adsabs/AstroCLIMB huggingface dataset:
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. IV. NIRISS Aperture Masking Interferometry Performance and Lessons Learned
Authors: Steph Sallum, Shrishmoy Ray, Jens Kammerer, Anand Sivaramakrishnan, Rachel Cooper, Alexandra Z. Greebaum, Deepashri Thatte, Matthew De Furio, Samuel M. Factor, Michael R. Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Sasha Hinkley, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Sarah K. Betti, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Daniel Kitzmann, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Cecilia Lazzoni, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Anna Lueber, Bruce Macintosh, Elena Manjavacas, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, B. A. Sargent, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Ben J. Sutlieff, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo
Figure caption: Example images of HIP 65426 (top panels) and HD 116084 (bottom panels) before and after bad-pixel correction (left and right panels, respectively). Red circles indicate two bad pixels in the left panels that have been corrected in the right panels. The color scale has been stretched so that it ranges from 0% to 1% of the peak counts in each image. Residual striping features are seen in the HD 116084 images, which we discuss in Section 4.1. The pixel size in all images is 65 mas, for a total field of view of 5.″2 × 5.″2.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The time evolution of the shock model. In each panel, the x-axis is time in days, and the y-axis is radius in 1000 R ⊙. From panel (1) to (6), they are ﹩{\mathrm{log}}_{10}\rho ﹩ with contours of [−10, −11, −12], ﹩{\mathrm{log}}_{10}{T}_{{\rm{g}}}﹩ with contours of [3.1, 3.7], ﹩{\mathrm{log}}_{10}({a}_{\mathrm{rad}}/g)﹩ with contours of [−2, 0], optical depth ﹩{\mathrm{log}}_{10}{\tau }_{R}﹩ with contours of [0, 1, 3], ﹩{\mathrm{log}}_{10}({E}_{r}/{e}_{{\rm{g}}})﹩ with contours of [−1, 0, 1], and ﹩{\mathrm{log}}_{10}{\kappa }_{{\rm{R}}}﹩ with contours of [−2, 0].
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The solid and dashed lines are the time-dependent inner boundary conditions of the shock and shock-free models, respectively. The red line indicates the escape velocity at the inner boundary. The orange region denotes the radiation-dominated ejecta. In the left panel, from top to bottom, each plot shows the velocity of the ejecta, v source calculated from Equation (26), and the temperature of the ejecta. In the right panel, from top to bottom, they are the mass-loss rate, cumulative mass loss, and E  r /e g, respectively. The shock model and shock-free model also differ in the duration of the ejecta.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The ρ–T diagram of H and He divided into six zones to improve the computational efficiency. The pure states are colored with blue, and the rest are mixture states that require solving Saha equations.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The solid line with black dots is the observed light curve of AT 2019zhd (Pastorello et al. 2021a), and the red and blue solid lines are the light curves of the shock and shock-free models, respectively.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The light curves of simple simulations with different mass and temperature of the ejecta. The physical parameters of the ejecta are listed in Table 1.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The first panel shows the combined specific heat capacity of X = 0.74 and Y = 0.26, and the bottom panel shows the adiabatic index.
Paper: Energy Deposition into the Ionosphere during a Solar Flare with Extreme-ultraviolet Late Phase
Authors: Jing Liu, Liying Qian, Wenbin Wang, Kevin Pham, Xiangliang Kong, Yao Chen, Wenlong Liu, Libo Liu, Xuanqing Liu
Figure caption: Time evolution of each spectral channel for the 2012 October 23 X1.8 solar flare. Panel (a) shows the normalized solar irradiance in four EVE lines including 9.3, 13.1, 17.1, and 33.5 nm and GOES 0.1–0.8 nm flux, with the total EUV radiative energy-loss rate overplotted (shaded area) as indicated in the right Y-axis. Panels (b)–(i) show snapshots of AIA images illustrating the evolution of solar flare at the preeruption, main phase peak, pre-ELP peak, and ELP peak as indicated by the four vertical dashed lines in Figure 1(a).
