adsabs/AstroCLIMB huggingface dataset:
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: Comparisons between predicted and observed masses and radii. Top: mass–radius relations assuming our isochrone-inferred system ages. We plot the mass–radius relation at each system’s age as the solid line and indicate its 1σ uncertainty as the shaded region. Bottom: mass–radius relations assuming a range of ages. Thicker lines refer to older ages. BD+45 1593 Ab has a significantly larger radius than predicted by the Baraffe et al. (2015) theoretical models. UCAC4 515-012898 b is slightly bigger than predicted by the Baraffe et al. (2015) theoretical models as is frequently observed for low-mass stars. TYC 2010-124-1 b is consistent with the Chabrier et al. (2023) models. The models we use assume solar metallicity, while our systems have slightly subsolar metallicities. However, these differences in metallicity are too small to produce a radius offset as large as we observe for BD+45 1593 Ab. Indeed, at the low-mass end of the MIST isochroe grid at M * ≈ 0.11 M ⊙ ≈ 110 M Jup a 0.2 dex decrease in [Fe/H] corresponds to no more than a 5% decrease in stellar radius.
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: Comparison between CHIRON and NEID velocity zero-point offsets for TOI-5427. We plot distribution medians as solid vertical lines and the 16th and 84th percentiles as dashed vertical lines. Left: Distributions of Monte Carlo samples from thejoker Doppler solution systemic velocities after fitting to radial velocity measurements taken by CHIRON and NEID. Right: Distribution of the differences between the two distributions in the left-hand panel. The resulting median offset is much smaller than the individual radial velocity uncertainties, suggesting that the data sets are consistent with each other.
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: Corner plots showing unimodal posteriors for BD+45 1593 (left), TYC 2010-124-1 (center), and UCAC4 515-012898 (right).
Paper: The Advantages of Global Photometric Models in Fitting Transit Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Three individual events of different S/N values. Top row: The blue error bars are the synthetic data points, the solid orange line is the best-fitting model, the vertical black dashed line is the true time of mid-transit, and the pink transparent stripes are the 1σ , 2σ , and 3σ confidence intervals of the time of mid-transit, as retrieved by the LM algorithm (on the left panel, they are too narrow to be distinguishable). The black dashed line denotes the true time of mid-transit. Bottom row: For each event, we show the χ 2 surface over different values of time of mid-transit (blue) and a best-fitting parabola for the points within the 1σ confidence interval. The small inserts show a zoom-in on the region where the parabolic fitting was performed, with a circle indicating the parabola vertex. In the high-S/N case (left-hand side), there is a clear depression in the χ 2 surface, with a shape similar, but not equal, to a parabola around the best-fitting value. As S/N is reduced toward unity (middle), there is still a minimum near the true time of mid-transit, but its shape deviates from a parabola even more than in the high-S/N case. In S/N values lower than unity, the transit shape is erased by the noise (one should note the relatively shallow vertical span of the entire panel), and other local minima begin to appear in the χ 2 surface, thus leading to a completely wrong estimate of the time of mid-transit.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: TESS TPFs of TOI-2373 (TIC 332558858; left), TOI-2416 (TIC 237922465; middle), and TOI-2524 (TIC 169249234; right), created using tpfplotter. Orange overlays show the apertures used to determine the flux (a white overlay indicates an automatically detected threshold aperture). Gaia DR2 catalog objects are shown as filled red circles sized according to their brightness relative to the target (marked with a white cross).
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Maximum likelihood periodogram analysis of TOI-2373, TOI-2416, and TOI-2524. The top two panels show the periodograms of the RV data, before and after subtracting a Keplerian model, and the following panels show the periodograms of stellar activity indicators and the RV window function. Shown as dashed blue vertical lines are the transit signal periods. Dashed horizontal lines correspond to FAP levels of 10%, 1%, and 0.1%.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Phase plots for TOI-2373 b. Top left: phase-folded light curves for all TESS sectors. Faint points correspond to the unbinned data, the strong points to binned data. Top right: phase-folded light curves of the photometry from the ground-based facilities. Individual data sets are offset for better visibility. LCO CTIO observed two different transits and thus appears twice. Bottom: phase-folded RVs.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: TLS analysis of TOI-2373, TOI-2416, and TOI-2524. The top panels show the TLS results of the raw light curves, the bottom panels show the TLS results after subtracting a photometric transit model. The dashed blue vertical lines show the transit signal periods. Dashed horizontal lines correspond to false-alarm probability (FAP) levels of 10%, 1%, and 0.1%.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Same as Figure 5, but for TOI-2416 b.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Same as Figure 5, but for TOI-2524.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Speckle observations from HRCam at SOAR. The black points and solid curves represent the 5σ contrast curves. The insets show the speckle ACFs.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Mass–radius diagram for planets around solar-analog stars. Shown as blue stars are the solar system giant planets, whereas the new planets TOI-2373 b, TOI-2416 b, and TOI-2524 b are shown as colored stars. Shown as solid lines are exoplanet composition models based on Mordasini et al. (2012), Zeng et al. (2019), and Emsenhuber et al. (2021b) and fixed densities of ρ = 0.1, 0.3, 1.0, 3.0, and 1.0 g cm−3 are shown as dashed gray lines. The shaded area around the fit to the data of Emsenhuber et al. (2021b) marks the moving standard deviation of their synthetic planets.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: TPF plots for Sectors 3, 4, 8, 28–31, and 38 for TOI-2416.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: TPF plots for Sectors 35, 45, and 46 for TOI-2524.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: TPF plot for Sector 31 for TOI-2373.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Mass-separation diagram for planets around solar-analog stars (definition according to Lehmann et al. 2022; see Section 1). The new planets TOI-2373 b, TOI-2416 b, and TOI-2524 b are shown as big stars.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Mass-separation diagram for planets around solar-analog stars (definition according to Lehmann et al. 2022; see Section 1). Shown as big stars are the new planets TOI-2373 b, TOI-2416 b, and TOI-2524 b.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Time series for TOI-2416. Top: photometric time series. Bottom: RV time series.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Time series for TOI-2524. Top: photometric time series. Bottom: RV time series.
