adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring Giant Barium Stars:12C/13C Ratio and Elemental Abundances of Carbon, Nitrogen, and Oxygen 
Authors: M. P. Roriz, N. A. Drake, N. Holanda, M. Lugaro, B. Cseh, S. Junqueira, C. B. Pereira
Figure caption: Carbon (top panel) and nitrogen (bottom panel) abundance ratios to Fe vs. sodium abundances observed in Ba giants (gray dots); typical error bars are shown. Data for normal giants (crosses, taken from R. E. Luck & U. Heiter 2007; Y. Takeda et al. 2019) and post-AGB stars (blue diamonds; see references in the caption of Figure 5) were added in these plots.
Paper: Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633
Authors: Taichi Uyama, Masayuki Kuzuhara, Charles Beichman, Teruyuki Hirano, Takayuki Kotani, Qier An, Timothy D. Brandt, Markus Janson, Dimitri Mawet, Mayuko Mori, Bun'ei Sato, Denitza Stoeva, Motohide Tamura, Masataka Aizawa, Bryson Cale, Thomas Henning, Hiroyuki Tako Ishikawa, Norio Narita, Masahiro Ogihara, Aniket Sanghi, Trifon Trifonov, Jerry Xuan, Eiji Akiyama, Hiroki Harakawa, Klaus Hodapp, Masato Ishizuka, Shane Jacobson, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Jungmi Kwon, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Huan-Yu Teng, Akitoshi Ueda, Sebastien Vievard
Figure caption: Common proper-motion test of the companion candidate around J1446. The blue and orange crosses indicate the relative location to the central star (ΔR.A. for x-axis and Δdecl. for y-axis). The gray solid line indicates a trajectory of a zero proper-motion background star and the red cross indicates an expected position of the background-star case in the second epoch. We insert the zoomed-in panel for the relative astrometry of the first and second epochs, whose error bars are small in the original panel.
Paper: Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633
Authors: Taichi Uyama, Masayuki Kuzuhara, Charles Beichman, Teruyuki Hirano, Takayuki Kotani, Qier An, Timothy D. Brandt, Markus Janson, Dimitri Mawet, Mayuko Mori, Bun'ei Sato, Denitza Stoeva, Motohide Tamura, Masataka Aizawa, Bryson Cale, Thomas Henning, Hiroyuki Tako Ishikawa, Norio Narita, Masahiro Ogihara, Aniket Sanghi, Trifon Trifonov, Jerry Xuan, Eiji Akiyama, Hiroki Harakawa, Klaus Hodapp, Masato Ishizuka, Shane Jacobson, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Jungmi Kwon, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Huan-Yu Teng, Akitoshi Ueda, Sebastien Vievard
Figure caption: Left: original postprocessed image (top: the 2023 August data with KL = 3, bottom: the 2024 January data with KL = 10) at the location of a point-like source. Middle: the best-fit forward-modeled PSF. Right: residual map after subtracting the forward-modeled PSF from the postprocessed image.
Paper: Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633
Authors: Taichi Uyama, Masayuki Kuzuhara, Charles Beichman, Teruyuki Hirano, Takayuki Kotani, Qier An, Timothy D. Brandt, Markus Janson, Dimitri Mawet, Mayuko Mori, Bun'ei Sato, Denitza Stoeva, Motohide Tamura, Masataka Aizawa, Bryson Cale, Thomas Henning, Hiroyuki Tako Ishikawa, Norio Narita, Masahiro Ogihara, Aniket Sanghi, Trifon Trifonov, Jerry Xuan, Eiji Akiyama, Hiroki Harakawa, Klaus Hodapp, Masato Ishizuka, Shane Jacobson, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Jungmi Kwon, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Huan-Yu Teng, Akitoshi Ueda, Sebastien Vievard
Figure caption: Postprocessed NIRC2 image of the J1446 data taken in 2023 August (see text for the postprocessing parameters). The white arrow indicates the location of the new companion. The central star is masked by the postprocessing algorithms.
Paper: Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633
Authors: Taichi Uyama, Masayuki Kuzuhara, Charles Beichman, Teruyuki Hirano, Takayuki Kotani, Qier An, Timothy D. Brandt, Markus Janson, Dimitri Mawet, Mayuko Mori, Bun'ei Sato, Denitza Stoeva, Motohide Tamura, Masataka Aizawa, Bryson Cale, Thomas Henning, Hiroyuki Tako Ishikawa, Norio Narita, Masahiro Ogihara, Aniket Sanghi, Trifon Trifonov, Jerry Xuan, Eiji Akiyama, Hiroki Harakawa, Klaus Hodapp, Masato Ishizuka, Shane Jacobson, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Jungmi Kwon, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Huan-Yu Teng, Akitoshi Ueda, Sebastien Vievard
Figure caption: Left: modeled projected orbits of J1446B from fitting the Gaia DR3 acceleration (a red arrow in left) and two measured Keck/NIRC2 relative astrometric measurements (blue dots in left), and Subaru/IRD RVs (red dots in right). The host star defines the origin and is indicated by a black star; one hundred random orbital draws are shown and color coded by companion mass, with the best-fit orbit (black). The fitted offset at 2016.0 is plotted in red, and the direction of the measured Gaia DR3 acceleration is indicated by the red arrow. Right: modeled RVs from a random sampling of orbits from the posterior are color coded by companion mass with the best-fit orbit.
