adsabs/AstroCLIMB huggingface dataset:
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: Residuals of our RV fits to the single eccentric planet in the HD 3651 system. We include a black horizontal dashed line at 0 m s−1 for illustrative purposes.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The phased RVs for the three Keplerians in our eccentric-orbit model for GJ 12 with a rotation GP.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The phased RVs for the three Keplerians in our circular-orbit model for GJ 12 with a rotation GP.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The MAROON-X RVs described in this paper. The RVs that are not used in the final analysis are shown in lighter colors and indicated with “x” markers. The grayed-out region represents the time during the September 1–18 temperature anomaly. We also include a dashed line indicative of the etalon drift slope as calculated for the calibrator star HD 3651 (see Section 4.1 for more details). We have not modified the data in any way for the purpose of producing this figure, and have not subtracted out any offsets or slopes.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: All of the RVs used in our analysis. Each data set shown is mean-subtracted to highlight the relative changes in RV of the star. We have also subtracted the etalon drift slope and offsets (calibrated using those from HD 3651; see Section 4.1 for more details) from the MAROON-X data. Our MAROON-X data have a much smaller scatter than the data from other instruments, indicating that our MAROON-X data will provide much more constraining power than previous observations.
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: Illustration of the internal energy balance calculation with melt for GJ-12 b. We illustrate the calculations of both Fconv (dashed) and Ftidal (solid lines) as a function of mantle temperature, with equilibria highlighted for each B value with black circles. The constraints on tidal heating fluxes on Jupiter’s moon Io are shown as a gray shaded region (G. J. Veeder et al. 2012).
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The inferred water contents of both our circular-orbit and eccentric-orbit GJ 12 b models using the L. Zeng et al. (2019) models (top panel) and A. Aguichine et al. (2021) models (bottom panel).
Paper: An Earthlike Density for the Temperate Earth-sized Planet GJ 12 b
Authors: Madison Brady, Jacob L. Bean, Ritvik Basant, Nina Brown, Tanya Das, Matthew C. Nixon, Rafael Luque, Caroline Piaulet-Ghorayeb, Michael Radica, Andreas Seifahrt, Julian Stürmer, Lily Zhao
Figure caption: The inferred CMF of both our circular-orbit and eccentric-orbit GJ 12 b models using the L. Zeng et al. (2019) models, assuming the planet lacks both water and an atmosphere.
Paper: The Dynamical Environment within the Habitable Zone of the Gaia-4 and Gaia-5 Planetary Systems
Authors: Stephen R. Kane
Figure caption: The eccentricity distribution of giant planets (Mp > 0.1 MJ) whose semimajor axis lies beyond the OHZ outer boundary (left panel). Both the shade and the size of the plotted data are logarithmically proportional to the planet mass, where dark green indicates a low mass and light green indicates a high mass. The right panel shows a subset (the wrecking ball planets) whose orbits either pass through the HZ or whose periastron distance lies within 20% of the outer OHZ boundary.
Paper: The Dynamical Environment within the Habitable Zone of the Gaia-4 and Gaia-5 Planetary Systems
Authors: Stephen R. Kane
Figure caption: System architectures and HZ boundaries for the Gaia-4 (left) and Gaia-5 (right) systems, showing the orbit of the planet in each case. The HZ regions are shown in green, where light green and dark green indicate the CHZ and OHZ, respectively. The scales of the figure panels are 2.5 and 1.5 au along each side for Gaia-4 and Gaia-5, respectively.
Paper: The Dynamical Environment within the Habitable Zone of the Gaia-4 and Gaia-5 Planetary Systems
Authors: Stephen R. Kane
Figure caption: Percentage of the simulation that the injected Earth-mass planet survived as a function of semimajor axis for the Gaia-4 (top panel) and Gaia-5 (bottom panel) systems. As for Figure 1, the CHZ is shown in light green and the OHZ is shown in dark green. The periastron passage of Gaia-5b is indicated by the vertical dotted line.