Paper: Three Warm Jupiters around Solar-analog Stars Detected with TESS 
Authors: Jan Eberhardt, Melissa J. Hobson, Thomas Henning, Trifon Trifonov, Rafael Brahm, Nestor Espinoza, Andrés Jordán, Daniel Thorngren, Remo Burn, Felipe I. Rojas, Paula Sarkis, Martin Schlecker, Marcelo Tala Pinto, Khalid Barkaoui, Richard P. Schwarz, Olga Suarez, Tristan Guillot, Amaury H. M. J. Triaud, Maximilian N. Günther, Lyu Abe, Gavin Boyle, Rodrigo Leiva, Vincent Suc, Phil Evans, Nick Dunckel, Carl Ziegler, Ben Falk, William Fong, Alexander Rudat, Avi Shporer, Stephanie Striegel, David Watanabe, Jon M. Jenkins, Sara Seager, Joshua N. Winn
Figure caption: Time series of TOI-2373. Top: photometric time series. Bottom: RV time series.
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: Time dependence of the position angle of the dust (blue) and plasma (orange) tails from HI-1 (top), COR2 (middle), and C3 (bottom). Position angle uncertainties on some points are comparable to the size of the symbols used to plot the data. Red and blue solid curves are the anti-Sun (−S) and anti-orbital-motion (−V) directions, respectively. The time of perihelion is marked with a vertical dotted line on the COR2 (middle) panel. The data points are presented in Tables 2, 3, and 4. Note that five orange data points are above the horizontal dotted line in the top panel. The comet aberration angles cannot be resolved with these data points using the current technique. The calendar dates are shown on the top horizontal axis.
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: The comet’s orbit (green arc) viewed from above, where r is the comet’s heliocentric distance, V  is the comet’s orbital velocity, –  S  is the antisolar direction, –  S   p  is the antisolar direction corresponding to the comet’s aberration, ε is the aberration angle, Δν = ν − ν  p  (where ν is the true anomaly at the observing time and ν  p  is the true anomaly at the time associated with the observed tail position angle),  L  is the plasma tail length, and η is the angle between –  S   p  and the plasma tail axis. The relation ε = η + Δν is independent of tail length. Taking η → 0, ε ∼ Δν.
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: Inferred solar wind radial velocity as functions of heliocentric distance (top), longitude (middle), and latitude (bottom). The three plots on the left present the solar wind velocities as S3 moves inbound; those on the right present the solar wind as S3 moves outbound. The symbols distinguish measurements made with HI-1 (blue squares), COR2 (orange circles), and LASCO/C3 (purple diamonds).
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: The comet plasma tail aberration angles as a function of time (bottom horizontal axis) and heliocentric distance (top horizontal axis) in the comet’s orbital plane. The three panels show the measurements from the three instruments: HI-1 (top), COR2 (middle), and C3 (bottom). Red horizontal lines show the Sun–comet line, ε = 0°.
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: The comet’s true anomaly (ν) as function of antisolar position angle (θ). Functions are plotted as solid black curves provided by JPL Horizons in all three panels. Light blue circles represent the comet’s true anomaly (ν) at the time of observation. Gray circles represent the comet’s true anomaly (ν  p ) inferred from the tail position angles (θ plasma). The three panels correspond to the HI-1, COR2, and C3 instruments. Note the five gray data points are not on the black curve on the top panel for HI-1. The true anomaly cannot be solved for these data points.
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: FWHM of the comet tails as a function of distance from the nucleus. The error bars are 3σ uncertainties of the tail width computed from the Gaussian fits. The coma positions are marked with vertical dotted lines for each camera. The embedded images are composites of the HI-1 and LASCO/C3 images from which the widths are measured (dust widths are from LASCO/C3 and plasma widths are from HI-1). Scale bars on the images are 1 Mkm at the comet.
Paper: Lensing in the Blue. II. Estimating the Sensitivity of Stratospheric Balloons to Weak Gravitational Lensing
Authors: Jacqueline E. McCleary, Spencer W. Everett, Mohamed M. Shaaban, Ajay S. Gill, Georgios N. Vassilakis, Eric M. Huff, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Paul Clark, Bradley Holder, Aurelien A. Fraisse, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Emaad Paracha, Susan F. Redmond, Jason D. Rhodes, Jürgen Schmoll, Ellen Sirks, Sut Ieng Tam
Figure caption: Average tangential shear profile for 30 simulated galaxy clusters with identical masses and redshifts. Each point represents the mean value of the tangential shear profiles across the cluster sample; error bars represent the standard deviation of the mean in each radial bin and illustrate the fluctuation of individual cluster measurements. Profiles are shown for observations in b, lum, and shape (3 hr of exposure time each). Top: clusters with M = 4.1 × 1014 M ⊙ h −1, z = 0.059. Bottom: clusters with M = 4.1 × 1014 M ⊙ h −1, z = 0.45. The bottom x-axes show distance from the cluster center in arcminutes, while top axes are scaled to show the projected distance from the cluster center in megaparsecs. The tangential shear profiles are easily detected in SUPERBIT b and lum observations, shown in blue and gold, with no obvious advantage for shape-band measurements (shown in red).