Paper: Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633
Authors: Taichi Uyama, Masayuki Kuzuhara, Charles Beichman, Teruyuki Hirano, Takayuki Kotani, Qier An, Timothy D. Brandt, Markus Janson, Dimitri Mawet, Mayuko Mori, Bun'ei Sato, Denitza Stoeva, Motohide Tamura, Masataka Aizawa, Bryson Cale, Thomas Henning, Hiroyuki Tako Ishikawa, Norio Narita, Masahiro Ogihara, Aniket Sanghi, Trifon Trifonov, Jerry Xuan, Eiji Akiyama, Hiroki Harakawa, Klaus Hodapp, Masato Ishizuka, Shane Jacobson, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Jungmi Kwon, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Huan-Yu Teng, Akitoshi Ueda, Sebastien Vievard
Figure caption: TESS lightcurves of J1446 ranging four sectors. Left: comparisons of the measured flux variations in the four sectors, where we adopted median time of each section as a reference date. Right: the same comparison as the left panel except for the y-axis with normalized fluxes.
Paper: Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633
Authors: Taichi Uyama, Masayuki Kuzuhara, Charles Beichman, Teruyuki Hirano, Takayuki Kotani, Qier An, Timothy D. Brandt, Markus Janson, Dimitri Mawet, Mayuko Mori, Bun'ei Sato, Denitza Stoeva, Motohide Tamura, Masataka Aizawa, Bryson Cale, Thomas Henning, Hiroyuki Tako Ishikawa, Norio Narita, Masahiro Ogihara, Aniket Sanghi, Trifon Trifonov, Jerry Xuan, Eiji Akiyama, Hiroki Harakawa, Klaus Hodapp, Masato Ishizuka, Shane Jacobson, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Jungmi Kwon, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Huan-Yu Teng, Akitoshi Ueda, Sebastien Vievard
Figure caption: Corner plot of the orbital fitting result combining Subaru/IRD radial velocity, Keck/NIRC2 direct imaging, and Gaia proper-motion acceleration. The orbital fit is described in Section 4.2.
Paper: Direct Imaging Explorations for Companions from the Subaru/IRD Strategic Program II; Discovery of a Brown-dwarf Companion around a Nearby Mid-M-dwarf LSPM J1446+4633
Authors: Taichi Uyama, Masayuki Kuzuhara, Charles Beichman, Teruyuki Hirano, Takayuki Kotani, Qier An, Timothy D. Brandt, Markus Janson, Dimitri Mawet, Mayuko Mori, Bun'ei Sato, Denitza Stoeva, Motohide Tamura, Masataka Aizawa, Bryson Cale, Thomas Henning, Hiroyuki Tako Ishikawa, Norio Narita, Masahiro Ogihara, Aniket Sanghi, Trifon Trifonov, Jerry Xuan, Eiji Akiyama, Hiroki Harakawa, Klaus Hodapp, Masato Ishizuka, Shane Jacobson, Eiichiro Kokubo, Mihoko Konishi, Tomoyuki Kudo, Takashi Kurokawa, Jungmi Kwon, Jun Nishikawa, Masashi Omiya, Takuma Serizawa, Huan-Yu Teng, Akitoshi Ueda, Sebastien Vievard
Figure caption: CCFs between the IRD spectra of J1446 and a reference single star GJ 699 over three epochs, showing single-peaked profiles and similarity between these two stars.
Paper: The Polar Orbit of TOI-2374 b, a Planet in the Neptunian Ridge
Authors: Samuel W. Yee, Patrick Tamburo, Gudmundur Stefánsson, Juliana García-Mejía, David Charbonneau, Khalid Barkaoui, Karen A. Collins, Richard P. Schwarz, Norio Narita, Akihiko Fukui, Andrew W. Howard, Howard Isaacson, Benjamin J. Fulton, Fei Dai
Figure caption: First row: the Tierras light curve at the native 30 s cadence (great points) along with the best-fit quasiperiodic Gaussian process (QP-GP; magenta). The data are colored by time and have been corrected with a linear function of sky background given by c0 + c1 · sky. The 1σ and 2σ uncertainty regions of the best-fit QP-GP model are shown as shaded regions. The white points show the data binned over two-night intervals. Second row: the residuals from the best-fit QP-GP model. The residual scatter is larger between days 210 and 245 due to a smaller number of visits per night during that time period. Third row: The LS periodogram of the data. The peak of the periodogram is at Ppeak  =  26.14 days. The next six highest peaks are indicated with triangles. These peaks are expected aliases of Ppeak given the periods at which the window function (fourth row) has significant power. Fifth row: the data phase-folded on a period of 26.38 days, the rotation period inferred from the GP model. The color of the points matches that in the first row and indicates the progression of time. White points show the data binned over equal widths in phase. We plot a sine model in black to show the periodic nature of the variability.
