adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Cross-correlation templates for H2O covering the wavelength range of ESPRESSO and ANDES for K2-139 b, K2-329 b, TOI-3362 b, WASP-130 b, WASP-106 b, and TOI-677 b. The cross-correlation templates assume the parameters indicated in the panels and were generated using FastChem Cond for the abundance profiles and petitRADTRANS for the computation. Apart from H2O, the template includes continuum absorption by He and H2.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Radial velocities of the planet (blue, solid), star (orange, solid), RM effect (green, dashed) and telluric contamination (orange, dotted) for K2-139 b, K2-329 b, TOI-3362 b, WASP-130 b, WASP-106 b, and TOI-677 b in the rest frame of the system. The dashed black lines indicate the transit contact times.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Same as Figure 8 but for TOI-677 b.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Same as Figure 6 but for TOI-3362 b. We note that the peak to the right, around 40 km s−1 is likely caused by a combination of telluric and stellar residuals.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Same as Figure 7 but for the simulated observations with ANDES of TOI-3362 b. Note the different scales for the different species.
Paper: Two Young Eclipsing Binaries in Orion with Temperatures and Radii Affected by Spots and Third Bodies
Authors: Marina Kounkel, Keivan G. Stassun
Figure caption: Model fit of the observational data toward 2M05−06. Left panel shows the fit of the available light curves (in T, G, GP, and RP bandpasses) as well as the residuals (normalized by the typical uncertainties in the fluxes to meaningfully be displayed on the same plot). The blue line shows a flat continuum to demonstrate the significants of spots onto the light curve. The top-right panel shows the fit of the radial velocities. The middle-right panel shows the model SED (with the SED of the individual stars being shown in yellow, the combined SED in read, the black lines showing the measurements with the uncertainties and the bandpass width, and blue dots showing interpolated model fluxes onto these bandpasses). In this system, the last three fluxes, corresponding to W1, W2, and W3 passbands, appear to show IR excess. We also note that the two stars have extremely similar fluxes integrated across the entire surface, thus the two yellow lines are plotted on top of one another. Finally, the bottom-right panel shows a mesh grid depicting the surface temperature, size, and the separation of the two stars.
Paper: Two Young Eclipsing Binaries in Orion with Temperatures and Radii Affected by Spots and Third Bodies
Authors: Marina Kounkel, Keivan G. Stassun
Figure caption: Top: Effective temperature (dashed line) and the temperature of the photosphere (solid line) for 2M05−00 (red) and 2M05−06 (blue) vs. their radii. The transformation of this parameter space onto mass and age using isochrones is also shown, alongside the masses of the stars in these two systems as a function of radius. Middle: mass vs. radius relative to the isochrones, showing the typical uncertainty in the measurements. Bottom: the difference between the observed masses (from the orbital fitting) and the interpolated model mass from temperatures, divided by the observed mass. Error bars include the uncertainty in the temperature. Left: nonmagnetic MIST isochrones (Choi et al. 2016). Right: magnetic SPOT isochrones (Somers et al. 2020), with 34% spot filling fraction.
Paper: Two Young Eclipsing Binaries in Orion with Temperatures and Radii Affected by Spots and Third Bodies
Authors: Marina Kounkel, Keivan G. Stassun
Figure caption: Same as Figure 2, but for 2M05−00. In the middle-right panel, SED marked with 1 corresponds to the primary in Table 1, and 2 to the secondary. The green line is the fitted SED of the third star in the system that is needed in order to match the observed flux while keeping the system fixed at the reported distance from Gaia.
Paper: Two Young Eclipsing Binaries in Orion with Temperatures and Radii Affected by Spots and Third Bodies
Authors: Marina Kounkel, Keivan G. Stassun
Figure caption: TESS light curves for 2M05−06 (top) and 2M05−00 (bottom)
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: LHS 1610 b in context with other brown dwarfs orbiting M stars (BD-M systems). The colored points are confirmed BD-M star systems drawn from the NASA Exoplanet Archive, the exoplanet.eu catalog, and the literature. Not all systems have measurements for the plot parameters, so the points on each plot are individually labeled. To highlight the yield that Gaia will help enable, the fainter points show candidate BD-M systems from Gaia two-body solutions within 25 pc. Some errors are smaller than the marker size. Top (A): brown dwarf masses (better than 3σ) as a function of distance from Earth colored by the host-star mass. LHS 1610 b is the third most nearby BD-M system with a precise mass measurement. Bottom (B): same as above, but showing eccentricity as a function of orbital period in days. LHS 1610 b is one of the shortest-period BDs orbiting an M dwarf, and is the most eccentric in our sample besides GJ 229 B. The dashed line shows the expected eccentricity at a given period for a circularization period of 10 days. Similar to panel A, the fainter points show candidate BD-M systems from Gaia two-body solutions within 25 pc. The colored data points are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: M-dwarf flare rates (A): log flare rate of flares with energies above the 3.16 × 1031 erg energy threshold discussed in Medina et al. (2022) as a function of stellar rotation period. Points are color-coded by distance to Earth. LHS 1610 is highlighted with the star. Systems with substellar companions are highlighted with black labels. Systems with published radio detections are highlighted in red. LHS 1610 joins a group of systems with high flare rates and long rotation periods. LHS 1610 flare orbital locations (B): orbit