adsabs/AstroCLIMB huggingface dataset:
Paper: The MOST Hosts Survey: Spectroscopic Observation of the Host Galaxies of ∼40,000 Transients Using DESI
Authors: Maayane T. Soumagnac, Peter Nugent, Robert A. Knop, Anna Y. Q. Ho, William Hohensee, Autumn Awbrey, Alexis Andersen, Greg Aldering, Matan Ventura, Jessica N. Aguilar, Steven Ahlen, Segev Y. Benzvi, David Brooks, Dillon Brout, Todd Claybaugh, Tamara M. Davis, Kyle Dawson, Axel de la Macorra, Arjun Dey, Biprateep Dey, Peter Doel, Kelly A. Douglass, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Or Graur, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Cullan Howlett, Alex G. Kim, Theodore Kisner, Anthony Kremin, Andrew Lambert, Martin Landriau, Dustin Lang, Laurent Le Guillou, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Adam D. Myers, Jundan Nie, Antonella Palmese, David Parkinson, Claire Poppett, Francisco Prada, Fei Qin, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, David J. Schlegel, Michael Schubnell, Joseph H. Silber, Gregory Tarlé, Benjamin A. Weaver, Zhimin Zhou
Figure caption: Distribution of magnitudes (dereddened) of the MOST Hosts candidates. The left panel shows the distribution for the entire sample. On the right panel, we show the distribution for hosts of transients for which a classification exists (top) and for hosts for which no classification is known (bottom).
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Graphical estimation of the parameters of DESC cohesive DDF strategies in the (﹩{N}_{{\rm{v}}}^{\mathrm{UDF}}﹩/observing night, ﹩{N}_{{\rm{v}}}^{\mathrm{DF}}﹩/season) parameter space. Black lines correspond to three configurations (﹩{N}_{{\rm{f}}}^{\mathrm{UDF}}﹩, ﹩{N}_{{\rm{s}}}^{\mathrm{UDF}}﹩) for a budget of 7%, a number of visits of 2.1 million, a cadence of observation of 2 days, and a season length of 180 days for the UDFs. The (﹩{N}_{{\rm{v}}}^{\mathrm{UDF}}﹩/observing night, ﹩{N}_{{\rm{v}}}^{\mathrm{DDF}}﹩/season) parameter space corresponding to the photo-z + WL (calibration) requirements (red dotted vertical lines) and SN Ia cosmological constraints (red dotted horizontal lines) is used to define the strategies (intersection points with the lines corresponding to the three (﹩{N}_{{\rm{f}}}^{\mathrm{UDF}}﹩, ﹩{N}_{{\rm{s}}}^{\mathrm{UDF}}﹩) configurations. On this plot are also reported the results corresponding to the SCOC phase 2 recommendations (SCOC_p2) and to a universal survey. Yellow areas around the photo-z + WL and SN Ia requirements correspond to ﹩{\rm{\Delta }}{m}_{5}^{b}﹩ = ± 0.05 and Δz complete = ±0.01, respectively. Markers correspond to strategies optimal for the SNe Ia (squares), fulfilling the photo-z/WL requirements (stars), or corresponding to compromises between the photo-z/WL and SN Ia constraints (circles).
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Photo-z metric Δm 5 for the proposed strategies, for each DDF and each band. The photo-z requirements are fulfilled if Δm 5 ≥ 0. The dashed line corresponds to Δm 5 = 0.
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: WL metric ﹩{r}^{\mathrm{WL}}=\tfrac{{N}_{\mathrm{visits}}^{\mathrm{OS}}}{{N}_{\mathrm{visits}}^{\mathrm{WL}\,\mathrm{req}}}﹩ for the proposed strategies and for each field/band. The dashed (dotted) line correspond to r WL = 1 (1.6). The WL requirements are fulfilled if r WL ≥ 1.
Paper: Investigating the Behavior and Spatiotemporal Variations of Green-line Emission in the Solar Corona
Authors: Jacob Oloketuyi, Yu Liu, Linhua Deng, Abouazza Elmhamdi, Fengrong Zhu, Ayodeji Ibitoye, Opeyemi Omole, Feiyang Sha, Qiang Liu
Figure caption: The wavelet analysis of green-line coronal emissions for high and low latitudes of the Sun.
