adsabs/AstroCLIMB huggingface dataset:
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: Top two panels: a comparison of the density of MPCORB objects with those objects that were matched in S3M by our hybrid catalog pipeline. Bottom panel: residuals between the two plots above.
Paper: Expected Impact of Rubin Observatory LSST on NEO Follow-up
Authors: Tom Wagg, Mario Juric, Peter Yoachim, Jake Kurlander, Sam Cornwall, Joachim Moeyens, Siegfried Eggl, R. Lynne Jones, Peter Birtwhistle
Figure caption: A comparison of the parameter distributions of S3M (T. Grav et al. 2011) and the hybrid catalog we created.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Spectral contamination model of Roman grism simulation. The panels show: (a) the reference image, the same direct image used to simulate the grism image; (b) the simulated grism image; (c) the spectral contamination model derived from the direct image and polynomial fits for the spectra for all objects; (d) the residuals after subtracting the contamination model from the simulated grism image.
Paper: Simulating Continuum-based Redshift Measurement in the Roman’s High Latitude Spectroscopic Survey
Authors: Zhiyuan Guo, 致远 郭, Bhavin Joshi, C. W. Walter, M. A. Troxel
Figure caption: Roman WFI grism sensitivity functions for the first spectral order (1–1). The gray dashed horizontal line marks the redshift range of the 4000 Å break (red) and Balmer break (blue) covered by Roman grism as the galaxy spectra get redshifted.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Progressive brightening of the central stellar position along wavelength, with respect to the optically brightest clump located at ∼0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩4 to the southwest. (a)–(c) HST images taken on 2016 May 17 with F606W, F814W, and F098M filters displayed in linear scales in units of Jy pixel−1 with a regridded pixel size of 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩04 × 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩04 (see H. Kim et al. 2021). (d)–(e) Gemini images in the NIFS J data cube at the shortest wavelength of 1.15 μm and the longest wavelength of 1.35 μm, respectively, displayed in linear brightness scales. The white contours are at 3 × 10−4 Jy pixel−1 in (d) and 15 × 10−4 Jy pixel−1 in (e), whose angulated vertices are coincident with the stretched clumpy structures in black contours showing the brightness levels of the (b) panel at 3×, 6×, 11×, and 16 × 10−6 Jy pixel−1. The bottom panel shows spectral energy distributions (SEDs) at the stellar position (red), the optical brightest peak (blue), and two background positions (green and black), derived from the HST F606W (∼0.606 μm), F814W (∼0.814 μm), and F098M (∼0.098 μm) images, and Gemini J (1.149–1.353 μm), H (1.484–1.791 μm), and K (2.010–2.419 μm) spectro-imaging data.
Paper: Near-infrared Integral-field Spectroscopy of the Wind Forming Region of CW Leo
Authors: Hyosun Kim, Youichi Ohyama, Ho-Gyu Lee, Ji Hoon Kim
Figure caption: Near-infrared brightness distributions obtained from median-based averages of the Gemini-NIFS spectra over the wavelengths within the J, H, and K bands. The color bars are shown in logarithmic scale in 0.0001–0.0028 Jy pixel−1, 0.001–0.035 Jy pixel−1, and 0.003–0.6 Jy pixel−1, respectively, with a regridded pixel size of 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩05 × 0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩05. Dotted lines indicate at their cross the brightest position in each band.
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: Top: the normalized raw white light curve of HAT-P-12 from the 2015 observation from HST/WFC3 (PI: Drake Deming, Proposal ID: 14260). Middle: the same raw white light curve divided by the best-fit model of the instrument systematics. Bottom: residuals from the best-fit transit model light curve.
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: Extracted 1D spectrum using Iraclis.
