adsabs/AstroCLIMB huggingface dataset:
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Corrected white light curves when the two WASP-121 b phase-curve visits are fitted together. We show our results with the IRACLIS extraction and compared to the ones in Mikal-Evans et al. (2022). Top: corrected light curves zoomed in the eclipses. Middle: full corrected light curves. Bottom: residuals between our best-fit light-curve model and corrected data with red and blue for the IRACLIS reductions and green for the reduced data in Mikal-Evans et al. (2022).
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: White light curves for the two WASP-121 b phase-curve visits obtained with our IRACLIS extraction and compared to the ones in ME22. The two visits were offset vertically (5  ×  106 e−) and in time (by −257 orbital periods) for clarity. The observation reacquisitions (reacq) are also annotated.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Corrected spectral light curves (left) and corresponding residuals (right) for the medium spectral binning. The binning is similar to previous works using reductions from IRACLIS, such as Tsiaras et al. (2018), Changeat et al. (2022), and Edwards et al. (2023).
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Corrected spectral light curves (left) and corresponding residuals (right) for the low spectral binning. This is the same binning employed in Mikal-Evans et al. (2022). Higher binning resolution fits (e.g., medium resolution) are also performed and presented in Figure B6.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Displacement of the raw images onto the detector for the 2019 observation. The three segments, separated by the reacquisition events, are clearly visible on those diagnostics.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Posterior distributions of the white light-curve fits with POP when fitting the two phase-curve visits independently. The recovered parameters show differences in both the phase-curve model and the instrument systematics.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Temperature–pressure profiles (T–p) obtained by the 1.5D retrievals on the low-resolution spectra by varying the hotspot size (A HS) and offset (D HS). Left panel: nightside. Middle panel: dayside. Right panel: hotspot. While the thermal structure are different, the conclusions on the thermal structure of WASP-121 b from those runs would be the same, independently from the hotspot assumptions. We also note that one model (A HS = 50, and D HS = 30) has a significantly higher Bayesian evidence. The models obtained: ln(E) = 1550.3, for A HS = 30, and D HS = 30; ln(E) = 1510.6, for A HS = 50, and D HS = 10; ln(E) = 1538.8, for A HS = 50, and D HS = 20; ln(E) = 1554.5, for A HS = 50, and D HS = 30; and ln(E) = 1537.5, for A HS = 50, and D HS = 40.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Posterior distributions for the atmosphere of WASP-121 b obtained on the low-resolution spectra by varying the hotspot size (A HS) and offset (D HS). The color code is the same as in Figure C5. Independently from the hotspot assumptions, all those retrievals of WASP-121 b phase-curve data have a supersolar C/O with 0.62 < C/O < 1.11, while the retrieved metallicity is between C/O with −1.27 < log(Z) < 0.77. For all cases, we do not find evidence of a fully opaque nightside cloud deck. One model (A HS = 50, and D HS = 30) has a significantly higher Bayesian evidence. The models obtained: ln(E) = 1550.3, for A HS = 30, and D HS = 30; ln(E) = 1510.6, for A HS = 50, and D HS = 10; ln(E) = 1538.8, for A HS = 50, and D HS = 20; ln(E) = 1554.5, for A HS = 50, and D HS = 30; and ln(E) = 1537.5, for A HS = 50, and D HS = 40.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Transit (left) and eclipse (right) spectra of WASP-121 b analyzed in this work. Different observations are offset in the y-axis. Best-fit models from the 1D retrievals are shown in solid lines. Dashed lines show featureless models for visual comparison.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Posterior distributions for the atmosphere of WASP-121 b obtained by the 1.5D retrievals on different reduction methods. Green: spectra at “Low” resolution from ME22. Red: spectra at low resolution obtained using the 4-short instrument systematic model. Blue: spectra at medium resolution obtained using the 4-short instrument systematic model.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Profiles of Brunt–Väisälä frequency squared ﹩{{ \mathcal N }}^{2}=\left(g/\rho \right)\left({\rm{d}}\rho /{\rm{d}}z\right)﹩ for the retrieved thermal profiles in Figure C1. Dotted lines at p = 101 and p = 105 Pa show the upper and lower boundary of the GCM model. In this region, flows are stably stratified (﹩{{ \mathcal N }}^{2}\geqslant 0﹩); hence, they satisfy the hydrostatic balance approximation of the model equations. For p > 106, the nightside, hotspot, and initial profiles exhibit a jump in stratification.