adsabs/AstroCLIMB huggingface dataset:
Paper: Open-source High-resolution Exoplanet Atmosphere Retrievals with POSEIDON
Authors: Ruizhe Wang, Ryan J. MacDonald, Neale P. Gibson, Nikole K. Lewis
Figure caption: Full corner plot of retrieval results on injected data (﹩\mathrm{log}{X}_{{{\rm{H}}}_{2}{\rm{O}}}=\mathrm{log}{X}_{\mathrm{CO}}=\mathrm{log}{X}_{{\mathrm{CH}}_{4}}=\mathrm{log}{X}_{{\mathrm{NH}}_{3}}=-4﹩) along with retrieved P-T profile using SYSREM. Runtime: 13 hr on 24 cores.
Paper: Open-source High-resolution Exoplanet Atmosphere Retrievals with POSEIDON
Authors: Ruizhe Wang, Ryan J. MacDonald, Neale P. Gibson, Nikole K. Lewis
Figure caption: Detection significance of an injected signal as a function of Kp and ΔVsys and detection significance as a function of phase and planet radial velocity (normalized by standard deviation per phase). Red: Emission. Blue: Transmission.
Paper: Open-source High-resolution Exoplanet Atmosphere Retrievals with POSEIDON
Authors: Ruizhe Wang, Ryan J. MacDonald, Neale P. Gibson, Nikole K. Lewis
Figure caption: Full corner plot of the retrievals on IGRINS WASP-77Ab data along with retrieved P-T profile. Blue: PCA; run time: 11 hr on 24 cores. Red: SYSREM; run time: 6.6 hr on 24 cores.
Paper: Open-source High-resolution Exoplanet Atmosphere Retrievals with POSEIDON
Authors: Ruizhe Wang, Ryan J. MacDonald, Neale P. Gibson, Nikole K. Lewis
Figure caption: Cross-correlation results with CO and H2O separately for WASP-77Ab. White dashed lines are approximately the published values.
Paper: Open-source High-resolution Exoplanet Atmosphere Retrievals with POSEIDON
Authors: Ruizhe Wang, Ryan J. MacDonald, Neale P. Gibson, Nikole K. Lewis
Figure caption: Full corner plot of the retrieval for the combined red and blue WASP-121b data along with retrieved P-T profile. Runtime: 7.3 hr on 24 cores.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Spectral energy distributions of WASP-102 (top row, left), WASP-116 (top row, middle), WASP-149 (top row, right), WASP-154 (second row, left), WASP-155 (second row, middle), WASP-188 (second row, right), WASP-194 (bottom row, left), WASP-195 (bottom row, middle), and WASP-197 (bottom row, right). Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit PHOENIX atmosphere model (black). The absolute flux-calibrated Gaia spectrum is shown as a gray swathe in the inset figure.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Global fit for WASP 116 b. Photometric lightcurves have been offset for visual clarity.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Final joint transit and RV model fit for WASP-154 b. The top panel shows the photometric data sets, offset for clarity, while the bottom panel shows the fit to the radial velocity data.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Final joint transit and RV model fit for WASP-149 b. The top panels show the available photometric data, offset for clarity. The bottom panel shows the final RV fit for SOPHIE and CORALIE data.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Transit and RV fit for WASP-102 b. Transit observations are offset for clarity. The three TRAPPIST observations were taken with the same filter, and they are plotted together.
Paper: A Swarm of WASP Planets: Nine Giant Planets Identified by the WASP Survey
Authors: N. Schanche, G. Hébrard, K. G. Stassun, B. Hord, K. Barkaoui, A. Bieryla, D. Ciardi, K. A. Collins, A. Collier Cameron, J. Hartman, N. Heidari, C. Hellier, S. B. Howell, M. Lendl, J. McCormac, K. K. McLeod, H. Parviainen, D. Radford, A. S. Rajpurohit, H. Relles, R. Sharma, S. Baliwal, G. Bakos, S. C. C. Barros, F. Bouchy, A. Burdanov, P. A. Budnikova, A. Chakaraborty, C. Clark, Laetitia Delrez, O. D. S. Demangeon, R. F. Díaz, J. Donnenfield, M. Everett, A. Fukui, M. Gillon, C. Hedges, J. Higuera, E. Jehin, J. M. Jenkins, F. Kiefer, D. Laloum, J. Livingston, M. Lund, P. Magain, P. Maxted, I. Mireles, F. Murgas, N. Narita, K. J. Nikitha, C. Opitom, E. Palle, Y. G. Patel, M. Rose, S. G. Sousa, I. A. Strakhov, P. Strøm, A. Tuson, R. West, J. Winn
Figure caption: Final joint transit and RV model fit for WASP-155 b. Photometric observations are offset for clarity.
