adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Orbital properties of five stars in the Lindblad diagram. Color-coded distribution of stellar angular momentum (Ltot) over the Milky Way stellar density map, with colored circles marking GC positions in the Galaxy (left panel). The same diagram is color-coded according to metallicity (right panel). The overplotted labeled markers indicate the positions of the selected stars (HD 122956, HD 189349, HD 005916, HD 122956, and HD 218857) used in this study. The vertical dashed line corresponds to Lz = 0, which separates prograde (right) and retrograde (left) orbits.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Toomre diagram for five HPM stars. The solid red isovelocity curves represent constant total space velocities from 50 to 500 steps of 50 km s−1. The vertical gray band corresponds to a velocity of SLSR = −230 ± 10 km s−1 (L. Necib & T. Lin 2022). Stars are classified as retrograde if their velocity relative to the LSR satisfies VLSR < −230 km s−1, whereas stars with VLSR ≥ −230 km s−1 are considered prograde in the Galaxy. Background blue points represent APOGEE DR17 stars selected using quality cuts as described in the text.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Distribution of selected stars in the [Mg/Mn] vs. [Al/Fe] abundance plane. The solid black lines indicate the empirical separation between the in situ and ex situ stellar populations, as proposed in recent chemical tagging studies. The colored error bars denote individual stars, with labels corresponding to their HD catalog numbers. The dashed horizontal line at [Mg/Mn] = 0.3 dex separates high-α and low-α populations, highlighted in red and blue, respectively. Background blue points represent APOGEE DR17 stars selected using quality cuts as described in the text.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Abundance ratios of α-elements ([Mg/Fe], [Si/Fe], [Ca/Fe], and [Ti I/Fe]) as a function of metallicity ([Fe/H]) for stars analyzed in this study (green diamonds with error bars and numbered from 1 to 5, in order of increasing metallicity: HD 2665 (1), HD 218857 (2), HD 122956 (3), HD 189349 (4), and HD 5916 (5)) compared to literature data. The data from J. P. Fulbright (2000) are shown as pink crosses, and the magenta squares indicate the mean values for metal-poor dwarfs from J. P. Fulbright (2000). The blue downward triangles represent halo stars from T. Bensby et al. (2014), and their mean values are shown as larger blue symbols. Black dots represent thick disk stars from T. Bensby et al. (2014), and large black dots indicate the average abundances in 0.25 dex intervals of [Fe/H] for thick disk stars. Individual error bars in the [X/Fe] axis for the metal-poor HPM stars are also indicated.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Comparison of elemental abundance ratios [X/Fe] for the five program stars analyzed in this study (purple stars with error bars) against values compiled from the literature (cyan circles). Each panel corresponds to a different star, with the vertical axis listing the atomic species and the horizontal axis representing the [X/Fe] abundance ratio in dex units. Error bars indicate the ±1σ uncertainties of the measurements derived in this study. For elements for which both neutral and ionized species are available (e.g., Ti I, Ti II, Cr I, and Cr II), we included all individual measurements as well as their averaged abundances. The combined [X/Fe] values are shown to facilitate comparison with literature studies that report only averaged quantities.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption:  ﹩{Z}_{{\rm{\max }}}\times {e}_{{\rm{p}}}﹩ diagram for five stars. The stars are color-coded according to their metallicities. Background blue points represent APOGEE DR17 stars selected using quality cuts as described in the text.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Comparison of atmospheric parameters for the five program stars derived in this study (red stars) with values from the literature (green circles) and the Gaia DR3 catalog (blue circles). From top to bottom, the panels show the effective temperature (Teff), surface gravity (﹩{\mathrm{log}}\,g﹩), and metallicity ([Fe/H]). The shaded background bands alternate for clarity between adjacent stars.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Likelihood of stars encountering various GCs, based on spatial and velocity parameters. The matrix displays three key probability values: spatial probability (P(θ)), velocity probability (P(ν)), and combined probability (P(origin∣θ, ν)) for each cluster. Colors in the matrix reflect the probability values, as indicated by the scale.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Comparison of observed (black dotted) and synthetic (blue) spectra for Mg I and Mn I lines in the program stars HD 189349, HD 2665, HD 122956, HD 5916, and HD 218857. The spectral regions shown include the Mg I and Mn I lines. Derived logarithmic abundances (﹩{\mathrm{log}}\,\epsilon ﹩) for Mg I and Mn I are also indicated.