Paper: Investigating the Behavior and Spatiotemporal Variations of Green-line Emission in the Solar Corona
Authors: Jacob Oloketuyi, Yu Liu, Linhua Deng, Abouazza Elmhamdi, Fengrong Zhu, Ayodeji Ibitoye, Opeyemi Omole, Feiyang Sha, Qiang Liu
Figure caption: The PSD analysis of green-line coronal emissions between the solar north and south regions across the solar cycles.
Paper: Investigating the Behavior and Spatiotemporal Variations of Green-line Emission in the Solar Corona
Authors: Jacob Oloketuyi, Yu Liu, Linhua Deng, Abouazza Elmhamdi, Fengrong Zhu, Ayodeji Ibitoye, Opeyemi Omole, Feiyang Sha, Qiang Liu
Figure caption: The wavelet analysis of green-line coronal emissions for (a) the global Sun, (b) the solar north, and (c) the solar south.
Paper: Revisiting the Hβ Size–Luminosity Relation Using a Uniform Reverberation-mapping Analysis
Authors: Shu Wang, Jong-Hak Woo
Figure caption: The R BLR–L relation for the sample with X-ray luminosity measured by H. Liu et al. (2021). The relation based on L 5100 (upper left), L Hβ  (upper right), L [O III] (lower left), and L 2−10keV (lower right) are presented. Twenty-four low and eight high-λ Edd AGNs (divided by logλ Edd = −0.3) are shown in blue and red color, respectively. The name of each high λ Edd AGN is given for comparing their different offset in different panels. The brown dashed lines represent the best-fit relations of the sub-Eddington subsample while the orange lines are randomly selected 50 realizations from the MCMC samples for illustrating the dispersion of the relation. The best-fit slope β and the intrinsic scatter σ int for the low-λ Edd subsample are presented at the upper left corner, while the values in the brackets represent the results for the total sample.
Paper: Revisiting the Hβ Size–Luminosity Relation Using a Uniform Reverberation-mapping Analysis
Authors: Shu Wang, Jong-Hak Woo
Figure caption:  R BLR as a function of different luminosity tracers in the average scheme, including L 5100 (left), L Hβ  (middle), and L [O III] (right). Sub- and super-Eddington objects are displayed using blue and red color, respectively. The brown dashed lines represent the best-fit relations based on the total sample, and the orange lines are randomly selected 50 realizations from the MCMC samples for illustrating the dispersion of the relation. In each panel, the best-fit slope β and the intrinsic scatter σ int of the relation is presented at the upper left corner.
Paper: Revisiting the Hβ Size–Luminosity Relation Using a Uniform Reverberation-mapping Analysis
Authors: Shu Wang, Jong-Hak Woo
Figure caption: Comparison between different luminosity tracers in the average scheme. The left and right panel show the L Hβ –L 5100 and L [O III]–L 5100 relation, respectively. Sub- and super-Eddington ratios are displayed using blue and red color, respectively. The core-dominated radio-loud AGNs are highlighted by additional left-triangle envelopes. The brown dashed lines represent the best-fit relations, while the orange lines are randomly selected 50 realizations from the MCMC samples for illustrating the dispersion of the relation. In each panel, the best-fit slope β and the intrinsic scatter σ int are labeled at the top left corner.
Paper: Revisiting the Hβ Size–Luminosity Relation Using a Uniform Reverberation-mapping Analysis
Authors: Shu Wang, Jong-Hak Woo
Figure caption: Histograms of the ratios of hard X-ray luminosity L 2−10keV to L 5100 (left), L Hβ  (middle), and L [O III] (right) based on a sample of 32 AGNs with hard X-ray luminosity available in H. Liu et al. (2021). The blue and red histograms represent the distribution of low and high λ Edd subsample, respectively, with the division set as logλ Edd ∼ −0.3. The vertical dashed lines in blue and red color indicate the median ratios for sub- and super-Eddington subsample, respectively. The gray histograms and vertical lines are the results for the total sample.
