adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: The left and middle panels show the dereddened CMDs of all stars within one half-light radius from the center of Cas III. The 50% completeness curve is marked with a dashed line in the left panel, and the typical photometric uncertainties at each magnitude are plotted in all three panels. Isochrones from Dotter et al. (2008) for an age of 12 Gyr and [Fe/H] values of −2.5, −2.0, −1.5, and −1.0 are marked (green lines) in the middle panel. The middle and right panels show the RGB selection box (red polygon). The right panel shows the CMD of stars within the rectangular background regions marked in Figure 5, with the numbers of sources rescaled so that the CMDs sample the same areas (see Section 4.1 for details).
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Spatial locations across the WIYN pODI field of view of the 5725 RGB star candidates selected from Cas III’s CMD (Figure 3). The positions of the stars are plotted in standard coordinates with respect to the galaxy center. The half-light radius derived in Section 4.3 is marked with a dashed ellipse, and the area of the image used to create the field CMD and measure the background density is shown as a blue rectangle. A red arrow indicates the direction to M31.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Spatial locations across the WIYN pODI field of view of the 1817 RGB star candidates selected from Per I’s CMD (Figure 4). The stars’ positions are shown in standard coordinates with respect to the center of Per I. The dashed ellipse marks the half-light radius derived in Section 4.3, and the blue rectangles show the regions used to create the field CMD. The red arrow shows the direction to M31.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: The left and middle panels show the dereddened CMDs of all stars within one half-light radius of the center of Per I. The right panel shows the CMD of stars in the rectangular background regions marked in Figure 6. The 50% completeness level, photometric uncertainties, RGB selection box, and isochrones are plotted in the figures in the same way as in Figure 3.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Surface density vs. elliptical radius for the RGB candidate stars in Per I, plotted in the same way as in Figure 7. The best-fitting exponential function appears in the left panel, and the best-fitting Sérsic function with n = 0.7 appears in the right panel.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Surface density of the RGB candidate stars in Lac I as a function of elliptical radius. The solid black line is the best-fitting function derived from the MLE process described in Section 4.3.1; the left panel shows the exponential function, and the right shows the Sérsic function with n = 0.83. Open diamonds indicate the surface density within each elliptical bin. The dashed line indicates the background surface density.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Example of the χ 2 selection criteria applied to the source lists for Cas III and Per I. The χ 2 value from DAOPHOT is plotted vs. i 0 magnitude; objects that we select are shown in red, and those in black are discarded.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Example of the selection criteria applied to the DAOPHOT photometry lists for Cas III and Per I. The sharp parameter is shown as a function of calibrated i 0 magnitude; selected objects are plotted in red, and rejected ones appear in black.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Surface density of RGB candidates in Cas III as a function of elliptical radius, plotted in the same way as in Figure 7. The exponential fit with n = 1 is shown on the left, and on the right is the Sérsic function fit with n = 0.57.
Paper: GJ 357 d: Potentially Habitable World or Agent of Chaos?
Authors: Stephen R. Kane, Tara Fetherolf
Figure caption: Eccentricity evolution over 106 yr for the three known GJ 357 planets and the injected planet for the case of M  p,d  = 6.1 M ⊕ and e  d  = 0.0 and the inserted planet at a semimajor axis of 0.225 au.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Spectra confidence intervals for N2–CO swap retrievals. Although both retrievals had true values of N2 = 0.78 and CO = 1.e-7, only the partial pressure retrieval was able to calculate accurate results. We see the N2–CO VMR retrieval sampled many iterations with a high CO abundance evidenced by the absorption feature at ∼1.6 μm.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Spectra comparison of different surface temperatures on our observed exoplanet. Our nominal model fixes the temperature as outlined in Section 2, t0 = 294 K.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: True 0.2–1.1 μm N2-dominated planet-to-star flux ratio spectrum (top) and CO-dominated spectrum (bottom) plotted against 1000 randomly sampled retrieved spectra with 95% confidence intervals.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Gas-pressure corner plots of N2-dominated (left) and CO-dominated (right) partial pressure retrievals with gas values shown as mixing ratios.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: N2–CO swap retrieval corner plots. The VMR retrieval could not constrain either N2 or CO accurately for the swapped case.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Partial pressure CO-dominated retrieval corner plot with gas abundances shown in their VMR values.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: N2-dominated partial pressure retrievals’ 95% confidence intervals with different S/Ns.
Paper: Constraining Background N2 Inventories on Directly Imaged Terrestrial Exoplanets to Rule Out O2 False Positives
Authors: Sawyer Hall, Joshua Krissansen-Totton, Tyler Robinson, Arnaud Salvador, Jonathan J. Fortney
Figure caption: Partial pressure CO-dominated retrieval full corner plot.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: The Galactic orbit of King 6 (panels (a)–(b)) and NGC 1605 (panels (c)–(d)) in the Z × R GC and R GC × t planes. The filled yellow circles are the present-day positions of the clusters. The triangle symbols indicate the birth positions. The red arrows show the motion vectors of the clusters. The pink and green dotted lines show the orbits when errors in the input parameters are considered. The pink filled triangles represent the birth locations of the clusters based on the upper error estimates, while the green filled triangles represent the birth locations based on the lower error estimates.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: The (U − B)0×(B − V)0 TCDs (upper panels) and histograms for the normalized δ 0.6 (lower panels) for 15 (King 6, panel (a)) and seven (NGC 1605, panel (b)) F- and G-type main-sequence stars statistically consider the most probably cluster members. The solid blue lines in the TCDs represent the main sequence of Hyades (in the upper subfigures) and Gaussian fits (in the lower subfigures).