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: (a) Spitzer 8 μm image of an area ∼0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩39 × 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩31, centered at (l, b) = (33﹩\mathop{.}\limits^{\unicode{x000b0}}﹩26, −0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩02), covering the IRDC associated with the bubble N59-North. The filamentary IRDC is marked with cyan arrows, while the bubbles N59 and N59-North are outlined by large and small ellipses, respectively. The orange contours present MAGPIS 20 cm radio continuum emission at levels [5, 8, 10 and 15] × σ, with 1σ = 0.4 mJy beam−1. The inset shows a zoomed-in view of the yellow rectangular region outlined over the IRDC. Blue contours indicate MeerKAT 1.3 GHz continuum emission at levels [5, 15 and 25] × σ, with 1σ = 20 μJy beam−1. The position of the ATLASGAL clump (from J. S. Urquhart et al. 2018) is shown with a black star symbol. The IR-dark filaments are highlighted by yellow dotted lines in the inset. (b) Same image as panel “a” for the magenta dotted–dashed rectangular region. The position of the IRDC candidates toward the filament obtained from J. Pari & J. L. Hora (2020) is marked using asterisk symbols. (c) GRS 13CO(J = 1–0) integrated intensity (moment-0) map for the velocity range of [94.5, 107.3] km s−1. For the moment-0 map 1σ = 0.21 K km s−1. The black and magenta star symbols indicate the position of the ATLASGAL clumps with and without signature of outflow activity, respectively. The ellipse corresponding to N59-North is highlighted in panels “b” and “c.” A scale bar of 2 pc is provided in the inset of panel “a,” while a 15 pc scale bar is shown in each panel for a distance of 4.66 kpc.
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: (a) The Galactic longitude–velocity (i.e., l–v) diagram of the 13CO(J = 3–2) data for the integration range in Galactic latitude = [−0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩046, 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩059]. The contours are drawn at about [6, 12, 18] × σ, where 1σ = 2 mK degree. The velocity gradients in the eastern and western parts of the filament are indicated by white arrows, and the corresponding velocity gradient values are provided in the figure in units of km s−1 pc−1. (b) The SCOUSEPY-generated position–position–velocity (PPV; here, l–b–v) diagram. The data points in the diagram represent the position and centroid velocity of the Gaussian components identified in the 13CO(J = 3–2) emission. The data points are also colored based on their velocity, according to the color scale shown at the top of the image. The 13CO(J = 3–2) integrated intensity map is shown in the l–b plane using filled contours at levels [5, 10, 15, 20, 25] K km s−1. The location of the bubble N59-North is highlighted with a red ellipse in the l–b plane. The blueshifted and redshifted velocity components toward N59-North are indicated with arrows.
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: (a) The N(H2) map in the y–z plane at 0.1 Myr, showing the collision of a turbulent molecular cloud (radius = 1.5 pc) and a sea of dense gas moving with a relative velocity of 10 km s−1 along the z-direction. (b) The N(H2) map in the y–z plane at 0.4 Myr. Panels (c) and (d) present the PV diagrams along the x- and y-axes, respectively, for a width of 0.4 pc. The area enclosed by the black lines indicates the velocity of the compressed gas. These figures are taken from A. K. Maity et al. (2024). The schematic diagrams in panels (e) and (f) depict the initial and current configurations of our target filament in position and velocity space, respectively. The current configuration shows the presence of a HFS at the center of the filament, bubble N59-North, and its role in creating blueshifted and redshifted velocity components. Stars indicate the presence of radio continuum sources toward N59-North. Similar to Figure 6, the x–z plane represents the plane of the sky, while the y-direction corresponds to the line of observation. The blue and red arrows represent the blueshifted and redshifted velocity components in the filament. Note that the schematic figures are not to scale.
