adsabs/AstroCLIMB huggingface dataset:
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We show the outer binary orbits for systems where we detect new companions in astrometric “wobble” and RV. We combine our new high-precision ARMADA epochs with historical speckle data published in WDS. We show the final fitted outer orbit, taking into account the “wobbles” from newly detected companions in these systems (which can be seen visually at this scale for HD 5143). The shaded gray lines depict 100 random orbits drawn from the posterior of the MCMC chains, while the green dashed line shows the best-fit solution. For the case of HD 37711 and HD 16753, additional orbit monitoring is needed to better constrain the long-period orbits.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We search for additional companions to the wide binary systems of Figure 1 on a grid over inner orbital period. We detect obvious inner periods for four of these six targets. Due to their short periods and small wobbles, we also include RV data for the period searches of HD 199766 and HD 37711 (the rest are purely astrometric searches). We have RV data on all of these targets to confirm the inner detection. Five of these six targets are new detections (in bold), while HD 199766 is the first astrometric detection of the inner 2-day orbit.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We plot the best-fit joint RV inner orbits for companions in Figure 3, obtained with new TSU-AST spectroscopic data. For each system, we designate the component we are seeing in the RV data (described in individual system notes). These RV data help confirm the newly detected inner orbital elements, tell us which component the companion is orbiting, and allow us to compute a distance. HD 16753 needs further orbit monitoring, due to its long orbital period.
Paper: SPORK That Spectrum: Increasing Detection Significances from High-resolution Exoplanet Spectroscopy with Novel Smoothing Algorithms
Authors: Kaitlin C. Rasmussen, Matteo Brogi, Fahin Rahman, Hayley Beltz, Miles Currie, Emily Rauscher, Alexander P. Ji
Figure caption: Results of S/N and t-tests on spectra with and without SPORK/iterative smoothing performed for HD 179949 b. Top panels: the implementation of SPORK/iterative smoothing in S/N tests result in a 1.1 planetary S/N increase. Bottom panel: in the t-test application, the implementation of SPORK/iterative smoothing results in a 1.2σ increase.
Paper: SPORK That Spectrum: Increasing Detection Significances from High-resolution Exoplanet Spectroscopy with Novel Smoothing Algorithms
Authors: Kaitlin C. Rasmussen, Matteo Brogi, Fahin Rahman, Hayley Beltz, Miles Currie, Emily Rauscher, Alexander P. Ji
Figure caption: Results of S/R and t-tests on spectral with and without SPORK/iterative smoothing performed for HD 209458 b. Top panels: the implementation of SPORK/iterative smoothing in S/R tests result in a 0.5 planetary S/N increase. Bottom panel: in the t-test application, the implementation of SPORK/iterative smoothing does not have an impact.
Paper: Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager
Authors: Evan A. Rich, John D. Monnier, Alicia Aarnio, Anna S. E. Laws, Benjamin R. Setterholm, David J. Wilner, Nuria Calvet, Tim Harries, Chris Miller, Claire L. Davies, Fred C. Adams, Sean M. Andrews, Jaehan Bae, Catherine Espaillat, Alexandra Z. Greenbaum, Sasha Hinkley, Stefan Kraus, Lee Hartmann, Andrea Isella, Melissa McClure, Rebecca Oppenheimer, Laura M. Pérez, Zhaohuan Zhu
Figure caption: Sample parameters of the 44 targets in the Gemini-LIGHTS survey. (A) is an infrared color–color diagram using WISE and 2MASS colors. The dashed line represents a flat spectrum SED, and the gray shaded region are objects with no near-infrared or mid-infrared excess. (B) HR diagram with pre-main-sequence mass tracks (colored lines) and the zero-age main sequence (ZAMS) assuming solar-metallicity mass tracks from Bressan et al. (2012). Targets are classified as: stars with mass >8 M⊙ (orange x’s), T Tauri stars (pink plus), and Herbig Ae/Be stars (green diamonds). (C) Histogram of estimated age. (D) Histogram of estimated stellar mass. (E) Age vs. stellar mass. (F) Histogram of target distances. Specific target parameter values can be found in Appendix A in Tables 2 and 3. Note that FU Ori is not plotted on the HR diagram as the T  eff  temperature is unknown.