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption:  UBV- and Gaia-based CMDs for the King 6 (panels (a), (b), and (c)) and NGC 1605 (panels (d), (e), and (f)) OCs. Membership probabilities of the most probable cluster stars are represented with different color scales that are shown by the color bars to the right, whereas field stars are shown as gray-colored dots. The best-fitting PARSEC isochrones and their errors are presented as the blue and green lines, respectively. Superimposed isochrone ages match to 200 Myr for King 6 and 400 Myr for NGC 1605.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: Gaia DR3-based trigonometric parallax histograms for King 6 (a) and NGC 1605 (b). The red dashed curve shows the Gaussian fit applied to the distributions.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: The (U − B) × (B − V) diagrams of King 6 (a) and NGC 1605 (b). The red dashed lines plot the dereddened ZAMS given by Sung et al. (2013). The green solid lines indicate the ±1σ standard deviation range limits. The reddening vector is represented by the dashed gray line.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: MFs of King 6 (a) and NGC 1605 (b). Blue lines show the MFs of the OCs, while green lines are the ±1σ standard deviations. The gray dashed lines in the panels represent the slope of Salpeter (1955).
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: The LFs for the King 6 (a) and NGC 1605 (b) OCs.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: The cumulative radial distribution of stars in different mass ranges for King 6 (a) and NGC 1605 (b).
Paper: Point Source C-band Mueller Matrices for the Green Bank Telescope
Authors: Paul Fallon, Derck P. Smits, Tapasi Ghosh, Christopher J. Salter, Pedro Salas
Figure caption: (a) Observed 3C 138 fractional Stokes parameters as a function of PA, fitted with Mueller matrix equations using solid line. The Lo-Cal ND observations are shown with larger symbols and dotted–dashed lines, and indicate a difference with the Hi-Cal ND results. Because all the Lo-Cal Q/I, U/I and V/I parameters are fitted simultaneously, the Lo-Cal Q/I and U/I values are offset from the calculated curve. (b) Differences between the observed and fitted fractional Stokes parameters for the Hi-Cal ND data points, indicating no systematic variation. The vertical scale is different to that in Figure 1(b) which has more scatter.
Paper: Point Source C-band Mueller Matrices for the Green Bank Telescope
Authors: Paul Fallon, Derck P. Smits, Tapasi Ghosh, Christopher J. Salter, Pedro Salas
Figure caption: Mueller matrix parameters as a function of frequency. (a) ΔG/2, (b) ψ, with a linear best fit through all the data points. The linear fit has values of 190.95 − 1.2067 × Frequency (GHz), (c) 2α, (d) 2ϵ, and (e) ϕ.
Paper: Point Source C-band Mueller Matrices for the Green Bank Telescope
Authors: Paul Fallon, Derck P. Smits, Tapasi Ghosh, Christopher J. Salter, Pedro Salas
Figure caption: Source Stokes parameters for (a) 3C 286 and (b) 3C 138 for the observed C-band frequencies. The points are average values from the frequency set of Spider scans. The error bars are the standard error of the mean and, for the Spider scan (Hi-Cal ND) data, are smaller than the plotted symbols; because the top and bottom of the error bar are almost on top of one another in some cases, the error bar appears as a single horizontal line. Figure (b) includes values from the Lo-Cal ND calibrator observations. Note that the Lo-Cal data points for the evenly spaced frequencies have been offset to the right by 30 MHz so that they do not lie on top of the Hi-Cal points.
Paper: Point Source C-band Mueller Matrices for the Green Bank Telescope
Authors: Paul Fallon, Derck P. Smits, Tapasi Ghosh, Christopher J. Salter, Pedro Salas
Figure caption: Polarization values as a function of frequency for (a) 3C 286 and (b) 3C 138. The points are average values and the error bars are the standard error of the mean from all the Spider scan observations, using Equation (6) to obtain source Stokes parameters. The NRAO reference values are the current polarization values on the NRAO website (see footnote 7).
Paper: Point Source C-band Mueller Matrices for the Green Bank Telescope
Authors: Paul Fallon, Derck P. Smits, Tapasi Ghosh, Christopher J. Salter, Pedro Salas
Figure caption: (a) Observed 3C 286 fractional Stokes parameters as a function of PA fitted with Mueller matrix equations. (b) Differences between the observed and fitted fractional Stokes parameters, indicating no systematic variation.
