adsabs/AstroCLIMB huggingface dataset:
Paper: EXPRES. III. Revealing the Stellar Activity Radial Velocity Signature of ϵ Eridani with Photometry and Interferometry
Authors: Rachael M. Roettenbacher, Samuel H. C. Cabot, Debra A. Fischer, John D. Monnier, Gregory W. Henry, Robert O. Harmon, Heidi Korhonen, John M. Brewer, Joe Llama, Ryan R. Petersburg, Lily L. Zhao, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Claire L. Davies, Tyler Gardner, Cyprien Lanthermann, Gail Schaefer, Benjamin Setterholm, Catherine A. Clark, Svetlana G. Jorstad, Kyler Kuehn, Stephen Levine
Figure caption: Corner plot showing posterior distribution draws of GP hyperparameters (celerite quasiperiodic covariance kernel), after burn-in by the nested sampler. The 16%, 50%, and 84% quantiles are marked with vertical dashed lines in the marginalized histograms, which are also used to define the median values and uncertainties printed above each column.
Paper: Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light
Authors: Boris S. Safonov, Ivan A. Strakhov, Maria V. Goliguzova, Olga V. Voziakova
Figure caption: Columns 1–4: the measurements of ﹩{{ \mathcal R }}_{Q}﹩ and ﹩{{ \mathcal R }}_{U}﹩ for CQ Tau, unpolarized star HIP38325, polarization standard HD19820, from the top to the bottom. Columns 1–2 contain the absolute part of the signal, and columns 3–4 contain its argument. The axes are shown in spatial frequency, normalized by the cutoff frequency λ/D, where D = 2.5 m is the aperture diameter. The rightmost column presents the image of the envelope in polarized intensity relative to the total flux of the star, reconstructed by the algorithm presented in Section 3.2. Dashes indicate the orientation of polarization. Please note the different brightness scales; the unit is polarized flux per pixel divided by the total unpolarized flux from the star. The gray circle in the upper right image indicates the typical angular resolution. In all images, north is up and east is to the left.
Paper: Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light
Authors: Boris S. Safonov, Ivan A. Strakhov, Maria V. Goliguzova, Olga V. Voziakova
Figure caption: The comparison of our data (indicated by gray contours) with the results from the literature. The green line is the spiral arm found using Subaru/HiCIAO (Uyama et al. 2020). The black ellipse is the 1.3 mm continuum ring obtained using ALMA by Ubeira Gabellini et al. (2019; the dashed lines indicate the approximate borders of this ring). The blue line indicates a possible orbit of the planet proposed by Ubeira Gabellini et al. (2019). The red ellipse shows the orientation and inclination of the inner disk according to PTI data (Eisner et al. 2004; enlarged 25 times for visual clarity). The gray segments are the assumed shadow cast by the inner disk on the outer ring; see Section 4.3.
Paper: Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light
Authors: Boris S. Safonov, Ivan A. Strakhov, Maria V. Goliguzova, Olga V. Voziakova
Figure caption: Scheme illustrating the first steps of the differential speckle polarimetry processing using a single frame as an example. The first row displays the raw frame with two images corresponding to orthogonal polarizations. In the second row the extracted subframes are presented. The third row shows the Fourier transforms of the subframes. The first and third panels contain the amplitude, and the second and fourth contain the argument of the complex Fourier transform.
Paper: Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light
Authors: Boris S. Safonov, Ivan A. Strakhov, Maria V. Goliguzova, Olga V. Voziakova
Figure caption: The rotation angle η determined from the approximation of individual observations with the reference observation (UT 2018 November 25 23:49). A positive value means that the given observation is rotated CCW with respect to the reference one. The black line indicates a weighted linear fit: η = η 0 + ω t, where η 0 = −0.°4 ± 1.°6 and ω = −0.°2 ± 1.°1 yr−1 (68% credible intervals). The red line indicates the expected CCW rotation for T = 75 yr.
Paper: Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light
Authors: Boris S. Safonov, Ivan A. Strakhov, Maria V. Goliguzova, Olga V. Voziakova
Figure caption: The same as in fifth column of Figure 3, but for observations obtained at the Nasmyth focus. From left to right: CQ Tau, an unpolarized star, and a polarization standard. The date of the respective observation is indicated in the title.
Paper: Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light
Authors: Boris S. Safonov, Ivan A. Strakhov, Maria V. Goliguzova, Olga V. Voziakova
Figure caption: Top and bottom panels show the dependence of the polarization angle and fraction of CQ Tau on time, respectively.
