adsabs/AstroCLIMB huggingface dataset:
Paper: RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites
Authors: Katelyn Horstman, Jean-Baptiste Ruffio, Konstantin Batygin, Dimitri Mawet, Ashley Baker, Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王, Sarah Blunt, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Shubh Agrawal, Quinn M. Konopacky, Geoffrey A. Blake, Clarissa R. Do Ó, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich
Figure caption: Measured RVs of GQ Lup B with KPIC. Each panel represents a different epoch. In the forward-modeling framework used, each spectral order is fit separately to measure a RV. Orange represents order 33, pink represents order 32, and purple represents order 31. Each marker shape denotes a specific KPIC fiber where “x” represents fiber 2, “+” represents fiber 3, “⋆” represents fiber 4. We limit our final data set to RVs with a CCF S/N > 3 and a measured value between −5 and 5 km s−1.
Paper: RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites
Authors: Katelyn Horstman, Jean-Baptiste Ruffio, Konstantin Batygin, Dimitri Mawet, Ashley Baker, Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王, Sarah Blunt, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Shubh Agrawal, Quinn M. Konopacky, Geoffrey A. Blake, Clarissa R. Do Ó, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich
Figure caption: An example GQ Lup B spectrum and forward model from a single exposure on 2023 June 29 (UT). Top: the full spectrum is in black, while the combined model, consisting of the planet model (purple) and the stellar model (orange), is in pink. The residuals (data model) are shown in gray, while the shaded gray region represents the data uncertainity measured by the KPIC DRP. Center: the forward model of the companion spectrum taken from a BT-Settl atmospheric model (﹩\mathrm{log}g=4.0;﹩                      T eff = 2700 K; F. Allard et al. 2012). The ten spline nodes used to model the continuum are shown in gray and black. Bottom: the forward model of the starlight derived from empirical observations of GQ Lup to account for speckle light leaking into the fiber. The three spline nodes used to model the continuum are shown in gray and black.
Paper: RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites
Authors: Katelyn Horstman, Jean-Baptiste Ruffio, Konstantin Batygin, Dimitri Mawet, Ashley Baker, Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王, Sarah Blunt, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Shubh Agrawal, Quinn M. Konopacky, Geoffrey A. Blake, Clarissa R. Do Ó, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich
Figure caption: Simulated cavity depth carved by a single satellite. The vertical axis represents the normalized surface density of the CPD, which must be ≤0.5 to produce an prominent cavity. Each colored line represents a different satellite-to-planet mass ratio (q). The blacked dashed line represents the measured radius of the CPD, 65 R Jup. We adjust the semimajor axis of the satellite to be consistent with forming a cavity at 65 R Jup, regardless of the mass ratio. We find a minimum satellite-to-planet mass ratio of 2 × 10−4 is capable of carving a cavity, while the maximum cavity size produced is ∼51 R Jup.
Paper: RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites
Authors: Katelyn Horstman, Jean-Baptiste Ruffio, Konstantin Batygin, Dimitri Mawet, Ashley Baker, Chih-Chun Hsu, Jason J. Wang, 劲飞 王, Ji Wang, 吉 王, Sarah Blunt, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Shubh Agrawal, Quinn M. Konopacky, Geoffrey A. Blake, Clarissa R. Do Ó, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Peter Wizinowich
Figure caption: Exosatellite detection limits around GQ Lup B with the Keck Planet Imager and Characterizer (KPIC) using the open-source python module RVsearch (L. J. Rosenthal et al. 2021). (Left) Periodogram of the RV times series shown in Figure 2 expressed a ΔBIC comparing a model with and a model without a satellite signal. The empirical detection threshold is indicated in the legend and is much higher than the power expressed for the strongest periodic signal, indicating the model without a satellite signal is favored over a model with a satellite signal. (Right) Exosatellite completeness derived from injection and recovery tests.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: The figure displays the structure of the neural network proposed in this 							paper, which incorporates multiple convolutional neural networks and 							residual blocks to efficiently encode the features of images.