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Emission spectra of WASP-121 b, obtained at different phases from various reduction methods. Green: spectra at “Low” resolution from ME22. Red: spectra at low resolution obtained using the 4-short instrument systematic model. Blue: spectra at medium resolution obtained using the 4-short instrument systematic model. Orange: spectra at medium resolution obtained using the 2-short instrument systematic model. All the reductions are consistent with each other. Note that phases 0.07 and 0.93 do not exist in ME22; hence, we instead plot their phase 0.05 and 0.095.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Temperature–pressure profiles (T–p) obtained by the 1.5D retrievals on the spectra from different reductions. Left panel: nightside. Middle panel: dayside. Right panel: hotspot. We show the extent of the radiative contribution function for the low-resolution retrieval with dashed lines. The retrievals on those different reductions are consistent and provide a similar picture.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Sensitivity tests for four forward models, modified at 3 × σ from the best-fit chemistry values inferred in the retrieval (on the low-resolution data). Top left: the metallicity is reduced to Z = 0.270. Top right: the metallicity is increased to Z = 1.419. Bottom left: the C/O ratio is reduced to C/O = 0.658. Bottom right: the C/O ratio is increased to C/O = 0.898. In all four cases, the simulated phase-curve spectra do not match the observations, highlighting the sensitivity of those data sets to chemistry parameters.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Chemistry of the main species recovered from the phase-curve data (low-resolution reduction). Red: hotspot. Orange: dayside. Blue: nightside. Those chemical profiles show thermal dissociation of main molecules such as H2, H2O, CO, CO2, TiO, and VO, at the hotspot of WASP-121 b.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: WASP-121 b chemical maps centered around the substellar point for H2, H, H− and e− at two different times (t = 49, and t = 62 days) and two pressure levels (p = 105 Pa, and p = 5 × 103 Pa). Those maps are obtained by postprocessing the temperature fields (top row) from the BOB dynamics calculations with the TAUREX library.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Posterior distributions obtained for the five eclipse fits. Yellow: Eclipse 1. Blue: Eclipse 2. Green: Eclipse 3. Red: Eclipse 4. Purple: Eclipse 5. Note that the chemistry parameters of the equilibrium model GGCHEM in those fits are fixed to the median values obtained by the 1.5D phase-curve retrieval (log Z = −0.19, C/O = 0.80). The five eclipses are consistent with similarly inverted thermal structures; however, the posterior distributions are not the same in the middle of the atmosphere (T 1 to T 3). Large-scale atmospheric variability could create those observable departures in the thermal profiles.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: WASP-121 b chemical maps centered around the substellar point for TiO, VO, and FeH at two different times (t = 49, and t = 62 days) and two pressure levels (p = 105, and p = 5 × 103 Pa). Those maps are obtained by postprocessing the temperature fields (top row) obtained from the BOB dynamics calculations with the TAUREX library.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: Posterior distributions obtained for the three transit fits. Yellow: Transit 1. Blue: Transit 2. Green: Transit 3. Note that the chemistry parameters of the equilibrium model GGCHEM in those fits are fixed to the median values obtained by the 1.5D phase-curve retrieval (log Z = −0.19, C/O = 0.80). Transit 1 shows an atmosphere with moderate hazes but absorption at high altitude from water. Transit 2 shows multimodal solutions involving either a fully ionized atmosphere with unphysically high temperatures or a cloudy/hazy atmosphere. Transit 3 displays an atmosphere with opaque clouds.
Paper: Is the Atmosphere of the Ultra-hot Jupiter WASP-121 b Variable?
Authors: Q. Changeat, J. W. Skinner, J. Y-K. Cho, J. Nättilä, I. P. Waldmann, A. F. Al-Refaie, A. Dyrek, B. Edwards, T. Mikal-Evans, M. Joshua, G. Morello, N. Skaf, A. Tsiaras, O. Venot, K. H. Yip
Figure caption: WASP-121 b chemical maps centered around the substellar point for H2O, CO, CH4, and CO2 at two different times (t = 49, and t = 62 days) and two pressure levels (p = 105, and p = 5 × 103 Pa). Those maps are obtained by postprocessing the temperature fields (top row) obtained from the BOB dynamics calculations with the TAUREX library.
