adsabs/AstroCLIMB huggingface dataset:
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Measurements flagged as outliers in APOKASC-3. The left panel shows data with ﹩{\nu }_{{\rm{\max }}}﹩ inconsistent with the spectroscopic prior. The right panels show measurements inconsistent with other pipelines in ﹩{\nu }_{{\rm{\max }}}﹩ (top right) and Δν (bottom right). Measurements consistent with the prior are not shown for visual clarity. The population of ﹩{\nu }_{{\rm{\max }}}﹩ measurements close to the unity line were rejected because their corresponding Δν measurements disagreed. The large majority of rejected measurements are strongly inconsistent with the prior.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Pipeline systematic offsets in ﹩{\nu }_{{\rm{\max }}}﹩ for RGB (left) and RC (right). We distinguish our seven core methods and show results for the Gold sample (top) and Silver sample (middle). Our ﹩{\nu }_{{\rm{\max }}}﹩-only methods are shown in the bottom panels. Different symbols and line styles demote different pipelines (see the legend). For ﹩{\nu }_{{\rm{\max }}}﹩ in the RGB Gold sample, fractional differences are at the ±0.004 level, rising to ±0.012 at low and high ﹩{\nu }_{{\rm{\max }}}﹩; a comparable ±0.009 range is seen for the RC. The Silver sample and the ﹩{\nu }_{{\rm{\max }}}﹩-only methods have larger scatter, especially in the low ﹩{\nu }_{{\rm{\max }}}﹩ domain.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Power spectral density of solar-like oscillators observed by Kepler from the main sequence (red) to evolved red giant branch stars (purple). The vertical dashed gray line indicates the Nyquist frequency for Kepler long-cadence observations. The arrow indicates the decrease in frequency and the increase in power density associated with stellar evolution up until the tip of the RGB.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Age distributions for different evolutionary states and chemical populations. The α-rich populations (right) show a strong age peak, while the α-poor ones are broader. The lower RGB (top) and RC (bottom) have similar high age cutoffs, but young stars are much more common in the RC. For the α-rich populations, the peak age and observed dispersion is overlaid for comparison (solid line); the predicted distribution is shown with a short dashed line. For the α-rich populations, the lines indicate the location of an edge in the age distribution (at 7.3 Gyr for the RGB and 6 Gyr for the RC) with the observed dispersions as derived in the right panels.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The α-rich populations in the mass–[Fe/H] (left) and age–[Fe/H] (right) planes for the RGB (top) and RC (bottom). The α-poor populations in age space are shown for comparison as faint gray points in the right panels; a clear division, corresponding to the difference between the thick and thin disks, is seen. The RGB masses are also shown in the lower-left panel, and the difference between them and the RC is clear evidence for mass loss.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The RGB (red, filled) and RC (blue, open) in the mass–radius plane for α-poor stars (left) and α-rich stars (right). Silver sample stars are shown as gray circles. The field turnoff in the RGB below the clump, mass loss in the RC, and a mixture of AGB and RGB stars above the clump are clearly seen.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The α-poor RC (top) and lower RGB (bottom) in the mass–[Fe/H] plane (left panels) and the age–[Fe/H] plane (right panels). The RC spans a wider range of masses and ages, while both populations have a sharp lower age boundary corresponding to the finite age of the α-poor population. More-massive and younger stars are concentrated around solar metallicity.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Pipeline systematic offsets in Δν for RGB (left) and RC (right). We show results for the Gold sample (top) and Silver sample (bottom). Different symbols and line styles demote different pipelines (see the legend). For Δν in the Gold RGB sample, fractional differences are at the ±0.004 level, rising to ±0.02 at low Δν; a ±0.01 range is seen in the primary RC, with a smaller ±0.005 range in the secondary RC. Note that the Silver RC sample is small, and not shown here.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Upper RGB stars in the α-rich population in the mass–[Fe/H] plane (left) and the age–[Fe/H] plane (right). Silver sample stars are dark gray symbols, and Gold sample ones are red symbols. A small number of points below 0.5 and above 3.5 M⊙ are not shown. The Silver sample includes a larger number of stars at lower metallicity, with higher scatter.
Paper: The Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) Active Galactic Nuclei Catalog: The Fourth Data Release
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Matt J. Jarvis, Daniel J. Farrow, Steven L. Finkelstein, Óscar A. Chávez Ortiz
Figure caption: An example of an AGN (agnid = 407) detected with extended diffuse ionized gas. (a) The HSC r-band 30″ × 30″ image with the red Lyα λ1215 narrowband 2σ density contour. (b) The HETDEX Lyα λ1215 narrowband image. (c) The radial profile of the Lyα λ1215 flux density map. Blue data points are surface brightness variations. The red curve is a (PSF + exponential) fit to the blue points, giving a rext = 47.6 kpc. The green dashed curve gives the PSF model using the image quality of this observation. The gray dashed horizontal line marks the standard deviation in the continuum subtracted background in the line flux map. (d) The spectrum extracted at the labeled coordinate in the observed frame. The yellow shaded region highlights the  ±21 Å wavelength range making the Lyα λ1215 density map. We refer the readers to E. Mentuch Cooper et al. (2025, in preparation) for more detailed analyses of the extended diffuse ionized gas around LAEs.
