adsabs/AstroCLIMB huggingface dataset:
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: An ﹩{{\ell }}_{\max }=2﹩ eclipse map fitted to the data in Figure 1. First panel: an eclipse map constructed with spherical harmonics up to ﹩{{\ell }}_{\max }=2﹩, fitted simultaneously with the orbital, planetary, stellar, and systematic parameters, via “pixel sampling” as described in Section 3.1. Note that the nightside of the map contains no latitudinal information, with longitudinal information from the phase curve only (out of eclipse). The plotted 2D map uses the median of the posterior distribution of each fitted spherical harmonic coefficient. Second panel: the posterior distribution of the longitudinal structure along the equator of the map, showing the first and second quantiles. Third panel: the posterior distribution of the latitudinal structure through the substellar point.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: A comparison of four GCM simulations of WASP-43b and how their spatial distributions could appear in an eclipse map with restricted spherical harmonic order. First row: the modeled outgoing longwave radiation (OLR) in the 5–10.5 μm MIRI/LRS bandpass for each of the four GCM simulations, expressed as a ratio of planetary to stellar flux. Second row: observable emission from the GCM simulations, with the null space removed as described by Luger et al. (2021) and Challener & Rauscher (2023). Third row: the OLR represented using spherical harmonics up to ﹩{{\ell }}_{\max }=3﹩, showing how structure is lost; this is the best map that could be achieved by a fit like the ﹩{{\ell }}_{\max }=3﹩ fit in Figure 5. Fourth row: the OLR represented using a basis of the eigenmaps used in Figure 5. Fifth row: the OLR represented using spherical harmonics up to ﹩{{\ell }}_{\max }=2;﹩ this is the best map that could be achieved by a fit like that in Figure 3. All of the simulations match the dayside and nightside amplitudes of the observed phase curve and eclipse map fairly well, as well as the small eastward phase curve shift. The succession of plots here shows how using low-order spherical harmonics limits the structures that can be fitted with an eclipse map.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: The observed data in the ingress and egress of the eclipses, subtracted by a phase curve fitted using an n = 2 Fourier series model. We fitted this Fourier series model using the orbital parameters derived using an eclipse map in Table 1, so that the residual signal depends entirely on the different models. This leaves a residual “eclipse mapping signal” showing the effect of partial stellar coverage of the nonuniform planetary emission. Green points show the first eclipse, purple points show the second eclipse, and black points show their mean. The blue shaded region labeled “Latitude-Longitude Map Fit” shows the range of fitted phase curves from the ﹩{{\ell }}_{\max }=2﹩ eclipse map in Figure 3, with the two shaded regions showing the first and second quantiles, containing 68.27% and 95.45% of the posterior distribution. The red shaded region labeled “Longitude-Only Map Fit” shows the fitted eclipse of the ﹩{{\ell }}_{\max }=2﹩ eclipse map with flat latitudinal structure shown in Figure 4. The poor fit of this model shows the presence of latitudinal information in the data set, and the need to fit the latitudinal structure of the map. This “longitude-only” residual is around 250 ppm at its largest, while the “latitude-only” signal (estimated from the difference between the 1D and 2D map fits) is around 200 ppm. The total eclipse mapping signal is around 450 ppm at its largest.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: Two alternative mapping methods to Figure 3. First row: an eclipse map using spherical harmonics up to order ﹩{{\ell }}_{\max }=3﹩, fitted using constant systematic and orbital parameters derived by the map fitted in Figure 3 (listed in Table 1) The median map, longitudinal structure, and latitudinal structure are laid out as in Figure 3. Bottom row: an eclipse map fitted with eigenmaps up to order ﹩{{\ell }}_{\max }=3﹩ as described in Section 3.4, for six basis maps selected by optimizing the BIC, using constant systematic and orbital parameters derived by the fit in Figure 3.