Paper: Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager
Authors: Evan A. Rich, John D. Monnier, Alicia Aarnio, Anna S. E. Laws, Benjamin R. Setterholm, David J. Wilner, Nuria Calvet, Tim Harries, Chris Miller, Claire L. Davies, Fred C. Adams, Sean M. Andrews, Jaehan Bae, Catherine Espaillat, Alexandra Z. Greenbaum, Sasha Hinkley, Stefan Kraus, Lee Hartmann, Andrea Isella, Melissa McClure, Rebecca Oppenheimer, Laura M. Pérez, Zhaohuan Zhu
Figure caption: Spiraled Disks: Q ϕ  images of disks classified as hosting spiral arms including targets HD 100453, HD 139614, HD 34700 A, and HD 142527. See online figure sets (e.g., Figure 2 for target specific color bars). The image flux scale is log and chosen to highlight the target structure. The point sources in the FOV are labeled with a dashed black circle. The name of the target and the epoch in YYYYMMDD format can be found in the upper left of each image. The type of polarized image (Q ϕ  ), the scale of the image (in au), and the photometry band (J or H) can be found along the bottom of each subimage.
Paper: Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager
Authors: Evan A. Rich, John D. Monnier, Alicia Aarnio, Anna S. E. Laws, Benjamin R. Setterholm, David J. Wilner, Nuria Calvet, Tim Harries, Chris Miller, Claire L. Davies, Fred C. Adams, Sean M. Andrews, Jaehan Bae, Catherine Espaillat, Alexandra Z. Greenbaum, Sasha Hinkley, Stefan Kraus, Lee Hartmann, Andrea Isella, Melissa McClure, Rebecca Oppenheimer, Laura M. Pérez, Zhaohuan Zhu
Figure caption: The % of Q ϕ /I flux vs. U ϕ /I in a 0.″4 annulus (30 pixels) for J-band (left) and H-band (right) observations. The dashed circle represents the 3σ significance.
Paper: Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager
Authors: Evan A. Rich, John D. Monnier, Alicia Aarnio, Anna S. E. Laws, Benjamin R. Setterholm, David J. Wilner, Nuria Calvet, Tim Harries, Chris Miller, Claire L. Davies, Fred C. Adams, Sean M. Andrews, Jaehan Bae, Catherine Espaillat, Alexandra Z. Greenbaum, Sasha Hinkley, Stefan Kraus, Lee Hartmann, Andrea Isella, Melissa McClure, Rebecca Oppenheimer, Laura M. Pérez, Zhaohuan Zhu
Figure caption: This figure shows the flux calibration scale for each of the targets and epochs in the sample. Blue dots are J-band observations, and orange dots are H-band observations. Observations that have their scale factors corrected (see Section 3.1) are noted with plus signs with their corrected values. Average J- and H-band scale factors are shown as dashed lines.
Paper: Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager
Authors: Evan A. Rich, John D. Monnier, Alicia Aarnio, Anna S. E. Laws, Benjamin R. Setterholm, David J. Wilner, Nuria Calvet, Tim Harries, Chris Miller, Claire L. Davies, Fred C. Adams, Sean M. Andrews, Jaehan Bae, Catherine Espaillat, Alexandra Z. Greenbaum, Sasha Hinkley, Stefan Kraus, Lee Hartmann, Andrea Isella, Melissa McClure, Rebecca Oppenheimer, Laura M. Pérez, Zhaohuan Zhu
Figure caption: Showing the Q (top) and U (bottom) example sky flats taken on 2018 January 3. Flux plotted as the percent deviation from the flux average of the frame.
Paper: 3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion
Authors: Salvador Curiel, Gisela N. Ortiz-León, Amy J. Mioduszewski, Joel Sanchez-Bermudez
Figure caption: Best-fitted solution using the full combined astrometric fit of the binary system GJ 896AB. (a) Orbital motion of the stellar companion GJ 896B around the main star GJ 896A (big ellipse) and the orbital motion of the main star GJ 896A around the center of mass (inner ellipse). The black pointed stars show the observed optical/infrared position, and the two red pointed stars show the observed VLBA positions. The green lines connect the observed positions of the binary system with the expected position along the orbit at each observed epoch. The red and magenta dots indicate the position of the periastron of the orbits of the main star around the center of mass of the binary system and the orbit of the secondary star around the main star, respectively. The red and magenta arrows show the position of the ascending and descending nodes, respectively. The black arrows indicate the direction of the orbital motions. Note that the reference central point is different for both. In the case of the binary system, the central point indicates the position of the main star GJ 896A, while in the case of the orbital motion of the main star, the central position corresponds to the center of mass of the binary system. The inner panel shows an expanded section of the orbital motion of GJ 896A around the center of mass for the observed epochs. In this case, all the plotted epochs correspond to VLBA observations. (b) Best-fitted solution including the astrometric signal due to the planetary companion GJ 896Ab, obtained from the full combined astrometric fit. The upper panels show the astrometric signal of the main star GJ 896A due to the planetary companion as a function of time, with the parallax and proper motion subtracted, and taking into account the orbital motion of the stellar companion GJ 896B around the main star GJ 896A. The lower panels also show the astrometric signal of the main star GJ 896A due to the planetary companion, but in this case the signal is folded in phase. The black dots correspond to the absolute astrometric observations of the main star GJ 896A. The red crosses indicate the fitted position on the orbit for each observed epoch. The bars correspond to the observational astrometric errors.