Paper: An Image Quality Evaluation and Masking Algorithm Based On Pretrained Deep Neural Networks
Authors: Peng Jia, Yu Song, Jiameng Lv, Runyu Ning
Figure caption: The figure illustrates the structure of the autoencoder, which first 							encodes input images into latent vectors and subsequently decodes the 							latent vectors to output images.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Marginalized 1D and 2D posterior distributions for selected orbital parameters of HD 19467 B corresponding to the fit of the RV, relative astrometry from direct imaging observations, and absolute astrometry from Hipparcos and Gaia with the use of orvara (Brandt et al. 2021). Confidence intervals at 15.85%, 50.0%, and 84.15% are overplotted on the 1D posterior distributions, with the median ±1σ values given at the top of each 1D distribution. The 1σ, 2σ, and 3σ contour levels are overplotted on the 2D posterior distribution.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Same as Figure 12 plotting our MCMC fits using the NEWERA-PHOENIX model grid for our continuum-subtracted NIRSpec spectra.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Same as Figure 12 plotting our MCMC fits using the NEWERA-PHOENIX model grid for our continuum NIRSpec spectra.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Same as Figure 12 plotting our MCMC fits using the Sonora Bobcat grid for our continuum NIRSpec spectra.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Same as Figure 12 plotting our MCMC fits using the Sonora Bobcat grid for our continuum-subtracted NIRSpec spectra.
Paper: JWST-TST High Contrast: Spectroscopic Characterization of the Benchmark Brown Dwarf HD 19467 B with the NIRSpec Integral Field Spectrograph
Authors: Kielan K. W. Hoch, Christopher A. Theissen, Travis S. Barman, Marshall D. Perrin, Jean-Baptiste Ruffio, Emily Rickman, Quinn M. Konopacky, Elena Manjavacas, William O. Balmer, Laurent Pueyo, Jens Kammerer, Roeland P. van der Marel, Nikole K. Lewis, Julien H. Girard, Sara Seager, Mark Clampin, C. Matt Mountain
Figure caption: Same as Figure 12 plotting our MCMC fits using the DRIFT-PHOENIX grid for our continuum-subtracted NIRSpec spectra.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The steps implemented on the data of WASP-127 b to highlight the weak CO signal. From the left-most panel, it is not possible to claim a confident detection of CO. The most notable increase in the significance of our CO detection comes by cropping the out-of-transit phases post-SVD and masking telluric features. Apart from the left-most CC map, the K  p  and V sys values at the peak (red cross) are consistent at ∼121 km s−1 and ∼−13.5 km s−1 in all the maps.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The solar RCTE model of CO (brown) used for our cross-correlation analysis. The best-fit RCPE model is also shown in green. The 38 IGRINS spectral orders used in our analysis are shown as the gray stripes. Among these, the eight spectral orders where the CO opacity is dominant as shown in light blue. Solar RCTE models of H2O, H2S, CO2, and SO2 are also shown in purple, yellow, black, and gold, respectively. H2O, CO, and H2S are strong opacity sources and contain a large number of spectral features within IGRINS wavelength coverage unlike CO2 and SO2. Therefore, our observations are not sensitive to CO2 or SO2.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: Our abundance profiles of H2O, CO, and CO2 from the RCPE retrieval compared against the constraints obtained from previous studies (square markers). For the three molecules, lighter shades of their color represent the 1σ confidence region. The error bars on the constraints of the abundances of H2O, CO, and CO2 are represented in blue, brown, and black bars, respectively. The constraints of J. J. Spake et al. (2021) were taken from their estimate on WASP-127 b metallicity from their chemically consistent retrieval (i.e., 17 ± 4×  solar). Our RCPE results agree well with the results of J. J. Spake et al. (2021) and the CO2 abundance of A. Boucher et al. (2023), suggesting a super-solar metal enrichment for WASP-127 b.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: The CC maps where were removed the best-fit RCPE model from the data and injected the best-fit RCTE model at V sys = 20 km s−1 (black-dashed vertical line in the maps). The cross correlation was performed with best-fit RCTE full model and H2S absorption only model to assess the level at which H2S can be detected, if present, dictated by thermochemical equilibrium. While not as strong as the full model (10.27σ), we would have been able to detect H2S at 3.08σ under thermochemical equilibrium.
