adsabs/AstroCLIMB huggingface dataset:
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Histograms of L Lyα  (upper panel), L FUV (middle panel), and W Lyα  (lower panel). In addition we also show histograms for data on high-redshift LAEs from the Very Large Telescope/MUSE observations (Leclercq et al. 2017). Thick dotted vertical lines show the median L Lyα , L FUV, and W Lyα  values for the net emitters in our data set, and the thin dashed lines show the medians for the MUSE LAEs.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Color composites for the ELARS 27–28, Tol 1214, Tol 1247, and J1156 galaxies. See the caption for Figure 2 for details.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Average growth curve of Lyα luminosity for the galaxies in the sample with W Lyα  > 0 Å. The dark-gray shaded area shows the standard deviation (capped at a ratio of 1) over the sample at each radius, and the light-gray shaded area shows the full envelope of the sample.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Compilation of measurements on ELARS08 (example of an intermediate Lyα emitter). A description of the elements in this figure is given in Figure 7.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Compilation of measurements on ELARS03 (example of a weak Lyα emitter). A description of the elements in this figure is given in Figure 7.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Color composites for the LARS 11–14 and ELARS 1–6 galaxies. See the caption for Figure 2 for details.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Color composites for the ELARS 7–16 galaxies. See the caption for Figure 2 for details.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Color composites for the ELARS 17–26 galaxies. See the caption for Figure 2 for details.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Comparison of the f esc-corrected Lyα SFR diagnostic with SFR derived from Hα. The color scale of the circles indicates the E(B − V) n  of the galaxies. Galaxies with a zero or negative Lyα luminosity are excluded from this plot. The dotted line shows the 1-to-1 relation. The upper plot shows the ratio SFRLyα /SFRHα . The light green band shows the standard deviation of the ratios for the full sample, while the darker-green band shows the standard deviation for a subsample with E(B − V) n  < 0.3.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Global escape fraction of Lyα vs. nebular extinction. The gray lines show where the points would fall for different ISM extinction curves. The curve labeled CCM is the galactic extinction curve from Cardelli et al. (1989), and SMC is from Prevot et al. (1984). Colored lines show curves derived from fitting a line to observation from this and other Lyα studies. Note that that Hayes et al. (2011) and Matthee et al. (2016) used stellar extinction; for this comparison, we multiply their E(B − V) values by a factor 2.27 (Calzetti et al. 2000). The dotted gray lines (labeled CCM (clumps)) show clumpy dust models with varying numbers of clumps along the line of sight.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Left panel: f esc vs. the ξ Lyα  parameter. Right panel: ξ Lyα  vs. nebular extinction. Galaxies with lower limits on r p,FUV (ELARS15 and ELARS22) are excluded from these plots.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Scatter plots of f esc vs. various properties of the galaxies.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Best-fit PSF model for the SBC F125LP filter. Observed data points come from a stack of stars in NGC 6681. The average residual for the observed data points is given in the legend.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Scatter plots of f esc vs. Petrosian radii in FUV (left panel) and Lyα (right panel). Note that the galaxy ID labels refer to the left panel; therefore, some of the galaxies with limits in the right panel are not shown as such in the legend. Please refer to Table 5 for individual galaxy limits.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Relative residual of PSF models compared to a maximum width PSF (filter setup and individual models from the ELARS01 data set). This figure shows residuals without performing any matching.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: PSF models for a selection of filters.
Paper: The Lyα Reference Sample. XIV. Lyα Imaging of 45 Low-redshift Star-forming Galaxies and Inferences on Global Emission
Authors: Jens Melinder, Göran Östlin, Matthew Hayes, Armin Rasekh, J. Miguel Mas-Hesse, John M. Cannon, Daniel Kunth, Peter Laursen, Axel Runnholm, E. Christian Herenz, Matteo Messa, Daniel Schaerer, Anne Verhamme, T. Emil Rivera-Thorsen, Lucia Guaita, Thomas Marquart, Johannes Puschnig, Alexandra Le Reste, Andreas Sandberg, Emily Freeland, Joanna Bridge
Figure caption: Relative residual of PSF models after matching them to the maximum width PSF using the technique described in this paper.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Hertzsprung–Russell diagrams for the stars of the WBE sample. Spectral types are color coded according to the legend in the initial panel (a). PARSEC evolutionary tracks are displayed as solid curves for main-sequence and post-MS trajectories, and dashed for the PMS Hayashi phase. Luminosity class is indicated by dark outlined circles for dwarfs and subgiants (V and IV), blue for ordinary giants (III), and gray for bright giants and supergiants (II and I). (a) Solar-metallicity MS and post-MS stars. The full evolutionary track for the Sun (1 M ⊙) is the thicker dark curve (dashed for the PMS phase). The current location of the Sun is marked by ⊙. Closely spaced double curves slanting from the middle left to lower right represent the “middle-aged” MS: the 5 Gyr isochrone for M ≤ 1 M ⊙, and the half total lifetime point for the heavier, more rapidly evolving stars. Dots, where visible, and numerical annotations indicate specific M/M ⊙ on the middle-aged MS. Additional annotations toward the upper left mark M/M ⊙ for representative higher-mass post-MS tracks. (b) T-Tauri stars. Only the pre-MS Hayashi tracks are displayed, except for the full solar evolution. (c) Metal-poor stars, about 1 dex deficient in [Fe/H]. Now, the middle-aged MS and the 1 M ⊙ full evolutionary track (as well as the higher-mass trajectories) refer to the [Fe/H] = −1 case. The solar-metallicity counterparts are shown as gray and yellow curves, respectively. (d) Extremely metal-poor stars, about 2 dex deficient in [Fe/H]. Highlighted tracks are for [Fe/H] = −2. The different curves are marked in the same way as in panel (c).