Paper: A Survey of Sulfur-bearing Molecular Lines toward the Dense Cores in 11 Massive Protoclusters
Authors: Mengyao Tang, Sheng-Li Qin, Tie Liu, Luis A. Zapata, Xunchuan Liu, Yaping Peng, Fengwei Xu, Chao Zhang, Ken'ichi Tatematsu
Figure caption: Illustration of dense core locations, continuum emissions, and S-bearing molecular gas distributions. The leftmost sequence of panels, numbered (1) to (11), showcases the continuum emissions, depicted with a red background and outlined in black contours. Contour levels are set at 6σ, 12σ, 24σ, and 48σ, and continue until reaching the peak intensities. The rms noises σ are listed in Table 1, alongside the locations of dense cores, indicated by numbered blue ellipses. The small panels, such as (1a) to (1h), display the distributions of S-bearing species, represented by green contours. Contour levels range from 5% to 95% of peak values in 20% increments. The dust continuum emissions are superimposed as red backgrounds. Gas distribution is generated by emissions with intensities 3 times higher than the rms noise. To ensure a clear representation of the gas distributions, the small panels are presented as magnified views. The red rectangles in the leftmost panels correspond to the areas that have been enlarged for detailed examination.
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Numerical comparisons between two cases without magnetic field β = 0 and with magnetic field β = 9.7 × 10−4 in the Schwarzschild spacetime. (a) Phase-space structures of r and p  r  described by Poincaré section at the plane θ = π/2. The two algorithms S 2 and AS 2 almost give the same structures. (b) Hamiltonian errors ΔH = H + p 0.″×0.01″ for S 2 means that the plotted errors are the practical ones multiplied by factor 0.01, and “s/1000” represents that the plotted new time s is the practical one divided by factor 1000. The term s is τ for S 2. (c) Relation between the original time τ and the new time s. (d) Different proper time steps Δτ in different radial separations r of the orbit for β = 0 or β = 9.7 × 10−4.
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Numerical comparisons in simulations of particles around the Schwarzschild–Melvin black hole. The step size is h = 1, and the parameters are E = 0.9905, L = 3.6, B = 0.001, and j = 100. (a) Poincaré section. Orbit 1 with the initial separation r = 10 seems to be regular for S 2 (colored red) but is weakly chaotic for AS 2 (colored black). Both methods almost give the same results to any one of orbits 2–6. (b) Accuracies of Hamiltonian K in integrations of orbit 1. (c) Relation between w (or s) and τ. (d) Relation between the proper time step Δτ and the distance r.
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Numerical comparisons between the two methods S 2 and AS 2 integrating the null geodesics in the Kerr spacetime. A photon orbit escaping to infinity has the parameters a = 0.3, E = 0.99, and ﹩L=3\sqrt{3}E/10﹩ and the initial conditions r = 3, θ = π/2, and p  r  = 0. (a) Hamiltonian errors K depending on the old time τ. (b) Different old time steps Δτ in different radial separations r of the escaping orbit.
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Poincaré sections for the motions of photons near the Schwarzschild–Melvin black holes with several values of the magnetic field. The method AS 2 with the step size h = 1 is adopted. The other parameters are E = 0.995 and j = 100. The angular momentum is always given by ﹩L=-E\sqrt{-{g}_{\phi \phi }/{g}_{{tt}}}﹩ with r = 15. The extent of chaos is weakened as the magnetic field strength B decreases in panels (a)–(f).
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Same as Figure 5(a) but only for the use of AS 2 in two different values of magnetic field parameter B. (a) In the case of B = 0.8 × 10−3, all orbits are regular KAM tori, and the shapes of orbits 2–6 are unlike those in Figure 5(a). (b) When B = 1.2 × 10−3, orbit 5 with the initial distance r = 48.7 and orbit 7 with the initial distance r = 45 are chaotic.
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Numerical comparisons between the two methods S 2 and AS 2 integrating the time-like geodesics in the Kerr spacetime. (a) Hamiltonian errors K of Equation (6). The time is w for S 2 and s for AS 2. The plotted errors are decreased 100 times for S 2. (b) Relation between the proper time τ and the new time w or s. (c) Different proper time steps Δτ in different radial separations r of the orbit.
Paper: Explicit Symplectic Integrators with Adaptive Time Steps in Curved Spacetimes
Authors: Xin Wu, Ying Wang, Wei Sun, Fuyao Liu, Dazhu Ma
Figure caption: Same as Figure 3, but a photon orbit falling into the black hole with the parameters a = 0.5, E = 0.996, L = −2.211 and the initial conditions r = 100, θ = π/2, p  r  = −1.016 is integrated. (a) Hamiltonian errors K; the best choice is j = 100. (b) Different old time steps Δτ in different radial separations r of the falling orbit.