Paper: The Dynamical Environment within the Habitable Zone of the Gaia-4 and Gaia-5 Planetary Systems
Authors: Stephen R. Kane
Figure caption: The mass and semimajor axis of a possible lost planet in a circular orbit whose angular momentum equals the angular momentum deficit (AMD) for each of the considered systems: Gaia-4 (solid line) and Gaia-5 (dashed line). The dots indicate the planet mass and semimajor axis of the known companions.
Paper: The Dynamical Environment within the Habitable Zone of the Gaia-4 and Gaia-5 Planetary Systems
Authors: Stephen R. Kane
Figure caption: Angular separation of Gaia-4b (solid line) and Gaia-5b (dashed line) from their respective host stars as a function of their orbital phase.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Fit results for two sample fields of standard, ﹩{2}^{{\prime} }\times {2}^{{\prime} }﹩ size. We stress that we do not bin the data in our analysis and that binning is solely for visualization. Panel (a) is a high-latitude field that effectively characterizes the Red Clump and background giant stars. Panel (b) is a low-latitude field that suffers from crowding and completeness issues. The exponential shape of the background giant branch stars is missing, resulting in B pushing against the prior lower limit to account for the lack of stars. This field is an example where we only report a lower limit on the extinction. Corner plots of the MCMC sampling are provided in the right panels, with blue lines indicating values from the maximum likelihood estimation.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Comparison of extinction maps from this work with those from G18, S20, and Z22. The top row shows the difference between our extinction map, derived from fitting Equation (1), and the literature maps, within the UKIRT fields. The middle row displays extinction distributions using a Gaussian kernel density estimator: black open contours represent values from the luminosity function fit, while gray filled contours show extinction derived from color excess and the S. Wang & X. Chen (2019) extinction law. The bottom row shows histograms of the differences in extinction values, with black bars for the luminosity function fit and gray bars for the color excess method. Dashed lines indicate the percentiles of ﹩{\rm{\Delta }}{A}_{{K}_{S}}﹩ from the luminosity function–based extinction.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Comparison of ﹩{A}_{{K}_{S}}/E(H-{K}_{S})﹩ from our work to the difference from our extinction values with O. A. Gonzalez et al. (2018), F. Surot et al. (2020), and M. Zhang & J. Kainulainen (2022). Each point is colored by vertical distance from the Galactic center in degrees. The top row shows ﹩{\rm{\Delta }}{A}_{{K}_{S}}﹩ from the luminosity function fit–derived extinction, while the bottom panel used S. Wang & X. Chen (2019) to convert color excess into extinction. The red square in the top left corner shows the median uncertainty on ﹩{A}_{{K}_{S}}/E(H-{K}_{S})﹩ and ﹩{A}_{{K}_{S}}﹩ from both methods. The median uncertainty in ﹩{A}_{{K}_{S}}﹩ does not account for contributions from the literature being compared against, but does account for the uncertainty in the S. Wang & X. Chen (2019) extinction law.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Comparison between various extinction laws against the UKIRT extinction map. Plotted against the KS-band extinction is the ratio of total-to-selective extinction ﹩{A}_{{K}_{S}}/E(H-{K}_{S})﹩. Points are colored by their distance from the Galactic plane (∣b∣). The red square in the top right corner shows the median uncertainty in ﹩{A}_{{K}_{S}}/E(H-{K}_{S})﹩ and ﹩{A}_{{K}_{S}}﹩.
Paper: The Influence of Tight Binaries on Protoplanetary Disk Masses
Authors: Kevin Flaherty, Peter Knowlton, Tasan Smith-Gandy, A. Meredith Hughes, Marina Kounkel, Eric Jensen, James Muzerolle, Kevin Covey
Figure caption: Location of our tight binary targets on a map of dust extinction (D. J. Schlegel et al. 1998). Green circles indicate the targets of our ALMA observations that made it through the cluster membership cuts (Section 2.2). The majority of our targets are located near the Orion Nebula Cluster, with some spread along the Orion A cloud; the more isolated targets in Orion A are marked with their ID numbers.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Distributions of the ﹩{A}_{{K}_{S}}﹩ extinction and E(H − KS) reddening. Histograms for high-latitude (∣b∣ > 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6) and low-latitude (∣b∣ ≤ 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6) fields are shown in red and brown, respectively, to highlight the location dependence of extinction and reddening.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Color–magnitude diagrams of six fields with varying ﹩{A}_{{K}_{S}}/E(H-{K}_{S})﹩. The color–magnitude diagrams are ordered from smallest ﹩{A}_{{K}_{S}}/E(H-{K}_{S})﹩ to largest. Each color–magnitude diagram here has a well-populated luminosity function (B > 0.4). The red dotted–dashed and orange dashed lines are the values of KS,RC and ﹩{(H-{K}_{S})}_{RC}﹩ for the given color–magnitude diagram, respectively.
