adsabs/AstroCLIMB huggingface dataset:
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: (a) Number of cores detected against the 1σ mass sensitivity. The mass of clump is coded as the size of circle. (b) Number of cores detected against the physical resolution. The distance of clump is coded as the size of circle.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: The cartoon of protocluster evolution from infrared dark, to infrared weak, and to infrared bright. The black filamentary structures connect the dense cores at the early stage (Morii et al. 2023) and transfer gas inwards (Xu et al. 2023a), and then fade away as the protocluster evolves (Zhou et al. 2022). The black arrows indicate inflow gas streams.  = prestellar cores;  = protostellar cores;  = OB stars.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: The ﹩{M}_{\max }﹩ vs. M cluster relation. The ASSEMBLE and the ASHES Pilots are plotted with errorbars. The blue solid line shows the second-order polynomial fitting of all the data points. ﹩{M}_{\max }\propto {M}_{\mathrm{cluster}}^{0.88}﹩ in the blue box indicates the power-law index in the first-order approximation. The gray dashed line shows the linear regression of all the data points. The green solid line shows the polynomial fitting of the data from 139 star clusters (Weidner et al. 2013), with first-order approximation of ﹩{M}_{\star \max }\propto {M}_{\star \mathrm{cluster}}^{0.58}﹩ in the upper green box. The dashed green line as well as the lower green box shows the relation from smoothed particle hydrodynamics simulation (Bonnell et al. 2003, 2004).
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The white-light images obtained from the SOHO/LASCO coronagraphs on 2015 June 18, capturing the first CME of CR2165. Subplots (a1) and (b1) show the LASCO-C2 and -C3 images, respectively. The traced GCS structure is superimposed on these images, indicated by the blue overlay in subplots (a2) and (b2). The temporal evolution of the traced CME’s propagation distance (h), speed (v), and acceleration (a) can be observed in subplots (c1), (c2), and (c3), respectively. Corresponding expansion properties (R, v  e , a  e ) are also shown in the right subplots.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption:                         The 1.28 GHz radio emissions of the ASSEMBLE protoclusters are shown with yellow contours, with logarithmically spaced levels starting from 5σ to the peak flux. The background gray color maps show the ATLASGAL 870 μm continuum emission. The overlaid black contours show the ALMA 870 μm continuum emission as the right panels in Figure 2.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Figure illustrates the flux rope model implemented in SWASTi-CME. The left subplot depicts the evolution of the formed flux rope structure as it propagates radially and crosses the inner boundary of the MHD domain. On the right subplot, the magnetic values are displayed for the overlapping region between the flux rope and the MHD boundary, shown as black circle in the left subplot.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: The ﹩{ \mathcal Q }﹩ values vs. luminosity-to-mass ratio L/M (left) and temperature T dust (right). The linear regression results including the fitting model, Pearson correlation coefficient ρ p, Spearman rank correlation coefficient ρ s, and scatter σ are shown on the upper left. ASHES clumps are shown in the ﹩{ \mathcal Q }﹩ vs. T dust panel with gray points.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: The mass segregation integrals ﹩{{ \mathcal I }}_{{\rm{\Lambda }}}^{\mathrm{MSR}}﹩ of the ASSEMBLE and the ASHES are shown as blue and gray histograms with errorbars. The p-values of the Mann–Whitney U test between ASSEMBLE, ASHES, and Gaussian distributions (μ = 1, σ = 0.1) are shown in three colors, which are attached in the upper right corner.