Paper: Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light
Authors: Boris S. Safonov, Ivan A. Strakhov, Maria V. Goliguzova, Olga V. Voziakova
Figure caption: Cartoon illustrating the assumed mutual orientation of the outer and inner dust disks. The size of the inner disk is exaggerated.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Grid of Robo-AO images of tight triple system candidates. The images are displayed either in linear or log stretch (when Δm > 2.5), for ease of visually seeing the fainter companion. The second row of images outlined in blue are the PSF-subtracted images in order to see the close-in companion(s) of the image above. The color of the circle indicating the companion is based on whether the companion is physically associated (solid green) or yet to be confirmed (dashed orange). The northeast orientation of the images is shown in the bottom right and the image scale in arcseconds is shown for each image cutout.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Grid of Robo-AO images of binary candidates. The images are displayed either in linear or log stretch (when Δm > 2.5), for ease of visually seeing the companion. The images outlined in blue are the PSF-subtracted images in order to see close-in companions. The color of the circle indicating the companion is based on whether the companion is physically associated (solid green) or yet to be confirmed (dashed orange). The northeast orientation of the images are shown in the bottom right and the image scale in arcseconds is shown for each image cutout.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Physical association thresholds (the two dashed lines at 0.35), identified by comparing the primary and companion proper motion and parallax Gaia EDR3 measurements. The wide Gaia comoving companions as well as those detected in Robo-AO images with Gaia EDR3 information are shown. For those found in the El-Badry et al. (2021) catalog, their ﹩{ \mathcal R }﹩ value is given and we show the subsample of stars within 50pc in El-Badry et al. (2021)'s binary catalog in green.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Detected companion candidates within 4″ with Robo-AO. Companions with Gaia EDR3 parallax and proper motion measurements consistent with their host star are determined to be physically associated (green circles). Companion candidates with Gaia parallax and proper motion measurements inconsistent with the host star are determined to be background objects (gray triangles). The remaining companion candidates were not found in Gaia EDR3 or the star; otherwise, companions were lacking parallax and proper-motion information to confirm comoving physical association (orange squares).
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Detected companions within 4″ as a function of projected separation in astronomical units and color coded by primary star spectral type. Filled circles are physically associated companions and empty squares are yet to be confirmed companion candidates, where the distance was assumed to be the same as the host star. The detections determined to be background objects were removed.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: (continued). Grid of Robo-AO images of binary candidates. The images are displayed either in linear or log stretch (when Δm > 2.5), for ease of visually seeing the companion. The images outlined in blue are the PSF-subtracted images in order to see close-in companions. The color of the circle indicating the companion is based on whether the companion is physically associated (solid green) or yet to be confirmed (dashed orange). The northeast orientation of the images are shown in the bottom right and the image scale in arcseconds is shown for each image cutout.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: The distribution of ﹩{\rm{\Delta }}\pi /{\pi }_{\mathrm{prim}}﹩ and ﹩{\rm{\Delta }}\mu /{\mu }_{\mathrm{prim}}﹩ for the wide comoving companions identified in Gaia EDR3 as well as the Robo-AO-detected companions found in Gaia EDR3.
Paper: An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO
Authors: Maïssa Salama, Carl Ziegler, Christoph Baranec, Michael C. Liu, Nicholas M. Law, Reed Riddle, Todd J. Henry, Jennifer G. Winters, Wei-Chun Jao, James Ou, Arcelia Hermosillo Ruiz
Figure caption: Sensitivity curves for all observed targets.
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: Flipping regions in the entire (e 0, i 0) space. The dynamical models are characterized by ϵ = 0.01 (left panel) and by ϵ = 0.02 (right panel). The initial angles of the points in the green regions are fixed at ω 0 = 0, Ω0 = π, and the ones of the points in the black regions are fixed at ω 0 = 0, Ω0 = 0. In both panels, there are three distinct regions, denoted by I, II, and III from left to right. When the eccentricities are greater than a critical value e  c (ϵ) (the location of e  c (ϵ) is marked by a vertical red dashed line), orbit flips can take place from nearly coplanar configurations. Comparing the flipping regions shown in the left and right panels, we can see that the flipping area is larger when the factor ϵ is higher.
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: Phase portraits (level curves of adiabatic invariant) at different levels of Hamiltonian (﹩{ \mathcal H }=-0.2,-0.3,-0.4,-0.8﹩). ΔΣ1 measures the size of flipping region. The red lines stand for the dynamical separatrices, dividing circulation regions from libration ones.
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: Comparisons of flipping boundaries produced by three approaches. The black stars stand for the numerical boundary based on Poincaré surfaces of section, the blue dots stand for the numerical boundary based on invariant manifolds of unstable polar orbits, and the red dots stand for the analytical boundary obtained by means of perturbative treatment. Three examples are marked by A (in region I), B (in region II), and C (in region III), and their evolution of elements is given in Figure 15. The shaded regions denoted by I, II, and III are the same as the left one of Figure 1.
