adsabs/AstroCLIMB huggingface dataset:
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Comparison of the source candidate (white) and the velocity kinks (magenta) with the 12CO (J = 2–1) channel maps obtained by MAPS (FWHM of the beam size: ﹩0\mathop{.}\limits^{^{\prime\prime} }15﹩; K. I. Öberg et al. 2021).
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Same as Figure 19, but with injected fake sources at the location of ALMA velocity kink #2 (with contrast levels ΔF410M = 10.6–11.4 mag).
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Three-color composite image combining the HST F336W (red), HST F275W (green), and GALEX FUV (blue) images of the region, highlighting how the UV clumps of star formation correspond to the structures and clusters of younger stars within the PDR shown in Figure 8.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Corner plot of samples drawn from the posterior distribution for Star 1 in Table 15 of the star in the PDR and projected inside the CO cores not detected in the F275W filter demonstrating the degeneracies between mass, age, distance, and dust.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Corner plot of samples drawn from the posterior distribution for Star 6 in Table 17 of stars away from the PDR and away from the CO cores not detected in the F275W filter demonstrating the degeneracies between mass, age, distance, and dust.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Corner plot of samples drawn from the posterior distribution for Star 1 in Table 16 of stars in the PDR and away from the CO cores not detected in the F275W filter demonstrating the degeneracies between mass, age, distance, and dust.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Corner plot of samples drawn from the posterior distribution for Star 2 in Table 13 of stars away from the PDR and projected inside the CO cores demonstrating the degeneracies between mass, age, distance, and dust.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Corner plot of samples drawn from the posterior distribution for Star 1 in Table 11 of stars inside the PDR and projected inside the CO cores demonstrating the degeneracies between mass, age, distance, and dust.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Corner plot of samples drawn from the posterior distribution for Star 3 in Table 12 of stars inside the PDR and away from the CO cores demonstrating the degeneracies between mass, age, distance, and dust.
Paper: Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews
Figure caption: Corner plot of samples drawn from the posterior distribution for Star 5 in Table 14 of stars away from the PDR and away from the CO cores demonstrating the degeneracies between mass, age, distance, and dust.
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Quiescent-flux-subtracted spectra for EVRT-3586872 at +69 and +145 minutes from flare peak. Near the secondary peak at +69 minutes, Balmer continuum and “conundruum” flux, potentially higher-order hydrogen series, dominate the excess emission, decaying to a mostly thermal spectrum at the end of observations. The shaded region indicates the window regions used for calculating the relative contributions of nonthermal emission.
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Comparison of EVRT-3586872 with a selection of other flares observed on M4 dwarfs and reported in W. S. Howard et al. (2019) and S. J. Schmidt et al. (2019). Flare contrast for events from S. J. Schmidt et al. (2019) have been adjusted by 0.1 mag to account for the color shift in the V band. The shaded region represents the range of bolometric energies reported for M4 dwarfs in G. W. Li et al. (2024).
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: The secondary peak of EVRT-3586872, modeled as a combination of a hydrogen recombination continuum, following P. J. A. Simões et al. (2024), and a simple thermal blackbody. The Hfb model predicts an order of magnitude density enhancement in the chromospheric plasma density preceding the peak.
Paper: EFTE-SOAR: Two Giant M Dwarf Flares with Rapid Spectroscopic Follow-up
Authors: Hank Corbett, Nathan Galliher, Amy Glazier, Ramses Gonzalez Chavez, Nicholas M. Law, Ward S. Howard, Alan Vasquez Soto, Jeffrey K. Ratzloff, Robert Quimby
Figure caption: Flux contributions to the spectra relative to the first SOAR epoch. The observations span the decay phase and secondary peaks of the flares.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Top: The mean DMs of pulsars in all globular clusters that host pulsars, sorted by increasing ∣b∣. We also include the DM of FRB 20220319D. Bottom: Fractional difference between the predicted DM and true DM of all globular clusters that host pulsars, sorted by increasing ∣b∣. Predictions are made for each globular cluster given its distance and location on the sky, using four different models for the warm ISM of the Milky Way. The two literature models are NE2001 (blue solid thick curve) and YMW16 (orange solid thin curve). We also convert the measured Hα emission measures (green dashed curve) and H I columns (red dots and shaded region) along each sightline to DM predictions using methods described in the text. We also include predictions for FRB 20220319D assuming a location beyond the Galactic disk.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: DSA-110 localization of FRB 20220319D. Top left: PSF of the DSA-110 for the observation of FRB 20220319D, assuming a flat-spectrum source. Top right: Dirty image of FRB 20220319D, with no deconvolution applied. Bottom left: Deconvolved image of FRB 20220319D. The synthesized beam is represented by an ellipse with half-power diameters of 26﹩\mathop{.}\limits^{\unicode{x02033}}﹩9 × 15﹩\mathop{.