Paper: The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation
Authors: Fengwei Xu, Ke Wang, Tie Liu, Mengyao Tang, Neal J. Evans II, Aina Palau, Kaho Morii, Jinhua He, Patricio Sanhueza, Hong-Li Liu, Amelia Stutz, Qizhou Zhang, Xi Chen, Pak Shing Li, Gilberto C. Gómez, Enrique Vázquez-Semadeni, Shanghuo Li, Xiaofeng Mai, Xing Lu, Meizhu Liu, Li Chen, Chuanshou Li, Hongqiong Shi, Zhiyuan Ren, Di Li, Guido Garay, Leonardo Bronfman, Lokesh Dewangan, Mika Juvela, Chang Won Lee, S. Zhang, Nannan Yue, Chao Wang, Yifei Ge, Wenyu Jiao, Qiuyi Luo, J.-W. Zhou, Ken'ichi Tatematsu, James O. Chibueze, Keyun Su, Shenglan Sun, I. Ristorcelli, L. Viktor Toth
Figure caption: MST results of ASSEMBLE protoclusters. Prestellar and protostellar cores are assigned with blue and red colors, with the size normalized by the square root of core mass ﹩\sqrt{{M}_{\mathrm{core}}}﹩ and stretched within the mass range. Yellow segments connect the cores to minimize the sum of the lengths of segments. The beam size is shown on the lower left, and the scale bar is on the right.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The evolution of real case CME in the heliosphere and its interaction with ambient solar wind of CR2165 is depicted in four time steps. Top row (a)–(d): represents the ecliptic plane, showcasing surface plot of the scaled density of the solar wind with the 3D CME (depicted in pink) propagating through it. Bottom row (e)–(f): a 2D slice of the 3D CME structure (shown in green), along with the surface plot of the solar wind speed, and line contours represent the scaled density.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Figure displays a time snapshot of the SWASTi-CME results for CR2165 on 2015 June 22 at 10:26 UT. Subplots (a1)–(a3) depict the speed, scaled density, and radial magnetic field results for the flux rope (FR) CMEs, while subplots (b1)–(b3) show the corresponding results for the cone CMEs. At this particular time, three CMEs, namely CME1, CME2, and CME3, are present in the simulation domain.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Figure showcases the drag force acting on the CME front due to anisotropic ambient conditions. Subplots (a1)–(f1) depict the evolution of the drag force pattern on the front of real case CME of CR2165 as it advances in the heliosphere. The positive drag has been displayed using color map while negative drag is in gray scale. Subplots (a2)–(f2) display the histogram of magnitude of drag force corresponding to (a1)–(f1) subplots.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Temporal evolution of median of the CME properties for CR2165. The panels (a1) to (f1) represent the temporal profile of median of CME thermal pressure (a1), magnetic pressure (b1), ram pressure (c1), speed (d1), density (e1), and temperature (f1) in log-log scale. In the subplots (a2) to (f2), just below the panels showing variations in the median of CME properties, the change in the gradient of these CME properties in log-log scale at different time steps is shown (see Equation (14)). The shaded regions in slope subplots correspond to the initial settling phase of the CME, which has been taken to be 24 hr.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Time-series plot of in situ measurements at 1 au for CR2165 (a1)–(a4) and CR2238 (b1)–(b4). The simulated results for the FR and cone CMEs are represented by blue and green colors, respectively, while the observed OMNI data are depicted in brown. Vertical dashed lines of various colors indicate the beginning of the sheath region corresponding to each CME. Both the SWASTi and OMNI data are plotted with a time cadence of 5 minutes.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The figure showcases the equatorial plane of the numerical setup used to study the influence of ambient solar wind on a coronal mass ejection (CME). Subplots (a1)–(a3) present the speed, scaled density, and radial magnetic field for the real case of CR2165, while subplots (b1)–(b3) depict the results of the synthetic case.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The temporal evolution of the total volume of the CME is presented for both the synthetic and real cases of CR2165 (a1), (a2), and (a3) and CR2238 (b1), (b2), and (b3). A rough sketch of negative and positive drag has been shown in subplot (c). And the evolution of the ratio of area on which positive and negative drag forces act is shown in (d1) and (d2).
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: The picture depicts the magnetic profile of a CME formed through FRi3D, where the strengths of magnetic fields are color coded. The 3D profile of Bz is shown in subplot (a), whose 2D slice has been cut in the X–Z plane at Y = 0 and shown in subplots (b1)–(b4). The 1D profile of magnetic field at Z = 0 of this 2D slice is shown in subplot (c).
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Figure demonstrates the tracing of the 3D structure of a CME (denoted by white) in the heliosphere. This volumetric plot showcases the changes in dynamic pressure of the solar wind (denoted by the color bar) caused by the propagation of the CME. The left subplot displays the deformation of the CME front resulting from the interaction with an SIR.
Paper: SWASTi-CME: A Physics-based Model to Study Coronal Mass Ejection Evolution and Its Interaction with Solar Wind
Authors: Prateek Mayank, Bhargav Vaidya, Wageesh Mishra, D. Chakrabarty
Figure caption: Comparison of FRi3D CME with the observed OMNI data having in situ signatures of CME. The magnetic field components are in nT and HEEQ coordinate system.
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: Instantaneous spatial temperature maps T(λ, ϕ, p, t), where λ is the longitude, ϕ is the latitude, p is the pressure, and t is the time; p = 105 Pa level, at t = {49, 62, 137} planetary days after the start of the simulation are shown. The maps demonstrate that very different temperature distributions arise at different times. Maps are in spherical orthographic projection, where the white circle marks the substellar point. The fields result from simulations that are thermally forced by the T–p profiles in Figure 2. The planet’s hotspot is highly variable not only in location and time but also in shape. These storms are planetary-scale, coherent, and exhibit repetitive behaviors, leading to high amplitude and identifiable periodic signature in the planet’s flux.
