adsabs/AstroCLIMB huggingface dataset:
Paper: JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b
Authors: Munazza K. Alam, Peter Gao, Jea Adams Redai, Nicole L. Wallack, Nicholas F. Wogan, Artyom Aguichine, Anne Dattilo, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, James Kirk, Mercedes López-Morales, Annabella Meech, Sarah E. Moran, Johanna Teske, Hannah R. Wakeford, Angie Wolfgang
Figure caption: The MIRI transit-depth precisions for each independent reduction compared to the predictions from PandExo.
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: Top: relative orbits of planet c (in arc seconds) from fitting RVs and absolute astrometry from the v.EDR3 HGCA. 100 random orbital draws are shown and color coded by companion mass. Positions at a few selected epochs are displayed for the maximum-likelihood orbital solution (black). The host star is marked by the star symbol at the origin. The change of proper motion from Hipparcos–Gaia to Gaia is indicated as a red vector. Bottom: The observed RVs of HAT-P-11 overplotted with the best-fit orbit (in black) and a random sampling of other orbits from the MCMC chain. The RV signal includes both the high-frequency oscillations from b and the long-term high-eccentricity undulation of c. The RV residuals with respect to the best-fit orbit are in the attached bottom subpanel.
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: Corner plot of the orbital elements, with respect to the star, for HAT-P-11 c. In the 1D histograms, the vertical-dashed lines about the center dashed lines give the 16% and 84% quantiles around the median. In the 2d histograms, the contours give the 1σ, 2σ, and 3σ levels. The result of inclination is bimodal (shown in lower-right 1D histogram), where the peaks of distribution are close to 30° and 150° (two modes are reflected with respect to 90°). As Figure 6 shows, the retrograde mode (i > 90) is slightly favored by the Hipparcos proper motion. The summary statistics of HAT-P-11 system orbit fit are given separately for both inclination modes in Table 1.
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: Orbital architecture of the HAT-P-11 system. The star (not to scale) is represented by the red sphere. North and line-of-sight (to Earth) are given. The orbit of c is described in gray, while the inner planet b is not shown. The two orange cones represent the possible stellar spins that R. Sanchis-Ojeda & J. N. Winn (2011) derived from obliquity measurements of b. The upper cone is the set of edge-on stellar-spin configurations and the bottom cone give the pole-on solutions. The blue vector is the orbital angular momentum of the outer planet c.
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: The obliquity posterior between the outer planet HAT-P-11 c and the star A, for the four possible orbital/stellar spin configurations. The top panel shows the two obliquity posteriors (one for each of the possible inclination modes of the planet) assuming the pole-on stellar inclination posterior from R. Sanchis-Ojeda & J. N. Winn (2011). The bottom panel uses the the edge-on stellar inclination posterior. In dashed violet is the geometric ﹩\sin i﹩ posterior, which would be expected if we had no constraint on the orbit of HAT-P-11 c.
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: Astrometric orbit of HAT-P-11 due to planet c. One hundred random orbital draws are shown and color coded by inclination; the maximum-likelihood orbit is plotted in black. Retrograde orbits (red) are slightly favored by the Hipparcos proper motion (yellow point with large error bar on left), and both modes fits well with Gaia proper motion (yellow point on the right, with an error bar smaller than the point size).
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: Difference between ﹩{\mathrm{log}}_{10}R{{\prime} }_{\mathrm{HK}}﹩ computed using the formulas in M. Mittag et al. (2013) and R. W. Noyes et al. (1984), neglecting a correction from photospheric effects (this correction is small for active stars). The difference between the two ﹩R{{\prime} }_{\mathrm{HK}}﹩ measurements is large and strongly color dependent. For HAT-P-11, with an S-index of 0.58 and a color of B − V = 1.19 (B. M. Morris et al. 2017b), the R. W. Noyes et al. (1984) and M. Mittag et al. (2013) relations give ﹩{\mathrm{log}}_{10}R{{\prime} }_{\mathrm{HK}}﹩ of −4.40 and −4.82, respectively, when including the photospheric term.
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: The mutual inclination posterior between the outer c and the inner planet b, for the two possible i  c  configurations, assuming i  b  = 88.°5 ± 0.6 from (K. G. Stassun et al. 2017).