Paper: Point Source C-band Mueller Matrices for the Green Bank Telescope
Authors: Paul Fallon, Derck P. Smits, Tapasi Ghosh, Christopher J. Salter, Pedro Salas
Figure caption: Source Stokes parameters for (a) 3C 286 and (b) 3C 138 calculated by applying Equation (6) to the observed values in Figures 1 and 2. The 3C 286 data shows some noise at PAs above and below 40°, this noise is seen in the observed fractional Stokes parameters in Figure 1.
Paper: Point Source C-band Mueller Matrices for the Green Bank Telescope
Authors: Paul Fallon, Derck P. Smits, Tapasi Ghosh, Christopher J. Salter, Pedro Salas
Figure caption: Polarization values for 3C 286 as a function of frequency (a) polarization angle and (b) linear polarization fraction. The graphs compare the frequency bespoke Mueller matrix analysis outcomes shown in Figure 5(a) with the results of using the generic Mueller matrix to determine the polarization.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Interpolation error across the parameter space. The blue curves represent the maximum interpolation error at each point in the parameter space over all off-axis parameters. The nonblue curves are created by sequentially filtering out all values other than an Earth-like value for each respective parameter (other parameters are not filtered unless noted). The locked parameters are set to Earth-like values (also listed in Table 3) of 0.002 for H2O, 1.205 for P 0, 7.796 × 10−7 for O3, 0.301 for O2, 10.642 for g, and 0.311 for A  s  and are represented by vertical black dashed lines. These are points on the test grid that are closest to realistic Earth-like values. The parameters are locked in descending order of impact on the maximum interpolation error SSE. The top left panel is the maximum interpolation SSE with no parameters locked; the top right panel adds the effect of locking P 0; the middle left panel adds the effect of locking O3; the middle right, bottom left, and bottom right panels add the effects of locking A  s , g, and H2O, respectively (the maximum interpolation SSE with P 0, O3, A  s , g, and H2O locked is entirely in line with the curve with P 0, O3, A  s , and g locked).
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: 2D posteriors of O3 and P 0 resulting from two separate 6D retrievals of data spectra both with O3 = 0.014. The corner plot on the left shows a retrieval with a low true surface pressure (P 0 = 0.0068), while the panel on the right shows a retrieval with an Earth-like value for the true surface pressure (P 0 = 1.2). The true and retrieved (median) values are shown as blue and orange vertical lines, respectively. The retrieval algorithm fails to recover the correct O3 and P 0, and it converges to several other solutions when O3 is high and P 0 is low but is more accurate when both O3 and P 0 are high.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: 6D retrieval evaluations showing the retrieval error across the parameter space. The retrieval error is defined as the absolute difference between the true and retrieved values. Blue points represent retrievals performed using an interpolated data spectrum, while orange points represent retrievals performed using true data spectra. Error bars on these points are drawn as the 68% credible regions. The left column shows the full extent of the y-axes, while the right column zooms in to the portion of the y-axes contained within the horizontal dashed black lines.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Number of forward-model evaluations of PSGnest for two-parameter (F18's Figure 7) and seven-parameter (F18's Figure 9) retrievals by number of live points. The number of live points is directly correlated with the completeness of the posterior’s sampling, but too many can increase the run time of the retrieval (proxied here by the number of forward-model evaluations) without significantly changing retrieval results. We found that 400 live points (marked with a vertical dashed line) is enough to sufficiently sample the posteriors and that a number of live points beyond this does not noticeably change the results.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Grid spectra at extreme parameter values compared to the fiducial baseline spectrum (﹩{\mathrm{log}}_{10}{{\rm{H}}}_{2}{\rm{O}}﹩ = ﹩-2.52,{\mathrm{log}}_{10}{P}_{0}﹩ = ﹩0.0,{\mathrm{log}}_{10}{{\rm{O}}}_{3}﹩ = ﹩-6.15,{\mathrm{log}}_{10}{{\rm{O}}}_{2}﹩ =﹩-0.68,{\mathrm{log}}_{10}g=0.99,{A}_{s}﹩=0.05). In each panel, only the parameter noted in the upper center legend is changed. The lower ﹩{\mathrm{log}}_{10}{P}_{0}﹩ spectrum was set to −1.11 rather than the grid’s minimum extreme of −3 because spectra with ﹩{\mathrm{log}}_{10}{P}_{0}\lessapprox -1.11﹩ appear as flat lines with geometric albedo ≈0.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Reproduction of F18's Figure 8 using PSGnest.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Reproduction of F18's Figure 9 using PSGnest.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Three steps in the grid construction process for H2O. Each step adds one grid point, with step 1 beginning with two grid points. The top panel shows the initial state (step 1), the middle panel an intermediate state (step 6), and the third panel the final grid point configuration (step 12). Each grid point is represented by a blue vertical line. Each black point is the maximum error for the particular H2O value across all other off-axis parameter values. The horizontal red dashed line is the 10% error threshold.
Paper: Grid-based Atmospheric Retrievals for Reflected-light Spectra of Exoplanets Using PSGnest
Authors: Nicholas Susemiehl, Avi M. Mandell, Geronimo L. Villanueva, Giuliano Liuzzi, Michael Moore, Tyler Baines, Michael D. Himes, Adam J. R. W. Smith
Figure caption: Reproduction of F18's Figure 7 using PSGnest.