adsabs/AstroCLIMB huggingface dataset:
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Schematic depiction of the relative positions of the ascending node (Ω0 and Ω1), perihelion (p 0 and p 1), and the moving vernal equinox (ϒ0 and ϒ1) at two sequential points in time, controlled by the clockwise movement of the axial precession (Ψ) on the Earth-like planet. Their relative direction of movement is indicated with arrows. N-body simulations provide the angle (longitude) of the ascending node relative to a reference point (﹩{\rm{\Upsilon }}{{\prime} }_{0}﹩) on the reference plane with orbit normal (n). The reference point is the first point of Aries during the year 2000. The orbital inclination (i) is the angle between the plane of reference and orbital plane with normal (﹩n^{\prime} ﹩).
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: The difference in (a) the annual global mean air temperature (in °C) and (b) the annual mean sea ice extent (in %) between eight steady-state runs and transient snapshots corresponding to the four examples in Figure 8.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Duration of the climatic precession (left panel) and obliquity (right panel) cycles as a function of the dynamical ellipticity scaling factor, following Laskar et al. (1993a), for a simulation where Jupiter is located at it is current position with an eccentricity of 0.05. A scaling factor of 1.0 equates to a dynamical ellipticity of 0.00328 equal to the value for the modern Earth.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Three different measurements for studying the escape of Lyα in galaxies. Left: Lyα equivalent width, W Lyα . Middle: ratio of Lyα to [O II] luminosity. Right: escape fraction, ﹩{f}_{\mathrm{esc}}^{\mathrm{Ly}\alpha }﹩. The colors are the same as in Figure 6. The median values for LAEs and SFGs are indicated by dashed blue and gray vertical lines, respectively.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Dependence of W Lyα  (left) and Lyα/[O II] luminosity ratio (right) on the stellar mass (top) and SFR (bottom). The zLAEs, pLAEs, and continuum-selected SFGs are shown as filled blue squares, open blue circles, and gray crosses, respectively. The red square, red circle, and black cross along with their corresponding error bars are the median and interquartile range for the subsets.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Main panel: separation (d SFMS) of LAEs and SFGs from the SFMS parameterization by Shivaei et al. (2015) as a function of stellar mass. The colors and symbols are the same as in Figure 7. Top panel: histogram of stellar masses for the different samples of galaxies. Right panel: histogram of d SFMS for the different samples of galaxies.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Escape fraction as a function of SFR surface density, ΣSFR (left), and sSFR surface density, ΣsSFR (right). The filled squares and open circles are zLAEs and pLAEs, respectively. Low-mass LAEs (﹩\mathrm{log}\,[{\text{}}{M}_{\star }/{{M}}_{\odot }]\,\leqslant \,8.5﹩) are shown in blue, while high-mass LAEs (﹩\mathrm{log}\,[{\text{}}{M}_{\star }/{{M}}_{\odot }]\gt 8.5﹩) are shown in red. The black crosses are from Reddy et al. (2022) and computed using the composite spectra of the SFGs.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Equivalent width, W Lyα  (left); Lyα/[O II] luminosity ratio (middle); and escape fraction, ﹩{f}_{\mathrm{esc}}^{\mathrm{Ly}\alpha }﹩ (right), as a function of effective radius r  e . The symbols and colors are the same as in Figure 12. In each panel, the left and right stars are the median values for the unresolved and resolved sources, respectively. The error bars denote the interquartile ranges for the individual parameters.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Distribution of sizes (r  e ; left), SFR surface densities (ΣSFR;  middle), and sSFR surface densities (ΣsSFR;  right) of the LAEs. The colors are the same as in Figure 6. The upper limits on the sizes of the unresolved galaxies and the corresponding lower limits on the surface densities are shown as dotted histograms.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Predicted relationship between Lyα/[O II] and nebular metallicity, Z neb, based on CLOUDY (Ferland et al. 2013) photoionization modeling. This assumes the anticorrelation between the ionization parameter, ﹩\mathrm{log}({\rm{U}})﹩, and Z neb from Pérez-Montero (2014), with values of the former indicated at each point. See text for further details.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Distribution of W Lyα  (left), the Lyα/[O II] ratio (middle), and ﹩{f}_{\mathrm{esc}}^{\mathrm{Ly}\alpha }﹩ (right) for LAEs in the DENS (dark green histograms) and FIELD (light green histograms) regions. The black histograms with circles are 14 LAEs that have close neighbors or extended features as seen visually in the HST images.
Paper: The Orbits of the Main Saturnian Satellites, the Saturnian System Gravity Field, and the Orientation of Saturn’s Pole 
Authors: Robert. A. Jacobson
Figure caption: Mimas in-orbit differences from SAT427.
