adsabs/AstroCLIMB huggingface dataset:
Paper: A Small Brown Dwarf in an Aligned Orbit Around a Young, Fully Convective M Star
Authors: Madison Brady, Jacob L. Bean, Gumundur Stefánsson, Nina Brown, Andreas Seifahrt, Ritvik Basant, Tanya Das, Rafael Luque, Julian Stürmer
Figure caption: A comparison between the model outputs of the T. Hirano et al. (2011), rmfit, Y. Ohta et al. (2005), and starry RM models. For these models, we assume λ = 0o veqsini  =  7.0 km s−1, u1  =  0.4, and u2  =  0.2. Both the T. Hirano et al. (2011) and rmfit models have β  =  3.5 km s−1 and ζ  =  1 km s−1. Finally, the T. Hirano et al. (2011) model assumes Gaussian line profiles, with γ  =  0, in order to allow for easier comparison to the rmfit models, which assume this formalism. The addition of macroturbulent and instrumental broadening result in a larger RM amplitude for a given veqsini⋆ value. It is thus obvious that the Y. Ohta et al. (2005) and starry models tend to underpredict the RM amplitude.
Paper: A Small Brown Dwarf in an Aligned Orbit Around a Young, Fully Convective M Star
Authors: Madison Brady, Jacob L. Bean, Gumundur Stefánsson, Nina Brown, Andreas Seifahrt, Ritvik Basant, Tanya Das, Rafael Luque, Julian Stürmer
Figure caption: The host star Teff vs. λ for all systems with transiting brown dwarfs with measured obliquities. The Kraft break is shown as an orange line, and the gray line corresponds to an aligned λ  =  0°. LP 261-75C is highlighted with a red star. The stellar temperatures are drawn from TIC (K. G. Stassun et al. 2019) and the obliquities are from A. H. M. J. Triaud et al. (2009), R. J. Siverd et al. (2012), A. H. M. J. Triaud et al. (2013), G. Zhou et al. (2019), S. Giacalone et al. (2024), and T. Ferreira et al. (2024).
Paper: A Small Brown Dwarf in an Aligned Orbit Around a Young, Fully Convective M Star
Authors: Madison Brady, Jacob L. Bean, Gumundur Stefánsson, Nina Brown, Andreas Seifahrt, Ritvik Basant, Tanya Das, Rafael Luque, Julian Stürmer
Figure caption: Left: the red- and blue-channel MAROON-X RVs of LP 261-75A. The RV uncertainties are too small to be visible in this plot. Right: all of the available RV data on LP 261-75A, with a fit model of the orbit of LP 261-75C in gray. The RV slope observed in the MAROON-X data is consistent with the brown dwarf's orbit inferred from the TRES data.
Paper: A Small Brown Dwarf in an Aligned Orbit Around a Young, Fully Convective M Star
Authors: Madison Brady, Jacob L. Bean, Gumundur Stefánsson, Nina Brown, Andreas Seifahrt, Ritvik Basant, Tanya Das, Rafael Luque, Julian Stürmer
Figure caption: The mass and radius of LP 261-75C, compared to brown dwarf isochrones from I. Baraffe et al. (2015, solid line), equilibrium chemistry ATMO 2020 models (M. W. Phillips et al. 2020, dotted–dashed line,), and solar-metallicity Sonora Bobcat models (M. S. Marley et al. 2021, dashed line). LP 261-75C has a radius consistent with a much older system than the  ≈100 Myr-old LP 261-75.
Paper: A Small Brown Dwarf in an Aligned Orbit Around a Young, Fully Convective M Star
Authors: Madison Brady, Jacob L. Bean, Gumundur Stefánsson, Nina Brown, Andreas Seifahrt, Ritvik Basant, Tanya Das, Rafael Luque, Julian Stürmer
Figure caption: Top: final RM fit to the MAROON-X RV data, with the Keplerian shifts subtracted out. Bottom: residuals of the RM fit to the MAROON-X data.
Paper: A Small Brown Dwarf in an Aligned Orbit Around a Young, Fully Convective M Star
Authors: Madison Brady, Jacob L. Bean, Gumundur Stefánsson, Nina Brown, Andreas Seifahrt, Ritvik Basant, Tanya Das, Rafael Luque, Julian Stürmer
Figure caption: TESS 2 minute PDCSAP photometry of the LP 261-75 system. Outliers due to flares and transit events are removed in order to focus on the rotational modulation of the host star.
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Overview of the PyHSTHAContSub (doi:10.5281/zenodo.14610187) pipeline background and continuum subtraction steps used to produce the HST-Hα images (see Section 4). In our workflow, we first generate synthetic HST filter images from the MUSE data (Section 4.1). We then smooth and regrid the HST images (while preserving flux) to the resolution and pixel grid of the synthetic MUSE images. We compare these images and determine a background correction, which we apply to the full-resolution HST images. For the continuum subtraction, we first subtract the Milky Way foreground extinction from each filter (for both the MUSE and HST data). We then determine the weights of the two broadband images and subtract a combination of these two from the narrowband image to produce the continuum-subtracted narrowband images. We do this for both the HST and MUSE observations. We then compare the MUSE Hα image with the continuum-subtracted MUSE image to determine the contribution of [N II] line emission in the narrowband filter, which we then apply to the full-resolution HST images. These final images are then passed to the post-processing steps to correct for oversubtraction, remaining cosmic-ray, and foreground-star residuals. Here the chickens represent the individual galaxy images.