Paper: Energy Deposition into the Ionosphere during a Solar Flare with Extreme-ultraviolet Late Phase
Authors: Jing Liu, Liying Qian, Wenbin Wang, Kevin Pham, Xiangliang Kong, Yao Chen, Wenlong Liu, Libo Liu, Xuanqing Liu
Figure caption: Percentage changes of electron density profiles at Yakutsk, Beijing, Wuhan, and Sanya on 2012 October 22 (left column; no flare) and 2012 October 23 (right column; flare). The percentage changes of electron density were calculated with respect to a 1 hr (02:10–03:10 UT) preflare mean values. The black lines indicate the height of the F2 layer peak.
Paper: Energy Deposition into the Ionosphere during a Solar Flare with Extreme-ultraviolet Late Phase
Authors: Jing Liu, Liying Qian, Wenbin Wang, Kevin Pham, Xiangliang Kong, Yao Chen, Wenlong Liu, Libo Liu, Xuanqing Liu
Figure caption: The simulated temporal variations of electron density (left column) and Pedersen conductivity profiles (right column) at the geographic equator and local noon without solar flare effects ((a) and (d), Run 0). Figures (b), (c), (e), and (f) show the changes in electron density and Pedersen conductivity due to solar flare impulsive phase ((b) and (e), Run 1–Run 0) and ELP effects ((c) and (f), Run 2–Run 1).
Paper: Energy Deposition into the Ionosphere during a Solar Flare with Extreme-ultraviolet Late Phase
Authors: Jing Liu, Liying Qian, Wenbin Wang, Kevin Pham, Xiangliang Kong, Yao Chen, Wenlong Liu, Libo Liu, Xuanqing Liu
Figure caption: Snapshots of global GNSS TEC distributions at 03:10 UT (top row) and 04:45 UT (middle row) and their differences (bottom row). The left and right columns are for no flare references on October 22 and flare day on 2012 October 23, respectively. The magenta crosses denote the locations of the four ionosonde stations.
Paper: Optical Appearance of Eccentric Tidal Disruption Events
Authors: Fangyi (Fitz) Hu, Daniel J. Price, Ilya Mandel
Figure caption: Bolometric luminosity (first), blackbody radius (second), blackbody temperature (third), and mass fallback and accretion rates (fourth) of the TDE simulations. Both the luminosity and radius increase rapidly at the beginning and then remain relatively constant, whereas the temperature drops sharply and stays roughly constant. Compared to observations (colored dots; from van Velzen et al. 2021), the temperature and radius are systematically lower and higher, respectively. The luminosity follows neither the fallback rate nor the accretion rate. All the lightcurve data are available.(The data used to create this figure are available.)
Paper: Optical Appearance of Eccentric Tidal Disruption Events
Authors: Fangyi (Fitz) Hu, Daniel J. Price, Ilya Mandel
Figure caption: Example spectra (blue) obtained by our ray tracing procedure from the 1M-particle simulation, for an observer at z = ∞ , perpendicular to the orbital plane, for our β = 5 simulation. Blackbodies are fitted to the ZTF optical/UV (orange) and Swift X-ray (green) band (magenta boxes) separately. Different opacities are used in each panel, i.e., κ = κ es, 0.1κ es, 0.01κ es, and κ therm in the first, second, third, and fourth panels, respectively. The lower the opacity, the deeper we can look into the gas envelope and the harder the spectrum. The spectra data are available.(The data used to create this figure are available.)