Paper: 3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion
Authors: Salvador Curiel, Gisela N. Ortiz-León, Amy J. Mioduszewski, Joel Sanchez-Bermudez
Figure caption: 3D orbital architecture of the binary system and planetary companion. (a) 2D plot of the fitted orbits of the binary system GJ 896AB (blue) and the planetary companion (green) projected on the plane of the sky. The orbit of the planet has been scaled by a factor of 20 to make the comparison easier. The blue squares show the observed relative position of GJ 896B around the main star GJ 896A. The thick lines indicate the side of the orbit that is closer to us, and the dotted lines indicate the side of the orbit that is on the other side of the plane of the sky. The straight dotted lines show the line of nodes of both orbits. (b) 3D plot of the fitted orbits of the binary system GJ 896AB (blue) and the planetary companion GJ 896Ab (green). The orbit of the planet has been scaled by a factor of 20 to make easier the comparison. The arrows indicate the direction of the rotation axis of both orbits. An animation presenting the 3D orbits is available at https://drive.google.com/file/d/11ogBAzY_SdIHIeLPeHJi2PbEqf_3M__I/view?usp=sharing. (c) 2D orientation (assuming Ω  =  0) of the orbital planes (solid lines) and the direction of the rotation axis (discontinue arrows) of the orbital motion of the binary system (blue) and the planetary companion (green), projected on a plane formed by the line of sight (right), the direction to the observed (left), and the east (down) and west (up) directions on the plane of the sky. The magenta arrow indicates the spin axis of the main star GJ 896A.
Paper: 3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion
Authors: Salvador Curiel, Gisela N. Ortiz-León, Amy J. Mioduszewski, Joel Sanchez-Bermudez
Figure caption: (a) Residuals obtained by subtracting the parallax, proper motions, and orbital motion of the stellar companion from the GJ896A positions using the combined astrometric fit. (b) Offsets between the position of the flare and the source position without the flare (the quiescent emission). (c) Offsets between the position of the flare and the average source position. (d) Offsets between the source position without the flare (the quiescent emission) and the average source position. The rms in each case is indicated at the top of the subpanels.
Paper: 3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion
Authors: Salvador Curiel, Gisela N. Ortiz-León, Amy J. Mioduszewski, Joel Sanchez-Bermudez
Figure caption: Radio flux density of GJ 896A as a function of time. These VLBA observations were obtained at a frequency of 8.4 GHz. The green symbols correspond to the flux intensity of the source, and the blue symbols correspond to the integrated flux density of the source. The flux density observed on the source presents a large variability in short periods of time. There seem to be periods in time when the source is weak, having a very low flux density (∼0.2 mJy), and other periods of time when the source is active, having flux densities between 1 mJy and 9 mJy. We did not find a temporal pattern in the flux variability.
Paper: 3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion
Authors: Salvador Curiel, Gisela N. Ortiz-León, Amy J. Mioduszewski, Joel Sanchez-Bermudez
Figure caption: Correlations between the fitted parameters from the MCMC analysis using the corner code. On top of each column, we show the 2D posterior probability histogram of each fitted parameter. The green lines indicate the mean value of each fitted parameter. The doted lines indicate the ±1σ estimated errors.