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: (a) Spitzer 8 μm image, (b) MeerKAT 1.3 GHz radio continuum emission map, (c) H2 column density (N(H2)) map, and (d) dust temperature (Td) map, corresponding to the region outlined by red dotted–dashed lines in Figures 1 and 3. In each panel, the 13CO(J = 3–2) emission is shown using a contour at about 3.7 K km s−1. The magenta star, black cross, and cyan plus symbols indicate the position of the ATLASGAL clumps, 6.7 GHz MMEs, and UC H II regions, respectively. The YSO candidates are shown using diamond symbols in panel “a.” The Class I, Flat Spectrum, and Class II sources obtained from the SPICY catalog (M. A. Kuhn et al. 2021) are colored red, cyan, and green, respectively. The blue diamonds are additional Class I YSO candidates satisfying the color conditions: [4.5] − [5.8] ≥ 0.7 and [3.6] − [4.5] ≥ 0.7 (K. V. Getman et al. 2007). A scale bar of 5 pc is marked in panel “d.”
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: (a) GRS 13CO(J = 1–0) moment-0 map, identical to Figure 1(c). (b) GRS 13CO(J = 1–0) intensity-weighted velocity (moment-1) map. (c) CHIMPS 13CO(J = 3–2) moment-0 map for the velocity range of [95.2, 106.2] km s−1 (1σ = 0.36 K km s−1). (d) CHIMPS 13CO(J = 3–2) moment-1 map. (e) RAMPS NH3(1–1) moment-0 map for the velocity range of [95.0, 106.2] km s−1 (1σ = 0.15 K km s−1). (f) RAMPS NH3(1–1) moment-1 map. The rectangular region highlighted in panels “a,” “c,” and “e” is identical to the one shown in Figure 1. A scale bar of 15 pc is provided in each panel.
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: A schematic view of the possible position–velocity (PV) diagrams for cylindrical filaments in different gas motions. The x–z plane represents the plane of the sky, and the y-direction corresponds to the line of observation, which forms a significant angle (∼45°) relative to the filament. (a) A rotating filament with a constant angular velocity, indicated by a curved arrow. (b) A filament undergoing central collapse (motivated from H.-L. Liu et al. 2019). (c) A filament undergoing end-dominated collapse (motivated from S. D. Clarke & A. P. Whitworth 2015). The blue and red arrows in each panel represent the blueshifted and redshifted velocity components.
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: The mass–effective radius plot for the ATLASGAL clumps. The data from J. S. Urquhart et al. (2018) for d = 6.5 kpc are displayed as open circles, while the red solid circles represent the data points scaled to our adopted distance of 4.66 kpc. The KP-10 condition for MSF is indicated by the blue dotted line. The mKP-10 condition for MSF as defined by J. S. Urquhart et al. (2018) corresponds to the white region above the gray-shaded area.
Paper: Investigating Embedded Structures and Gas Kinematics in the Infrared-dark Cloud Hosting Bubble N59-North
Authors: A. K. Maity, L. K. Dewangan, O. R. Jadhav, Saurabh Sharma, Ram Kesh Yadav, Y. Fukui, H. Sano, T. Inoue
Figure caption: (a) A large-scale view of our target site is shown using a two-color composite image. Colors red and green present the MeerKAT 1.3 GHz radio continuum emission and 13CO(J = 3–2) moment-0 map, respectively. The radio continuum emission is displayed on a linear scale from 5σ to 100σ, where 1σ∼ 20 μJy beam−1. The moment-0 map is shown on a linear scale from 3σ to 30σ, where 1σ∼ 0.36 K km s−1. The white dotted rectangle indicates the area shown in Figure 1(a). A scale bar of 15 pc is marked in this panel. (b) This panel presents a similar two-color composite image as panel “a,” with red representing the MIPSGAL 24 μm image. The MIPSGAL image is displayed on a logarithmic scale, ranging from 25 to 200 MJy sr−1. The distribution of the ATLASGAL clumps for different velocity ranges and distances is indicated using various symbols, as described in the figure. The extent of a candidate H II region from L. D. Anderson et al. (2014) is marked with a dotted circle in each panel.
