adsabs/AstroCLIMB huggingface dataset:
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: Scatter plots of the semi-amplitude of the photometric variation and detectable depth vs. rotation period. The color bar shows the minimum detectable transit depth in the Kp band. The red points are the detectable targets at a threshold of 1% in the J band, but not in the Kp band. In the left, middle, and right panels, the planetary orbital periods of the samples are 5 days, 10 days, and 15 days, respectively.
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: Scatter plots of the rotation period vs. the semi-amplitude of the photometric variation for each cluster. The color bar corresponds to the minimum detectable transit depth ﹩[{({R}_{{\rm{p}}}/{R}_{{\rm{s}}})}^{2} \% ﹩] when the orbital period is 10 days. The contour lines represent borders of 1.0%, 0.6%, and 0.2% detectable minimum transit depths, respectively; e.g., the targets existing above the 1.0% border could not be detected when the transit depth was shallower than 1.0%.
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: PDFs for the planets around stars whose T eff are 3000–4000 K discovered by the transit method. The black dots are the orbital properties of the planets. The probability density is calculated using the Gaussian kernel density estimation.
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: Scatter plots of p eff, the effective recovery rate based on the current planet distribution, colored by cluster. The upper and lower panels show the detectability, assuming the PDF in Figure 4, in relation to the rotation period and the semi-amplitude of the flux modulation, respectively.
Paper: Color Dependence of the Transit Detectability of Young Active M Dwarfs
Authors: Kohei Miyakawa, Teruyuki Hirano, Bun'ei Sato, Satoshi Okuzumi, Eric Gaidos
Figure caption: The same heat maps as the right side of Figure 2, but in the J band. The dashed green lines represent the border in the Kp band from Figure 2 for comparison.
Paper: The Arizona Radio Observatory 1 mm Spectral Survey of the Hypergiant Star NML Cygni (215–285 GHz)
Authors: A. P. Singh, J. L. Edwards, L. M. Ziurys
Figure caption: The 1 mm survey (214.5–285.5 GHz) of NML Cyg displayed in consecutive ∼1 GHz frequency segments. Temperature scale in T A*(K) and spectral resolution is 2 MHz. There is 40–80 MHz overlap between consecutive spectra in order to show any lines on the edge of a given range for display purposes. For frequencies with lines stronger than T A* ∼ 50 mK, a second version of the spectrum is shown with a more sensitive scale. Each emission feature is marked with its molecular identification. First order baselines were removed from each spectrum. Integration time per spectrum is typically ∼15 hr. 1 of 21 image
Paper: The Arizona Radio Observatory 1 mm Spectral Survey of the Hypergiant Star NML Cygni (215–285 GHz)
Authors: A. P. Singh, J. L. Edwards, L. M. Ziurys
Figure caption: The composite 1 mm survey of NML Cyg covering the frequency range 214.5–285.5, plotted on a temperature scale (T A*) set by the strongest feature, CO, J = 2→1. Also prominent in the spectrum is HCN and SiO, while SO, SO2, and SiS have weaker emission.
Paper: The Arizona Radio Observatory 1 mm Spectral Survey of the Hypergiant Star NML Cygni (215–285 GHz)
Authors: A. P. Singh, J. L. Edwards, L. M. Ziurys
Figure caption: Spectra of CS (J = 5 → 4), SiS (J = 15 → 14), H2S (J Ka,Kc  =  22,0 → 21,1), SO2 (J Ka,Kc  =  43,1 → 42,2), SO2 (J Ka,Kc  =  52,4 → 41,3), and NaCl (J = 17 → 16), observed in the survey of NML Cyg (in black), overlayed with the model profile from the ESCAPADE analysis (in dashed red or gray scale). Temperature scale in T R (K). CS and SO2 was modeled with three velocity components (spherical outflow, redshifted wind, and blueshifted flow; see text), while NaCl, SiS, and H2S were fit with only a single, spherical component. The line profile of NaCl is narrower than the other molecules. Spectral resolution in 2 MHz.