Paper: The Polar Orbit of TOI-2374 b, a Planet in the Neptunian Ridge
Authors: Samuel W. Yee, Patrick Tamburo, Gudmundur Stefánsson, Juliana García-Mejía, David Charbonneau, Khalid Barkaoui, Karen A. Collins, Richard P. Schwarz, Norio Narita, Akihiko Fukui, Andrew W. Howard, Howard Isaacson, Benjamin J. Fulton, Fei Dai
Figure caption: Distribution of known transiting planets in the planet radius–orbital period plane, showing the boundaries of the “hot Neptune desert” and “Neptunian ridge” (the overdensity of intermediate-sized planets between 3 and 6 days between the vertical dashed lines), as defined by A. Castro-González et al. (2024). TOI-2374b is part of the Neptunian ridge and is shown as the red star. Planets with no obliquity measurements are shown in gray, planets with low measured obliquities are shown in blue, while planets with misaligned orbits (λ more than 1σ greater than 15°) are shown in red. Square symbols denote planets with radii between 5.5 and 8.5 R⊕, while triangles denote those with Rp between 4.0 and 5.5 R⊕. Planet properties were drawn from the NASA Exoplanet Archive PSCompPars table (NASA Exoplanet Archive 2022) as of 2025 June 5, while obliquity measurements were compiled from S. H. Albrecht et al. (2022), E. Knudstrup et al. (2024), and the TEPCat catalog (J. Southworth 2011).
Paper: The Polar Orbit of TOI-2374 b, a Planet in the Neptunian Ridge
Authors: Samuel W. Yee, Patrick Tamburo, Gudmundur Stefánsson, Juliana García-Mejía, David Charbonneau, Khalid Barkaoui, Karen A. Collins, Richard P. Schwarz, Norio Narita, Akihiko Fukui, Andrew W. Howard, Howard Isaacson, Benjamin J. Fulton, Fei Dai
Figure caption: KPF RVs showing the detection of the Rossiter–McLaughlin effect for TOI-2374b (bottom panel), along with contemporaneous multicolor photometry from MuSCAT3 (top panel). Red lines show the maximum-likelihood model from the respective EXOFASTv2  and rmfit  fits. The KPF RV data show a clear anomaly during the time of the photometric transit.
Paper: The Polar Orbit of TOI-2374 b, a Planet in the Neptunian Ridge
Authors: Samuel W. Yee, Patrick Tamburo, Gudmundur Stefánsson, Juliana García-Mejía, David Charbonneau, Khalid Barkaoui, Karen A. Collins, Richard P. Schwarz, Norio Narita, Akihiko Fukui, Andrew W. Howard, Howard Isaacson, Benjamin J. Fulton, Fei Dai
Figure caption: Top: residual CCFs obtained by subtracting each observation’s CCF from the out-of-transit template. The in-transit CCFs are colored according to the time from midtransit. For reference, the residual CCFs for the out-of-transit observations are shown in gray, showing no significant deviations above the noise level. Bottom: this panel shows the residual CCFs with time flowing upward on the vertical axis. Horizontal dashed lines show the planet ingress and egress times (first and fourth contacts).
Paper: The Polar Orbit of TOI-2374 b, a Planet in the Neptunian Ridge
Authors: Samuel W. Yee, Patrick Tamburo, Gudmundur Stefánsson, Juliana García-Mejía, David Charbonneau, Khalid Barkaoui, Karen A. Collins, Richard P. Schwarz, Norio Narita, Akihiko Fukui, Andrew W. Howard, Howard Isaacson, Benjamin J. Fulton, Fei Dai
Figure caption: Local RVs computed from the centroids of a Gaussian fit to the local CCFs. The red line shows the best-fitting model to the local RVs, assuming solid-body rotation for the star.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Deep learning implementation of the classification design in Figure 1. The dotted red boxes indicate the difference between ExoMiner++ and the original ExoMiner (H. Valizadegan et al. 2022). Note that this is a general architecture of ExoMiner++. The details of this model, after optimizing different parameters, are discussed in Section 5.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Classification architecture.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Difference image data for TESS SPOC TCE TIC 309787037-1-S35 (TOI 1046.01, an NEB), as shown in the DV mini-report. From left to right, top to bottom, the images show the difference flux, out-of-transit flux, in-transit flux, and difference SNR flux images. The red triangle marks the estimated transit source location, the red cross indicates the TIC’s coordinates in the CCD frame, the green plus represents the out-of-transit centroid estimate, and the white asterisks denote the positions of neighboring stars in the postage stamp. The photometric aperture is outlined with a dashed white line, while the target mask is indicated by a solid white line.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: Momentum dump data for TESS SPOC TCE TIC 82707763-1-S37 (TOI 1991.01, classified as an SEB). The top panel displays the phase-folded time series for the momentum dump flag array, while the bottom panel presents the corresponding binned version obtained through the preprocessing steps described in Section 4.2. The solid blue and dashed red lines indicate the average binned value and one standard deviation, respectively.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: PDCSAP flux for TIC 167526485 in Sector 6.