}\limits^{\unicode{x02033}}﹩6, at a position angle of 80∘. Briggs weighting was used with a “robust” parameter of 0.5, in order to partially suppress PSF sidelobes. Baselines shorter than 200λ were excluded from the analysis because they were affected by spurious cross-coupling. Contours in the preceding three panels are at −0.4, −0.2 (dashed), 0.2, 0.4, 0.6, 0.8, and 0.9 (solid) of the peak intensity. The images are centered on the coordinates (R.A. J2000, decl. J2000) = (02:08:42.7, +71:02:06.9). Bottom right: Offsets of known astronomical sources from their true positions as measured by the DSA-110. The blue disks show offsets of sources from cataloged positions in the NVSS (J. J. Condon et al. 1998) in a 5 minutes DSA-110 image formed from data taken at a time centered on the burst detection. Only sources with cataloged flux densities >50 mJy and measured major-axis diameters <20″, within 2 deg of the pointing center, were considered. The symbol size is proportional to flux density. The red crosses show measured offsets of nine Radio Fundamental Catalog calibrator sources (see text for details) observed immediately preceding and after the burst. The ellipse indicates the 90% confidence containment region for FRB 20220319D, derived from the Radio Fundamental Catalog calibrators.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Dedispersed temporal profile and dynamic spectrum of FRB 20220319D. A value of DMobs = 110.95 pc cm−3 was used. The top panel shows the estimated absolute position angle based on an approximate parallactic angle, the ∼20∘ error due to rotation measure uncertainty is not included in the error bars. The middle panel shows temporal profiles in total intensity, linearly polarized intensity, and Stokes V, as labeled. The bottom panel shows the dynamic spectrum of the total-intensity data. The time resolution in the time-series and dynamic-spectrum plots is 32.768 μs, and the temporal profile is in units of S/N. The reference time is MJD 59657.93275696795, which was the burst arrival time at OVRO at 1530 MHz. The polarized data on the burst was corrected for the measured rotation measure of 50 rad m−2.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Pan-STARRS i-band image of IRAS 02044+7048, with the 3﹩\mathop{.}\limits^{\unicode{x02033}}﹩7 × 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 90% confidence localization region of FRB 20220319D indicated as a white ellipse.
Paper: Deep Synoptic Array Science: A 50 Mpc Fast Radio Burst Constrains the Mass of the Milky Way Circumgalactic Medium
Authors: Vikram Ravi, Morgan Catha, Ge Chen, Liam Connor, James M. Cordes, Jakob T. Faber, James W. Lamb, Gregg Hallinan, Charlie Harnach, Greg Hellbourg, Rick Hobbs, David Hodge, Mark Hodges, Casey Law, Paul Rasmussen, Kritti Sharma, Myles B. Sherman, Jun Shi, Dana Simard, Jean J. Somalwar, Reynier Squillace, Sander Weinreb, David P. Woody, Nitika Yadlapalli
Figure caption: Predicted DMISM from WHAM Hα measurements surrounding the sightline of FRB 20220319D (yellow cross). The box shows the 4 deg by 2 deg region used to compute the uncertainty in the predicted DMISM for FRB 20220319D. The location of the nearest pulsar within 1 deg of the burst in Galactic latitude, PSR J0231+7026, is shown as a red plus symbol. This pulsar has a DM of 46.7 pc cm−3.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Distribution of members of Melotte 111, Melotte 25, NGC 2632, and NGC 2451A in this work and in S.-Y. Tang et al. (2019) (Tang 19), S. Röser et al. (2019) (Röser 19), J. Alfonso & A. Garcìa-Varela (2023) (Alfonso 23), and S. Meingast et al. (2021) (Meingast 21), respectively. The upper-left panel shows the distribution of the selected clusters in Galactic coordinates, while two panels on the upper-right show their spatial distribution in Galactocentric Cartesian coordinates. Directions to Galactic centers are given by black arrows. The four plots in the lower panel show the CMDs for individual OCs, where the red solid curves represent the empirically corrected PARSEC isochrones in F. Wang et al. (2025) with a solar metallicity, labeled with their age.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Proper motion and spatial distribution for candidate members of HSC 2986 in this work. Its distribution on the proper motion is divided into three parts, Part 1, Part 2, and Part 3, which correspond to the near-core members, the core members, and the possible extended structures, respectively. The colored arrows in the middle two plots indicate the relative mean projected velocity vector of the corresponding part with respect to the mean projected velocity vector of part 2, whereas the colored arrows in the right plot indicate the relative velocity vectors of the corresponding part with respect to the mean velocity vector of part 2, (U, V, W) = (6.9, 228.2, 0.7) km s−1.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Radial and angular distribution of selected OCs Melotte 111, NGC 2451A in this paper. The top panels show histograms of the fraction of stars at different radii from the cluster center, with error bars plotted on each bin. The lower panels show the angular distribution of the fraction of members at the tidal and maximum radii of the cluster whose distance from the cluster center is less than that radius, using the Galactic coordinates in the X–Y plane as the expansion plane, starting from the direction of the center of the Milky Way and rotating counterclockwise. For these OCs, two distinct peaks can be seen in their lower plots, indicating their leading and trailing arms.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Spatial distribution for HSC 2986, IC 2391, Melotte 22, Melotte 25, Melotte 111, NGC 2632, NGC 2451A, Platais 3, Platais 8, Platais 9, and UPK 640 in Galactocentric Cartesian coordinates. The black circle denotes the tidal radius of each OC (typical errors are 0.07–0.13 pc). The black cross symbol indicates the position of the Sun. The morphology and age of these OCs are discussed in Section 4.2.
