adsabs/AstroCLIMB huggingface dataset:
Paper: H2 Chemistry and Protonation in the Dayside Venusian Upper Atmosphere
Authors: Shiqi Wu, Xiaoshu Wu, Yanxing Liu, Jun Cui
Figure caption: The solar extreme-ultraviolet and soft X-ray spectrum at 0.05–189.95 nm used as model input at moderate solar activity, retrieved from the Flare Irradiance Spectral Model version 2 at the Earth (P. C. Chamberlin et al. 2020) and extrapolated to the mean heliocentric distance of Venus.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: The O − C diagram of the 10 targets presented in this paper. The top panel shows the curve (O − C)1 determined by Equation (1). The residuals, which remove the quadratic correction term from the (O − C)1 curve, are plotted in the lower panel. The units of the (O − C)1 and residual are in days. The errors not given in Table 4 are set to 0.001.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: The O − C diagram of J0132, J1300, and J1402 with periodic variations. The top panel shows the (O − C)1 curve determined by Equation (1) as in the top panel of Figure 3. The (O − C)2, which remove the quadratic correction term from the (O − C)1 curve, are plotted in the middle panel. The residuals from the full ephemeris of Equation (2) are displayed in the lower panel. The units of (O − C)1, (O − C)2, and residual are in days. The different colors of the symbols represent different data, as explained in the diagram.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: Mass–luminosity diagram (left panel) and mass–radius diagram (right panel). The solid and dotted lines represent the ZAMS and TAMS lines constructed using the binary star evolution code provided by J. R. Hurley et al. (2002). The solid and open stars for different colors represent the more massive star (M) and less massive star (L) of the 10 targets, respectively.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: The relation between orbital angular momentum and total mass for detached and contact binaries. The detached binaries (Z. Eker et al. 2006) and the contact binary (K. Yakut & P. P. Eggleton 2005; Z. Eker et al. 2006) are separated by the boundary line (Z. Eker et al. 2006). The black crosses represent the detached binaries, and the black solid and open circles refer to the A-type and W-type contact binaries, respectively. Different colored stars represent different targets.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: Left panel: Theoretical light curves (orange solid line) fitted by the W-D code compared to all available TMTS observations (gray dots) for the 10 targets. One dark spot is added to the primary or secondary star for each target. Right panel: RVs and fitted curves of W-D code. The gray filled triangles and circles represent the observed primary (hotter) and secondary (cooler) components, respectively. The blue and red solid lines represent the best-fit RV curves.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: The Hα region of LAMOST LR spectra (black line), synthetic spectra (yellow line), and subtracted spectra (blue line) for the eight targets. The EWs of Hα are shown in each panel for each spectra, with units in Å.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: Geometrical structures of 10 targets at phases 0, 0.25, 0.5, and 0.75. The areas marked with blue cross symbols represent the added dark spots on the components.
Paper: Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
Authors: Qiqi Xia, Xiaofeng Wang, Kai Li, Xiang Gao, Fangzhou Guo, Jie Lin, Cheng Liu, Jun Mo, Haowei Peng, Qichun Liu, Gaobo Xi, Shengyu Yan, Xiaojun Jiang, Jicheng Zhang, Cui-Ying Song, Jianrong Shi, Xiaoran Ma, Danfeng Xiang, Wenxiong Li
Figure caption: The LAMOST low-resolution spectra of eight targets. The spectral types and positions of some characteristic spectral lines are labeled in the plot. Each spectrum is accompanied by the corresponding name of the target on the right side.
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: A star-forming complex in NGC 1672 is shown in optical broadband HST filters in panel (a) and in HST-Hα in panel (c). MUSE-defined H II regions and DIG are outlined in panel (b). The complexity of the H II region is highlighted in panel (d), which shows the locations of several star clusters and massive stars (star symbols) and full to partial shells of ionized gas (curved lines). Ionizing radiation leaks out of H II regions from open shells and beyond their walls, as illustrated in panel (e). Panel (f) shows examples of different kinds of shell structures visible even in compact nebulae, many of which are leaking ionizing radiation into their surroundings. The left image in each pair shows just Hα emission, and the right image is a composite of B, V, and Hα.