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Predicted TTVs for planets g (left) and h (right) through 30 transits, starting from the first epoch of the Kepler data and modeled using TTVfaster with the best joint fit parameters (bold line) and the Monte Carlo distribution (gray lines, N = 6438). The linear ephemerides used here for each planet are those of the best fit to the joint RV and Kepler TTV model. The four non-Kepler transits reported in this work (see Section 2.1) lie within the range of expected O-C values from our results. The max spread in modeled transit times for the final predicted epoch (29) is 6.65 d for K90g and 1.21 d for K90h. The revised linear ephemeris for planet g, including post-Kepler transits (dotted–dashed line), shows the preference for a longer period than that suggested by the RV and Kepler data alone.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Distributions of average orbital periods for K90g (left) and K90h (right) from our joint RV-TTV model, including only Kepler transits (blue) and all transits (orange). The histograms are normalized to unit area for consistent comparison. The full data set’s distributions are difficult to visualize when shown on the same scale as those of the Kepler-only data set, so we present a more narrow binning window in the insets of each plot. We overlay normal distributions with mean and standard deviation equal to the values reported in Table 4 (which represent the 16th, 50th, and 84th percentiles of the distributions) to show the Gaussian nature of our MCMC posteriors derived from the full data set.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Distributions of masses for K90g (left) and K90h (right) from four different models: the joint RV-TTV data set with only Kepler transits (blue), the joint RV-TTV data set with all transits (orange), the TTV-only data set, including post-Kepler transits (purple), and the RV-only data set (green). The posterior mass distributions of the full RV-TTV analysis are nearly identical to those of the TTV-only analysis. The histograms are all normalized to unit area for consistent comparison. As in Figure 7, normal distributions with mean and standard deviations taken from Table 4 are plotted over joint RV-TTV distributions in the inset for K90g.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Minimum RV and Kepler TTV ﹩{\chi }_{{\rm{joint}}}^{2* }﹩ values (Equations (2) + (3) with fixed best-fit σjitter) projected onto the 1D parameter subspaces for the masses of K90g (left) and K90h (right). In each case, the mass was held fixed at a given value while ﹩{\chi }_{{\rm{joint}}}^{2}﹩ was minimized as described in Section 3.2. The resulting change in ﹩{\chi }_{\mathrm{joint}}^{2* }﹩ above the minimum approximately follows a χ2 distribution with one degree of freedom, giving 1σ confidence limits on the masses of planets g (﹩{M}_{g}=17.{0}_{-3.1}^{+3.9}﹩M⊕) and h (﹩{M}_{h}=21{2}_{-20}^{+21}﹩M⊕).
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Kepler-90 photometry from the SG1 collaboration capturing ingress and egress of K90g between UT 2024 May 25 and 2024 May 29. The preliminary transit midpoint of ﹩2460458.72405{4}_{-0.00330}^{+0.00164}﹩ BJD-TDB at epoch 26 occurred approximately 1.4 days later than predicted by our model (Figure 6). This transit delay is consistent with other post-Kepler observations in suggesting that our best-fit period for planet g from the RV and Kepler data alone is shorter than the true value. The observations from these various facilities are described in Section 4.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: (Top) Lomb–Scargle (LS) periodogram of the 34 RV measurements over an orbital period range of 2–5000  days. There is a clear peak in power near the orbital period of planet h, while no other signal is detected above a 1% false-alarm probability. (Middle) LS periodogram of residual RV data after subtraction of planet h’s RV model based on the best-fit parameters. Even after subtraction, no clear signal is seen at the period of planet g. (Bottom) LS periodogram of residual RV data after subtraction of both planet h and g’s RV models based on best joint fit parameters. The power peak at 2.77 days is not from any known planet and is likely from noise and/or aliasing.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Predicted TTVs for 35 epochs of K90g as in Figure 6 but with our joint model fit to all RVs and TTVs, including post-Kepler observations. The solid line shows the best-fit solution, and the gray lines correspond to 1000 draws from the MCMC posteriors. These predictions extend through 2029 January.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Observed RVs for Kepler-90 as in Figure 2, but with our joint model fit to all RVs and TTVs, including post-Kepler observations. The solid red line shows the best-fit solution, and the gray dashed lines correspond to 1000 draws from the MCMC posteriors.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Same as Figure 9 but for planet h. The predictions extend through 2040 April.