Paper: Optical Appearance of Eccentric Tidal Disruption Events
Authors: Fangyi (Fitz) Hu, Daniel J. Price, Ilya Mandel
Figure caption: Profiles of the density (first), temperature (second), radial (third), and azimuthal (fourth) velocities at t = 100 days of the 1M-particle simulation. Colors in the plot represent the density of particles in the parameter space (yellow, blue, red, and black correspond to low to high). The dashed line shows Keplerian orbital velocity. The material is approximately spherically symmetric inside the estimated photosphere and more asymmetrical outside. A small amount of material inflows within r < 1  au, with the remaining material outflowing. The simulation dump is available.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: Upper panel: light curves of the last 10 days of the shock (s) and shock-free (sf) models and their corresponding dust deficit models. Bottom panel: the time evolution of ﹩{\mathrm{log}}_{10}({\kappa }_{{\rm{R}}}{F}_{r}/({cg}))﹩ and ﹩{\mathrm{log}}_{10}{\kappa }_{{\rm{R}}}﹩ of the shock dust deficit model.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The Rosseland mean opacity that includes dust opacity at different densities. Solid and dashed lines denote the gas and dust opacities, respectively. The red zone indicates the dust formation temperature, the gray zone indicates the temperature of hydrogen dissociation and H− formation, and the orange zone indicates the ionization temperature of H and He.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The black line with dots shows the light curve of AT 2019zhd. The red and blue colors indicate the shock (s) and shock-free (sf) models. The solid and dashed lines indicate the original and low-resolution models, respectively.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The black line with dots shows the light curve of AT 2019zhd. The red and blue colors indicate the shock (s) and shock-free (sf) models. The solid and dashed lines indicate our original models and their counterparts when we turn off the radiation force.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: The upper and lower panels show the light curves of an H and He mixture EoS and a perfect gas EoS with various γ of the shock (s) and shock-free (sf) models, respectively.
Paper: Bridging the Gap between Luminous Red Novae and Common Envelope Evolution: The Role of Recombination Energy and Radiation Force
Authors: Zhuo Chen, 卓 陈, Natalia Ivanova
Figure caption: From left to right, the first row shows the time evolution of the mass fraction of He, He+, and He2+, and the second row shows the time evolution of the mass fraction of H2, H, and H+.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. IV. NIRISS Aperture Masking Interferometry Performance and Lessons Learned
Authors: Steph Sallum, Shrishmoy Ray, Jens Kammerer, Anand Sivaramakrishnan, Rachel Cooper, Alexandra Z. Greebaum, Deepashri Thatte, Matthew De Furio, Samuel M. Factor, Michael R. Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Sasha Hinkley, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Sarah K. Betti, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Daniel Kitzmann, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Cecilia Lazzoni, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Anna Lueber, Bruce Macintosh, Elena Manjavacas, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, B. A. Sargent, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Ben J. Sutlieff, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo
Figure caption: Left panels show the observed standard deviation of each visibility phase (top) and closure phase (bottom) vs. baseline length. The dashed lines show the predicted scatter for phase observables with a fringe visibility equal to 1. Right panels show the ratio between the predicted and observed scatter for the two phase quantities. The decrease in this ratio as a function of baseline length is consistent with a systematic decrease in fringe visibility. In all panels, the small black circles, medium gray circles, and large purple circles show observables for HD 115842, HD 116084, and HIP 65426, respectively.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. IV. NIRISS Aperture Masking Interferometry Performance and Lessons Learned
Authors: Steph Sallum, Shrishmoy Ray, Jens Kammerer, Anand Sivaramakrishnan, Rachel Cooper, Alexandra Z. Greebaum, Deepashri Thatte, Matthew De Furio, Samuel M. Factor, Michael R. Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Sasha Hinkley, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Sarah K. Betti, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Daniel Kitzmann, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Cecilia Lazzoni, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Anna Lueber, Bruce Macintosh, Elena Manjavacas, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, B. A. Sargent, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Ben J. Sutlieff, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo
Figure caption: Left: comparison between HIP 65426 calibration quality and expectations for photon noise. The purple solid line shows the scatter in the time-averaged calibrated HIP 65426 closure phases, as a function of the number of integrations that were included in the average. The dashed black line shows the expected closure phase scatter for photon noise. The noise in the HIP 65426 closure phases calculated using all 10,950 integrations is inflated by a factor of 22.25 compared to photon-noise expectations. Right: contrast curves calculated from the observed HIP 65426 observations (using all 10,950 integrations) calibrated with the entire HD 116084 data set, compared to theoretical predictions. The purple solid line shows the observed contrast, and the black dashed line shows the predicted contrast. The observations underperform compared to predictions by a factor of ∼3 mag.