Paper: The Orbits of the Main Saturnian Satellites, the Saturnian System Gravity Field, and the Orientation of Saturn’s Pole 
Authors: Robert. A. Jacobson
Figure caption: Enceladus in-orbit differences from SAT427.
Paper: The Orbits of the Main Saturnian Satellites, the Saturnian System Gravity Field, and the Orientation of Saturn’s Pole 
Authors: Robert. A. Jacobson
Figure caption: Tethys in-orbit differences from SAT427.
Paper: The Orbits of the Main Saturnian Satellites, the Saturnian System Gravity Field, and the Orientation of Saturn’s Pole 
Authors: Robert. A. Jacobson
Figure caption: Dione in-orbit differences from SAT427.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Parameter space spanned by the clusters belonging to the CLUES sample (cyan stars). The clusters that pass the first selection (class 1 and 2 with mF275W < 18 mag, E(B − V) ≤ 0.3 mag, age ≤30 Myr) are shown in both panels as gray dots. The left panel shows the FUV color, F275W−F438W (or F435W) vs. the optical color, F555W (or F606W)−F814W, of the clusters. Yggdrasil evolutionary tracks spanning the metallicity range of the LEGUS sample are included, and the main age steps are outlined. The arrow shows in which direction clusters would move if corrected by an internal reddening corresponding to E(B − V) = 0.3 mag. In the right panel, we show the age vs. mass diagram of the sample. The violet band shows the detection limit corresponding mF275W = 18 mag as function of the metallicity (Z = 0.004 and 0.02) and distance range of the LEGUS galaxies.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: (Top panel) Ratio of light flux from the star cluster vs. the total flux within the COS aperture, for each of the HST filters indicated on the x-axis as well as for the fictitious FUV filter (Population 1 weight; see the text in Section 6.3). Each CLUES source is represented with a different marker. The colors of the markers and the lines divide the sources into three groups according to the age of Population I: <4 Myr (cyan), 4–10 Myr (olive green), and ≥10 Myr (red). (Bottom panel) Color–color plot V − I vs. U − B for both the light flux from the central star cluster (0.″2 radius aperture) marked in blue and the diffuse stars (outside the 0.″2 radius aperture and within the COS aperture) marked in orange. The black line marks the stellar track of a single stellar population with Z = 0.02, with the main age steps printed in black along the line. The reddening vector for E(B − V) = 0.1 is shown in red.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Values of the best-fit parameters for ages, metallicities, reddening attenuations, and masses of our different models. The gray dots represent the values derived from photometry. The blue and orange squares are the values for Population I and Population II, respectively, of our double-population model of the FUV spectroscopy, with their size proportional to their light flux contribution at 1270 Å. The green stars are the average values of our multiple-population model.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Two targets (M-74-YSC2 and NGC-1566-YSC2) as examples of the fits to the FUV spectra (black line) with the single/double-population model and the multipopulation model (purple and green lines, respectively). The two panels below each target show a zoom into the P-Cygni lines C III, N V, and C IV. The example targets chosen for this figure are a good and a poor agreement for the stellar age between single/double-population models and multipopulation models.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Overview of the CLUES sample. On top of the LEGUS F555W (F435W for M74) images of the targets, we mark with red circles the positions of the regions where FUV spectroscopy with COS has been acquired and presented in this work. Images are all rotated north-up, and intensities are in logarithmic scales. See Table 1 for a summary of the galactic properties.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: F275W images of the CLUES targets sorted by increasing cluster age as derived by FUV spectroscopy. The larger white circle represents the COS aperture of 2.″5 diameter, which corresponds to the physical size printed with the same color in each frame. The smaller red circle has a diameter of 0.″4 (physical size printed in red) within which lies the targeted YSC. The number at the end of the target name is the identifier of the cluster, as for most of the host galaxies, we have selected two YSCs as part of the CLUES sample. The targets with an asterisk (*) in front of their name have been observed using different position angles.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Atlas of the CLUES FUV spectra at 0.4 Å spectral resolution, sorted by age (see the text). The vertical dashed lines indicate some of the photospheric lines, stellar wind P-Cygni lines, and absorption lines due to the ISM along the line of sight. These marked lines are labeled on top of the figure. The regions of the spectra that are not included in our analysis such as the Lyα emission, the O I geocoronal line, and the detector gaps at about 1300 Å and 1600 Å are omitted for clarity. See Section 5 for the full description of the mask used when modeling the FUV spectroscopy.