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Examples of solar Mg II hk profiles from spatially resolved areas of different activity (solid curves) plus quiet-Sun disk averages (dots). The specific intensities, I  λ , of the resolved regions were converted to surface fluxes, F  λ , according to the uniform-disk approximation. The three lower curves (the middle of which is partly hidden by the dots) represent the quiet-Sun: darker than average, average, and brighter than average. The three upper profiles are from active plages of similarly diverse strengths. Thin vertical lines mark the peaks of the medium-quiet hk profiles. The plage k2 peak separations tend to be slightly narrower than those of the quiet-Sun profile, whereas the h1 and k1 minimum features are significantly wider. The wings of the full-disk profiles are dimmer than the spatially resolved counterparts owing to limb darkening. Weak emission features, of unknown origin, are visible at +1.5 Å from k-line center and +1.3 Å from the h-line center.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Lower panel: 1D solar model of Maltby et al. (1986). The blue curve is temperature vs. column mass density (lower x-axis) or height (upper axis). The red dashed curve is the Mg II k-line “source function.” Formation depths of the three characteristic profile features are depicted. Vertical dotted–dashed lines are τ = 1 for k (left), and the visible continuum (right). The symbol m * marks the initial chromospheric temperature rise; m Λ is the “thermalization depth” (see the text). Upper panel: density curves for hydrogen and electrons. At high temperatures, at the right side or left side of panel, n e approaches n H owing to nearly complete ionization of hydrogen. In the cooler layers of the photosphere, in contrast, n e falls to a floor of 10−4 n H dictated by the easily ionized metals. In the chromosphere itself, remarkably, the electron density is nearly constant despite a factor of 104 hydrostatic decline of n H, the so-called “ionization-valve” effect.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Upper panel: overview of solar Ca II H (red) and K (blue), in the violet part of the visible spectrum, based on high-resolution NSO FTS scans. The inset expands the extreme line cores, on a relative wavelength scale, revealing the barely visible emission reversals of the solar HK features (same color scheme as in main panel). Lower panel: an equivalent broad view of analogous Mg II h (red) and k (blue) in the NUV, although in this case an HST STIS observation of solar twin α Cen A. The inset shows a blow-up of, now, the solar hk features based on flux profiles derived from Interface Region Imaging Spectrograph (IRIS) full-disk spectral scans (Gunár et al. 2021). The wavelength scales of the two main panels and insets were adjusted to cover roughly the same velocity span. The Mg II cores are broader than the Ca II counterparts and display larger intensity contrasts.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Comparison of three different approaches to determine stellar effective temperatures. “T CAT” refers to filtered averages of curated literature values collected from the PASTEL Catalog, supplemented by SIMBAD. “T TIC” was taken from the TESS Input Catalog v8.2, which employed alternative assessments. “T G” was obtained from a transformation based on the Gaia (BP − RP) color, as corrected for reddening, and accounting for surface gravity and metallicity. The various objects are color coded according to spectral type (legend, upper left), and luminosity class: dark outlined circles for dwarfs and subgiants (V and IV), blue outlined for ordinary giants (III), and gray outlined for bright giants and supergiants (II and I). The dashed line represents 1:1 correspondence. Agreement among the different approaches is good, aside from a few outliers.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Iconic features in the doubly reversed chromospheric emission cores of the Mg II (and Ca II) emission lines. As in the previous figure, h is in red, k is in blue. λ 0 is the laboratory wavelength of h or k in the adopted stellar radial velocity (RV) frame. The inner-wing profile minima are designated “1,” the emission peaks are “2,” and the central reversal is “3.” The former two designators are occasionally provided suffix “v” or “r” to specify the short-wavelength or long-wavelength side of the profile, respectively. Gray “W” marks the FWHM of the (k-line) emission core.