Paper: Exoplanet Ephemerides Change Observations (ExoEcho). I. Transit Timing Analysis of 37 Exoplanets Using HST/WFC3 Data
Authors: Xinyue Ma, Wenqin Wang, Zixin Zhang, Cong Yu, Dichang Chen, Jiwei Xie, Shangfei Liu, Li Zhou, Bo Ma
Figure caption: The detector image of a forward scan.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Cross-correlation functions (CCFs) with the custom PHOENIX atmospheric model using the methodology described in Section 4.2. The model is selected from a linear interpolation of a fixed model grid described in Section 5.2 and has an effective temperature of 1600 K with a surface gravity of ﹩\mathrm{log}\,g﹩ = 4.8. The model is then spin broadened to the highest likelihood value, 12 km s−1 incorporating both instrumental broadening, expected to be ∼8 km s−1, and projected rotational velocity of the companion. This value was determined by a coarse grid search varying the spin broadening from 0 to 50 km s−1 by 2 km s−1. The solid blue line is the CCF of the model template with the data on the planet. The dashed gray line is the CCF of the same template with extracted spectra of a background trace on the detector. The value of the SNR of the peak of the CCF is scaled based on the wings of the CCF where the average SNR = 1, deriving from formalism of the likelihood model (J.-B. Ruffio et al. 2019). Each individual data set shows the detection of the planet signature at >8σ.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: GPI IFS K-band data (1.95–2.30 μm), shown with shaded uncertainties representing the 1σ envelope, with the three best-fit broadened custom PHOENIX models. All three models fit the data well and are similar to one another despite the 400 K variation and 0.5 dex change between the 2000 K, ﹩\mathrm{log}\,g=5.0﹩ and 1600 K, ﹩\mathrm{log}\,g=4.5﹩ models. However, the higher-temperature models imply a smaller companion radius of 0.69 RJup, whereas the lower-temperature, lower-log(g) model equates to a more physically motivated radius of 1.0 RJup.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: We plot the GPI J-band, H-band, and K-band spectra from K. Ward-Duong et al. (2021) along with the best-fit retrieval model from petitRADTRANS including all three spectral bands. In addition, we show the best-fit models from the GPI retrievals using only one spectral band at a time while using the same pressure-temperature parameterization and prior range.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: The 1D extracted spectra (red) from KPIC, Fiber 2, with the fiber located at the position of the planet. The best-fit PHOENIX stellar plus planet model is shown in purple, with the best-fit planet model plotted separately in blue. The best-fit star + planet model is built from a linear combination of the stellar spectrum, taken from our exposures of the host star alone, and the planet model described in Section 5.2. The residual values between the data and the star + planet model are shown in gray points toward the bottom.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Corner plot for HD 206893 B showing effective temperature, surface gravity, ﹩v\sin i﹩, and RV using the full PHOENIX model grid and the KPIC K-band spectra.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Full GPI IFS (J band: 1.114−1.350 μm, H band: 1.495−1.797 μm, and K band: 1.886–2.396 μm) of HD 206893 B. The 1σ uncertainty envelope is shown in the matching shaded color. The best-fit PHOENIX-ACES K-band models are plotted and scaled to match peak flux in K band, showing the previously observed extreme extinction in J band and H band.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: Corner plot for forward-modeling results of the KPIC spectrum of HD 206893 B. We vary the effective temperature, surface gravity, ﹩v\sin i﹩, and RV. In this corner plot, we limit the prior space from 1200 to 1750 K, motivated by our analysis of the GPI LRS best-fit model and retrieval results.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: GPI K-band data with the spectra generated by the maximum likelihood values from petitRADTRANS disequilibrium chemistry free retrievals and the best-fit custom Phoenix models. Model parameters are listed in Table 4.
Paper: HD 206893 B at High Spectral Resolution with the Keck Planet Imager and Characterizer
Authors: Ben Sappey, Quinn Konopacky, Clarissa R. Do Ó, Travis Barman, Jean-Baptiste Ruffio, Jason Wang, 劲飞 王, Christopher A. Theissen, Luke Finnerty, Jerry Xuan, Katelyn Hortsman, Dimitri Mawet, Yapeng Zhang, Julie Inglis, Nicole L. Wallack, Aniket Sanghi, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Michael P. Fitzgerald, Chih-Chun Hsu, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Evan Morris, Jacklyn Pezzato-Rovner, Caprice L. Phillips, Garreth Ruane, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Ji Wang, 吉 王, Peter Wizinowich, Yinzi Xin
Figure caption: C/O ratio fit using PHOENIX models with Teff = 1600 K and ﹩\mathrm{log}\,g﹩ = 4.5.
Paper: Long-term X-Ray Variability on the Benchmark YSO HL Tau
Authors: Steven M. Silverberg, Scott J. Wolk, David A. Principe, P. C. Schneider, Hans Moritz Günther, Jinyoung Serena Kim, Joel H. Kastner
Figure caption: XMM-Newton EPIC-PN spectra from each of the six ∼40 ks observations (represented by different colors as listed in the legend) in the the 2020 monitoring campaign. Spectra are binned by 15 counts bin–1.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Continuum-subtracted MIRI-MRS spectra (reduced by the JDISCS team; K. M. Pontoppidan et al. 2024) for the four sources with the highest reported CO2 column densities: MY Lup (this work), Sz 98 (D. Gasman et al. 2023), GW Lup (S. L. Grant et al. 2023), and DF Tau (S. L. Grant et al. 2024). The DF Tau line spectrum has been divided by four for clarity. The colored bars in the central panel mark the locations of the primary Q branches of CO2 and its isotopologues. The left and right panels show other regions with CO2 emission features consistent with high ﹩{{N}_{\mathrm{CO}}}_{2}﹩.