Paper: IGRINS Observations of WASP-127 b: H2O, CO, and Super-solar Atmospheric Metallicity in the Inflated Sub-Saturn
Authors: Krishna Kanumalla, Michael R. Line, Megan Weiner Mansfield, Luis Welbanks, Peter C. B. Smith, Jacob L. Bean, Lorenzo Pino, Matteo Brogi, Vatsal Panwar
Figure caption: VMR profiles of several dominant absorbers in IGRINS coverage. These profiles are calculated for an atmosphere with 10×solar metallicity with f and C/O fixed at 1 and 0.5, respectively. The solid lines indicate the VMR profiles from a RCPE model and the dashed lines indicate the same from a RCTE model. Both H2O and H2S are highly impacted by photochemistry; however, H2S is heavily depleted deeper in the atmosphere, unlike H2O.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Comparison of Theia 456's phase space at the present epoch with that of a sphere forward integrated under the MilkyWayPotential, centered at the mean position given by backwards integrating dynamical members to time T opt, with a radius of R opt. Each contour contains 95% of model stars forward integrated, drawn from a Maxwell–Boltzmann distribution at different values of σ  v . Black and gray points denote our sample of stars with Hectochelle radial velocities and the entire Theia 456 catalog, respectively. Our model (the red contour) prefers a relatively low velocity dispersion at birth, ﹩{\sigma }_{{v}_{\mathrm{opt}}}=0.14\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩; larger velocity dispersions produce overly diffuse position and proper-motion spaces.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Mock stars (shown as colored points) with different hypothetical ages, denoted in the top-left corner of the top panels, forward integrated and plotted under our catalog in position and proper-motion space. The proper-motion dispersion, defined as ﹩{\sigma }_{{pm}}=\sqrt{{\sigma }_{{\mu }_{{\alpha }^{\star }}}^{2}+{\sigma }_{{\mu }_{\delta }}^{2}}﹩, is shown for each model stream. The inset shows the density distribution of parallax, and its dispersion in the legend, for each model stream, compared with the entire Theia 456 catalog in solid black.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Mock phase space of Theia 456 at the present epoch from various initial conditions, compared with the observed phase space of our sample with precise radial velocities (black points) and the entire Theia 456 catalog (gray points). Contours contain 95% of the data and are drawn at different birth ages, while columns refer to different birth sizes. Red contours in the middle column most closely represent our best-fit model.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Mock stars integrated forward, color-coded by their initial positions (top three rows) and velocities (bottom three rows) in Galactocentric cylindrical coordinates, with dynamical members overplotted as black points. Rows are sorted by the Maxwell–Boltzmann initialization velocity σ  v . Positions are measured relative to the Galactic center, and velocities are measured relative to the bulk cluster velocity.
Paper: Theia 456: Tidally Shredding an Open Cluster
Authors: Kyle R. Tregoning, Jeff J. Andrews, Marcel A. Agüeros, Phillip A. Cargile, Julio Chanamé, Jason L. Curtis, Simon C. Schuler
Figure caption: Comparison of the typical acceleration that a model star in Theia 456 feels solely due to the Milky Way potential (black line) and due to the sum of N-body interactions (red lines). Shown is the median (for 2166 stars) magnitude of the acceleration at each time step. The Milky Way potential is the dominant driver for the acceleration of stars in Theia 456.
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption: Color–color and reduced magnitude–color diagrams for SMDET discoveries (black points) and known ultracool dwarfs (colored data points) from the PanSTARRS 3π survey (W. M. J. Best et al. 2018). Objects from VHS and observed with the K  s  filter are marked as X symbols. Objects from UKIDSS LAS DR9 and observed with the K MKO filter are marked as diamond symbols. Points associated with numbers refer to subdwarf candidates discussed in Section 6, and correspond to 1: CWISE J024822.37+674812.6, 2: CWISE J052544.47+443409.9, and 3: CWISE J120642.54+762641.6.