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: Phase portraits (similar to the ones shown in Figure 11) as well as numerically propagated trajectories, shown by black lines. The starting points of numerical trajectories are marked by red stars and the initial angle σ 2(0) is set as zero for all numerical trajectories. The initial state Σ2(0) can be produced from the given Hamiltonian. The green dots stand for the points on the numerical trajectories holding σ 2( = ω) = 0. It is observed that the green points on the section follow closely along the level curves shown in the phase portraits.
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: Time histories of inclination i and resonant argument σ 1 for three representatives of flipping orbits shown in Figure 14. For convenience, the points with i < 90° on the numerical trajectories are shown in red and the points with i > 90° are shown in black. For trajectories A (in region I) and C (in region III), the critical argument σ 1 librates around 180°, and for trajectory B (in region II), the critical argument σ 1 librates around 0°.
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: Analytical boundaries of flipping regions shown in the (e 0, i 0) space. Similarly, the regions of orbit flips are denoted by I, II, and III from left to right. In particular, the libration center of the critical argument σ 1 is at σ 1 = π in regions I and III, and it is at σ 1 = 0 in region II.
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: The distribution of ﹩\left\langle {\dot{\sigma }}_{1}\right\rangle =0﹩ in the initial inclination–eccentricity (i 0, e 0) space. Here ﹩\left\langle {\dot{\sigma }}_{1}\right\rangle ﹩ stands for the average of ﹩{\dot{\sigma }}_{1}﹩ over one period of a rotating Kozai cycle starting from (ω 0 = 0, e 0, i 0).
Paper: A Systematic Study about Orbit Flips of Test Particles Caused by Eccentric Von Zeipel–Lidov–Kozai Effects
Authors: Hanlun Lei
Figure caption: Schematic diagram for the definition of i  e  and Ω e  adopted by Katz et al. (2011).
Paper: Confirmation of the Long-period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate
Authors: Spencer A. Hurt, Benjamin Fulton, Howard Isaacson, Lee J. Rosenthal, Andrew W. Howard, Lauren M. Weiss, Erik A. Petigura
Figure caption: ΔBIC periodograms for each data set (first four panels) and the combined RVs (bottom panel). The horizontal dashed gray lines mark the 0.1% FAP threshold for each periodogram. The vertical dashed lines mark the periods of interest, with blue corresponding to GJ 411 b (∼12.9 days), red denoting the long-period, disputed signal (∼2900 days), green marking the candidate signal (∼215.2 days), and purple indicating the rotation period (∼55.3 days).
Paper: Confirmation of the Long-period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate
Authors: Spencer A. Hurt, Benjamin Fulton, Howard Isaacson, Lee J. Rosenthal, Andrew W. Howard, Lauren M. Weiss, Erik A. Petigura
Figure caption: Plots of the RVs vs. activity indices for each data set. Signals corresponding to GJ 411 b, the candidate, and stellar rotation have been subtracted from the RVs using the model presented in Section 4.4. Samples of linear models from the MCMC posterior for each pair of variables are shown as red lines. The 68.3% confidence interval for the slope is given in the top-right corner of each subplot. No correlations are observed for the APF and HIRES ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ values while the rest of the correlations appear to be weak and can be explained by nonastrophysical signals or stellar magnetic cycles that span even longer than 2900 days.
Paper: Confirmation of the Long-period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate
Authors: Spencer A. Hurt, Benjamin Fulton, Howard Isaacson, Lee J. Rosenthal, Andrew W. Howard, Lauren M. Weiss, Erik A. Petigura
Figure caption: GLS periodograms of the activity indices for each instrument. The three horizontal dashed lines in each panel represent the 1%, 0.5%, and 0.01% FAP levels for the corresponding periodogram. As with Figure 1, the vertical dashed lines represent the signals of interest, with blue corresponding to GJ 411 b, purple representing the rotational modulation, green marking the candidate signal, and red denoting the long-period disputed signal. No significant or resolved peaks appear near these four periodicities; however, periodograms for the APF, SOPHIE, and CARMENES indices do show elevated power near the long-period signal of ∼2900 days. This structure likely appears because the baselines for these data sets are too short to constrain any long periods.
Paper: Confirmation of the Long-period Planet Orbiting Gliese 411 and the Detection of a New Planet Candidate
Authors: Spencer A. Hurt, Benjamin Fulton, Howard Isaacson, Lee J. Rosenthal, Andrew W. Howard, Lauren M. Weiss, Erik A. Petigura
Figure caption: The time series data and best-fit Keplerian models for the ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ (top) and H α  (bottom) activity indices. We observe less than one cycle of the long-period signals contained in both, whereas our RV data span nearly two cycles of the 2900 day signal (see Figure 8 for comparison). This indicates that the disputed signal does not correspond to stellar magnetic activity and instead originates from a planet designated as GJ 411 c.