Paper: The Arizona Radio Observatory 1 mm Spectral Survey of the Hypergiant Star NML Cygni (215–285 GHz)
Authors: A. P. Singh, J. L. Edwards, L. M. Ziurys
Figure caption: Radial abundance plots for the molecules in the blueshifted wind (upper) and redshifted flow (lower) for the envelope of NML Cyg, derived from the modeling. The abundances were extrapolated from their maximum values to f ∼ 10−10, assuming a distribution Gaussian centered at the peak (see text). As is evident in the figure, CO has the largest extent in these directed outflows, and is followed by HCO+. The three sulfur-bearing species CS, SO, and SO2 lie closer to the star and appear to have correlated abundances.
Paper: The Arizona Radio Observatory 1 mm Spectral Survey of the Hypergiant Star NML Cygni (215–285 GHz)
Authors: A. P. Singh, J. L. Edwards, L. M. Ziurys
Figure caption: Radial abundance plots for the molecules in the spherical outflow of the envelope of NML Cyg, derived from the modeling. The abundances were extrapolated from their maximum values at r inner to f ∼ 10−10, assuming a Gaussian centered at r inner (∼20 R *; see text). As the figure shows, CO, HCN, and H2S are the most extended molecules in the envelope.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Visual orbits of HD 61859 (top left), HD 89822 (top right), HD 109510 (bottom left), and HD 191692 (bottom right). The primary star is located at the origin (black cross). The relative positions of the secondary star from CLIMB data are marked by the gray points corresponding to the sizes of the error ellipses. The relative positions from MIRC-X data are marked by black circles with red error ellipses, which are often to small to be seen. The solid blue curves represent the best-fit model visual orbits, and thin black lines connect each observed and model position. The arrows indicate the directions of orbital motion.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption:  Radial velocity curves of HD 61859 (top left), HD 89822 (top right), HD 109510 (bottom left), and HD 191692 (bottom right). The observed data for the primary and secondary star are shown with the filled and open points, respectively. The triangles, diamonds, and circles represent the APO, CTIO, and Fairborn data, respectively. The model curves are shown with the solid lines, and the residuals to the fit are shown in the bottom panels.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Evolutionary tracks for HD 61859 (top left), HD 89822 (top right), HD 109510 (bottom left), and HD 191692 (bottom right). The observed stellar parameters are shown as the filled points for the primary stars and open points for the secondary stars. The Yonsei–Yale models are shown as dashed lines and the MESA models are shown as solid lines, with green for the primary and blue for the secondary. The crosses represent the position of the mean system age on each track.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: SEDs of HD 61859 (top left), HD 89822 (top right), HD 109510 (bottom left), and HD 191692 (bottom right). The observed fluxes are shown in black, and the best-fit binary model fluxes are shown as the red crosses. The full binary model is shown in gray. For clarity, we do not show the uncertainties in the Burnashev (1985) spectra of HD 109510.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Reconstructed spectra of HD 89822 around the Ca H & K lines (top), the Mg b triplet (middle), and Hα (bottom), for example. The reconstructed spectra are shown in black, and the best-fit model spectra are overplotted in green for the primary and blue for the secondary. In the top panel, lines relevant to HgMn and Am stars are labeled, including Ca K 3934 Å, a blend of Ca H 3969 Å with Hϵ 3970 Å, and Hg II 3984 Å. The Hg II line is much stronger in the primary star than in the models as expected for HgMn stars, and the Ca K line of the secondary component is much weaker than in the models as expected for metallic line stars.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Reconstructed spectra of HD 61859 around Hβ (top), the Mg b triplet (middle), and Hα (bottom), for example. The reconstructed spectra are shown in black, and the best-fit model spectra are overplotted in green for the primary and blue for the secondary.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Reconstructed spectra of HD 191692 around Hβ (top), the Mg b triplet (middle), and Hα (bottom), for example. The reconstructed spectra are shown in black, and the best-fit model spectra are overplotted in green for the primary and blue for the secondary.
Paper: Visual Orbits of Spectroscopic Binaries with the CHARA Array. IV. HD 61859, HD 89822, HD 109510, and HD 191692
Authors: Kathryn V. Lester, Gail H. Schaefer, Francis C. Fekel, Douglas R. Gies, Todd J. Henry, Wei-Chun Jao, Leonardo A. Paredes, Hodari-Sadiki Hubbard-James, Christopher D. Farrington, Kathryn D. Gordon, S. Drew Chojnowski, John D. Monnier, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Theo Ten Brummelaar, Claire L. Davies, Tyler Gardner, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Reconstructed spectra of HD 109510 around Hβ (top), the Mg b triplet (middle), and Hα (bottom), for example. The reconstructed spectra are shown in black, and the best-fit model spectra are overplotted in green for the primary and blue for the secondary.