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: One-dimensional (1D) thermal structure recovered by our retrieval analysis of the five eclipse observations with 1σ confidence region (left), and T–p profiles from multiple times (t ∈ [40, 185] days) at the substellar point from a three-dimensional (3D) atmospheric dynamics simulation (right). The magnitude of variability in p ∈ [105, 103] Pa is ∼300 K, which is consistent with the variation predicted by the 3D simulation. Dashed gray lines show the vertical extent of the atmosphere modeled by the simulations in this study. Note these profiles are not like-for-like comparable because the retrieved thermal structure is global and substellar temperature predictions are local.
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: Disk-averaged blackbody flux variations at 1.3 μm using Planck’s law for a single layer in the middle of our modeled domain (104 Pa), and centered on four regions: dayside (substellar point), eastern terminator, western terminator, and nightside (antistellar point). The flux is normalized by the mean value of the dayside. The fluxes are quasiperiodic on periods of ∼5 days, with variations of ∼5% to ∼10%. The normalized flux for the west terminator is generally lower than that of the east terminator, indicating that a phase-curve observation of this planet is more likely to have an eastward-shifted phase offset. The level of variability is compatible with the uncertainties of our HST observations; however, note that the HST instrument systematics makes absolute flux measurements at such p-level highly uncertain (see, e.g., Yip et al. 2021; 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: Examples of observed transit (left) and eclipse (right) spectra of WASP-121 b analyzed in this work. The spectra shown are corrected for vertical offsets to highlight the differences in spectral shapes. Variability in the planet’s weather patterns could create such variations in the spectroscopic data; this is strongly suggested in high-resolution simulations carried out for this planet in this work (see, e.g., Figures 6 and 7). For example, during the transits, the observed temporal variations could be interpreted as a formation of intermittent clouds and/or hazes; during the eclipse, the observed variations may be due to subtle changes in the thermal structure of the atmosphere—induced by motions of hot/cold regions from the planet’s atmospheric dynamics.
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 distribution of the chemistry retrieved from the phase-curve data using the “Low” resolution spectra (left), the “Medium” resolution spectra (middle), and the spectra from ME22 (right). The constraints obtained on metallicity Z and C/O ratio are consistent with a solar to slightly subsolar metallicity and a supersolar C/O ratio, indicating the formation of the planet likely occurred beyond the snow line. The blue line indicates the solar values for Z and C/O ratio. The full posterior distributions for the low-resolution retrieval are available in Figure C3.
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 individually. The two observations, while close, present differences that could come from either atmospheric variability or instrument systematics. Note that the second-order coefficients from the sine phase-curve models are fixed to the best-fit values from the combined fit (see Figure B3).
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: Comparison of recovered white light curves, fitted with the POP when using different assumptions for the detector and long-term ramp models. We show in solid line the median of each tested model, and for our preferred set of assumption, we show the resulting observations. Red: two-parameter exponential ramp model from Tsiaras et al. (2016c) and hybrid long-term ramp. Blue: four parameters exponential ramp model from de Wit et al. (2018) and hybrid long-term ramp. Green: two-parameter exponential ramp model and linear long-term ramp for each segment. Orange: two-parameter exponential ramp model and quadratic long-term ramp for each segment. The hybrid long-term ramp consists in a quadratic trend for the first segment of each visit and a linear ramp for the remaining four segments, as done in ME22. This, as well as Figure B2, demonstrates that the recovered light curve depends on the assumption for the long-term ramp.
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 using four different detector ramp models (see Figure B1). Red: two-parameter exponential ramp model from Tsiaras et al. (2016c). Blue: four parameters exponential ramp model from de Wit et al. (2018). Green: two-parameter exponential ramp model and linear long-term ramp for each segment. Orange: two-parameter exponential ramp model and quadratic long-term ramp for each segment. The recovered orbital parameters are independent of the detector short-term ramp, but they are impacted by the choice of the long-term trend.
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: Spectroscopic eclipse flux obtained at three different times, t = {49, 62, 137} days, when the dynamics calculations are postprocessed (top), and spectroscopic differences between two times, t = 62 days, and t = 49 days. In the top panel, the eclipse spectra obtained for Observation 3 (green) and Observation 4 (purple) are also shown for reference. The simulation shows that the atmospheric variability should be wavelength dependent since, e.g., H− is highly sensitive to thermal dissociation (impacting the short wavelengths) while H2O remains more chemically stable.