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Number of visits as a function of the season for the COSMOS, XMM-LSS, CDF-S, ELAIS-S1, EDFS-a, and EDFS-b fields for several considered DESC cohesive DDF strategies. Red points correspond to nights with a lunar phase lower than 20%. Blue crosses correspond to nights with a lunar phase higher than 20%. The filter allocation (per observing night) and the cadence of observation (per season) are specified for each season (magenta).
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Number of visits as a function of the season for the COSMOS, XMM-LSS, CDF-S, ELAIS-S1, EDFS-a, and EDFS-b fields for the remaining DESC cohesive DDF strategies. Red points correspond to nights with a lunar phase lower than 20%. Blue crosses correspond to nights with a lunar phase higher than 20%. The filter allocation (per observing night) and the cadence of observation (per season) are specified for each season (magenta).
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: SN Ia metric SMOM as a function of season for all the strategies designed in this paper. A prior on Ω m  is added to Equation (10) (﹩{\sigma }_{{{\rm{\Omega }}}_{m}}=0.0073﹩; N. Aghanim et al. 2020) to achieve these results. The observed sample is composed exclusively of SNe Ia with a spectroscopic host galaxy redshift.
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Photo-z (top) and WL (bottom) metric values for field/band/strategy that do not fulfill the photo-z or WL requirements. The dotted lines correspond to ﹩{\rm{\Delta }}{m}_{5}^{b}﹩ = 0 (photo-z requirement, top) and r WL = 1 (WL requirement, bottom). The southernmost fields (EDFS-a and EDFS-b) were not included.
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Cumulative DDF budget as a function of season. A large fraction of the budget is consumed in a few seasons for strategies with two UDFs (i.e., the DDF_DESC* scenarios).
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: The number of well-sampled SNe Ia with z ≥ 0.8, N SN, normalized to the configuration where the Moon phase is equal to 0 (i.e., no swap), as a function of the Moon phase threshold corresponding to the swap of the u filter.
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption:  z complete variation, normalized to the configuration where the Moon phase is equal to 0 (i.e., no swap), as a function of the Moon phase threshold corresponding to the swap of the u filter.
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Number of well-sampled SNe Ia with z ≥ 0.8.
Paper: A Cohesive Deep Drilling Field Strategy for LSST Cosmology
Authors: Philippe Gris, Humna Awan, Matthew R. Becker, Huan Lin, Eric Gawiser, Saurabh W. Jha
Figure caption: Number of SNe Ia after 10 yr for the WFD survey of baseline_v3.0_10yrs.
Paper: X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4
Authors: Satoshi Yamada, Taiki Kawamuro, Misaki Mizumoto, Claudio Ricci, Shoji Ogawa, Hirofumi Noda, Yoshihiro Ueda, Teruaki Enoto, Mitsuru Kokubo, Takeo Minezaki, Hiroaki Sameshima, Takashi Horiuchi, Shoichiro Mizukoshi
Figure caption: Top left: logV out vs. logξ. Top right: logN H vs. logξ. The symbols indicate the optical classification. The cyan region shows typical values for BLRs or tori. Bottom left: logV out vs. logξ. Bottom right: logN H vs. logξ. The symbols mark the outflow groups: UFO, low-IP UFO, and WA, as classified in Figure 3.
Paper: X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4
Authors: Satoshi Yamada, Taiki Kawamuro, Misaki Mizumoto, Claudio Ricci, Shoji Ogawa, Hirofumi Noda, Yoshihiro Ueda, Teruaki Enoto, Mitsuru Kokubo, Takeo Minezaki, Hiroaki Sameshima, Takashi Horiuchi, Shoichiro Mizukoshi
Figure caption: Logarithmic V out vs. logarithmic ξ. The symbols indicate the optical classification. The dashed lines show the thresholds of the three groups of X-ray winds: UFO, low-ionization parameter (low-IP) UFO, and WA. The top and right histograms indicate the distributions of the parameters. The yellow histogram represents the UFOs and low-IP UFOs (i.e., with ﹩\mathrm{log}{V}_{\mathrm{out}}\geqslant 4﹩).