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Filter transmission curves for the F657N (middle panel) and F658N (bottom panel) HST-Hα filters on WFC3/UVIS used in this survey. The solid vertical lines show the wavelength of the Hα line for the systemic velocity of each galaxy in our sample, while the shaded regions show the full velocity range. Observations with the narrow F658N filter are preferred, but Hα emission for galaxies with velocities higher than ≈​​​​​1500 km s−1 is redshifted outside of this passband, and we use F657N instead (see Figure 10; see also Figure 16 for a comparison of HST to MUSE Hα flux as a function of velocity for two galaxies that have a velocity range close to the edge of the filter transmission curve). Archival observations for three galaxies (NGC 628-C, NGC 1300, and NGC 1672) use the F658N filter from the ACS/WFC camera (top panel).
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Example MUSE spectra compared with HST filter transmission curves (ACS/WFC and WFC3/UVIS). Example spectra from NGC 628 (top panel) and NGC 2835 (bottom panel) are shown as solid black lines, overlaid with the F555W (blue), F658N (orange), and F814W (green) filter transmission curves for ACS/WFC (top panel) and WFC3/UVIS (bottom panel). The left panel displays the full wavelength range of the MUSE observations, with dashed vertical lines marking the coverage limits. In the right panel, we focus on the Hα line within the F658N filter bandpass, which includes contributions from the [N II] λ6548 and [N II] λ6583 emission lines.
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Results of the extinction correction, continuum subtraction (Section 4.5), and [N II] correction (Section 4.6) of a portion of NGC 628-C (same as Figure 6). Top row, from left to right: shown is the F658N filter image after background subtraction and extinction correction, and the continuum-subtracted and continuum F658N filter images. Bottom row, from left to right: the continuum-subtracted F658N image produced from the synthetic HST filter MUSE images (i.e., including the contribution from the [N II] lines convolved with the F658N filter transmission curve), the MUSE DAP Hα-emission-only image (E. Emsellem et al. 2022), and the final [N II]-corrected HST-Hα image.
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Fits to determine the background level in HST images by calibrating to MUSE observations (Section 4.4). Intensities from matched-resolution pixels in the HST vs. synthetic MUSE images measured in the F555W, F658N, and F814W filters for NGC 628-C. The colored circles represent 25 binned data points (spaced by data density), and the dashed line in each panel shows the best linear fit to these points (y = ax + b), where y represents measurements from the degraded HST pixels and x represents the MUSE pixels (see Table 4). The dotted line in each panel shows the 1-to-1 line. The best-fit offsets are subtracted from the full-resolution HST images to correct for the sky background level.
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: HST and MUSE Filters for NGC 628. First row, left to right: HST F555W, F658N, and F814W filters at their native resolution (∼0﹩\mathop{.}\limits^{\unicode{x02033}}﹩​​​​​​​1) and pixel grid. Second row, left to right: HST filters smoothed to the resolution and grid size matching the MUSE observations (see next row of panels). Third row, left to right: synthetic images produced by applying the HST transmission curves to the lower-resolution MUSE spectroscopic observations. These are used to improve the flux calibration of the HST images. Fourth row, left to right: HST filter maps (again at native resolution and pixel grid) with zero-point offsets applied; offsets determined by comparing with the synthetic MUSE images (see Figure 7).
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Results of the [N II] λ6548 and [N II] λ6583 line correction routine (Section 4.6). Hα fluxes are from the continuum-subtracted MUSE synthetic filter maps as a function of the Hα flux densities measured from the MUSE spectroscopic data. The blue circles represent 20 binned data points (equally spaced), and the dashed blue line shows the best linear fit to these points (y = ax + b), where y represents the HST image data points and x represents the MUSE data points (see Table 4). The dotted line shows the 1-to-1 line.
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Left: galaxies from the SDSS sample with z ≲ 0.1 form the backdrop of the left panel, where the galaxy star-forming sequence is the prominent upper feature. Coverage of the SFR–M* plane by galaxies in the parent PHANGS sample (N = 74; open circles) is shown. Red plus signs show that the 19 galaxies observed as part of the HST-Hα project tend to have higher SFRs. Right: the star formation and molecular gas surface brightness (J. Sun et al. 2022) for the parent PHANGS sample (open circles) and the PHANGS-HST-Hα subsample studied here (red plus signs). Outlier NGC 3239 is noted.