Paper: The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. IV. NIRISS Aperture Masking Interferometry Performance and Lessons Learned
Authors: Steph Sallum, Shrishmoy Ray, Jens Kammerer, Anand Sivaramakrishnan, Rachel Cooper, Alexandra Z. Greebaum, Deepashri Thatte, Matthew De Furio, Samuel M. Factor, Michael R. Meyer, Jordan M. Stone, Aarynn Carter, Beth Biller, Sasha Hinkley, Andrew Skemer, Genaro Suárez, Jarron M. Leisenring, Marshall D. Perrin, Adam L. Kraus, Olivier Absil, William O. Balmer, Sarah K. Betti, Anthony Boccaletti, Mariangela Bonavita, Mickael Bonnefoy, Mark Booth, Brendan P. Bowler, Zackery W. Briesemeister, Marta L. Bryan, Per Calissendorff, Faustine Cantalloube, Gael Chauvin, Christine H. Chen, Elodie Choquet, Valentin Christiaens, Gabriele Cugno, Thayne Currie, Camilla Danielski, Trent J. Dupuy, Jacqueline K. Faherty, Michael P. Fitzgerald, Jonathan J. Fortney, Kyle Franson, Julien H. Girard, Carol A. Grady, Eileen C. Gonzales, Thomas Henning, Dean C. Hines, Kielan K. W. Hoch, Callie E. Hood, Alex R. Howe, Markus Janson, Paul Kalas, Grant M. Kennedy, Matthew A. Kenworthy, Pierre Kervella, Daniel Kitzmann, Masayuki Kuzuhara, Anne-Marie Lagrange, Pierre-Olivier Lagage, Kellen Lawson, Cecilia Lazzoni, Ben W. P. Lew, Michael C. Liu, Pengyu Liu, Jorge Llop-Sayson, James P. Lloyd, Anna Lueber, Bruce Macintosh, Elena Manjavacas, Sebastian Marino, Mark S. Marley, Christian Marois, Raquel A. Martinez, Brenda C. Matthews, Elisabeth C. Matthews, Dimitri Mawet, Johan Mazoyer, Michael W. McElwain, Stanimir Metchev, Brittany E. Miles, Maxwell A. Millar-Blanchaer, Paul Molliere, Sarah E. Moran, Caroline V. Morley, Sagnick Mukherjee, Paulina Palma-Bifani, Eric Pantin, Polychronis Patapis, Simon Petrus, Laurent Pueyo, Sascha P. Quanz, Andreas Quirrenbach, Isabel Rebollido, Jea Adams Redai, Bin B. Ren, Emily Rickman, Matthias Samland, B. A. Sargent, Joshua E. Schlieder, Glenn Schneider, Karl R. Stapelfeldt, Ben J. Sutlieff, Motohide Tamura, Xianyu Tan, Christopher A. Theissen, Taichi Uyama, Arthur Vigan, Malavika Vasist, Johanna M. Vos, Kevin Wagner, Jason J. Wang, Kimberly Ward-Duong, Niall Whiteford, Schuyler G. Wolff, Kadin Worthen, Mark C. Wyatt, Marie Ygouf, Xi Zhang, Keming Zhang, Zhoujian Zhang, Yifan Zhou, Alice Zurlo
Figure caption: Self-calibration charge migration tests. The left panel shows the ratio between the observed closure phase scatter and the prediction for photon noise of the HIP 65426 13-group data set calibrated using HIP 65426 data sets with varying numbers of groups. The right panel shows the resulting achievable contrast for each calibration (solid lines with color scale), the predicted achievable contrast (dashed lines with color scale), and the HIP 65426 contrast when calibrated with HD 116084 (thick black line).