Paper: X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4
Authors: Satoshi Yamada, Taiki Kawamuro, Misaki Mizumoto, Claudio Ricci, Shoji Ogawa, Hirofumi Noda, Yoshihiro Ueda, Teruaki Enoto, Mitsuru Kokubo, Takeo Minezaki, Hiroaki Sameshima, Takashi Horiuchi, Shoichiro Mizukoshi
Figure caption: Histogram of redshift for the whole X-WING sample, compared with the samples of Tombesi et al. (2011a, 2013a), Gofford et al. (2013), Laha et al. (2014), Matzeu et al. (2023), and Chartas et al. (2021).
Paper: X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4
Authors: Satoshi Yamada, Taiki Kawamuro, Misaki Mizumoto, Claudio Ricci, Shoji Ogawa, Hirofumi Noda, Yoshihiro Ueda, Teruaki Enoto, Mitsuru Kokubo, Takeo Minezaki, Hiroaki Sameshima, Takashi Horiuchi, Shoichiro Mizukoshi
Figure caption: Top: logarithmic observed 2–10 keV flux (F 2–10) vs. z. Bottom: logarithmic intrinsic AGN luminosity in the 2–10 keV band (L 2–10) vs. z. Symbols mark optical classification of NLSy1 (blue triangle), Seyfert 1.0 (green diamond), 1.2–1.5 (light-green diamond), 1.8–1.9 (orange square), 2.0 (red square), and z > 1 QSOs (cyan star).
Paper: Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars
Authors: Lifu Zhang, Hongwei Ge, Xuefei Chen, Zhanwen Han
Figure caption: Evolutionary track of a naked 1.6 M ⊙ helium star in the HRD. In this paper, “log” represents base-10 logarithm. In panel (a), we show the complete processes of building the helium star. The black dashed line shows the 10 M ⊙ progenitor star from ZAMS to HG. Its hydrogen envelope is ejected during the green line. We stop the mass-losing stage until stellar mass reaches 1.6 M ⊙. The blue line shows the helium star evolution stage. The code stops after carbon ignition. Panel (b) is the helium star evolution stage. It is divided into three phases by radius: radius-increasing phase on He-MS, radius-decreasing phase on He-MS, and He-HG/GB phase.
Paper: Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars
Authors: Lifu Zhang, Hongwei Ge, Xuefei Chen, Zhanwen Han
Figure caption: Same as the previous figure, but use q crit instead. This figure focuses on the He-MS and early He-HG stage at the short-period side. The data points are the potential helium star channel AM CVn stars in Solheim (2010).
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption: Observed and best-fit model lightcurves (one transit event) for WASP-79 b, WASP-94A b, WASP-131 b, and WASP-82 b. For each observed transit, the top panel shows the unprocessed lightcurve (cyan), lightcurve after wavelet denoising (magenta), and the best-fit transit model (blue). The middle panel shows the residual after modeling without GP regression (magenta), the mean (blue), and the 1σ interval (cyan) of the best-fit GP regression model. The bottom panel shows the mean residual flux (blue). The mean residual flux corresponds to the residual flux considering the mean of the best-fit GP regression model.
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption: Same as Figure 1, but for HAT-p-67 b, WASP-117 b, WASP-127 b, KELT-18 b, and HAT-P-49 b.
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption: Same as Figure 1, but for KELT-23A b, WASP-101 b, HAT-P-30 b, HAT-P-8 b, and KELT-6 b.
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption: Same as Figure 1, but for WASP-62 b, XO-6 b, WASP-34 b, WASP-77 b, and WASP-187 b.
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption: Comparison plot of estimated values of b from this work and the literature (top); the residuals from the comparison in parameter units (middle) and in uncertainties (bottom). The residuals in the units of the uncertainties have been estimated by dividing the residuals by the uncertainties of the estimated parameters from the present work.
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption: Same as Figure 10, but for a/R ⋆.
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption:  O – C diagrams showing the estimated midtransit times for WASP-62 b, XO-6 b, KELT-23A b, and HAT-P-7 b, considering a linear ephemeris. The rms and median absolute deviation (MAD) of the midtransit times have also been indicated.
Paper: Precise Transit Photometry Using TESS. II. Revisiting 28 Additional Transiting Systems with Updated Physical Properties
Authors: Suman Saha
Figure caption: Same as Figure 1, but for WASP-73 b, HAT-P-6 b, HAT-P-7 b, and KELT-21 b.