adsabs/AstroCLIMB huggingface dataset:
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Bootstrapped sampling distributions of neighborhood star count (top left) and astrophysical parameters: ﹩\langle \mathrm{log}g\rangle ﹩ (top right), 〈T eff〉 (bottom left), and 〈AbsoluteMagnitude〉 (bottom right) of the 10 pc environment of HD 165155. Gray dotted lines represent the standard deviation and black dashed lines represent the median.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Intersatellite distance over two months. The distance of a 300 km altitude orbit is plotted in blue point, and the distance of a 400 km altitude orbit is plotted in red point.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Distribution of parallax_over_error for stars in a 25 pc neighborhood around six HZSs. The names of the three HZSs with the highest star count in their 10 pc regions are indicated in the legend with red.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: The 25 pc neighborhood star count for 84 HZSs and their distance from the Sun. The color bar represents the effective temperature T eff (in kelvin) of HZ stars. The names of the five HZSs with the highest star count are also labeled.
Paper: The 10 pc Neighborhood of Habitable Zone Exoplanetary Systems: Threat Assessment from Stellar Encounters and Supernovae
Authors: Tisyagupta Pyne, Ravinder K. Banyal, C. Swastik, Ayanabha De
Figure caption: Distribution of photometric mean G magnitude for objects with available T eff, ﹩\mathrm{log}g﹩, and radial velocity in Gaia.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Graphic representation of the Mars-SST mission configuration.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree for four scenarios at different observation durations. The rms amplitude of the a priori mgm-120 gravity field model is represented by a blue solid line. The solved gravity field model for 5, 10, and 15 month observation duration are represented by an orange dotted line, a green dashed line, and a red dashed–dotted line, respectively. The formal uncertainties of the solved gravity field models for the same observation duration are depicted by a purple dotted line, a brown dashed line, and a pink dashed–dotted line, respectively.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree at different orbital altitudes. Subfigures (a)–(c) represent the gravity solution with 1 μm s−1 noise, while subfigures (d)–(f) represent the gravity solution with 10 μm s−1 noise. The rms amplitude of the a priori mgm-120 gravity field model is plotted in a blue solid line. For the solved gravity field models, the 300 km altitude solution is plotted in an orange dashed line and the 400 km altitude solution in a green dotted line. The formal uncertainties for the solved gravity field models are represented by a red dashed line for 300 km and a purple dotted line for 400 km altitudes.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree at different measurement noises. Subfigures (a)–(c) depict the gravity solutions at 300 km altitude, while subfigures (d)–(f) depict the gravity solutions at 400 km altitude. The rms amplitude of the a priori mgm-120 gravity field model is plotted in a blue solid line, that of the solved gravity field model for 1 μm s−1 SST noise is plotted in an orange dashed line, and for 10 μm s−1 SST noise, it is plotted in a green dotted line. The formal uncertainties of the solved gravity field model for 1 μm s−1 SST noise are plotted in a red dashed line, and for 10 μm s−1 SST noise, in a purple dotted line.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree for 5, 10, and 15 month observation durations at 300 km orbital altitude by considering an rms error of 1 μm s−1 for the SST tracking data. The rms amplitude of the a priori mgm-120 model is represented by a blue solid line, the solved gravity field model by an orange dashed line, the error between the a priori and solved models by a green dashed line, and the formal uncertainty of the solved gravity field models by a red solid line. The presentation style for the remaining figures in Section 3 follows the same format.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Coverage of subsatellite points at 300 and 400 km altitudes for different observation durations. The higher altitude is plotted in red, while the lower altitude is plotted in blue.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree for 5, 10, and 15 month observation durations at 400 km orbital altitude by considering an rms error of 10 μm s−1 for the SST tracking data.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Daily Earth-based two-way range-rate data acquisition schedule for three globally distributed stations. The data schedule of the Argentina station is plotted in green, that of the Jiamusi station is plotted in orange, and that of the Kashi station is plotted in blue.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree for 5, 10, and 15 month observation durations at 300 km orbital altitude by considering an rms error of 10 μm s−1 for the SST tracking data.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree for 5, 10, and 15 month observation durations at 400 km orbital altitude by considering an rms error of 1 μm s−1 for the SST tracking data.