Paper: 3D Orbital Architecture of a Dwarf Binary System and Its Planetary Companion
Authors: Salvador Curiel, Gisela N. Ortiz-León, Amy J. Mioduszewski, Joel Sanchez-Bermudez
Figure caption: Residuals from the combined astrometric fit using lmfit.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: Diagnostic information from the HST data reduction. From top to bottom, the rows show the band-integrated raw flux, the background counts, and the wavelength shift of the spectrum relative to the first exposure of the first visit. From left to right, the columns show the four HST visits in chronological order. The open circles in the raw flux correspond to data points that we did not include in our light-curve fits due to larger amplitude instrumental ramps. The vertical offset in the top row is due to spatial scanning, which alternates between forward and reverse directions on the detector. The total counts are higher when the detector is read out in the same direction as the spatial scan.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: HST/WFC3 transit light curves. The left panel shows the phase-folded light curve from all four HST visits (points) compared to the best-fit models (lines) for the broadband light curve (top) and the spectroscopic light curve (bottom). The right panel shows the residuals from the best-fit models (right). The figure is annotated with the central wavelength for each spectroscopic light curve and the rms of the residuals (in ppm). The data are corrected for instrument systematics, normalized to an out-of-transit baseline flux of unity, and offset on the y-axis by a constant value for visual clarity.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: Core fraction vs. envelope metallicity from interior structure modeling for a rocky core (red line with 1σ uncertainty shaded) and a water core (blue line with 1σ uncertainty). The retrieval results for the envelope metallicity are overplotted as a histogram, with the 1σ credible interval indicated by the blue shaded region.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Sea ice extent and fractional habitability on an Earth-like planet for four exemplar dynamically stable planetary systems. (a) Current Earth with Jupiter eccentricity e  J  = 0.05 and Jupiter semimajor axis a  J  = 5.20 au. (b) Highly eccentric Jupiter-mass planet with e  J  = 0.40 and a  J  = 4.56 au. (c) Close-in Jupiter-mass planet with a circular orbit, with e  J  = 0.00 and a  J  = 3.20 au. (d) Close-in Jupiter-mass planet with a circular orbit, with e  J  = 0.00 and a  J  = 3.21 au. Eccentricity (solid) and obliquity (dashed) over time are shown in the upper panels. The areal extent of perennial (year-round) and seasonal sea ice (in 106 km2 and % ocean area covered in ice) are displayed in the lower panels. (e) The annual mean fractional habitability over land vs. ocean for each 2500 yr time interval of the four Earth-like planets. The gray area indicates the seasonal range in fractional habitability over land and ocean.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Schematic depiction of the impact of nodal precession Ω on the obliquity ϵ of a planet. (a) The orbit is tilted i° relative to the reference plane with orbital normal n. The northern hemisphere of the planet is tilted away during a given time of year with an angle ϵ between the rotational axis and the orbit normal ﹩n^{\prime} ﹩. (b) The nodal precession has rotated the orbital plane by 180° and the orbit is tilted −i°  relative to the reference plane. If the rotational axis would remain fixed relative to the fixed background stars, the new obliquity is ϵ − 2i. (c) However, solar and lunar torques pull the equatorial bulge toward the solar and lunar planes, driving precession of the rotational axis while affecting the obliquity.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: The maximum variation in the obliquity (in degrees) of an Earth-like planet, under different planetary architectures, i.e., the presence of a Jupiter-like planet with different initial semimajor axes and eccentricities. Both panels display the same data on (a) linear and (b) logarithmic scales to distinguish between high- and low-amplitude variations. The red circle tagged “a” indicates the current position of Jupiter in our solar system. Pink circles tagged “b”, “c”, and “d” indicate simulations used for the reconstruction of surface climate conditions in Section 3.3.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Schematic depiction of the impact of apsidal and axial precession on the planet’s climatic precession. The upper panels show top-views, and the bottom panels show side-views. (a) A planet in a plane of reference with the southern hemisphere tilted to the star during perihelion and the position of the vernal equinox indicated with ϒ. (b) The orbit has rotated relative to the fixed background stars, a movement known as apsidal precession ω. If the rotational axis would remain fixed relative to the background stars, the vernal equinox now occurs during perihelion. (c) However, the planetary axis rotates over time so that the location of the vernal equinox moves relative to the reference direction. The apsidal precession direction is opposite from the axial precession, thus climatic precession cycles experienced by the planet are more rapid than the axial precession cycles.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: The period of the main climatic precession cycle of an Earth-like planet under different planetary architectures, i.e., with a Jupiter-like planet having different initial semimajor axes and eccentricities. Climatic precession is defined here as ﹩e\sin \varpi ﹩. The red circle indicates the current position of Jupiter in our solar system.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Eccentricity e, inclination i, and obliquity ϵ cycles over nine million years for two example Earth-like planets. (a) High-obliquity Earth-like planet that varies with an amplitude greater than the amplitude of orbital inclination. (b) Chaotic behavior in the obliquity cycles of an Earth-like planet. Note the different y-axis scales for the bottom panels.