adsabs/AstroCLIMB huggingface dataset:
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Polarization as a function of the reddening under different conditions of the ISM. Left:  uniform magnetic field and constant/uniform dust properties. Right: magnetic field with uniform and fluctuating components, dust properties vary.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Left: deviations from the median value in polarization fraction and polarization angle of potential outliers in polarization efficiency (Section 4.2) and variable stars known in the IPS-GI database (Appendix A.1). The deviations from P and θ are the modulus of the difference between the median and the first or the third quantile in the distributions. Right: the logarithm of the variability proxy as a function of the G-band magnitude of IPS-GI data (blue dots). The red solid line is the logarithm of the expected mean G-magnitude error. The orange squares are potential outliers in polarization efficiency (Section 4.2.4). The black triangles and red stars are variable sources identified in the filtered cross-matched lists with ASAS-SN and ATLAS-VAR databases (Section A.1).
Paper: Inner Planetary System Gap Complexity is a Predictor of Outer Giant Planets
Authors: Matthias Y. He, Lauren M. Weiss
Figure caption: The highest planet mass (﹩{M}_{p}\sin i﹩ or mass from an M-R relation; y-axis) vs. the gap complexity (﹩{ \mathcal C };﹩                         x-axis) of the system for the KGPS and various other planetary systems. Blue circles denote systems with at least three inner SPs and no OGs (i.e., those included in the blue line of Figure 2). Red circles indicate systems with at least three small inner planets and at least one OG planet, where the OG(s) are either excluded (hollow circles) or included (filled circles), corresponding to the solid and dashed red lines in Figure 2, respectively; the dashed lines connecting these points indicate which system they belong to, as labeled. The four inner small-planet systems with OG(s) (hollow red circles) have preferentially high gap complexities, higher than the majority of the inner small-planet systems without any OGs (hollow blue circles). Red triangles denote systems with three or more planets only after including the giant(s) in the systems. Two systems (KOI-2169 and KOI-3158; orange) have stellar binary companions in addition to ≥3 transiting planets; the inclusion of the stellar companions significantly increases both ﹩{M}_{p}\sin i﹩ and ﹩{ \mathcal C }﹩, as expected. For reference, the solar system is also plotted (cyan markers), including (1) just the inner/terrestrial planets (square), (2) the inner planets and Jupiter (pentagon), and (3) all eight planets (octagon), as labeled. Four other known exoplanetary systems with at least three inner planets (though not necessarily transiting or small) and an outermost giant planet (55 Cnc, WASP-47, HD 219134, and HD 191939) are also shown in this plot for comparison (black circles/lines).
Paper: Inner Planetary System Gap Complexity is a Predictor of Outer Giant Planets
Authors: Matthias Y. He, Lauren M. Weiss
Figure caption: Architecture gallery of the KGPS and other systems with at least three planets. Each row corresponds to one planetary system (as labeled on the left y-axis) and is plotted along the semimajor axis (x-axis, log scale). The point sizes are proportional to the square root of the planet masses (﹩{M}_{p}\sin i﹩ or masses from a mass–radius relation). The point colors denote SPs (blue), OGs (red), and SCs (orange), as also labeled in the legend. Black points indicate inner planets in systems that are not part of the KGPS sample (also denoted by dotted lines). Faded points indicate nontransiting planets. The systems are sorted by the gap complexity (﹩{ \mathcal C }﹩) of the inner system (where there are at least three planets, excluding any OGs or SCs), as labeled on the right y-axis, or ﹩{ \mathcal C }﹩ of the whole system when there are fewer than three SPs (in parentheses; these systems are also denoted by the dashed lines). For reference, the solar system is also plotted (cyan points) with the same convention, where the planets from Jupiter and beyond are categorized as OGs and are excluded from the calculation of ﹩{ \mathcal C }﹩.
Paper: Inner Planetary System Gap Complexity is a Predictor of Outer Giant Planets
Authors: Matthias Y. He, Lauren M. Weiss
Figure caption: Cumulative distributions of the gap complexity (﹩{ \mathcal C }﹩). Left: distributions for all systems with at least three planets within 1 yr in the Kepler DR25 catalog (black) and in the KGPS sample (magenta). While there are fewer such systems in the KGPS sample (as indicated by the numbers in parentheses), the distribution of ﹩{ \mathcal C }﹩ is consistent with being drawn from the same distribution as the Kepler DR25 systems. Right: distributions for subsets of the KGPS sample (all with at least three inner SPs); the blue line includes systems without OGs, and the red lines include only the systems with at least three SPs and at least one OG planet, where the OG(s) are either excluded from (solid) or included in (dashed) the calculation of ﹩{ \mathcal C }﹩.