Paper: Emission from Multiple Molecular Isotopologues in a High-inclination Protoplanetary Disk
Authors: Colette Salyk, Klaus M. Pontoppidan, Andrea Banzatti, Edwin Bergin, Nicole Arulanantham, Joan Najita, Geoffrey A. Blake, John Carr, Ke Zhang, Chengyan Xie
Figure caption: Upper-level energies of emission lines in the regions highlighted in Section 4.2 (from the HITRAN database; I. E. Gordon et al. 2022); the labels show the upper-state quantum numbers (v1, v2, l2, v3, and r), where vi are ith vibrational levels, l2 is the angular momentum of the v2 state, and r is the Fermi resonance symmetry. The dashed vertical lines mark regions with large modeling residuals discussed in the text.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Power-law radial gradient profiles with a cutoff radius based on the slab model fit approach presented in C. E. Romero-Mirza et al. (2024a). A range of temperature gradient slopes between 0.4 and 0.7 and cutoff radii between 0.75 and 10 au are sufficient to reproduce the line ratios measured in this sample in the principal diagnostic diagram (light-gray data points and model tracks in the right panel, the same as in Figure 10). A grid of radial gradient models with temperature slope and cutoff radius as labeled is shown for reference in the diagnostic diagram. Their line ratios are reported in Appendix D in Table 9. The temperature slopes inferred from this plot for CI Tau (≳0.7) and GQ Lup (≲0.5) match well those measured from the line broadening in Figure 20. A range in pebble mass fluxes is estimated using Equation (11) in C. E. Romero-Mirza et al. (2024a) from two extreme cases of minimum/maximum cold water enrichment, as shown by the shaded areas in the middle panel.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Slab model series used as reference frame for the diagnostic line-ratio diagram in Figure 10. “H” stands for the hot (850 K) model, “W” for the warm (400 K) model, and “C” for the cold (190 K) model. These models are summed up into an “H+W” and “H+W+C” series producing the model tracks shown here (see the text for details), with specific model parameters reported in Table 7.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: General procedure for the analysis of water spectra based on the findings and analysis presented in this work. The plot in Step 1 shows only a narrow range extracted from Figures 1–4, as an example. The plot in Step 2 shows the principal diagnostic diagram introduced and explained in Figures 10 and 22. The plot in Step 3 gives one example of a radial excitation gradient as measured from water lines where Doppler broadening is detected (Figures 17 and 20).
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Example of the continuum-subtraction procedure as applied to CI Tau. The entire original spectrum is shown at the top in black, and divided into smaller portions in the other panels. The excluded regions listed in Appendix B are colored in orange. The continuum estimated with the procedure described in K. M. Pontoppidan et al. (2024) is shown in light green. The red line shows the continuum after applying a wavelength-dependent offset determined from the line-free regions marked with blue points (see Appendix B).
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Compact water spectral atlas for JDISCS targets, highlighting the three temperature components discussed in the text. Shown here are the disks that are consistent with a small to moderate warm-water component in Figure 10.
Paper: Water in Protoplanetary Disks with JWST-MIRI: Spectral Excitation Atlas and Radial Distribution from Temperature Diagnostic Diagrams and Doppler Mapping
Authors: Andrea Banzatti, Colette Salyk, Klaus M. Pontoppidan, John S. Carr, Ke Zhang, Nicole Arulanantham, Sebastiaan Krijt, Karin I. Öberg, L. Ilsedore Cleeves, Joan R. Najita, Ilaria Pascucci, Geoffrey A. Blake, Carlos E. Romero-Mirza, Edwin A. Bergin, Lucas A. Cieza, Paola Pinilla, Feng Long, Patrick Mallaney, Chengyan Xie, Abygail R. Waggoner, Till Kaeufer
Figure caption: Compact water spectral atlas for JDISCS targets (continued from Figure 28). These targets have peculiarities discussed in the text or lower S/N (bottom two targets).