Paper: Discovery of 118 New Ultracool Dwarf Candidates Using Machine-learning Techniques
Authors: Hunter Brooks, Dan Caselden, J. Davy Kirkpatrick, Yadukrishna Raghu, Charles A. Elachi, Jake Grigorian, Asa Trek, Andrew Washburn, Hiro Higashimura, 村滉 東, Aaron M. Meisner, Adam C. Schneider, Jacqueline K. Faherty, Federico Marocco, Christopher R. Gelino, Jonathan Gagné, Thomas P. Bickle, Shih-Yun Tang, Austin Rothermich, Adam J. Burgasser, Marc J. Kuchner, Paul Beaulieu, John Bell, Guillaume Colin, Giovanni Colombo, Alexandru Dereveanco, Deiby Pozo Flores, Konstantin Glebov, Leopold Gramaize, Les Hamlet, Ken Hinckley, Martin Kabatnik, Frank Kiwy, David W. Martin, Raúl F. Palma Méndez, Billy Pendrill, Lizzeth Ruiz, John Sanchez, Arttu Sainio, Jörg Schümann, Manfred Schonau, Christopher Tanner, Nikolaj Stevnbak, Andres Stenner, Melina Thévenot, Vinod Thakur, Nikita V. Voloshin, Zbigniew Wȩdracki
Figure caption: All-sky distribution of the 124 new SMDET discoveries in equatorial coordinates with the Aitoff projection. Sources are color-coded based on spectral-type estimates from Section 4, while those with a black interior are either candidate subdwarfs discussed in Section 6 or lack a photometric spectral-type estimate.
Paper: Analyzing JWST/NIRSpec Hydrogen Line Detections at TWA 27B: Constraining Accretion Properties and Geometry
Authors: Yuhiko Aoyama, Gabriel-Dominique Marleau, Jun Hashimoto
Figure caption: Flux ratios or emission color of several hydrogen lines. The blue–orange squares represent the predictions for postshock emission, while the blue–red points correspond to the preshock emission. The observational results are marked by a black circle with error bars. Across all panels, the observed emission color aligns with both emission models due to large uncertainty. As a reference, a successful case of Delorme 1(AB)b, analyzed in Betti et al. (2022b), is shown as blue cross in panel (e).
Paper: Analyzing JWST/NIRSpec Hydrogen Line Detections at TWA 27B: Constraining Accretion Properties and Geometry
Authors: Yuhiko Aoyama, Gabriel-Dominique Marleau, Jun Hashimoto
Figure caption: Mass accretion rate for each parameter set. The white shaded area indicates parameter combinations rejected at 1 σ (﹩{\chi }_{\mathrm{red}}^{2}\gt 1.13﹩). At the fiducial case of (v 0, n 0) = (130 km s−1, 1013 cm−3), ﹩\dot{M}=2.5\times {10}^{-9}\,{M}_{{\rm{J}}}\,{\mathrm{yr}}^{-1}﹩.
Paper: Analyzing JWST/NIRSpec Hydrogen Line Detections at TWA 27B: Constraining Accretion Properties and Geometry
Authors: Yuhiko Aoyama, Gabriel-Dominique Marleau, Jun Hashimoto
Figure caption: Over our model grid, ﹩{\chi }_{\mathrm{red}}^{2}﹩ of fitting to Pa-α (upper left), Pa-β (upper right), Pa-γ (lower left), and Pa-δ (lower right) of TWA 27 B. Similar to Figure 2 but independently fitting to each line. The degrees of freedom are 5, 4, 1, and 2 for Pa-α, Pa-β, Pa-γ, and Pa-δ, respectively.
Paper: Analyzing JWST/NIRSpec Hydrogen Line Detections at TWA 27B: Constraining Accretion Properties and Geometry
Authors: Yuhiko Aoyama, Gabriel-Dominique Marleau, Jun Hashimoto
Figure caption: Constraint of shock parameters from flux ratios. The solid lines represent the parameter sets where our model reproduces the observed flux ratios of Pa-β/Pa-α (black), Pa-γ/Pa-α (red), and Pa-δ/Pa-α (blue). The shaded region, bordered by the dashed lines, encompass values that agree with the observation within 1σ uncertainty.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: O-C diagram for ATLAS 1 from 37 times of maximum light.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Sample light curves for all six targets.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: O–C diagram for ATLAS 8 from 13 times of maximum light. Note that the AAVSO data is not included here since it happens significantly before the other data points.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Phased data for ATLAS 1 from BYU, ATLAS, ASAS-SN, and TESS using the period from Equation (1).
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Phased data for ATLAS 8 from BYU, ATLAS, ASAS-SN, and TESS using optimal periods found by Period04 for each survey.
Paper: Establishing Baselines for Six Short-period δ Scuti Variables
Authors: Christiana Z. Suggs, Eric G. Hintz, Denise C. Stephens
Figure caption: Phased data for ATLAS 4 from BYU, ATLAS, ASAS-SN, and TESS using the calculated period.