Magnetic-Thermohaline">https://github.com/afraser3/Empirical-Magnetic-Thermohaline</a> (a copy of the code from this Github repository is located in this Zenodo repository in: Empirical-Magnetic-Thermohaline-main.zip)</p>
Machine Learning the Tip of the Red Giant Branch
<p># Reproduction package for the Paper "Machine Learning the Tip of the Red Giant Branch"<br> ## Authors<br> Mitchell T. Dennis (mtde226@hawaii.edu)<br> Jeremy Sakstein (sakstein@hawaii.edu)<br> ## Software<br> MESA version 15140 (http://mesa.sourceforge.net/) <br> MESASDK version 20210401 (http://www.astro.wisc.edu/~townsend/static.php?ref=mesasdk) <br> GFORTRAN GCC version 9.2.0<br> ## Citation Policy<br> If you use any part of this reproduction package for independent work, we recommend you cite the following papers:</p> <p>* This paper<br> * Astrophys. J. Suppl. 192, 3 (2011)<br> * Astrophys. J. Suppl. 208, 4 (2013)<br> * Astrophys. J. Suppl. 234, 34 (2018)<br> * Astrophys. J. Suppl. 243, 10 (2019)</p> <p> </p> <p>For more information, see the Readme.md</p>
Tip of the Red Giant Branch Bounds on the Axion-Electron Coupling Revisited
<p># Reproduction package for the Paper "Tip of the Red Giant Branch Bounds on the Axion-Electron Coupling Revisited"<br> ## Authors<br> Mitchell T. Dennis (mtde226@hawaii.edu)<br> Jeremy Sakstein (sakstein@hawaii.edu)<br> ## Software<br> MESA version 12778 (http://mesa.sourceforge.net/) <br> MESASDK version 20200325 (http://www.astro.wisc.edu/~townsend/static.php?ref=mesasdk) <br> GFORTRAN GCC version 9.2.0<br> Python 3.8.10<br> TensorFlow 2.4.1<br> ## Citation Policy<br> If you use any part of this reproduction package for independent work, we recommend you cite:<br> * This paper<br> If you use any of the MESA outputs found in the LOGS folder, we recommend you cite the MESA papers<br> * Astrophys. J. Suppl. 192, 3 (2011)<br> * Astrophys. J. Suppl. 208, 4 (2013)<br> * Astrophys. J. Suppl. 234, 34 (2018)<br> * Astrophys. J. Suppl. 243, 10 (2019)</p> <p> </p> <p>For more information, see the Readme.md</p>
Tip of the Red Giant Branch Bounds on the Neutrino Magnetic Dipole Moment Revisited
<p>Reproduction Package for the Paper "Tip of the Red Giant Branch Bounds on the Neutrino Magnetic Dipole Moment Revisited".</p> <p><strong>File Organization</strong></p> <ul> <li>MESA: MESA modifications to include losses due to the neutrino magnetic dipole moment, scripts to run the grid of models, and post processing pipeline scripts including the Worthey \& Lee bolometric correction code.</li> <li>ML_models: Machine learning code to train and use the models as well as the models themselves.</li> <li>analysis: Plotting code to create figures for papers and presentations.</li> <li>makeGrids: Scripts to create the different input grid files to run MESA on.</li> <li>mcmc: Scripts and plots for the MCMC analysis.</li> <li>mesa_data: All MESA models generated in this project.</li> <li>environment.yml: Conda environment for analysis and the mcmc. </li> </ul> <p>More details can be found in the README files within each directory.</p> <p><strong>Citation Policy</strong><br> If you use any part of this reproduction package for independent work, we recommend you cite the following papers:</p> <ul> <li>This paper</li> <li>https://arxiv.org/abs/2303.12069</li> <li>https://arxiv.org/abs/2305.03113</li> <li>Astrophys. J. Suppl. 192, 3 (2011)</li> <li>Astrophys. J. Suppl. 208, 4 (2013)</li> <li>Astrophys. J. Suppl. 234, 34 (2018)</li> <li>Astrophys. J. Suppl. 243, 10 (2019)</li> </ul> <p><strong>Software</strong></p> <p>Python version 3.8, NumPy version 1.22.3, Pandas version 1.4.3, Matplotlib version 3.5.1, Seaborn version 0.11.2, Tensorflow version 2.4.1, corner version 2.2.1, emcee version 3.1.2, MESA version 12778, MESASDK version x86_64-linux-20.3.2.</p>
Red_Giants Catalog
<p>This dataset is provided by a red giant search method based on convolutional neural networks. This data set is located in the sub-area of the SMSS survey project. After data cleaning and search through the CBAMResNets model, and comparison with models such as CVGG16 and TPC, a relatively complete and reliable red giant star catalog-provided area for this sub-area was obtained.</p>
Stellar models for "Realistic Uncertainties for Fundamental Properties of Asteroseismic Red Giants and the Interplay Between Mixing Length, Metallicity and Numax" by Li, Yaguang et al. (2024)
<p>This dataset includes a grid of stellar models from Li, Yaguang et al. (2024), titled "Realistic Uncertainties for Fundamental Properties of Asteroseismic Red Giants and the Interplay Between Mixing Length, Metallicity and Numax".</p> <p>The stellar models are first-ascent red giant branch (RGB) models, sampled using a Sobol sequence within the following six-dimensional initial parameter space: mass (0.7, 2.3) solar mass, Y_init (0.22, 0.37), [M/H] (-0.1.0, 0.60) dex, α_MLT (1.3, 2.7), fov_core (0, 0.02), fov_shell (0, 0.008). The evolutionary tracks are computed up to the point on the RGB where the p-mode large separation (Δν) equals 2 μHz. Approximately 32,768 unique evolutionary tracks are presented, divided into 33 individual chunks.</p> <p>To load the models into a Python Pandas dataframe, use the following command: "import pandas as pd; pd.read_parquet(filepath)". Each model (dataframe row) is provided with global parameters (Teff, radius, luminosity, mass, age, ...) and pure p modes with l=0-2 (frequency, mode inertia, angular degree, ...).</p> <p>For detailed descriptions of the stellar models, please refer to the original paper and the github repository.</p>
Asymptotic analysis of dipolar mixed modes of oscillations in red giant stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2016PASJ...68..109T">Asymptotic analysis of dipolar mixed modes of oscillations in red giant stars</a></p>
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