Paper: A Near-infrared Extinction and Reddening Map toward the Galactic Bulge Using UKIRT
Authors: Aiden S. Zelakiewicz, Samson A. Johnson, B. Scott Gaudi, Geoffrey Bryden, David M. Nataf, Yossi Shvartzvald
Figure caption: Map of total-to-selective extinction ﹩{A}_{{K}_{S}}/E(H-{K}_{S})﹩ for each field in the map. We omit fields where B < 0.2 to highlight the variance in better-characterized fields.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Two-color diagrams of XSL synthetic photometry, color-coded by ﹩\mathrm{log}(g)﹩ and [Fe/H] from the XSL parameters.
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: Eclipse depth measurements from KELT and TESS observations for all EB systems with changing depths. Error bars indicate the uncertainty of the Gaussian fit used to measure eclipse depth. Lines illustrate the linear least-squares fit across all KELT measurements. Each EB is separated according to color, and KELT and TESS measurements are indicated by marker shape: circle for KELT and triangle for TESS. Filled and unfilled triangles show when SPOC data or QLP data were used, respectively. Unseen error bars are smaller than the symbols.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Total response curves of the g, i, and N B515 filters of HSC, overlaid by the observed spectrum of an M giant (blue) and of an M dwarf (purple) from the X-shooter Spectral Library. Both spectra have been down-sampled to a resolving power of 2000 and arbitrarily normalized for clarity. The zoomed-in plot highlights the N B515 filter, which is centered around 5150 Å and includes the MgH+Mgb absorption features.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Color–magnitude and two-color diagrams of the observed data (left) and training set (right) for this field in the inner halo of M31, with giants in the training set color-coded by [Fe/H].
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: O − C vs. median time of observation for AH Cep utilizing individual eclipse times from KELT for the years 2012–2017 and all eclipses from TESS Sectors 17, 18, 24, 57, 58, 77, 78, 84, and 85.
Paper: Eclipse Depth Variations in Seven Eclipsing Binaries as Observed by KELT and TESS
Authors: Anna C. Baum, Joshua Pepper, James R. A. Davenport, Steve B. Howell
Figure caption: The Gaussian fits for all years of AH Cep KELT observations and all sectors of TESS observations. We fit each eclipse with a Gaussian curve in order to obtain an eclipse depth and timing measurement.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Gaia color–magnitude diagram of stars in the MaStar Library and two-color diagram of MaStar synthetic photometry, color-coded by ﹩\mathrm{log}(g)﹩ and [Fe/H] from the mean MaStar Library parameters. A reddening vector is shown in the top left panel, with length corresponding to the mean extinction of the catalog (Av = 0.37).
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Confusion matrix for giant/dwarf classification in M31. Predicted labels with giant probability greater than 0.85 are compared against reference labels from I. Ogami et al. (2025) with ρM31 greater than 0.9. Diagonal elements show agreements, while off-diagonals indicate disagreements.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: The M − DDO51 and N B515 − g two-color diagrams of the cross-matched sample between our MaStar synthetic photometry catalog and the APOGEE stellar parameters catalog; both use synthetic (g − i)0 along the x-axis for ease of comparison. The diagrams exhibit similar dwarf/giant separation, despite the different shapes of the giant sequences.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Two-color and color–magnitude diagrams of the Fornax dwarf galaxy spectroscopic members indicated by E. N. Kirby et al. (2010), color-coded by the predicted membership label from the machine learning model.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Two-color diagram and color–magnitude diagram of a field in the inner halo of M31. The cross-matched sample with the DESI spectroscopic members is color-coded by the predicted membership label.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Two-color diagram and color–magnitude diagram of a field in the inner halo of M31, color-coded by the predicted red giant label.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Two-color diagram and color–magnitude diagram of a field at the NW stream of M31, color-coded by the predicted red giant label.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Two-color diagram and color–magnitude diagram of Fornax, color-coded by the predicted membership label.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Comparison of synthetic HSC g − i colors with observed g − i colors.