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: The ratio of the HST to MUSE Hα fluxes checked against other nebula properties for NGC 1566 and NGC 4303. We show (from left to right) the Hα flux ratio vs. the MUSE Hα flux, MUSE Hα velocity, galactocentric radius, and the Hα equivalent width measured directly from the MUSE spectra. There is no obvious trend in the flux ratio with Hα velocity or galactocentric distance (middle two panels), although for NGC 4303 there appears to be a decline in the HST-to-MUSE flux ratio at higher velocities (>100 km s−1), likely due to the filter response.
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: Demonstration of how measurements of the radii of H II regions from HST-Hα images drastically reduce the uncertainties on stellar feedback calculations. The red points and orange bars indicate the range in size and pressure spanned by the lower and upper limits determined for H II regions in NGC 1672 (A. T. Barnes et al. 2021). The dominant uncertainty comes from having only upper limits on H II region size measurements in the ground-based observations. The blue points show that with the addition of HST-based size measurements, the pressure can be measured to within a factor of ∼2–3, rather than being constrained to a factor of ∼​​​​​​​100.
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: Histograms of the final HST-to-MUSE Hα flux ratios. We show histograms of the HST-to-MUSE Hα flux ratios for all regions (left panel) and for regions with MUSE Hα fluxes higher than 10−15 erg s cm−2 (right). The dashed curves show the best-fit Gaussian distribution in each panel, and the 1σ standard deviation is written in the upper right corner. For the bright Hα regions, ≈70% of the pixels in the HST-Hα maps have fluxes within just ≈15% of those measured from the MUSE spectra.
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: Median HST-based SEDs of young, gas- and dust-rich clusters (blue points) and old globular clusters (red points) for 10 PHANGS-HST-Hα galaxies. The SEDs are normalized at the I band. The young and old populations can have similar declining broadband fluxes toward shorter wavelengths but have very different Hα fluxes (see the clear separation between red and blue data points at 658 nm). Figure adapted from K. Henny et al. (2025, in preparation).
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: Difference between using the F555W vs. F550M and F547M filters for continuum subtraction. The top row shows the difference between using the F555W (left) and F550M (middle) filters for continuum subtraction in NGC 1672, while the bottom row shows the difference between F555W and F547M for NGC 3351. The right panels show 2D histogram density plots of the Hα flux at each pixel for both cases. Overlaid is a dashed line showing the y = x relation, and the dotted line in the bottom panel shows an offset of y = x − 0.3.
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: The ratio of HST to MUSE Hα fluxes in NGC 628-C is checked against other nebula properties. We show (from left to right) the Hα flux ratio vs. the MUSE Hα flux (left panel), MUSE Hα velocity (second panel), galactocentric radius (third panel), and the Hα equivalent width measured directly from the MUSE spectra (right panel). There is no obvious trend in the flux ratio with Hα velocity or galactocentric distance (middle two panels).
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: Footprints of the HST-Hα images (red) and MUSE IFU observations (white) are shown on HST BVI color images for the 17 galaxies that currently have Hα observations available. A 1 kpc scale bar is shown in each panel.
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: Spectra of ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩ (top left), ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩ (top right), ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩ (bottom left), and ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩ (bottom right). The dots with error bars represent the median values from the MCMC sampling with 68% credible intervals. The colored dots indicate the case using α(λ) estimated from (Ttot + Tfull)/2, while the small gray dots indicate the case using α(λ) = 1. The central panel shows the positions on the planet that correspond to these spectra, along with the xi-axis, yi-axis, xe-axis, and ye-axis. The color of the points indicating those positions corresponds to the color of the dots in each spectrum. Since these spectra are not exact radii but rather projected lengths of the planet’s shadow disk onto the xi-axis or xe-axis, measured from the planet’s center of mass (Figure 4), the uncertainties of Δc shown in Figure 20 are also illustrated to indicate the uncertainties of the positions from which these values are projected.
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: Posterior distributions of each parameter for the ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩ spectrum (orange). The Rp at 10 bars is common for all four limbs (Figures 23–26). The posterior distributions from the analysis with the intrinsic spectral resolution (∼2700), assuming a uniform atmosphere (H. Kawahara et al. 2025, submitted), are overlaid for reference (gray).