Paper: Inner Planetary System Gap Complexity is a Predictor of Outer Giant Planets
Authors: Matthias Y. He, Lauren M. Weiss
Figure caption: Cumulative distributions of planet mass partitioning (﹩{ \mathcal Q };﹩ top), mass dispersion (﹩{\sigma }_{M}^{2};﹩ middle), and mass monotonicity (﹩{ \mathcal M };﹩ bottom) for various subsets of the KGPS sample (systems with at least two planets). In each panel, the solid lines include the inner small planets for systems with no OG planets (blue) and for systems with OG planet(s) (red). We also show the distribution for the latter sample including the OG planets in the calculation (dashed red line), which by definition typically increase all three metrics. For reference, all KGPS systems with at least two planets are denoted by the dashed gray line; there are more systems in this sample than the sum of the samples in the blue and red lines because some systems have exactly one transiting planet and one OG planet.
Paper: Inner Planetary System Gap Complexity is a Predictor of Outer Giant Planets
Authors: Matthias Y. He, Lauren M. Weiss
Figure caption: Architecture gallery of the KGPS systems with at least two planets. The axes, legend, and conventions are identical to those in Figure 1. Left: The systems sorted by the mass partitioning (﹩{ \mathcal Q }﹩) of the inner system (i.e., SPs only, where there are at least two), as labeled on the right y-axis, or the mass partitioning of the whole system when there are fewer than two SPs (denoted by the numbers in parentheses; these systems are also denoted by the dashed lines). Middle: The same systems, sorted and labeled by mass dispersion (﹩{\sigma }_{M}^{2}﹩). Right: The same systems, sorted and labeled by mass monotonicity (﹩{ \mathcal M }﹩). As in Figure 1, the solar system is also plotted (cyan points) with the same convention, where the planets from Jupiter and beyond are excluded from the calculation of ﹩{ \mathcal Q }﹩ or ﹩{\sigma }_{M}^{2}﹩ or ﹩{ \mathcal M }﹩. For all three metrics, there is no apparent correlation between the inner system and the occurrence of OG planets.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: NIR cross sections of OH (Δv = 2 and Δv = 3) produced from the completely populated states plotted, overlaid in the top panel for scale and individually below, all at a temperature of 3050 K and a pressure of 0.01 bar. (Note that as we progress to the final two cross-section sets, the Δv = 4 and Δv = 5 bands start to become visible.)
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Individual band contributions for cross sections of OH in LTE, with the NIR (Δv = 2 and Δv = 3) bands shown for the 3050 K, 0.01 bar point on the T-P grid.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Observation simulation points and errors of the WASP-33b emission spectra plotted over the forward model for observations over ten secondary eclipses.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: The Guillot T-P profile adopted for modeling the atmosphere of WASP-33b.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Retrieval nested sampling posteriors for one simulated secondary eclipse with bands 0–2.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Retrieved mixing ratios for OH compared with the theoretical Boltzmann distribution used in generating cross sections for OH in LTE. Retrieved from 50 simulated secondary eclipses.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Individual band contributions of OH in NIR retrieved using the completely populated band cross sections for 0–3 with five simulated secondary eclipses, with the plot highlighting the wavelength region with the strongest lines.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Posteriors for ten simulated secondary eclipses with bands 0–5, using artificial completely populated band cross sections.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Posteriors for five simulated secondary eclipses with bands 0–3, using artificial completely populated band cross sections.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Posteriors for the retrieval including bands 0 through 6 for 50 simulated secondary eclipses.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Retrieval nested sampling posteriors for five simulated secondary eclipses with bands 0–3.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Retrieval nested sampling posteriors for ten simulated secondary eclipses with bands 0–3.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Retrieval nested sampling posteriors for one simulated secondary eclipse with bands 0–3.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: Mix ratios retrieved for bands 0 through 6 for 50 simulated secondary eclipses.