Paper: Ephemerides of the Irregular Saturnian Satellites from Earth-based Astrometry and Cassini Imaging 
Authors: Robert A. Jacobson, Marina Brozović, Nickolaos Mastrodemos, Joseph E. Riedel, Scott S. Sheppard
Figure caption: (a) A single raw Cassini frame containing Ymir in 2 × 2 bin-addition mode showing severe radiation-induced signatures and noise. (b) A close-up view of the Ymir image in the same frame. (c) A closeup in a composite image of a dozen frames coregistered and added at the position of the first frame. (d) A single 7 minute exposure of Mundifari, showing the very long exposure tails of the stars Mundifari is near the center of the frame.
Paper: Ephemerides of the Irregular Saturnian Satellites from Earth-based Astrometry and Cassini Imaging 
Authors: Robert A. Jacobson, Marina Brozović, Nickolaos Mastrodemos, Joseph E. Riedel, Scott S. Sheppard
Figure caption: S/2004 S 31 Argument of Periapsis .
Paper: Ephemerides of the Irregular Saturnian Satellites from Earth-based Astrometry and Cassini Imaging 
Authors: Robert A. Jacobson, Marina Brozović, Nickolaos Mastrodemos, Joseph E. Riedel, Scott S. Sheppard
Figure caption: Kiviuq Argument of Periapsis.
Paper: Ephemerides of the Irregular Saturnian Satellites from Earth-based Astrometry and Cassini Imaging 
Authors: Robert A. Jacobson, Marina Brozović, Nickolaos Mastrodemos, Joseph E. Riedel, Scott S. Sheppard
Figure caption: Ijiraq Argument of Periapsis.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The overall SUPERBIT configuration bandpass that is constructed by taking the product of the throughput of all of SUPERBIT’s optical elements, filter transmission, and science camera quantum efficiency. The top panel shows the bandpass for the photometric bands U (330–430 nm), B(370–570 nm), G(520–700 nm), and R(640–800 nm). The bottom panel shows the bandpass for the broadbands L(400–700 nm) and S(530–830 nm). The flat configuration bandpass would be simple a series of horizontal lines at 0.5.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The median number of electrons per second from galaxies in the EL-COSMOS catalog for the SUPERBIT (blue) and flat (orange) configurations for all three observing environments. Note that due to identical atmospheric transmission curves, the values in orbit and stratosphere are identical.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The modeled number of electrons per second per pixel, generated on a detector by the sky background, for the SUPERBIT (blue) and flat (orange) instrument configurations, in all three observing environments.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The background flux density in units of ﹩\tfrac{\mathrm{photons}}{s\ {nm}\ {m}^{2}\ {\mathrm{arcsec}}^{2}}﹩ at the aperture for the three environments considered.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: Atmospheric transmission at an altitude of 5 km above sea level in desert conditions at mid-latitude winter, as calculated by the MODTRAN webapp.
Paper: The Detectability of Rocky Planet Surface and Atmosphere Composition with the JWST: The Case of LHS 3844b
Authors: Emily A. Whittaker, Matej Malik, Jegug Ih, Eliza M.-R. Kempton, Megan Mansfield, Jacob L. Bean, Edwin S. Kite, Daniel D. B. Koll, Timothy W. Cronin, Renyu Hu
Figure caption: Predicted Spitzer 4.5 μm eclipse depth for the explored atmospheric models in combination with a metal-rich surface as a function of the surface pressure compared to the Spitzer measurement (black horizontal line). Oxidizing/O2-dominated atmospheres are on the left and reducing/N2-dominated atmospheres on the right. The gray shaded area corresponds to a 1σ uncertainty, and the pink shaded area to a 3σ uncertainty in the negative direction from the observed value.