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: Results from the retrieval frameworks applied to WASP-121 b's transmission spectrum obtained from the phase-curve analysis. The temperature and abundance profiles inferred from the different retrievals are depicted using lines with shaded regions indicating the extent of the corresponding 1σ regions. All NEMESIS results shown here were inferred from a simultaneous retrieval of both hemispheres. Any atmospheric variable varied between the hemispheres in that framework is presented using dotted magenta and purple lines, and the molecular abundances that are held identical in both hemispheres are shown using dotted green lines.
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: Selection of the spectrophotometric transit-only light curves at a spectral resolution of R ∼ 600 and respective models. The selected spectrophotometric light curves are the 10th, 20th, 30th, 40th, 50th, 60th, 70th, 80th, and 90th percentile light curves in ﹩{\chi }_{\nu }^{2}﹩. Upper panel: colored dots with error bars show the data and solid black lines depict the model light curves generated employing the median values of the parameters’ samples explored using MCMC. The wavelength ranges over which the light curves were integrated are given on the left and the ﹩{\chi }_{\nu }^{2}﹩ of each model fit is given on the right. Lower panel: the relative residuals between the selected data and the models binned to a lower resolution in time are shown using solid lines in the color that corresponds to the light curve in the upper panel they belong to. The dashed black line shows the median of the binned residuals of all spectrophotometric light curves (not just the ones plotted in the upper panel).
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: WASP-121 b's transmission spectra from the transit-only analysis and the phase-curve analysis (T. M. Evans-Soma et al. 2025) at two different spectral resolutions. Upper panels: the blue diamonds and red circles show the transit-only and phase-curve transmission spectra, respectively. Middle panels: the blue diamonds and red circles show the 1σ uncertainties of the transit-only and phase-curve transmission spectra, respectively. Lower panels: the purple circles show the transit depths inferred from the transit-only analysis subtracted by the transit depths from the phase-curve analysis. Horizontal gray lines at zero were added to guide the eye. The solid magenta lines present linear fits (f(λ) = c0 + c1λ) to the plotted residuals. For R ∼ 600, c0 ≈ 142 ppm and c1 ≈ −65 ppm μm−1 and for R ∼ 3000, c0 ≈ 68 ppm and c1 ≈ −47 ppm μm−1.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: Phase curve (left panel) and transit-only (right panel) transmission spectra at R ∼ 600 along with the median model spectra of the applied retrievals. The 1σ intervals of the model spectra are illustrated using shaded regions.
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: MCMC results for the fits to the spectrophotometric transit-only light curves at R ∼ 600. For the fit parameters, we indicate the medians and 1σ intervals of the white light curve fit's posteriors (see Table 1) for both the NRS1 and NRS2 detectors using dashed blue lines and shaded blue regions. For the limb darkening parameters (u1 and u2), we adopted Gaussian priors, whose μ and σ are shown using solid red lines and red shadings, respectively. The transit midtimes were subtracted by their median.
Paper: WASP-121 b’s Transmission Spectrum Observed with JWST/NIRSpec G395H Reveals Thermal Dissociation and SiO in the Atmosphere
Authors: Cyril Gapp, Thomas M. Evans-Soma, Joanna K. Barstow, Joshua D. Lothringer, David K. Sing, Djemma Ruseva, Eva-Maria Ahrer, Jayesh M. Goyal, Duncan Christie, Laura Kreidberg, Nathan J. Mayne
Figure caption: Comparison of the transmission spectra for the batman and catwoman models. Top panel: trailing and leading limb depths compared to the depths found from the batman model fitting. Middle panel: differences between the trailing and leading limb depths. The red line shows the mean value of 0.006%. Bottom panel: difference in logarithmic evidence between the catwoman model (﹩\mathrm{ln}({{ \mathcal Z }}_{2})﹩) and the batman model (﹩\mathrm{ln}({{ \mathcal Z }}_{1})﹩) as estimated from dynesty. The pink line shows the mean value of 0.06.