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: The measurements of the power spectra, ﹩{C}_{{\ell }}^{{yy}}﹩ (y-auto; upper left), ﹩{C}_{{\ell }}^{\mathrm{TT}}﹩ (ISW-auto; upper right) and ﹩{C}_{{\ell }}^{y{\rm{T}}}﹩ (ISW-y; lower). The black dots and bars in each case are the means of the spectrum measured from the associated map and the error bars are estimated as the square root of the diagonal values of the corresponding covariance matrix. Other curves have been defined in the legend of each plot.
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: Left: a comparison between the constraints on the amplitude of the mass fluctuations σ 8 scaled by the square root of the matter density Ωm estimated in this study using angular power spectra and the results from other studies. Right: a comparison between the constraints on the matter density parameter and the estimates from other studies. These studies include data from SPT-3G (Dutcher et al. 2021), ACT DR4 (Aiola et al. 2020), DES Y3 2 × 2 pt MAGLIM (Porredon et al. 2022), DES-Y3 cosmic shear (Secco et al. 2022), DES-Y1 cosmic shear (Troxel et al. 2018), Subaru HSC Y1×tSZ (Osato et al. 2019), HSC-Y1 ξ ± cosmic shear (Hamana et al. 2020b), the HSC-Y1 power spectrum (Hamana et al. 2020a), and KiDS-1000 ξ ± (Heymans et al. 2021) and KiDS-1000 × tSZ (Tröster et al. 2022). We also compare our results with measurements from Planck Collaboration et al. (2020).
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: Posterior distributions from MCMC with the full covariance matrix for the six free parameters in our model. The figure shows the joint constraints for all parameter pairs and the marginalized distributions for each parameter along the table diagonal. ﹩{\widetilde{W}}^{\mathrm{SZ}}﹩ is a dimensionless quantity defined in Equation (12).
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: The six independent blocks of the full correlation matrix defined in Equation (7). The diagonal blocks show the standard correlations for the TT, yy, and Ty spectra; the off-diagonal blocks show the additional cross correlations between different spectra. The correlation values are shown for pairs of the effective band power multipoles defined in Table 1.
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: Upper left: the measurements of the ISW autopower spectrum using the true Planck ISW map (black solid line) and the 100 simulated ISWs map (colored lines). Upper right: the respective S/Ns of the 100 simulated ISW maps (red dots; with mean 2.90 and rms 0.24) and the true ISW map (black dashed line; 2.32). Lower left: the cross correlation power spectra of the 100 simulated ISWs map with the Planck tSZ map (colored lines) and the true Planck ISW map cross correlation. Lower right: the significance of the true ISW–tSZ cross correlation (black dashed line; 5.63) and the 100 simulated ones (blue dots; with mean 3.12 and rms 0.70).
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: Cross power spectrum of the CIB in three Planck frequencies with the ISW. The spectrum was measured using the public code NaMaster.
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: The ISW map (ΔT/T 0) with a 40% Galactic-plane mask superimposed.
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: All-sky Compton parameter map (y-map) measured by Planck based on the NILC algorithm. The point-source mask and the 40% Galactic-plane mask have been applied.
Paper: Cross Correlation between the Thermal Sunyaev–Zeldovich Effect and the Integrated Sachs–Wolfe Effect
Authors: Ayodeji Ibitoye, Wei-Ming Dai, Yin-Zhe Ma, Patricio Vielva, Denis Tramonte, Amare Abebe, Aroonkumar Beesham, Xuelei Chen
Figure caption: The effective redshift range driving the auto- and cross-power spectra, shown for three reference effective multipoles at ℓ = 10, 50, and 100.