visualization of the LHS 1610 b (outer ellipse) and its host star (inner ellipse) around the common center of mass using the joint Gaia-RV parameters from Table 2. The orbit is inclined ∼114° and the orbital direction is clockwise. The red vector denotes the orbit normal, and the periastron location is highlighted with the dotted line between the white squares. Locations of flares are highlighted twice per flare with the colored points, with a star/circle marker at the corresponding star/companion location. We do not see statistically significant evidence for a phase dependence of flare locations. The shaded regions define the intersection of the plane of the orbit with the plane of the sky along the line of nodes. The data shown in panel (B) are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: Visualization of joint Gaia-RV sampling with inflation. A: RVs using TRES from Winters et al. (2018), with our best-fit model laid over the points. B: our new RVs using HPF, with the best-fit model in red. This shows the significant increase in the observing baseline provided by the additional HPF RVs, which span more than 500 days. C and D: phase-folded RVs and residuals using the parameters produced by the joint sampling. Both sets of RVs are in agreement with the best-fit model. Errors in panels A, B, and C are smaller than the marker size. The RVs are available as the data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: Comparison of Z-score values for the two joint-sampling methodologies we considered. The joint-sampling Z-scores where we fix σ scale = 1 are shown with red circles. Same as before but where we let σ scale be a fit parameter in the MCMC sampling, shown with blue squares. The red dashed lines show Z-score values of ±1. The former sampling highlights inconsistencies (absolute Z-score values larger than 1) for the parameters e, P, and B. From the latter sampling, we see that through letting σ scale inflate the Gaia covariance matrix, this correspondingly increases the uncertainties in the derived parameters (see Table 2) and thus results in Z-scores that are in better agreement (absolute Z-scores <1).
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: Estimated powers from both sub-Alfvénic interactions between LHS 1610 b and its host star (red and orange curves), and auroral emission from the brown dwarf’s magnetosphere due to the incident stellar wind (purple curves). Each solid line and shaded region shows the median and the 1σ region, respectively. The powers are shown as a function of orbital phase, which are modulated due to the eccentricity of the orbit. For the sub-Alfvénic powers, we show the cases where the brown dwarf is both magnetized (red curves) and unmagnetized (orange curves). The powers are computed assuming an age of 7 Gyr for the brown dwarf. The differences in the curves at the ages of 2 and 12 Gyr are small, as the radius of the brown dwarf does not change significantly, and the size of its magnetosphere varies weakly with the magnetic field strength (see Equation (27)). In all cases, a fraction of the energy (10−4–10−2) is expected to be released at radio wavelengths, resulting in flux estimates that are within reach of sensitive radio telescopes such as LOFAR and the VLA. Note that the sub-Alfvénic interaction scenario is only possible provided the host star has a sufficiently low mass-loss rate and strong surface magnetic field (see Figure 6).
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: Flares in TESS photometry. Panels A, B, and C show individual sector light curves for TESS Sectors 42, 43, and 44, respectively. Points are colored by flare probability assigned by stella; red show a probability >60%, and gray points a probability <60%. Flares that passed our cuts are highlighted by the vertical gray bars. Panel D contains the combination of all sectors phase-folded on the period centered on the time of periastron. Flares are again highlighted by vertical gray bars. We do not see statistically significant evidence for phase-dependent flaring.
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: The fraction of the orbit that LHS 1610 b orbits sub-Alfvénically as a function of the stellar wind mass-loss rate and unsigned average large-scale surface magnetic field of the host star. The gray shaded region shows where sub-Alfvénic interactions are not possible. Provided the mass-loss rate is sufficiently low and the surface magnetic field is sufficiently strong, the brown dwarf can magnetically interact with the host star, enhancing the star’s activity.
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: The fraction of the wind velocity (top) and magnetic field vectors (middle) that points in the radial direction, and the fraction of open field lines (bottom) as a function of distance for the wind of the LHS 1610 analog Proxima Centauri. The shaded regions in the top two panels show the 1σ  interval, highlighting the variations in the wind inside the closed field. At distances greater than around 10 stellar radii, the wind flow direction and magnetic field becomes aligned with the radial direction. Note that this happens at a distance significantly smaller than the average size of the Alfvén radius, inside of which sub-Alfvénic interactions can occur between the star and companion, enhancing the activity of the star. Therefore, most sub-Alfvénic orbits experience a radial magnetic field.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: The difference between the [Fe/H] metallicity determined from the 8498 Å Ca ii line and the [Fe/H] metallicity determined from different photometric G-band light-curve−metallicity relationships in the literature. The dispersion for the RRLs with RVS spectra with S/N > 35 and S/N < 35 is indicated in each panel. Our CaT metallicities have dispersions comparable to the precision of the photometric [Fe/H] metallicities for RRLs with S/N > 35. The bottom left panel shows the photometric metallicity from this study; the calibration is described in the Appendix.