Paper: Shallow Transits—Deep Learning. II. Identify Individual Exoplanetary Transits in Red Noise using Deep Learning
Authors: Elad Dvash, Yam Peleg, Shay Zucker, Raja Giryes
Figure caption: Example F. Panels follow the structure of Figure 7. Note the wrong identification of a short transit around day seven.
Paper: Shallow Transits—Deep Learning. II. Identify Individual Exoplanetary Transits in Red Noise using Deep Learning
Authors: Elad Dvash, Yam Peleg, Shay Zucker, Raja Giryes
Figure caption: Example B. Panels follow the structure of Figure 7. Note the more prominent long-term variability in this specific case.
Paper: Shallow Transits—Deep Learning. II. Identify Individual Exoplanetary Transits in Red Noise using Deep Learning
Authors: Elad Dvash, Yam Peleg, Shay Zucker, Raja Giryes
Figure caption: Example H. Panels follow the structure of Figure 7. The segmentation is completely wrong, except for the transit around day 26, as reflected by the very low Dice coefficient.
Paper: Shallow Transits—Deep Learning. II. Identify Individual Exoplanetary Transits in Red Noise using Deep Learning
Authors: Elad Dvash, Yam Peleg, Shay Zucker, Raja Giryes
Figure caption: Example G. Panels follow the structure of Figure 7. All transits were identified in spite of the low S/N, resulting in a high Dice coefficient value.
Paper: Shallow Transits—Deep Learning. II. Identify Individual Exoplanetary Transits in Red Noise using Deep Learning
Authors: Elad Dvash, Yam Peleg, Shay Zucker, Raja Giryes
Figure caption: Example C. Panels follow the structure of Figure 7. Note the complex patterns of red-noise variability.
Paper: Shallow Transits—Deep Learning. II. Identify Individual Exoplanetary Transits in Red Noise using Deep Learning
Authors: Elad Dvash, Yam Peleg, Shay Zucker, Raja Giryes
Figure caption: Example E. Panels follow the structure of Figure 7. Note the partial coalescence of the third and six transits with the downlink gap.
Paper: Shallow Transits—Deep Learning. II. Identify Individual Exoplanetary Transits in Red Noise using Deep Learning
Authors: Elad Dvash, Yam Peleg, Shay Zucker, Raja Giryes
Figure caption: Example D. Panels follow the structure of Figure 7. Note the presence of many quasiperiodic transit-like features in the red noise.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: The same as Figure 4, but for the likelihood distributions of our ESPaDOnS observations alone. Note that the axis ranges of some subplots differ between these figures.
Paper: Dayside Fe I Emission, Day–Night Brightness Contrast and Phase Offset of the Exoplanet WASP-33b
Authors: Miranda K. Herman, Ernst J. W. de Mooij, Stevanus K. Nugroho, Neale P. Gibson, Ray Jayawardhana
Figure caption: The same as Figures 4 and 9, but for the likelihood distributions of our HDS observations alone.
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: The full systematics-corrected flux light curve for TOI-2184b with transit times marked by triangles. The alternating triangle colors represent the even and odd transits. The gray sections mark the data gaps due to data downlinks or the spacecraft entering safe mode. While the even transits (blue) fall almost exclusively in the middle of continuous data collection, the odd transits (orange) fall primarily near the beginning or end of a data gap when the TESS detector is experiencing increased scatter due to thermal sensitivity variation and scattered light. This trend is most present in the first seven observing sectors (top two rows), and disappears for the final four sectors (bottom row).
Paper: TESS Giants Transiting Giants. I.: A Noninflated Hot Jupiter Orbiting a Massive Subgiant
Authors: Nicholas Saunders, Samuel K. Grunblatt, Daniel Huber, Karen A. Collins, Eric L. N. Jensen, Andrew Vanderburg, Rafael Brahm, Andrés Jordán, Néstor Espinoza, Thomas Henning, Melissa J. Hobson, Samuel N. Quinn, George Zhou, R. Paul Butler, Lisa Crause, Rudi B. Kuhn, K. Moses Mogotsi, Coel Hellier, Ruth Angus, Soichiro Hattori, Ashley Chontos, George R. Ricker, Jon M. Jenkins, Peter Tenenbaum, David W. Latham, Sara Seager, Roland K. Vanderspek, Joshua N. Winn, Chris Stockdale, Ryan Cloutier
Figure caption: The LCOGT light curve and model for TOI-2184b in Pan-STARRS z-short band. The light gray symbols show the unbinned photometry. The purple and red symbols show the photometry from SAAO and CTIO, respectively, in 8 minute bins. The transit model is shown as purple and red lines, and the shaded regions represent the 68.3% highest-density region in the posteriors. The fitted parameters are consistent with the transit parameters from the TESS data within 1σ uncertainty (see Sections 3 and 5).