Paper: The Detectability of Rocky Planet Surface and Atmosphere Composition with the JWST: The Case of LHS 3844b
Authors: Emily A. Whittaker, Matej Malik, Jegug Ih, Eliza M.-R. Kempton, Megan Mansfield, Jacob L. Bean, Edwin S. Kite, Daniel D. B. Koll, Timothy W. Cronin, Renyu Hu
Figure caption: Secondary eclipse spectra for each of the tested surfaces and the gray albedo control case, shown at R = 100. The actual Spitzer 4.5 μm measurement is shown in black, where the y-axis error bar represents the uncertainty and the x-axis error bar represents the width of the bandpass. Modeled Spitzer points for each surface are shown in their respective color. We find the gray, metal-rich, iron-oxidized, and basaltic surfaces to be consistent (bold), i.e., <3σ from the observation, and the ultramafic, granitoid, and feldspathic surfaces to be inconsistent with the Spitzer measurement. The granitoid and feldspathic mock Spitzer points are almost directly overlapping.
Paper: The Detectability of Rocky Planet Surface and Atmosphere Composition with the JWST: The Case of LHS 3844b
Authors: Emily A. Whittaker, Matej Malik, Jegug Ih, Eliza M.-R. Kempton, Megan Mansfield, Jacob L. Bean, Edwin S. Kite, Daniel D. B. Koll, Timothy W. Cronin, Renyu Hu
Figure caption: Secondary eclipse spectra for each atmosphere and metal-rich surface model at the maximum surface pressure consistent with the Spitzer observation. On each plot, the spectrum labeled ”No Atmosphere” represents the surface-only spectrum for the metal-rich surface for comparison. The Spitzer 4.5 μm point is shown in black, where the y-axis error bar represents the uncertainty and the x-axis error bar represents the width of the bandpass. The atmospheric models with the largest features (bold) are used in the JWST observability analysis. No models are picked for the N2 with CO2 and the N2 with CO cases as the former is very similar to O2 with CO2 and the latter does not exhibit any noticeable features.
Paper: The Detectability of Rocky Planet Surface and Atmosphere Composition with the JWST: The Case of LHS 3844b
Authors: Emily A. Whittaker, Matej Malik, Jegug Ih, Eliza M.-R. Kempton, Megan Mansfield, Jacob L. Bean, Edwin S. Kite, Daniel D. B. Koll, Timothy W. Cronin, Renyu Hu
Figure caption: Secondary eclipse spectra of the surface-only models, mock data points for observations with the JWST MIRI LRS (left) and NIRSpec G395H (right), and corresponding blackbody fits. Shown here are the surfaces inconsistent with the Spitzer 4.5 μm eclipse depth. The mock data points are rebinned to R = 3 for the chi-square analysis and rebinned to R = 10 for the blackbody fitting. Error bars correspond to five eclipse observations. The model spectra are downsampled from their native resolution to R = 100 for clarity.
Paper: The Detectability of Rocky Planet Surface and Atmosphere Composition with the JWST: The Case of LHS 3844b
Authors: Emily A. Whittaker, Matej Malik, Jegug Ih, Eliza M.-R. Kempton, Megan Mansfield, Jacob L. Bean, Edwin S. Kite, Daniel D. B. Koll, Timothy W. Cronin, Renyu Hu
Figure caption: Number of secondary eclipse observations needed to distinguish the metal-rich and the granitoid surfaces as dependent on the binning resolution of the mock data. These two surfaces are used as an example pair to demonstrate the correlation between the resolution and eclipse number that is found to similarly hold for any surface pair. Eclipse observations with MIRI LRS are shown in cyan while observations with NIRSpec G395H are shown in dark gray.
Paper: The Detectability of Rocky Planet Surface and Atmosphere Composition with the JWST: The Case of LHS 3844b
Authors: Emily A. Whittaker, Matej Malik, Jegug Ih, Eliza M.-R. Kempton, Megan Mansfield, Jacob L. Bean, Edwin S. Kite, Daniel D. B. Koll, Timothy W. Cronin, Renyu Hu
Figure caption: Secondary eclipse spectra of the surface-only models, mock data points for observations with the JWST MIRI LRS (left) and NIRSpec G395H (right), and corresponding blackbody fits. Note that the blackbody models do not appear as smooth curves because the emitted flux is divided by the stellar spectrum model to obtain the eclipse depth. Only the surfaces consistent with the Spitzer 4.5 μm eclipse depth are shown here. The mock data points are rebinned to R = 3 for the chi-square analysis and rebinned to R = 10 for the blackbody fitting. The error bars correspond to five eclipse observations. The original model spectra are downsampled from their native resolution to R = 100 for clarity.