Paper: Machine Learning Techniques to Distinguish Giant Stars from Dwarf Stars Using Only Photometry—Pushing Redward
Authors: Keyi Ding, 可怿 丁, Carrie Filion, Rosemary F.G. Wyse, Evan N. Kirby, Itsuki Ogami, Masashi Chiba, Yutaka Komiyama, László Dobos, Alexander S. Szalay
Figure caption: Gaia color–magnitude diagram of stars in the MaStar Library and two-color diagram of MaStar synthetic photometry, color-coded by [α/Fe] from the mean MaStar Library parameters.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: The ﹩{M}_{{K}_{s}}﹩ vs. (J − Ks) CMD for stars in the Population I Hα sample compiled for this work. The data herein have not been corrected for interstellar reddening or absorption. (a) In the upper panel stars known to exhibit Hα emission on at least one occasion (Table 1) are shown as filled circles, with open circles being used to depict stars not known to exhibit such emission. (b) In the lower panel symbols are used to designate stars of different variability type: (open circle) a star not listed as variable in SIMBAD; (filled circle) an LPV with a known period; (filled square) LPV, semiregular, irregular, RV Tauri, or other pulsating giant without a known period; (filled triangle) Cepheid or δ Scuti star; (six-pointed stellated symbol) RS CVn type or interacting close binary; (four-pointed stellated symbol) FK Com type or other rotational or ellipsoidal variable; (three-pointed stellated symbol) eclipsing Algol system; (open triangle) other type of variable such as BY Dra variables or flare stars; and (open square) listed as a variable star in SIMBAD but no information given about the type.
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: The WISE (W3 − W4) color vs. ﹩{M}_{{K}_{s}}﹩ absolute magnitude in the top panel, and (V − Ks) color in the lower panel, for stars in the Population I Hα sample. In the case of all Hαe stars the plotted data (blue symbols) are listed in Table 4, and have been corrected for interstellar reddening and absorption. Upper panel: blue circles depict Hαe stars of luminosity classes I and I–II, blue squares correspond to stars of class II or III, while open blue symbols depict post-AGB stars. The vertical dotted line corresponds to MK,s = −4.5. Lower panel: the blue symbols for the Hαe stars are coded by stellar variability according to the scheme used in the lower panel of Figure 4. Of particular note are the LPVs of known period (filled blue circles), and the LPVs for which there is no measured period (filled blue squares). Red open circles in both panels depict stars not known to exhibit Hα emission, for which the plotted colors and magnitudes are not corrected for interstellar reddening (hence the red symbols for contrast).
Paper: Hα Emission among Evolved FGKM Stars: A Compendium from the Literature
Authors: Graeme H. Smith
Figure caption: The MV,0 vs. (B − V)0 CMD for the sample of Population I stars with Hα emission from Table 1. Both absolute magnitude and color have been corrected for interstellar reddening (column 2 of Table 4), and the plotted data are from columns 4 and 5 of Table 4. In the upper panel the symbols are coded according to spectral class: M type (circles), K (hexagons), G (squares), and F (triangles). Post-AGB stars are depicted with open symbols; all other stars are shown with filled symbols. Some Hα stars in Table 1 exhibit a range in spectral classes due to either time variability or binarity. In such cases the symbol in the upper panel of the figure corresponds to the latest spectral class that is listed in Table 1. In the lower panel the symbols are in accord with luminosity class: luminosity class I and I–II (circles), and luminosity class II and III (squares), with post-AGB stars again being distinguished with open symbols.