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: Eclipse maps fitted using each eclipse separately. First row: an eclipse map fitted using spherical harmonics up to ﹩{{\ell }}_{\max }=2﹩, using a ∼2.2 hr section of the data centered on the first eclipse. The orbital and systematic parameters are fixed to those derived using the map fitted in Figure 3 (except the time-dependent systematics, which are refitted), listed in Table 1. Only the dayside of the map is shown as there is no information about the nightside in this limited data set. The map has a similar longitudinal structure to Figure 3, but finds more latitudinal asymmetry. Second row: an eclipse map fitted using a ∼2.2 hr section of the data centered on the second eclipse. This finds a similar map to that in Figure 3. These two maps show that both eclipses are mostly consistent, although the first eclipse implies more latitudinal asymmetry. Third row: an eclipse map fitted using both the first and second eclipses as defined above, excluding the rest of the phase curve. This combined fit is similar to the individual fits, especially in its longitudinal structure.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: Left: the phase curve offset derived from the n = 2 fit using a Fourier series model (giving the same result as Bell et al. 2024), compared to the phase curve offset simulated from each GCM. Right: the (meridionally averaged) longitudinal offset in each 2D map. The ﹩{{\ell }}_{\max }=2﹩ and ﹩{{\ell }}_{\max }=3﹩ offsets (using all the data set) are from the map fits in Figures 3 and 5. The ﹩{{\ell }}_{\max }=2﹩ map fits using the eclipses only correspond to the fits in Figure 6 (the black point shows the fit to both eclipses, and the gray points show the fits to the first and second eclipses). The eclipse-only eigenmap fits and the eclipse-only ﹩{{\ell }}_{\max }=3﹩ map fits are not plotted in full elsewhere. The GCM points show the ﹩\cos \phi ﹩-weighted offset for the GCMs truncated to the ﹩{{\ell }}_{\max }=2﹩ and ﹩{{\ell }}_{\max }=3﹩ representations shown in Figure 7, as well as for the maps with no truncation.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: An eclipse map fitted to the data set in Figure 1, using the parameters listed in Table 1 derived with the ﹩{{\ell }}_{\max }=2﹩ eclipse map model, and constructed from ﹩{{\ell }}_{\max }=2﹩ spherical harmonics averaged in latitude. This is distinct from the “Fourier series” phase curve model used in Table 1, which models the phase curve directly and does not represent the partial coverage of the map in eclipse. The fit to the ingress and egress data is shown in red in Figure 2; as described in Section 3.2, this map cannot accurately fit the observed eclipse shape, showing the presence of latitudinal information in the observations.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: A comparison of the GCM simulation results in Figure 7 to the eclipse maps fitted to the data in Figure 1. First row: the GCM maps in the first row of Figure 7. Second row: the ﹩{{\ell }}_{\max }=2﹩ map in Figure 3 compared to the ﹩{{\ell }}_{\max }=2﹩ GCM maps in the fourth row of Figure 7. Third row: the eigenmap in Figure 5 compared to the eigenmap representations of the GCMs. Fourth row: the ﹩{{\ell }}_{\max }=3﹩ map in Figure 3 compared to the ﹩{{\ell }}_{\max }=3﹩ GCM maps in the third row of Figure 7.
Paper: Two-dimensional Eclipse Mapping of the Hot-Jupiter WASP-43b with JWST MIRI/LRS
Authors: Mark Hammond, Taylor J. Bell, Ryan C. Challener, Neil T. Lewis, Megan Weiner Mansfield, Isaac Malsky, Emily Rauscher, Jacob L. Bean, Ludmila Carone, João M. Mendonça, Lucas Teinturier, Xianyu Tan, Nicolas Crouzet, Laura Kreidberg, Giuseppe Morello, Vivien Parmentier, Jasmina Blecic, Jean-Michel Désert, Christiane Helling, Pierre-Olivier Lagage, Karan Molaverdikhani, Matthew C. Nixon, Benjamin V. Rackham, Jingxuan Yang
Figure caption: An ﹩{{\ell }}_{\max }=2﹩ eclipse map fitted using the orbital and systematic parameters derived by fitting the Fourier series model, shown in Figure 10 and listed in Table 1. The map is almost identical to that in Figure 3, showing that the small (but statistically significant) differences between the two fits in Figure 10 do not meaningfully affect the resulting ﹩{{\ell }}_{\max }=2﹩ eclipse map.