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: Corner plot of the orbital elements, with respect to the star, for HAT-P-11 b, which demonstrating a constraint on ﹩{{\rm{M}}}_{b}\sin i﹩. In the 1D histograms, the vertical-dashed lines about the center dashed lines give the 16% and 84% quantiles around the median. In the 2d histograms, the contours give the 1σ, 2σ, and 3σ levels. The summary statistics of HAT-P-11 system orbit fit are given separately for both inclination modes in Table 1.
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: Zoom in of Figure 7 between 0° and 40° obliquities. We show the most likely case (edge on) and the i c < 90° orbital solution. Two lower limits are presented as gray vertical lines: the 3σ lower-limit on the obliquity is 32°, and the 4σ (99.9936%) lower-limit is 22°.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: None of the initial volatile gradients tested in this work can explain the observed gradient of uncompressed densities in TRAPPIST-1. Each panel provides the median final WMF for all TRAPPIST-1 planet analogs (red points and error bars, see definitions in Section 2.1) formed in our current simulations, compared to the inferred values from E. Agol et al. (2021; black points, assuming CMFs of 0.25 for planets b, c, and e, and 0.18 for the other planets) for a range of different initial volatile gradients (blue and light blue lines). The error bars enclose 95% of the results from our complete simulation set. While the black points for the real system are plotted at the location of the observed semimajor axes of the planets, the red points for our simulated planets are positioned at the average semimajor axis of all planets encompassed by the data point.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: The compact nature of TRAPPIST-1 is most consistent within a disk with a steep surface density profile. This figure plots the cumulative distribution of orbital period ratios of neighboring planets in the solar system (thick gray line), the real TRAPPIST-1 system (thick orange line), all known multiplanet systems hosted by M dwarfs (thick blue line; compiled 2024 May 1), our simulations testing various values of α (red, black, and gold lines for α = −1.0, −1.5, and −2.5, respectively), and similar simulations around a 0.1 M ⊙ star from M. S. Clement et al. (2022) that did not include a collisional fragmentation scheme (black line). These lines only plot systems that form between five and nine planets. The salmon line, however, only depicts results from simulations with α = −2.5 that formed seven or more planets.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: Example evolution of a system that was initialized with α = −2.5 and M Disk = 6.0 M ⊕ that successfully formed a system of seven planets in total with orbits and masses very similar to those of the actual TRAPPIST-1 exoplanets (bottom panel). The semimajor axis and eccentricity of each body are plotted at each time interval, and the planets are color-coded to match their respective analog in the real system. Additionally, it is worthwhile to note that our 100 Myr follow-on tidal evolution simulation (fourth panel) produced four resonances in total (2:1, 8:5, 5:3, 3:2, labeled on the figure), two of which were of higher order.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: High-velocity collisions are more likely to alter the Fe–Si contents of the TRAPPIST planets than in similar simulations of accretion in the inner solar system. The figure plots the cumulative distribution of final CMFs for planets formed using different values of α (solid and dashed black lines), compared with all TRAPPIST-1b, e, and h analogs (blue, green, and light blue lines, respectively; see definitions in Section 2.1). Of note, TRAPPIST-1e has the highest bulk density and the third lowest mass of all the planets in the actual system (S. L. Grimm et al. 2018). For reference, the thick gray line plots all Earth analogs (0.85 au < a < 1.20 au and 0.60 M ⊕ < m < 1.5 M ⊕) in simulations of terrestrial planet formation in the solar system presented by M. S. Clement et al. (2019) using the same collisional fragmentation scheme and settings. The vertical blue and black lines represent the interpreted values for Earth and Mercury, respectively (S. A. Hauck et al. 2013).
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: The TRAPPIST-1 mass distribution is consistent with in situ formation. This figure plots the cumulative distribution of mass ratios of neighboring planets in the solar system (thick gray line), the real TRAPPIST-1 system (thick orange line), all known multiplanet systems hosted by M dwarfs (thick blue line; compiled 2024 May 1), our simulations testing various values of α (red, black, and gold lines for α = −1.0, −1.5, and −2.5, respectively), and similar simulations around a 0.1 M ⊙ star from M. S. Clement et al. (2022) that did not include a collisional fragmentation scheme (black line). These lines only plot systems that form between five and nine planets.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: A gradient in core mass fraction is a natural outcome of accretion in the TRAPPIST-1 system. This figure plots the comparison of median final CMF for TRAPPIST-1 planet analogs (red points, see definitions in Section 2.1) formed in our current simulations that set α to −1.0, compared to the inferred values from the fully differentiated model of E. Agol et al. (2021; black points and error bars).