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: Results of MCMC sampling for the spectra: (a) ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩, (b) ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩, (c) ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩, and (d) ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩. The dots with error bars represent the spectra shown in Figure 21, calculated using α(λ) estimated from (Ttot + Tfull)/2. The gray regions in each panel indicate the 68% credible intervals for each spectrum from the MCMC sampling. The black lines in each panel represent 10 randomly selected sampled models. The contributions of each molecule, gray clouds, and CIA to these models are also shown as colored or hatched shading, with an offset of −0.01Rs.
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: Posterior distributions of each parameter for the ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩ spectrum (dark orange). The Rp at 10 bars is common for all four limbs (Figures 23–26). The posterior distributions from the analysis with the intrinsic spectral resolution (∼2700), assuming a uniform atmosphere (H. Kawahara et al. 2024, submitted), are overlaid for reference (gray).
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: Posterior distributions of each parameter for the ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩ spectrum (dark blue). The Rp at 10 bars is common for all four limbs (Figures 23–26). The posterior distributions from the analysis with the intrinsic spectral resolution (∼2700), assuming a uniform atmosphere (H. Kawahara et al. 2024, submitted), are overlaid for reference (gray).
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: Posterior distributions of each parameter for the ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩ spectrum (blue). The Rp at 10 bars is common for all four limbs (Figures 23–26). The posterior distributions from the analysis with the intrinsic spectral resolution (∼2700), assuming a uniform atmosphere (H. Kawahara et al. 2024, submitted), are overlaid for reference (gray).
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: Variation of μ0.5, defined as the μ value where the specific intensity satisfies I(μ) = I(1)/2, across different wavelengths. These values were calculated using the specific intensities of a star with an effective temperature of 5500 K, ﹩\mathrm{log}g\,[{\rm{cgs}}]=4.5﹩, and metallicity [Fe/H] = 0.0, computed by T. O. Husser et al. (2013) using the spherically symmetric model of PHOENIX, and binned into 5 nm intervals.
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: Normalized specific intensities of a star with an effective temperature of 5500 K, ﹩\mathrm{log}g\,[{\rm{cgs}}]=4.5﹩, and metallicity [Fe/H] = 0.0, computed by T. O. Husser et al. (2013) using the spherically symmetric model of PHOENIX. The right panel provides a magnified view around the μ value where the intensity begins to drop sharply.
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: Spectra of ﹩{R}_{{\rm{p}}}^{x{\rm{e}}-}﹩ (top left), ﹩{R}_{{\rm{p}}}^{x{\rm{i}}+}﹩ (top right), ﹩{R}_{{\rm{p}}}^{x{\rm{i}}-}﹩ (bottom left), and ﹩{R}_{{\rm{p}}}^{x{\rm{e}}+}﹩ (bottom right). The dots with error bars represent the median values from the MCMC sampling with 68% credible intervals. The colored dots indicate reduction B, while the gray dots indicate reduction A.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: Fourier spectra of the O − C residuals for OGLE-BLAP-006. The upper panel shows the spectrum for long orbital periods, from 500 to 8000 days, derived from the residuals for OGLE’s 1.0 yr segments and KMTNet’s 0.5 yr segments. The lower panel displays the spectrum for short-period regions, from 4 to 600 days, obtained using the O − C residuals (shown in the inset) for KMTNet’s 2.0 day segments.
Paper: KMTNet View of Blue Large-amplitude Pulsators Toward the Galactic Bulge. I. Discovery of Wide-orbit Companions in OGLE-BLAP-006
Authors: Seung-Lee Kim, Chung-Uk Lee, Kyeongsoo Hong, Jae Woo Lee, Dong-Jin Kim, Sang-Mok Cha, Yongseok Lee, Dong-Joo Lee, Byeong-Gon Park
Figure caption: O − C diagram for the pulsation periods of OGLE-BLAP-007 (left) and OGLE-BLAP-009 (right). Red lines in the upper panels represent the parabolic fits; the corresponding residuals are shown in the lower panels.