Paper: Revisiting Open Clusters within 200 pc in the Solar Neighborhood with Gaia DR3
Authors: Penghui Liu, Min Fang, Yue-Lin Sming Tsai, Xiaoying Pang, Fan Wang, Xiaoting Fu
Figure caption: Distribution of the HSC 2986 of our members and the members of Hunt 23 on the position of the sky, the proper motion, the CMD, and the Galactocentric Cartesian coordinates.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: (a) Color–magnitude diagram for the training sample (∼1.5 million stars). (b) Kiel diagram for objects in common between the training sample and SIMBAD, colored by metallicity (∼20,000 stars). The stellar parameters are those given in SIMBAD, and come from a diversity of independent works.
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Comparisons between input spectral energy distribution (SED), in blue, and the reconstructed SED, in orange, for a normal source (left panel) and for an anomalous source (right panel).
Paper: An Unsupervised Machine Learning Approach to Identify Spectral Energy Distribution Outliers: Application to the S-PLUS DR4 Data
Authors: F. Quispe-Huaynasi, F. Roig, N. Holanda, V. Loaiza-Tacuri, Romualdo Eleutério, C. B. Pereira, S. Daflon, V. M. Placco, R. Lopes de Oliveira, F. Sestito, P. K. Humire, M. Borges Fernandes, A. Kanaan, C. Mendes de Oliveira, T. Ribeiro, W. Schoenell
Figure caption: Schematic representation of the autoencoder architecture after hyperparameter tuning.
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: HST/WFC3-UVIS Hα (F656N filter) observations of the candidate protoplanet AB Aur b. Epochs E1–E5 originate from our accretion light echo experiment, which spans a 14 month time baseline in 2023–2024, while epoch E0 (originally presented in Y. Zhou et al. 2022) was acquired in 2022 and has been reprocessed here in the same way as the new epochs. Upper panel: Hα flux density in millijanskys as a function of epoch number. AB Aur b shows strong variability at the 14.7σ level, with brightness increasing by 330% from E3 to E4; see Section 4.1 for details. Panel (a): primary-subtracted images of AB Aur for epochs E0–E5. AB Aur b as well as fainter disk features are clearly visible in each frame. Orbits 2, 3, and 4 are used for frames E1–E5, while E0 represents all five orbits from that program (GO-16651). Panel (b): zoom-in on AB Aur b, located 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩6 south of the host star. The dark lobes on either side of the source are artifacts caused by self-subtraction of AB Aur b using frames acquired at different roll angles. Panel (c): best-fit 2D Gaussian model of AB Aur b from the forward-modeling procedure described in Section 3.4. AB Aur b is resolved, with greater extended emission in the azimuthal direction. Panel (d): residuals after subtracting the best-fit model in panel (c). North is up and east is to the left in all images. For scale, the inner radius is 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩4 (62 au), and the outer annulus in panels (a) and (d) is 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 (312 au).
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: Comparison between normalized HST Hα photometry of AB Aur and delayed brightness measurements of the candidate protoplanet AB Aur b (yellow stars). If AB Aur b is an unobscured static disk feature, a positive linear correlation would be expected between AB Aur and AB Aur b. Instead, in this accretion light echo experiment, we find that AB Aur varies by about 15% while AB Aur b varies by 330% (epochs E1–E5). For comparison, our new reduction of the HST “E0” epoch from Y. Zhou et al. (2022) is displayed with an orange star. Note, however, that this data set does not include the time delay between the host and candidate accreting planet. All measurements have been normalized to the mean values of the host star and companion from epochs E1–E5.
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: Coadded F656N image of AB Aur with HST. Observations represent the average of six epochs (E0–E5) of high-contrast imaging in Hα, amounting to a total integration time of 2.5 hr from 25 orbits over 2 yr (2022–2024). The short-dashed line is the line of nodes—the intersection of the sky and disk planes—and the long-dashed line is the projected rotation axis of the disk based on ALMA and NOEMA observations (Y.-W. Tang et al. 2017; P. Riviére-Marichalar et al. 2020). The disk is rotating counterclockwise, with the northeast portion approaching and the southeast portion receding. AB Aur b (T. Currie et al. 2022; Y. Zhou et al. 2022) is readily visible south of AB Aur (black  × ), but the point source f2 north of AB Aur from A. Boccaletti et al. 2020 is not recovered. Known Hα spiral features (S1Hα—S4Hα) and new scattered-light disk structures (S5Hα and S6Hα) are labeled. No new Hα point sources are identified.