Paper: Mars Gravity Field Determination Based on Satellite-to-Satellite Tracking Technique
Authors: Jianguo Yan, Chongyang Wang, Xinbo Zhu, Shanhong Liu, Jean-Pierre Barriot
Figure caption: Rms amplitude as a function of the spherical harmonic degree for 300 km altitude with 10 μm s−1 noise and 400 km altitude with 1 μm s−1 noise. The rms amplitude of the a priori mgm-120 gravity field model is plotted in a blue solid line. The rms amplitude of the solved gravity field models for 300 km altitude with 10 μm s−1 noise and for 400 km altitude with 1 μm s−1 noise are plotted in an orange dashed line and a green dotted line, respectively. The formal uncertainties of the solved gravity field models for the same conditions are plotted in a red dashed line and a purple dotted line, respectively.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: HiPERCAM light curves of ZTF J1539 in the u  s , g  s , r  s , i  s , and z  s  bands folded on the latest ephemeris. The opaque data points represent the binned data, while the raw data are shown as semitransparent data points for each corresponding color. Light curves have been normalized and offset from one another for clarity.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: Best-fit position of ZTF J1539 on the JWST NIRCam detector in the short- (left) and long-wavelength channels for Epochs 1 (top) and 2 (bottom). X and Y pixel positions were determined by the PSFPhotometry function in photutils. In each panel, we also show the one-dimensional histograms of best-fit X and Y pixel values, where N represents the number of pixels in each histogram bin.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: TS of the JWST/NIRCam Epoch 1 (left) and Epoch 2 (right) light curves in the F070W (blue), F277W (red), and F322W2 (orange) bands.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: JWST/NIRCam Epoch 2 light curves of ZTF J1539 in the F070W (left) and F322W2 (right) bands folded on the most recent ephemeris. In both subfigures, we also show the best-fit model to the light curve as a solid line and the resultant residuals in the bottom panels of each subfigure.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: JWST/NIRCam Epoch 1 light curves of ZTF J1539 in the F070W (left) and F277W (right) bands, folded on the most recent ephemeris. In both subfigures, we also show the best-fit model to the light curve as a solid line and the resultant residuals in the bottom panels of each subfigure.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: JWST/NIRCam light curves of ZTF J1539 in the F070W (blue) and F322W2 (orange) bands, folded on the most recent ephemeris and zoomed in on the primary eclipse.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: The evolution of ΔT 0 with time, tracking the drift of JWST's clock. In Epoch 2, the points are colored blue to represent the fact that we only used the F070W data to measure the drift. The gray shaded regions represent the times at which JWST was in contact with a ground station, at which time the spacecraft clock is updated. The horizontal dotted lines in each panel represent the maximum expected offset of ΔT 0 ≈ 116 ms when accounting for all expected sources of errors in the clock (see Section 3.1).
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: JWST/NIRCam Epoch 2 light curves of ZTF J1539 in the F070W (top) and F322W2 (bottom) bands.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: JWST/NIRCam Epoch 1 light curves of ZTF J1539 in the F070W (top) and F277W (bottom) bands.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: JWST/NIRCam Epoch 2 light curve of ZTF J1539 in the F070W band only folded on the most recent ephemeris. We also show the best-fit model to the light curve—after discarding the F322W2 light curve from the fit—as a solid line and the resultant residuals in the bottom panel.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: Corner plot of the fit to the F070W light curve in Epoch 2 after disregarding the F322W2 light curve from the fit. Parameter definitions are given in Section 3.1 and Table 2.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: Corner plot of the fit to the light curve data from Epoch 2. Parameter definitions are given in Section 3.1 and Table 2.