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Cross-correlation signal-to-noise ratio (SNR) as a function of systemic velocity (V sys) and planet Keplerian velocity (K  p ) for detections of, from left to right, H2O, CO, and OH on night 1 (top), night 2 (middle) and from both nights combined (bottom). SNR is calculated following Equation (1) after performing a 3σ  clipping using astropy.stats.sigma_clipped_stats. For the CO detection, we used only the orders containing the two distinct absorption bands near 1.61 and 2.45 μm. Black x marks denote the maximum cross correlation in each plot, while white dashed lines indicate expected values for WASP-76b from previous studies (West et al. 2016; Gaia Collaboration et al. 2018). All three molecules are clearly detected in both nights of data, and the combined data set shows SNRs of 6.93, 6.47, and 3.90 for H2O, CO, and OH, respectively. The right-most column shows non-detections of HCN on each night and in the combined data set.
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Trail plots showing cross-correlation strength as a function of radial velocity shift and orbital phase, in the rest frame of the planet WASP-76b, for H2O (left), CO (middle), and OH (right) on night 1 (top) and night 2 (bottom). On all plots, horizontal white dotted lines indicate the beginning and end of transit and the vertical white dashed line indicates the location of the planetary signal. Signals in the trace that move diagonally from the upper left to lower right show the cross-correlation detections of the signal from the host star WASP-76 and tellurics. Gray shading indicates phases that were masked during the retrievals to remove any contamination from the stellar and telluric signals.
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Posterior distributions for all parameters in the fiducial retrieval. Off-diagonal plots show 2D posterior probabilities for pairs of parameters, with 1, 2, and 3σ  intervals shaded in dark, medium, and light blue. On-diagonal plots show marginalized posterior probability distributions for each parameter.
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Comparison of retrieved abundances from the break pressure retrieval to expectations for models in chemical equilibrium. Solid lines with 1σ  shaded error bars show retrieved profiles for H2O (black), CO (purple), and OH (red). As described in Section 4.1, each abundance was fit with a two-parameter model including a deep atmosphere abundance and a pressure at which the abundance dropped to 0. For CO and OH, the retrieved break pressure was consistent with the top of the atmosphere, indicating the retrieval preferred a model with constant abundances with altitude for both gases. Dashed and dotted lines show predictions from chemical equilibrium models with compositions consistent with the best-fit results from this retrieval ([M/H]  = –0.75 and C/O = 0.8) and from the self-consistent gridtrieval ([M/H]= –0.75 and C/O = 0.6), respectively.
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Comparison of retrieved abundances from the fiducial retrieval to expectations for a solar composition gas in chemical equilibrium. Dashed lines show expected abundance of various species as a function of pressure for a model with a composition consistent with the best-fit results from this retrieval ([M/H]=  −0.125 and C/O = 0.9). Solid points with 1σ error bars show retrieved abundances for H2O (red), CO (purple), and OH (brown). The points are placed near the mean photospheric pressure across the observed wavelengths.
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Carbon-to-oxygen (C/O) ratio as a function of mass for all planets with constrained abundances of both oxygen-bearing and carbon-bearing species. Purple, pink, and yellow points indicate results from JWST, high-resolution observations, and combined analyses of both JWST and high-resolution data (citations given in Table 2). The black point indicates the value for Jupiter based on the Galileo and Juno missions. The pink points with black outlined, star-shaped markers are our results for WASP-76b. Planets with multiple measurements have small offsets in mass applied between the different results for clarity. While there is no clear trend with mass, overall the population of exoplanets shows a mean C/O ratio greater than solar.