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Upper panel: scatter plot of bolometrically normalized net hk fluxes vs. stellar temperatures. Only grade A–C fits were included. Gray triangles, where visible, indicate ﹩{f}_{\text{LO}}﹩ fluxes; overlying adorned circles mark the f UP values. Symbol colors and coding are the same as in previous diagrams. The larger ⊙ symbol represents the disk-average quiet-Sun flux profile; smaller ⊙ symbols are for spatially resolved quiet and active regions. The dark dashed line is a schematic lower boundary to the solar-metallicity points. Note, however, that the K dwarfs seem to depart somewhat from the trend. Lower panel: similar scatter plot, but now for the normalized f 1 minimum, or “basal,” fluxes. The dashed line is repeated from the upper panel.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Surface gravity vs. temperature-corrected W 50 for the WBE sample, grades A–C. Symbol markings are the same as previously given. The thick slanted dashed line is an iterated O–C filtered fit to the main trend, ∼g −0.218(±0.002). The same W 50 hinge point as in Figure 20 was adopted, but now at solar gravity on the y-axis. Red dashed lines show the effect of changing the exponent by ±0.01 (much larger than the formal uncertainties). The slanted gray region encompasses the giants and supergiants utilized in the previous T EFF vs. W 50 diagram (Figure 20).
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Left panel: effective temperature vs. W 50 for the gravity-selected solar-composition dwarfs illustrated in the previous diagram. The symbol coding is the same as in previous figures. The thick dashed curve has a power-law exponent of β ≈ 1.27. The thinner red dashed curves illustrate the result of changing the exponent by ±0.1, which is more than 3σ with respect to the formal fit. Right panel: similar comparison for selected targets in luminosity classes III–I (contained in the gray area of subsequent Figure 21). The lower gravity objects apparently have a stronger temperature dependence, β ≈ 2.34. The thinner red dashed curves again illustrate the result of changing the exponent by ±0.1. The “g” subscript on the W 50 width in the x-axis title indicates that the values (in both panels) were corrected for an assumed gravity correlation (g −0.218). For this reason, the corrected dwarf and giant plus supergiant line widths cover about the same velocity span, despite the fact that the uncorrected widths are quite different.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption:                         Examples of the Mg II hk fitting procedure for metal-poor and high-velocity stars. The Δλ scales are compressed relative to the giants and supergiants, but are similar to those of earlier Figure 11 (dwarfs). (a) Low-metallicity dwarfs and giants; [Fe/H] noted in lower frame across from the HD number. (b) High-velocity stars; catalog RV (kilometers per second) listed in lower frame across from the HD number.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: Temperature vs. surface gravity for the solar-composition ([Fe/H] > −0.5), non-T-Tauri members of the WBE sample. Symbol markings are as in previous figures. Stars in the confined gravity range bounded by the shaded area populate the dwarf panel in subsequent Figure 20. There is a rough systematic shallow correlation between temperature and gravity among the giants and supergiants, T EFF ∼ g +0.06, and a steeper inverse relation among the dwarfs, T EFF ∼ g −0.35. Temperature subgroups a–c will appear later.
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: The classical WBE diagram for Mg II. W 50 widths are expressed in equivalent velocity units to conform to the original WBE study. All of the fits (grade A–D) are shown. While the general WBE width–luminosity trend is visible, the diagram is littered with outliers, especially the T-Tauri stars and fast-rotating Hertzsprung-gap giants, much more so than the original HK counterpart. There also appears to be distinct substructure, for example, in the red dwarfs, dF stars, and among the metal-deficient objects. Symbol markings are the same as in the previous figures. The broken power-law model (thick dark dashed lines, meeting at the solar position) has a slope of −13.1 for the lower branch and −19.0 for the upper; the thinner red dashed lines show the result of ±1 changes in those slopes (≈3σ with respect to the formal fits).
Paper: In the Trenches of the Solar–Stellar Connection. VII. Wilson–Bappu 2022
Authors: Thomas Ayres
Figure caption: The two “stretching” parameters, δ f in flux density and δ λ in wavelength, invoked in the h-line hybridization process, and displayed for the stars with grades A or B. Individual objects are marked as in the previous figures. Smaller ⊙ symbols are for the spatially resolved IRIS intensity profiles of Figure 4; the larger ⊙ symbol represents the quiet-Sun disk average. The gray cross depicts the average values of each parameter with ±1 σ standard deviations: h systematically is about 93% the width of k, and about 75% the average peak brightness in flux density.