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: The radial wind velocity profile estimated for LHS 1610. The red shaded region shows the 1σ uncertainty. The range of orbital separations between the brown dwarf and host star is shown by the gray shaded region. During its orbit, the brown dwarf is subjected to stellar wind velocities of ∼800 to 900 km s−1.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: The calibrated linear relation (red line) between spectroscopic [Fe/H] and EW of the Ca ii line at 8498 Å. The color-coding illustrates the S/N of the individual measurements. The individual measurements with all their available measurements are shown, so some individual RRLs are represented here repeatedly. The green line represents the calibration relation from Wallerstein et al. (2012).
Paper: Astrometry and Precise Radial Velocities Yield a Complete Orbital Solution for the Nearby Eccentric Brown Dwarf LHS 1610 b
Authors: Evan Fitzmaurice, Guđmundur Stefánsson, Robert D. Kavanagh, Suvrath Mahadevan, Caleb I. Cañas, Joshua N. Winn, Paul Robertson, Joe P. Ninan, Simon Albrecht, J. R. Callingham, William D. Cochran, Megan Delamer, Eric B. Ford, Shubham Kanodia, Andrea S. J. Lin, Marcus L. Marcussen, Benjamin J. S. Pope, Lawrence W. Ramsey, Arpita Roy, Harish Vedantham, Jason T. Wright
Figure caption: Corner plot showing the posterior distributions of the joint Gaia and RV sampling with the scaled Gaia covariance matrix (σ scale > 1) from Section 4.3. Median values are highlighted in Table 2.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: Left: a typical BRAVA-RR spectrum used for [Fe/H]CaT abundance determination from the measured EW of the CaT line at 8498 Å. Right: the total energy (E tot) vs. the z component of the angular momentum (L  z ) for the Galactic bulge RRLs studied here. Stars belonging to the same physical structure cluster together in integrals of motion such as E tot and angular momentum, and the major substructure of GE/S is labeled. The E tot and angular momentum regime where Aurora is seen is also where the potential Heracles/Kraken substructure is thought to reside.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: Left: [Fe/H]phot metallicities of Galactic bulge stars as compared to our [Fe/H]CaT metallicities, where ﹩\lt {[\mathrm{Fe}/{\rm{H}}]}_{\mathrm{CaT},{\phi }_{\mathrm{all}}}\gt ﹩ is the metallicity from individual [Fe/H]CaT measurements averaged over all phases, and ﹩{[\mathrm{Fe}/{\rm{H}}]}_{\mathrm{CaT},{\phi }_{\mathrm{optimal}}}﹩ is where only [Fe/H]CaT at the optimal phases of ϕ = 0.4–0.5 and ϕ = 0.6–0.7 are used. Right: the [Fe/H] metallicity distribution of the RRLs in NGC 6441 from [Fe/H]CaT, from [Fe/H]phot, and from Clementini et al. (2005). Unlike [Fe/H]photo, [Fe/H]CaT is also able to reproduce the metallicities of the peculiar, long-period metal-rich RRLs seen in the massive GCs NGC 6441 and NGC 6388.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: Left: the high-resolution [Fe/H] metallicities of Crestani et al. (2021a), [Fe/H]Crestani21, compared to [Fe/H]CaT of the same stars. Bottom right: the [α/Fe] abundance as a function of the difference between [Fe/H]CaT and [Fe/H]Crestani21. The [Fe/H]CaT calibration does not appear significantly affected by α, but the sample size is small. Top right: the Gaia coadded RVS spectra of RRLs with S/N ∼ 35. The blue and red continua of the spectra are manually selected (green regions), as is the position of the CaT line at 8498 Å, for which the EW is then measured.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: Comparison of the photometric metallicities predicted from newly derived PM relations for RRab (left) and RRc (right) in this study based on Gaia G-band photometry.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: Left: an example of how the EW of an RRL changes with phase. Middle: the difference between each individual [Fe/H]CaT measurement as compared to the stars 〈[Fe/H]CaT〉. The light curve of a type ab RRL is overplotted. Right: same as the middle panel, but only the scatter about each phase is reported. Phases with the largest scatter in [Fe/H]CaT are highlighted in red, and the optimal phases with low [Fe/H]CaT scatters are highlighted in blue.
Paper: The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
Authors: Andrea Kunder, Zdenek Prudil, Claire Skaggs, Henrique Reggiani, David M. Nataf, Joanne Hughes, Kevin R. Covey, Kathryn Devine
Figure caption: The [α/Fe] abundance as a function of the difference between [Fe/H]CaT and [Fe/H]phot, where the different [Fe/H]phot relations of Clementini et al. (2023), Iorio & Belokurov (2021), Li et al. (2023), Dékány & Grebel (2022), Jurcsik & Hajdu (2023), and this study (Appendix) are compared. In all cases, [Fe/H]phot is a function of the α-enrichment of the RRL, with Δ[Fe/H] > 0.5 indicating a star with a low [α/Fe] abundance.