Paper: Significant Mutual Inclinations Between the Stellar Spin and the Orbits of Both Planets in the HAT-P-11 System
Authors: Qier An, Tiger Lu, G. Mirek Brandt, Timothy D. Brandt, Gongjie Li
Figure caption: The predicted accelerations for two inclination modes of planet c, in unit of milli-arcsecond per year squared. The 1σ contour of the retrograde mode is plotted with a dashed line, and the corresponding contour of prograde mode is shown with a solid line. The center yellow crosses indicate the mean values. Zero accelerations in both R.A. and decl. are marked for reference.
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: Continuum intensity (left), 12CO line integrated intensity (moment-0; middle, rms of 0.8 mJy beam–1), and 12CO first-moment maps (right) show detections of circumstellar dust and gas orbiting both the primary and secondary stars of DF Tau. In the left and middle panels, the relative binary orbit of the secondary around the primary is overplotted in white, and the centers of the continuum emission, determined using imfit, are shown as white stars, confirming alignment with the binary orbit. The first-moment map (right, continuum emission and beam size are shown with overplotted white contours; the hatched region in the color bar indicates velocities that are highly obscured by molecular cloud absorption) shows rough agreement in the direction of rotation of the disks. Beam sizes are shown for all panels in the bottom left.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: The population of an asteroid belt region with scattered objects occurs as a consequence of the formation of the TRAPPIST-1 planets. This figure provides the distribution of semimajor axes and eccentricities of surviving collisional fragments (red points) and planetesimals (black points) in the hot debris disk (exo-asteroid belt) region of our TRAPPIST-1 analog systems. The three panels separate our systems formed from disks with different initial values of α. The figure only displays objects with semimajor axes greater than that of the most distant planet at the end of each simulation.
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: Light curves from TESS, K2 and the Lowell 0.7/1.1 m telescopes (top three panels, respectively) and resulting periodograms (bottom panel) for the blended DF Tau system. Maximum rotation periods for the observed ﹩v\sin i﹩, assuming alignment between stellar obliquity and disk inclination, and theoretical predictions of stellar radii (the 2 Myr tracks from G. A. Feiden 2016), are indicated by the shaded regions in red and yellow for the primary and secondary, respectively. There is no significant power at these periods, and therefore the variability in the light curve is dominated by stochastic accretion and/or other processes in the inner disk of the primary.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: Tidal evolution damps post-formation eccentricities. The various panels plot the cumulative distribution of system orbital parameters (top: orbital period ratios of neighboring planets; middle: eccentricity; bottom: Inclination) before (black lines) and after (red lines) our tidal evolution simulations (Section 3.5 compared with the solar system (thick gray line), the real TRAPPIST-1 system (thick orange line), and all known multiplanet systems hosted by M dwarfs (thick blue line; compiled 2024 May 1).
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: Continuum visibility fitting. Results are shown for spectral window 1. Left panels: data and model for the real and imaginary visibilities as a function of uv-distance. Right panels: maps of the data, model, and residuals. Contours in the residual image are set at −3σ and 3σ in the dashed and solid lines, respectively. The residuals are largely <±3σ.
Paper: On the Local Formation of the TRAPPIST-1 Exoplanets
Authors: Matthew S. Clement, Elisa V. Quintana, Kevin B. Stevenson
Figure caption: Capture of a TRAPPIST-1 analog in the 3:2 MMR after the completion of planet formation. Top: example of eccentricity evolution in our tidal evolutionary modeling of a TRAPPIST-1 analog system. The periastron and apastron of each planet are plotted in different colors. Bottom: resonant angle for the 3:2 mean motion resonance between the first and second planets in the system.
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: The expected location of the inner edge of a potential circumbinary disk (white dashed line) lies at approximately 3 times the semimajor axis of the binary orbit and is centered on the approximate center of mass of the binary. This does not show significant emission in our final continuum map. However, we place an upper limit on the amount of dust hidden in the circumbinary disk by tracing its inner edge with 48 beams (overplotted gray ovals).
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: Orbital motion of DF Tau B relative to A based on the AO imaging and measurements from the literature. The solid blue line shows the best-fitting orbit, while the gray lines show 100 orbits selected at random from the posterior distribution.
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: Angularly resolved photometry of DF Tau A (squares) shows a clear UV Excess when compared with DF Tau B (circles) and an appropriate BT-Settl (CIFIST) stellar photosphere model (gray). Yellow and orange regions denote the Kepler and TESS bandpasses, respectively. Photometry is reproduced from T. S. Allen et al. (2017), and the error bars are smaller than the markers.