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: Examples heat maps of the transit SDEs for the eight targets. The colors correspond to the SDE in the TLS (Hippke & Heller 2019a) test, with respect to the log-scale orbital period P orb and relative planetary radius R p/R s of the injected planet. The horizontal lines are the converted planet radii of Earth, Neptune, or Jupiter, which are included as guides. The vertical and horizontal dotted lines represent the rotational period and the square root of the flux variation semi-amplitude, respectively. The white line shows the boundary of SDE = 7 (the detection threshold). The photometric variation semi-amplitude, the rotation period, and the mean of the standard deviation in 0.3 day sized bins for the detrended light curves (A, P rot, σ 0.3day) of the targets are given at the top of the panels. The black star on the panel for EPIC 211120664 is a projection of K2-25 b, whose host star is the fastest rotator in confirmed planetary systems and shows similar light-curve modulation to EPIC 211120664.
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 colored by cluster. Panels (a), (b), and (c) plot the recovery rate p (the relative number of recovered tests to all tests) using the 10 × 10 planetary parameters vs. the effective temperature, the rotation period, and the semi-amplitude of the photometric variation of the host stars, respectively. Panel (d) plots the semi-amplitude of the variation vs. the rotation period.
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: Upper panels: scatter plots of the rotation period vs. the apparent Kp magnitude for stars with 3000–4000 K in four clusters. Lower panels: histograms of the rotation periods in the clusters. The gray and blue data indicate original members in the literature and selected targets in this study, respectively.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Continuation of Figure 9.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Weight of the FUV-dominant stellar population as a function of the distance of the target galaxy, color coded with the age of the stellar population. A different marker is used for each source, as listed in the legend.
Paper: CLusters in the UV as EngineS (CLUES). I. Survey Presentation and FUV Spectral Analysis of the Stellar Light
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Shannon Osborne, Svea Hernandez, John Chisholm, Matteo Messa, Linda J. Smith, Alessandra Aloisi, Aida Wofford, Andrew J. Fox, Andrew Mizener, Christopher Usher, Arjan Bik, Daniela Calzetti, Elena Sabbi, Eva Schinnerer, Göran Östlin, Kathryn Grasha, Michele Cignoni, Michele Fumagalli
Figure caption: Fits to the FUV spectra of the CLUES sample (black line) with the double-population model and the multipopulation model (purple and green lines, 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: Light curves and TLS results for EPIC 211000411, EPIC 210892390, and EPIC 210947895. For each target, from top to bottom, we show the light curve after the subtraction of long-term modulation and the light curves detrended with FFT + 1 day median filtering, FFT + 0.3 day median filtering, only the 0.3 day median filtering, the 0.3 day biweight filtering, and the 0.3 Huber spline detrending; from left to right, we show overall and close-up views of the light curves as well as the TLS periodogram. In the middle column, we indicate transit signals with the orange lines; in the right column, the horizontal dashed line represents the SDE of 7.
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:  T eff vs. R p/R s plot, when R p = 3R ⊕, with Mann et al. (2015; solid lines) and MIST (Choi et al. 2016; Dotter 2016; dashed lines); the black and orange lines represent 10 Myr and 100 Myr, 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 SDE map for EPIC 211150528, which is a rapidly rotating target, for comparison with the lower panels of Figure 7 in Rizzuto et al. (2017).
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: Comparisons of the results from the 10 × 10 (Figure 2) and 30 × 30 simulations for EPIC 211000411, EPIC 210892390, and EPIC 210947895.
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: Left: Bond albedo vs. inferred albedo for simulated MIRI LRS data at R = 10. The black dotted line represents the location where the inferred and Bond albedos are equal. The inferred albedo is determined using once the full spectrum (i.e., both planetary emission and reflected light contributions) and once the emitted radiation only. The nominal case uses the full spectrum. Right: analogous to the left panel but using simulated NIRSpec G395H data at R = 10.
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 atmospheric models vs. surface-only models, overlaid with MIRI LRS (left) and NIRSpec G395H (right) simulated data points at R = 10 over the whole instrument bandpass. The metal-rich surface is used for this test. The error bars show the uncertainties for five eclipse observations. The model spectra are downsampled from the 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: Posterior distributions of retrieved volume mixing ratios using atmospheric forward models without a nongray surface. The retrieved mean and 1σ width are given on top of each panel and shown with black solid and dashed vertical lines. The input mixing ratio (the “true” value) is shown as a red vertical line. The corresponding T–P profiles are shown on the right with the input profile (from the forward model) in blue, and the profiles realizations from the retrieval modeling are shown as red lines.
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: Left: Bond albedo vs. inferred albedo for simulated MIRI LRS data at R = 10. The black dotted line represents the location where the inferred and Bond albedos are equal. Three values of emissivity, 1.0, 0.9, and 0.7, are assumed for the planetary emission when inferring the temperature and the albedo. The nominal value used is 1.0. Right: analogous to the left panel but using simulated NIRSpec G395H data at R = 10.
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: Same as Figure C8 but showing here the retrieval results using the surface-only (no atmosphere) forward models with different surface crusts.