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Same as Figure 3 but for the break pressure retrieval. In this retrieval, each detected molecule is represented with two parameters: a deep atmosphere abundance (﹩{\mathrm{log}}_{10}(n)﹩) and a break pressure where the abundance drops to zero (P  b ).
Paper: The Metallicity and Carbon-to-oxygen Ratio of the Ultrahot Jupiter WASP-76b from Gemini-S/IGRINS
Authors: Megan Weiner Mansfield, Michael R. Line, Joost P. Wardenier, Matteo Brogi, Jacob L. Bean, Hayley Beltz, Peter Smith, Joseph A. Zalesky, Natasha Batalha, Eliza M.-R. Kempton, Benjamin T. Montet, James E. Owen, Peter Plavchan, Emily Rauscher
Figure caption: Same as for Figure 3, but for the gridtrieval described in Section 4.2.
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Results of the shape-based granulation mitigation simulation described in Section 4.3. Each set of plots corresponds to simulations of spectra observed at spectral resolutions approximately representative of those of existing instruments, except for the bottom right panel, which is meant to represent a fictionalized ultra-high-resolution instrument as the best-case, fiducial scenario. The rms RVs reported in left-hand panels of each figure correspond to measurements performed without any granulation mitigation. The rms RVs in the right-hand panels were calculated from RVs corrected using the procedure described in Section 4.3.1. The reported rms RVs are the mean of many trials; the typical errors on the mean are at the ≲1.5% level (not shown). Note that the step sizes for SNR and number of lines are not of fixed size. Unsurprisingly, both the raw and mitigated rms RVs improve as the SNR and number of lines are increased. Notably, though, the achievable mitigation is strongly dependent on spectral resolution — only the three highest-resolution simulations achieve statistically significant reductions in the rms RV (see Figure 6 and associated text).
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Line-by-line differences in granulation-induced variability. Left: colored circles indicate the mean rms RV measured from time series of individual disk-integrated line profiles, following from the procedure outlined in Section 4.1. The colored diamonds show the mean residual rms RV after using the tuned BIS to correct granulation velocities, as detailed in Sections 4.2 and 4.2.2. In both cases, the error bars are the 1σ width of the rms RV distributions measured from many trials, as described in Section 4.1. Right: the amount of variability (expressed as the rms RV) exhibits no clear correlation with T 1/2 (see Al Moulla et al. 2022), or any other single quantity, including wavelength, line depth, and potential of the lower and upper states of each transition (not shown). Although there is an appreciable difference between the most and least variable lines, it is not immediately apparent how the variability of a line could be predicted from the formation or atomic properties of a line.
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Ensemble of synthetic disk-integrated bisectors for the 22 lines analyzed in this work; compare to Figure 17.14 of Gray (2008). These bisectors were measured from significantly oversampled spectra synthesized at R ∼ 700,000 to ensure smoothness. Classical “C”-shaped bisectors are shown in the left-hand figure, and bisectors of deeply blended lines are shown in the right-hand figure. The velocity offsets in both panels of each figure are arbitrary and for illustrative purpose only. As in Figure 17.14 of Gray (2008), the bisectors are composited at right in each figure to show their (dis)similarity.
Paper: GRASS. II. Simulations of Potential Granulation Noise Mitigation Methods
Authors: Michael L. Palumbo, Eric B. Ford, Elizabeth B. Gonzalez, Jason T. Wright, Khaled Al Moulla, Rolf Schlichenmaier
Figure caption: Collage of continuum-normalized, disk-center solar spectra originally observed for Löhner-Böttcher et al. (2018, 2019), Stief et al. (2019), with annotations for the lines used as input in this work. Lines denoted with a double dagger (C I 5380 Å and Na I 5896 Å) were included in the convective-blueshift analysis presented in Löhner-Böttcher et al. (2019), but are excluded from the analyses presented in this work, as explained in Section 2. Other lines are of telluric origin, significantly blended, and/or very shallow. Note the breaks in the wavelength axis; eight spectral regions spanning only a few Å each were observed. Spectroscopic properties and parameters for these lines are tabulated in Table 1.