Paper: ExoMiner++: Enhanced Transit Classification and a New Vetting Catalog for 2-minute TESS Data
Authors: Hamed Valizadegan, Miguel J. S. Martinho, Jon M. Jenkins, Joseph D. Twicken, Douglas A. Caldwell, Patrick Maynard, Hongbo Wei, William Zhong, Charles Yates, Sam Donald, Karen A. Collins, David Latham, Khalid Barkaoui, Michael L. Calkins, Kylee Carden, Nikita Chazov, Gilbert A. Esquerdo, Tristan Guillot, Vadim Krushinsky, Grzegorz Nowak, Benjamin V. Rackham, Amaury Triaud, Richard P. Schwarz, Denise Stephens, Chris Stockdale, Cristilyn N. Watkins, Francis P. Wilkin
Figure caption: PDCSAP flux for TIC 82707763 in Sector 37. The occurrence of momentum dump events is shown as vertical dashed green lines.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Equivalent widths of Hα for HIP 67522 b spanning observations on 2021 May 14 UT. Each of the 100 overlapping blue lines represents a single set of realizations from our Monte-Carlo error perturbation. The black dots are the average equivalent width for each time step, with error bars marking a 1σ range of uncertainties. The vertical red lines denote the start and end times of the predicted transit (T14).
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: The time evolution of the reduced and template-corrected spectra for HIP 67522 spanning observations on 2023 February 28 UT. The observations occurred 1 day after the predicted transit of HIP 67522 b, resulting in a planet-less series of observations. The color bar shows the time of observation relative to the simulated midpoint of the transit had observations spanned the actual predicted transit time. The line in red denotes ingress of the actual transit time +1 day. The vertical dashed lines mark the region used for the in-transit feature.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Planetary equilibrium temperature versus planetary density for targets with Hα observations. Detections are shown in blue, with non-detections in red; the three targets considered here are shown as colored stars (outline for detection/nondetection). This plot suggests the major deciding factor is low ρ and high Teq more than age. However, age and density are correlated as <200 Myr planets planets are known to be puffier than their older counterparts (S. Vach et al. 2024).
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: The equivalent widths of the Ca I absorption feature located near 6103 Å plotted against the time of observation in relation to the predicted transit times for HIP 67522 b, HD 63433 b, and two nights for DS Tuc A b in descending order. The transit ingress and egress are marked by the vertical red lines. This feature is relatively stable within uncertainties, indicating no detections of atmospheric calcium.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Same as Figure 9 for HD 63433 b. A marginally significant dip is seen near transit egress, but this is unlikely to be associated with the planet given the timing and resulting stacked Hα profile (Figure 11).
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Median combination of the telluric and stellar-corrected spectra of HIP 67522 taken within the predicted transit times of HIP 67522 b. We fit a Gaussian to the blueshifted absorption feature and use this feature to estimate the best region of integration for our equivalent width measurements.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Same as Figure 7 but for DS Tuc A b for the two different transits observed. Top is 2019 August 19 and bottom is 2019 October 7 UT. The orange lines indicate the bounds of integration for the equivalent width calculation (Figure 12). A feature is present, but it shows excess emission (weaker absorption)—an exosphere would manifest as excess absorption.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Same as Figure 7, but for HD 63433 b. A feature consistent with excess absorption is visible, but the profile and location are consistent with a stellar origin.
Paper: Ever Elusive Exospheres: One Probable Detection and Two Nondetections of Hα Transits in Young Systems
Authors: Reilly P. Milburn, Andrew W. Mann, Keighley Rockcliffe, Erin E. Flowers, Alexis Heitzmann, Benjamin T. Montet, George Zhou, Madyson G. Barber
Figure caption: Same as Figure 9 for the two transits of DS Tuc A b. The top is 2019 August 19 UT and the bottom is 2019 October 7 UT.