Paper: The Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) Active Galactic Nuclei Catalog: The Fourth Data Release
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Matt J. Jarvis, Daniel J. Farrow, Steven L. Finkelstein, Óscar A. Chávez Ortiz
Figure caption: The completeness and contamination of the HETDEX HDR4 AGN sample in each HETDEX g-band magnitude bin. Completeness is estimated from the crossmatched sample between the SDSS DR16Q sample and all HETDEX HDR4 fibers. The black squares connected with a dashed line show the completeness of the parent sample of this work (Sections 3.1 and 3.2). The blue circles connected by a solid line show the completeness of the AGN identified either by the LP method (Section 3.3.1) or by the sBL method (Section 3.3.2). The magenta triangles and the cyan stars show the completeness of the LP method (Section 3.3.1) and the sBL method (Section 3.3.2), respectively. The gray diamonds connected by a dotted line present the contamination rate from the unconfirmed redshifts (zflag = 0, column 6 in Table 2). The orange crosses connected by a dashed–dotted line show the contamination rate from the unconfirmed AGN (agn_flag = 0, column 7 in Table 2).
Paper: The Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) Active Galactic Nuclei Catalog: The Fourth Data Release
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Matt J. Jarvis, Daniel J. Farrow, Steven L. Finkelstein, Óscar A. Chávez Ortiz
Figure caption: The FoF experiments with linking lengths of δr =  3﹩\mathop{.}\limits^{\unicode{x02033}}﹩0, 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩5, 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩0, 4﹩\mathop{.}\limits^{\unicode{x02033}}﹩5, 5﹩\mathop{.}\limits^{\unicode{x02033}}﹩0, 5﹩\mathop{.}\limits^{\unicode{x02033}}﹩5, 6﹩\mathop{.}\limits^{\unicode{x02033}}﹩0 for the 63,827 AGN detections. The 2D FoF tests are the red crosses. The 3D FoF tests (δz = 0.1) are the blue data points.
Paper: The Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX) Active Galactic Nuclei Catalog: The Fourth Data Release
Authors: Chenxu Liu, Karl Gebhardt, Erin Mentuch Cooper, Dustin Davis, Donald P. Schneider, Matt J. Jarvis, Daniel J. Farrow, Steven L. Finkelstein, Óscar A. Chávez Ortiz
Figure caption: Left: distributions of the separations between the “best” detections (detectid_best) to their emission-line flux-weighted FoF centers. Right: distributions of the separations between all AGN detections to their emission-line flux-weighted FoF centers.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: Fractional change in disk maximality, ﹩{{ \mathcal F }}_{{\rm{disk}}}﹩, as a function of inverse Tully–Fisher inclination (iTF, top) and K-band magnitude (MK, middle) due to the switch from the M. A. W. Verheijen (2001) Vflat relation in Equation (8) to the A. A. Ponomareva et al. (2017) ﹩{V}_{{\rm{\max }}}﹩ relation in Equation (9). Points in the top and middle panels are colored according to there MK and vrot, respectively. Points encircled in black are the 28 galaxies in the DMS VII. The bottom panel applies these ﹩\delta \mathrm{ln}{{ \mathcal F }}_{{\rm{disk}}}﹩ corrections to the disk-maximality measurements from DMS VII (solid gray points) to obtain updated measurements (open circles); the results are plotted as a function of the disk central K-band surface brightness, μ0,K, from DMS VII. The best-fit trend (solid gray line) and scatter (dotted gray lines) are reproduced from DMS VII as a reference; i.e., the trend has not been refit to the updated data.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: Left: histogram of Hα velocity dispersions for single and double-component fits. Right: summary of trends of Hα velocity dispersion with line surface brightness for narrow (blue) and broad (orange/red) components for lines exhibiting single- or double-Gaussian profiles. Solid and short-dashed colored lines represent the median and median absolute deviation (scaled to the standard deviation assuming a Gaussian distribution) in bins of line surface brightness. The horizontal long-dashed line represents the instrumental resolution of the SparsePak data. Comparison is made to earlier DensePak measurements (open circles; see the text) at higher instrumental spectral resolution denoted by a horizontal dotted line.