Paper: Calibrating the Clock of JWST
Authors: A. W. Shaw, D. L. Kaplan, P. Gandhi, T. J. Maccarone, E. S. Borowski, C. T. Britt, D. A. H. Buckley, K. B. Burdge, P. A. Charles, V. S. Dhillon, R. G. French, C. O. Heinke, R. I. Hynes, C. Knigge, S. P. Littlefair, Devraj Pawar, R. M. Plotkin, M. E. Ressler, P. Santos-Sanz, T. Shahbaz, G. R. Sivakoff, A. L. Stevens
Figure caption: Corner plot of the fit to the light curve data from Epoch 1. Parameter definitions are given in Section 3.1 and Table 2.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Here we compare the continuum and Hα. Reduced the same as in Figures 3–4, except pyKLIP movement = 5 (instead of 0), and a high-pass filter at 19.5 pix (instead 5.3 pix), with these settings, the fainter extended disk features are preserved. In the 2024 continuum image (lower left), we see light scattered from the PDS70 transition disk, with the dark cavity fit (r = 49 au; 0.437 mas) with the thin green ellipse. We scale down this ellipse and center them on b and c in the Hα images. We then copy identical ellipses to the continuum images. The sizes of these ellipses are set by the peak illumination at the front of the CPD. We see this “bright spot” in the continuum at ∼20 mas from b in 2023 and ∼35 mas in 2024. This suggests an average disk of radius of ∼30 mas around the b planet (or r disk ∼3 au when deprojected). We do not detect a disk around c in 2023 (nor in the 2022 data, which are too low quality), but in 2024, there is a “bright arc” feature that is well fit by the long edge of disk (see the “c” green ellipse in lower-left image). Hence, c might also have ∼3.5 au disk (deprojected). The lower-left FOV is 1.38 × 1.″14.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: Here we show the Hα SDI mode of the MagAO-X instrument used in this work (see L. M. Close et al. 2018 for a full optical description). This photo is of the lower optical table (circa 2022–2023). The upper bench (not shown) contains the 97 element woofer deformable mirror (DM) followed by the ADCs and the 2040 actuator Tweeter DM. Then a f/57 periscopic relay passes the AO and atmospheric-corrected beam down onto the lower bench (this is represented by the white arrow to the upper right of this Figure). Then the white light is collimated and passed through a special custom beamsplitter that transmits all of the continuum and Hα light to the dual science cameras at f/69 shown to the far left. The rest of the light is reflected to the pyramid wave front sensor (PyWFS). The bad edges (∼3% undersized) of the primary and the one bad Tweeter DM actuator are blocked with the clean-up pupil “bump-mask” mask. In the Hα SDI mode shown above, the beamsplitter optics are designed to optimize the total instrument atmosphere-to-CCD Hα throughput to 16.6% at Hα.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: The top row shows the Strehl ratio of the long-term Hα PSF for each data set (see Appendix A for our methodology to measure Strehl). Note how the amount of PSF light dramatically fades quickly at r = 150 mas (where b is located) as Strehl increases. The bottom row shows the final ASDI images (from Figures 2–4), but with a stretch to represent the observed Hα line flux. Hence, in 2022, planet b has a much higher intensity appearance than it does in 2023, where its line flux falls by 4.6x. Planet c is clearly 2.3× brighter in 2024 compared to 2023. Variability of the line flux of both planets is obvious and significant.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: The pyKLIP reduced 6573 2 s image 2023 March data set. Data and pyKLIP parameters are 10 KLIP modes removed, movement = 0, high-pass filtered at 5.3 pix, 3.6 hr of integration (219× 60 s images fed into pyKLIP with 137° of rotation). The green circles are identical centers in all images. Following D. Mawet et al. (2014), the SNR of the ASDI b detection is 10.4, while c is also very well detected at SNR = 13.1. This image is 762.75 × 454.3 mas in the RA and decl. directions.
Paper: Three Years of High-contrast Imaging of the PDS 70 b and c Exoplanets at Hα with MagAO-X: Evidence of Strong Protoplanet Hα Variability and Circumplanetary Dust
Authors: Laird M. Close, Jared R. Males, Jialin Li, 嘉霖 李, Sebastiaan Y. Haffert, Joseph D. Long, Alexander D. Hedglen, Alycia J. Weinberger, Katherine B. Follette, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Jay Kueny, Jennifer Lumbres, Avalon McLeod, Eden McEwen, Clarissa Pavao, Logan Pearce, Laura Perez, Lauren Schatz, Judit Szulágyi, Kevin Wagner, Ya-Lin Wu
Figure caption: The pyKLIP reduced 7124 1 s image 2024 March data set. Data and pyKLIP parameters are 10 KLIP modes removed, movement = 0, high-pass filtered at 5.3 pix, 2 hr of integration (118× 60 s images fed into pyKLIP; 89° of rotation). The green circles have identical centers in all images and are centered on the predicted planet orbital location from the orbit of J. J. Wang et al. (2021) at this epoch. Following D. Mawet et al. (2014), the SNR of the ASDI b detection is 4.3, while c is well detected at SNR = 12.3. Each of the images is 762.75 × 454.3  mas in size.