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: R-band photometric variability of V1298 Tau observed using the ground-based TSU C14 0.36 m AIT at Fairborn Observatory (gray points). See Section 2.2 and Appendix G for further details of the ground-based monitoring observations. We show observations from Sectors 2 and 5 from this monitoring campaign, which coincided with the HST (left) and JWST (right) observations. We have assumed the median of the two epochs as the quiescent stellar flux and subtracted it. We have scaled the R-band variability to the median HST (1.35 μm) and JWST/NIRSpec NRS2 (4.5 μm) wavelengths, respectively, using the formalism outlined in J. M. Désert et al. (2011b). We assume a photosphere temperature of 5000 K (T. J. David et al. 2019a) and a spot temperature of 4000 K (A. Biagini et al. 2024). The scaled variability in the two bands is shown with a blue dashed line. The solid red lines show the stellar baseline (derived from the respective best-fit white light curves) during the HST/JWST observations. These baselines have been median subtracted and vertically offset for visual comparison with the scaled relative variability model.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Comparison between metallicity (solar units) and C/O ratio derived from the PICASSO free atmospheric chemistry retrieval performed on the combined HST and JWST transmission spectrum of V1298 Tau b (Appendix D) and the best-fit PICASSO grid model (Appendix E). The red contours are from the free retrieval, and the blue square represents the estimate from the grid fit. The contours represent 1σ level confidence intervals. The retrieved atmospheric parameters from both the free retrieval and grid fit are given in Table 1. The blue dots show the spacing of the grid used (see Appendix E). We find that both the metallicities and the C/O ratio are consistent within a 1σ level of confidence between the free retrieval and the grid.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Internal temperature for V1298 Tau b for different values of tidal quality factor (log Q) and planetary spin axis obliquity. The tidal heating luminosity has been derived using the formalism outlined in S. Millholland (2019), S. Millholland et al. (2020; see Appendix I). To estimate the total, we add the energy of formation derived using scaling relations from L. A. Rogers & S. Seager (2010) to tidal luminosity. We convert the luminosity to an internal temperature assuming a blackbody function and a planet radius equal to the radius of the radiative–convective boundary calculated in Figure 12. We assume 1% eccentricity based on ongoing TTV modeling efforts (J. Livingston 2025, private communication). We require very high spin–orbit obliquities (>80∘) and very low tidal quality factor (<100) to reproduce internal temperatures higher than 400 K.
Paper: Photometric Mapping of Carbonaceous/Siliceous Dust and Water Ice in the ISM with JWST: Applications to the Dense Sightlines
Authors: Burcu Günay, Karl D. Gordon, Joshua E. G. Peek, Marjorie Decleir, Dries Van De Putte, Kirill Tchernyshyov, Michael G. Burton
Figure caption: The BBs (without absorption, τ0 = 0) are used to derive correlations between spectral index values and differences arising from the linear continuum fit approximation. The optical depths at 3.0 μm, 3.35 μm, and 10.0 μ are measured. The model spectra set was generated using a polynomial fit to the observational spectra set ([G04]) that exhibit different slope values in the NIR (αNIR) and MIR (αMIR), covering αNIR from −2.2 to 9.3 and αMIR from −0.1 to 3.3. The slope (α) of each spectrum was used to estimate linear continuum fit related differences (Δτcont.) in the optical depth values based on the correlations between α and Δτcont. derived using BBs. Comparative models include BBs at T = 500 K (αNIR = 6.1, αMIR = 0.1), 3000 K (αNIR = −1.1, αMIR = −1.7), and 10,000 K (αNIR = −1.8, αMIR = −1.9) are also presented. The names of selected sources are labeled to indicate variations in slope levels.
Paper: Photometric Mapping of Carbonaceous/Siliceous Dust and Water Ice in the ISM with JWST: Applications to the Dense Sightlines
Authors: Burcu Günay, Karl D. Gordon, Joshua E. G. Peek, Marjorie Decleir, Dries Van De Putte, Kirill Tchernyshyov, Michael G. Burton
Figure caption: The photometric optical depths and spectroscopic optical depths are compared to investigate deviations across the applied optical depth ranges (τ0[3.0] = 0–2, τ0[3.4] = 0–1, and τ0[10.0] = 0–2.5). The optical depths obtained with standard spectra model parameters are indicated with blue, gray, and green solid lines for the water ice, aliphatic hydrocarbons, and silicate features, respectively. Upper panels: optical depths compared using exploratory spectral models created with CW shifts. The optical depths obtained with shifted CWs to shorter and longer wavelengths are indicated in blue and red, respectively. Bottom panels: optical depths compared using exploratory spectral models created with FWHM variations. The optical depths obtained with narrower and broader FWHMs are indicated in blue and red, respectively. The CW and FWHM values applied in exploratory models are summarized in Table 3.