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: Spatially resolved and continuum normalized spectra of DF Tau A (top) and B (bottom, separated by an offset) in black. Fifty randomly selected model spectra from the trimmed MCMC chain are overplotted in blue.
Paper: Sites of Planet Formation in Binary Systems. II. Double the Disks in DF Tau
Authors: Taylor Kutra, Lisa Prato, Benjamin M Tofflemire, Rachel Akeson, G. H. Schaefer, Shih-Yun Tang, Dominique Segura-Cox, Christopher M. Johns-Krull, Adam Kraus, Sean Andrews, Eric L. N. Jensen
Figure caption: Seasonal variation of the DF Tau periodogram using ground-based photometry obtained with the Lowell robotic 0.7 m telescope and the Lowell Hall 1.1 m telescope.
Paper: Quantifying the Contamination from nearby Stellar Companions in Gaia DR3 Photometry
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Daniel Huber
Figure caption: The Gaia G - KIC ﹩r^{\prime} ﹩ color plotted against binary separation. The right-hand y-axis shows spectral types estimated using synthetic G–r colors from A. L. Kraus et al. (2024, in preparation), while the left-hand y-axis shows the G–r color for the stars in our sample. At small separations the color is bluer because both Gaia G and KIC r are contaminated by the secondary star, while at wider separations KIC r is contaminated while Gaia G is not, producing a redder color than expected even for mid-M dwarfs.
Paper: Quantifying the Contamination from nearby Stellar Companions in Gaia DR3 Photometry
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Daniel Huber
Figure caption: Contamination fraction versus binary angular separation in terms of the secondary star flux. At small separations, nearly all of the secondary star flux is contaminating the Gaia system flux. The secondary star contribution decreases toward zero, reaching approximately zero around ﹩0\mathop{.}\limits^{^{\prime\prime} }4﹩. The zero point has been adjusted an arbitrary amount to ensure that the resolved binaries at wide separations are centered at zero contamination from the secondary.
Paper: Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars
Authors: Joseph D. Long, Logan Pearce, Sebastiaan Y. Haffert, Jared R. Males, Laird M. Close, Olivier Guyon, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Maggie Y. Kautz, Jay K. Kueny, Jialin Li, Jennifer Lumbres, Eden A. McEwen, Avalon L. McLeod, Lauren Schatz
Figure caption: Diagram of the paired MagAO-X science channel cameras. (a) Light enters after correction by the exAO system and starlight suppression by the coronagraph. (b) The selectable beamsplitter either sends Hα light to camsci2 and continuum in an adjacent narrowband filter to camsci1, or makes a 50/50 split. (c) Light passes through a selectable filter. (d) Light is imaged onto the EMCCD detectors in each science channel. (e) Both detectors sit on focus stages that can be adjusted independently. For a detailed description, see L. M. Close et al. (2018).
Paper: Quantifying the Contamination from nearby Stellar Companions in Gaia DR3 Photometry
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Daniel Huber
Figure caption: Binary contrast versus separation, color coded by the Gaia RUWE. Almost all of the binaries in the sample with separations ρ < 1″ have RUWE >1.2. However, not all systems have a published RUWE value, especially in the intermediate-separation regime, leading to the gap in the separation distribution. Missing systems with no reported RUWE are show in contrast-separation space with black “x” markers.
Paper: Quantifying the Contamination from nearby Stellar Companions in Gaia DR3 Photometry
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Daniel Huber
Figure caption: Gaia contrast versus binary separation, with the colorbar showing the Gaia ipd_frac_multi_peak parameter, which tracks the percentage of images showing multiple peaks for a given source. The multipeak percentage increases with decreasing separation, up to a cutoff at ∼0﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩15, which is the diffraction limit for the Gaia spacecraft. This indicates that for all but the closest binaries, the multipeak percentage is a reliable indicator of unresolved multiplicity.
Paper: Quantifying the Contamination from nearby Stellar Companions in Gaia DR3 Photometry
Authors: Kendall Sullivan, Adam L. Kraus, Travis A. Berger, Daniel Huber
Figure caption: Gaia contrast versus binary separation, with the colorbar showing the residual between the composite and primary star G magnitudes. The residual is correlated with both binary separation and Gaia contrast, verifying that the secondary flux contaminates the system flux and that the impact increases with decreasing separation and increasing contrast, as expected.