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: K-band Tully–Fisher relation for this relatively face-on sample of galaxies. The dashed line is the K-band TF relation from M. A. W. Verheijen (2001), while the solid line is the K-band TF relation from A. A. Ponomareva et al. (2017). The projected rotation speed uses the kinematic observed rotation speed corrected for redshift and divided by the sine of the kinematic inclination. The absolute magnitude uses the distance determined from Cosmic-Flows 3 project (E. Kourkchi et al. 2020). The size of the spots is proportional to the inclination error divided by the inclination (typically galaxies observed at higher inclinations are smaller in this plot). The color is set by the asymmetry of the galaxy. Low-asymmetry galaxies are blue, while high-asymmetry galaxies are yellow. Left: 77 galaxies with kinematic inclinations inconsistent with zero and Aϕ < 0.1. Galaxies with two-armed spiral structure that visibly affects isovelocity contours are circled in red. Right: excluding 12 two-armed spiral structures that affect isovelocity contours yields a much tighter Tully–Fisher relation that is consistent with the A. A. Ponomareva et al. (2017) relation.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: A comparison of three kinematic asymmetry parameters, ARC, Aϕ, and ﹩{\sigma }_{{\rm{mod}}}/{v}_{{\rm{rot}}}﹩, shows that they are tightly correlated. Galaxies chosen for the Phase-B sample are marked with solid squares. As expected, these Phase-B galaxies exhibit a smaller range in kinematic asymmetry than the sample overall, since one of the selection criteria for Phase-B was a regular velocity field.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: Inverse Tully–Fisher inclination versus kinematic inclinations (determined from modeling the velocity field) for 65 galaxies. This plot excludes galaxies with kinematic inclinations consistent with zero, Aϕ > 0.1, and strong two-armed spiral structure. The size of the spots is proportional to Aϕ, and the color is set by the absolute K-band magnitude (MK). Galaxies that were part of the Phase-B sample have red error bars.
Paper: The DiskMass Survey. XI. Disk Geometries and Star Formation Surface Densities from Ionized Gas Kinematics and Line Intensities for the Full Hα Sample
Authors: Robert A. Swaters, David R. Andersen, Matthew A. Bershady, Thomas P. K. Martinsson, Paul Scholz, Marc A.W. Verheijen, Kyle B. Westfall
Figure caption: Absolute magnitude, MK, versus kinematic asymmetry, Aϕ. Solid, filled points are galaxies from the Phase-B sample.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: Stellar properties at fixed metallicity and variable mass. APOKASC-3 stars with −0.05 < [Fe/H] < +​​​​​​0.05, shown in the asteroseismic ﹩{\rm{log}}g﹩–spectroscopic Teff plane. Filled symbols are Gold sample RGB stars, open symbols are Gold sample RC stars, and crosses are Silver sample stars. Symbol types and colors reflect mass. The upper panel shows stars between 0.85 and 1.55 M⊙, while the lower panel shows stars between 1.55 and 2.95 M⊙. Higher-mass stars (upper panel) and lower-mass ones (lower panel) are shown in gray.
Paper: APOKASC-3: The Third Joint Spectroscopic and Asteroseismic Catalog for Evolved Stars in the Kepler Fields
Authors: Marc H. Pinsonneault, Joel C. Zinn, Jamie Tayar, Aldo Serenelli, Rafael A. García, Savita Mathur, Mathieu Vrard, Yvonne P. Elsworth, Benoit Mosser, Dennis Stello, Keaton J. Bell, Lisa Bugnet, Enrico Corsaro, Patrick Gaulme, Saskia Hekker, Marc Hon, Daniel Huber, Thomas Kallinger, Kaili Cao, Jennifer A. Johnson, Bastien Liagre, Rachel A. Patton, Ângela R. G. Santos, Sarbani Basu, Paul G. Beck, Timothy C. Beers, William J. Chaplin, Katia Cunha, Peter M. Frinchaboy, Léo Girardi, Diego Godoy-Rivera, Jon A. Holtzman, Henrik Jönsson, Szabolcs Mészáros, Claudia Reyes, Hans-Walter Rix, Matthew Shetrone, Verne V. Smith, Taylor Spoo, Keivan G. Stassun, Ji Wang
Figure caption: The distribution of ﹩v\sin i﹩ for giants without a seismic detection (black), with partial data (red), and with full seismic data (green) are shown in bins of 5 km s−1 in ﹩v\sin i﹩ in the top panel. Stars of different type are slightly offset at the same bin location for clarity. In the middle panel, we present spectroscopic log g vs. Teff taken from APOGEE DR17 for the rotationally enhanced giants. The RC stars are plotted as blue circles and first-ascent giants are plotted as red ones. In the bottom panel, we show mass as a function of [Fe/H] for the sample with full asteroseismic data.