Paper: Long-term Variations in the Orbital Period of Hot Jupiters from Transit-timing Analysis Using TESS Survey Data
Authors: Wenqin Wang, Zixin Zhang, Zhangliang Chen, Yonghao Wang, Cong Yu, Bo Ma
Figure caption: Part of the transit-timing residuals of CoRoT-2 b. The top panel presents the raw data, which are taken from Öztürk & Erdem (2019), while the bottom panel displays the same data with inflated error bars. In both panels, we show the residuals of the linear model fit to provide a clearer visual comparison, where it is clearly seen that the original measurement uncertainties from Öztürk & Erdem (2019) are too small.
Paper: Long-term Variations in the Orbital Period of Hot Jupiters from Transit-timing Analysis Using TESS Survey Data
Authors: Wenqin Wang, Zixin Zhang, Zhangliang Chen, Yonghao Wang, Cong Yu, Bo Ma
Figure caption: Distribution of the 3σ error bars of the rate of change of the period a for the 133 hot Jupiters with a good quadratic model fit. As can be seen from this distribution, we can detect a change in the period at an absolute rate ∣a∣ greater than ∼100 ms yr−1 for most of these hot Jupiters.
Paper: Long-term Variations in the Orbital Period of Hot Jupiters from Transit-timing Analysis Using TESS Survey Data
Authors: Wenqin Wang, Zixin Zhang, Zhangliang Chen, Yonghao Wang, Cong Yu, Bo Ma
Figure caption: The phase-folded light curve of WASP-12 b from TESS. The best-fit transit light-curve model from Mandel & Agol (2002) is also shown as a black solid line.
Paper: Long-term Variations in the Orbital Period of Hot Jupiters from Transit-timing Analysis Using TESS Survey Data
Authors: Wenqin Wang, Zixin Zhang, Zhangliang Chen, Yonghao Wang, Cong Yu, Bo Ma
Figure caption: TESS transit times for WASP-12 b. The epoch number is calculated relative to a reference zero epoch from the literature.
Paper: Long-term Variations in the Orbital Period of Hot Jupiters from Transit-timing Analysis Using TESS Survey Data
Authors: Wenqin Wang, Zixin Zhang, Zhangliang Chen, Yonghao Wang, Cong Yu, Bo Ma
Figure caption: Posterior distribution of the fitted model parameters of HAT-P-16 b from our MCMC quadratic model fitting.
Paper: Long-term Variations in the Orbital Period of Hot Jupiters from Transit-timing Analysis Using TESS Survey Data
Authors: Wenqin Wang, Zixin Zhang, Zhangliang Chen, Yonghao Wang, Cong Yu, Bo Ma
Figure caption: Individual transit light curve of WASP-12b from sector 1 observations of TESS.
Paper: The Presolar Grain Database. I. Silicon Carbide
Authors: Thomas Stephan, Reto Trappitsch, Peter Hoppe, Andrew M. Davis, Maitrayee Bose, Asmaa Boujibar, Frank Gyngard, K. Mairin Hynes, Nan Liu, Larry R. Nittler, Ryan C. Ogliore
Figure caption: A periodic table of the elements showing for each element the number of SiC grains with data in the PGD.
Paper: The Presolar Grain Database. I. Silicon Carbide
Authors: Thomas Stephan, Reto Trappitsch, Peter Hoppe, Andrew M. Davis, Maitrayee Bose, Asmaa Boujibar, Frank Gyngard, K. Mairin Hynes, Nan Liu, Larry R. Nittler, Ryan C. Ogliore
Figure caption: Carbon, nitrogen, silicon, and inferred aluminum isotope ratios of individual presolar SiC mainstream grains from the PGD. Horizontal and vertical solid lines show solar and terrestrial values for comparison. Colored areas show the ranges allowed for mainstream grains. Data points outside the colored areas have large uncertainties (not shown here) such that they are still consistent with being mainstream grains. Most mainstream grains plot in the silicon three-isotope plot (b) between the dashed line and the line marked M2 around the mainstream weighted regression line (M0) drawn in red. However, we extend the allowed area for mainstream grains to the line marked M1 to include the tail of the distribution. The horizontal line in panel (c), labeled solar, refers to the initial 26Al/27Al ratio of the solar system (5.2 × 10−5; Jacobsen et al. 2008). Shown in (d) is the horizontal distance from the mainstream line (Δ30Si) plotted against the carbon isotope ratio. Further details are given in the main text and the Appendix.