Paper: The PHANGS-HST-Hα Survey: Warm Ionized Gas Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Rupali Chandar, Ashley T. Barnes, David A. Thilker, Miranda Caputo, Matthew R. Floyd, Adam K. Leroy, Leonardo Úbeda, Janice C. Lee, Médéric Boquien, Daniel Maschmann, Francesco Belfiore, Kathryn Kreckel, Simon C. O. Glover, Ralf S. Klessen, Brent Groves, Daniel A. Dale, Eva Schinnerer, Eric Emsellem, Erik Rosolowsky, Frank Bigiel, Guillermo Blanc, Mélanie Chevance, Enrico Congiu, Oleg V. Egorov, Chris Faesi, Kathryn Grasha, Stephen Hannon, Kirsten L. Larson, Laura A. Lopez, Angus Mok, Justus Neumann, Eve Ostriker, Alessandro Razza, Patricia Sánchez-Blázquez, Francesco Santoro, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: B − V − I+Hα blue–green–red color composite images for the 17 (of 19) galaxies in our sample that have HST-Hα images available at this time. The Hα emission (red) shows the locations of recent (≲6 Myr) star formation. A 1 kpc scale bar is indicated for each galaxy. The images show a variety of environments and morphologies.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: (a) The variation in the difference of the disk-integrated Earth OLR between an ellipsoidal and a spherical model during 2022. (b) The variation in the difference of the observational solid angle between an ellipsoidal and a spherical model with changing Earth–Moon distance.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: (a) Observational solid angle difference comparison between different radius definitions. (b) Variation in the observational solid angle difference with Earth–Moon distance changes.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: The differences in the disk-integrated Earth OLR change with the nadir point’s latitude.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: (a) Observational solid angle variation during 2022. (b) The observational solid angle varies with the Earth–Moon distance.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: Comparisons of the observational solid angles between WGS 84, GRS 80, and CGCS 2000 during 2022.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: (a) Moon-based disk-integrated measurements during 2022. (b) Moon-based disk-integrated measurements with changing Earth–Moon distance.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: (a) Moon-based disk-integrated Earth OLR during 2022. (b) Moon-based disk-integrated Earth OLR with changing Earth–Moon distance.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: Moon-based Earth observation geometry.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: The variation of the observational solid angles for different nadir point latitudes at the same Earth–Moon distance.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: (a)–(d) The fitting error distributions of the observational solid angles for Groups A, B, C, and D, respectively. (e)–(h) The fitting error distributions of the disk-integrated Earth OLRs for Groups A, B, C, and D, respectively.
Paper: On the Observational Solid Angle in Estimating the Moon-based Disk-integrated Earth Outgoing Longwave Radiation
Authors: Hanlin Ye, Huadong Guo, Dong Liang, Zhen Xu, Yin Jin, Guang Liu
Figure caption: Variation of (a) fitting the spherical model radius r and (b) the parameter a1 with changes in the Earth–Moon distance.
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Definitions of ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩, ﹩{R}_{{\rm{p}}}^{Y+}﹩, and ﹩{R}_{{\rm{p}}}^{Y-}﹩. The origin of the xi–yi and xe–ye coordinate systems corresponds to the planet’s center of mass. Gray shadows represent the planet’s shadow at a certain wavelength, with two-dimensional displacement vectors Δc. ﹩{R}_{{\rm{p}}}^{Y+}﹩ and ﹩{R}_{{\rm{p}}}^{Y-}﹩ are the lengths of the projected planetary shadow onto the Y-axis measured from the planet’s center of mass in the positive Y-direction and negative Y-direction, respectively. Similarly, ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩ and ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩ are the lengths of the projected planetary shadow onto the xi-axis measured from the planet’s center of mass in the positive and negative xi-direction, respectively. The xi–yi plane corresponds to the X–Y plane at ingress (left). ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩ and ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩ are the lengths of the projected planetary shadow onto the xe-axis measured from the planet’s center of mass in the positive and negative xe-direction, respectively. The xe–ye plane corresponds to the X–Y plane at egress (right).
Paper: Probing Two-dimensional Asymmetries of an Exoplanet Atmosphere from Chromatic Transit Variation
Authors: Shotaro Tada, Hajime Kawahara, Yui Kawashima, Takayuki Kotani, Kento Masuda
Figure caption: Inferred values of ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩, ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩, and ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩ based on the MCMC analysis of light curves simulated using catwoman (K. Jones & N. Espinoza 2020; N. Espinoza & K. Jones 2021). The values were converted using the estimated orbital parameters. The dots represent the median values from the MCMC sampling, while the error bars indicate the 68% credible intervals. Results are shown for both noiseless data and data with added Gaussian noise (mean = 0, standard deviation = 250 ppm). The true values of ﹩{R}_{{\rm{p}}}^{{\rm{morning}}}﹩ (blue) and ﹩{R}_{{\rm{p}}}^{{\rm{evening}}}﹩ (red) are shown as colored lines. The arrangement of the panels reflects the positional relationship between the regions on the planet contributing to each spectrum, as viewed from the nightside. The central panel shows the shape of the planetary shadow, along with the xi-axis and xe-axis. φ is the angle between the direction of the planet’s orbital motion and the boundary of the semicircles, set to 90∘ to model a morning–evening asymmetry. The radius of the morning-side semicircle is denoted as ﹩{R}_{{\rm{p}}}^{{\rm{morning}}}﹩, and the radius of the evening-side semicircle is denoted as ﹩{R}_{{\rm{p}}}^{{\rm{evening}}}﹩.