Paper: TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star
Authors: Luke C. Powers, Jessica Libby-Roberts, Andrea S. J. Lin, Caleb I. Cañas, Shubham Kanodia, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Arvind F. Gupta, Sinclaire Jones, Henry A. Kobulnicky, Andrew Monson, Brock A. Parker, Tera N. Swaby, Chad F. Bender, William D. Cochran, Leslie Hebb, Andrew J. Metcalf, Paul Robertson, Christian Schwab, John Wisniewski, Jason T. Wright
Figure caption: The transit observations conducted for TOI-3785 b. In each case, we fit a model to the light curve via exoplanet (Section 4). The best-fit model is shown in black, with the 1, 2, and 3σ confidence intervals in progressively lighter shades of blue. A 10 minute bin of our data is included as red points in each panel. It is also important to note that the reported median errors are dependent on their respective exposure time of the instrument used. The subpanels show the ARCTIC transit observed in the Semrock filter (top left), the RBO transit observed in Bessell I (top right), TESS Sector 20 data taken at long cadence (1800 s; bottom left), and TESS Sector 47 data taken at short cadence (120 s; bottom right).
Paper: TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star
Authors: Luke C. Powers, Jessica Libby-Roberts, Andrea S. J. Lin, Caleb I. Cañas, Shubham Kanodia, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Arvind F. Gupta, Sinclaire Jones, Henry A. Kobulnicky, Andrew Monson, Brock A. Parker, Tera N. Swaby, Chad F. Bender, William D. Cochran, Leslie Hebb, Andrew J. Metcalf, Paul Robertson, Christian Schwab, John Wisniewski, Jason T. Wright
Figure caption: Top: planet radius against planet mass of only M-dwarf targets (restricted by an upper bound on effective temperature of T eff < 4000K). The points with attributed effective temperatures are M-dwarf planets that have >3σ mass precision. Gray points represent >3σ FGK targets. The dashed lines are density contours with specific values listed in the bottom right. Bottom: planetary radius against stellar effective temperature, to place TOI-3785 b against a broader range of stellar host types. Colored points represent >3σ mass precision while targets under this threshold are grayed out. We also highlight the lack of planetary confirmation between (4000 K < T eff < 4700 K). This is most likely a result of the shallow transit depths that are characteristic of K-dwarf stars. This creates a detection bias as K-dwarf planets produce weaker transiting signals. In both figures, similar M-dwarf Neptunes to TOI-3785 b are labeled and listed in Table 6.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: (a) The K P–v sys map after combining the cross-correlation functions of all of the data sets using a non-preprocessed OH LTE model. The upper panel shows the S/N curve at the K P of 231.8  km s−1, while the right panel shows the S/N curve at the v sys of −1.1 km s−1. The color bar shows the S/N of the K P–v sys map. (b) The marginalized likelihood distribution of K P, v sys, and α using a preprocessed OH LTE model. The red dashed lines show the median value of the corresponding distribution. The upper right panel is the K P–v sys map of the detection from the likelihood. The color bar shows the significance of the K P–v sys map. This map is produced by dividing the median value of the conditional likelihood distribution of α by its uncertainty at every combination of K P and v sys.
Paper: A Spectroscopic Thermometer: Individual Vibrational Band Spectroscopy with the Example of OH in the Atmosphere of WASP-33b
Authors: Sam O. M. Wright, Stevanus K. Nugroho, Matteo Brogi, Neale P. Gibson, Ernst J. W. de Mooij, Ingo Waldmann, Jonathan Tennyson, Hajime Kawahara, Masayuki Kuzuhara, Teruyuki Hirano, Takayuki Kotani, Yui Kawashima, Kento Masuda, Jayne L. Birkby, Chris A. Watson, Motohide Tamura, Konstanze Zwintz, Hiroki Harakawa, Tomoyuki Kudo, Klaus Hodapp, Shane Jacobson, Mihoko Konishi, Takashi Kurokawa, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Akitoshi Ueda, Sébastien Vievard, Sergei N. Yurchenko
Figure caption: The K P–v sys significance map of the combined data sets (N 1 + N 2 + N 3) for the preprocessed individual band model (a), the unpeeling model from band 0 only to the total 0 + 1 + 2 + 3 + 4 + 5 + 6 + 7 + 8 + 9 bands (b), and the unpeeling model from band 9 only to the sum of bands 0, 1, 2, 3, 4, 5, 6, 7, 8, and 9 (c). The white dashed lines indicate the location of the OH LTE model signal as a reference. The color bar shows the significance of the maps.