adsabs/AstroCLIMB huggingface dataset:
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The Venus/Earth separation, Δa, and the average eccentricities/inclinations, 〈e, i〉, for 111 successful simulations from 0.01 au (the narrow ring at 0.85 au with a 20% background) that produced good terrestrial planets (as defined in Section 3.1). The triangles show the results of individual simulations with good final planets. The red dot represents the real planets.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The planet growth and migration in the ring05 model: A. The initial distribution of planetesimals in the inner ring with r1 = 0.5 au and σ1 = 0.05 au. B. The growth of protoplanets from the inner ring. C. The end of the gas disk stage. Several relatively large protoplanets formed and migrated to ∼1 au. D. The final result of the simulation with four good terrestrial planets. The rectangles delimit our target regions for good terrestrial planets (Section 3.1). The colored dots show the semimajor axes and masses of the real planets. The figure illustrates a rare case where good Mars formed in the ring05 simulation—only 1.3% of simulations produced good planets, including Mars, in this model.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The Venus/Earth separation, Δa, and the average eccentricities/inclinations, 〈e, i〉, for 61 simulations from model203 (r1 = 0.6 au and r2 = 1.7 au, no background, strong convergent migration) that produced good terrestrial planets (as defined in Section 3.1). The triangles show the results of individual simulations with good final planets. The red dot is the real planets. We found that 57% of simulations produced good AMD of the terrestrial planet system with Sd < 0.005 (Equation (11); to be compared to real Sd ≃ 0.003.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The result of 61 simulations from model203 (r1 = 0.6 au and r2 = 1.7 au, no background, strong convergent migration) that simultaneously produced a good match to Mercury, Venus, Earth, and Mars (as defined in Section 3.1). The black dots show the final results in each simulation. The bigger red dots are the real planets.
Paper: Terrestrial Planet Formation from Two Source Reservoirs
Authors: David Nesvorný, Alessandro Morbidelli, William F. Bottke, Rogerio Deienno, Max Goldberg
Figure caption: The growth of planets in the successful simulations from model203 (two planetesimal reservoirs with r1 = 0.6 au r2 = 1.7 au, σ2 = 0.1 au and w2 = 1/3; the gas disk with r0 = 0.9 au and Σ0 = 3000 g cm−2). We collected all successful simulations that produced good analogs to the terrestrial planet system (four planets with good orbits and masses; Section 3.1). In panel (A), the accretion sequence in each simulation was recalibrated such that the model Earth ended up exactly with 1 MEarth. In panel (B), the accretion sequence was recalibrated such that the model Mars ended up exactly with 1 MMars. The vertical dashed line marks the end of the disk stage.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: Event identification from TESS images with TESSELLATE. Left: example image section that has been background subtracted and differenced. Sources identified with TESSELLATE are indicated with red boxes. Center and right: example TESS light curves with events detected by TESSELLATE highlighted. For the recovered exoplanet (lower right) we show the phase-folded light curve with raw data (gray) and 10 minute binned light curve (black). Similarly for the dwarf nova (top right) we show the raw data (gray) and 6 hr binned light curve (black). The asteroid detection (lower left) shows an individual detection at a position on the detector and time.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: Targeted search for an optical counterpart to GRB 180807A. Left: event light curve for the detected event with the red insert zooming in on the detected transient. The transient is highlighted by the orange shaded region and the input trigger time is shown with the blue dashed line. Center: plot of the spatial search area, where the central coordinates and uncertainty are shown with a black point and black line, respectively. Cuts of the TESS CCD that lie within the error region and are searched are highlighted in red, with the blue star representing the detected candidate. Right: cutout of the difference image at the brightest point of the detected transient.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: An example of a plot provided to the citizen scientists on Zooniverse. The upper left shows a zoomed-in section of the difference image from the TESS light curve (lower left). The upper right displays an image from the brightest frame around the detected source, while the lower-right panel shows the frame one hour after the brightest observation. With this information citizen scientists are asked to classify the target.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: Mean recovery rates for the cameras in Sector 29. The recovered sources are flagged by their detection methods (Starfind and SourceDetect). The black line indicates the magnitude at which the recovery rate drops below 50% for each camera.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: The light curves of eight variable stars characterized by the SourceDetect RFC. The top and middle rows contain previously discovered variable stars with classes matching the classifications made by the SourceDetect RFC. The bottom row has previously unclassified objects with variable classifications made by SourceDetect.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: Mean recovery rates across Sector 29 of ePSFs injected within a one pixel radius of a bright source. These are flagged using the TESSELLATE source mask.
Paper: TESSELLATE: Piecing Together the Variable Sky with TESS
Authors: Hugh Roxburgh, Ryan Ridden-Harper, Andrew Moore, Clarinda Montilla, Brayden Leicester, Zachary G. Lane, James Freeburn, Armin Rest, Michele T. Bannister, Andrew R. Ridden-Harper, Lancia Hubley, Qinan Wang, Rebekah Hounsell, Jeff Cooke, Dave A. Coulter, Michael M. Fausnaugh
Figure caption: Schematic of the TESSELLATE pipeline. The detection workflow is expanded upon in the purple box. The section relevant to each step is indicated by the number at the top of the boxes.
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: Examples of companion mass–separation predictions calculated using Hipparcos-Gaia astrometry from HGCA. For stars with significant accelerations, such as 10 Canum Venaticorum (left panel), 1 and 2σ confidence intervals are computed to identify the joint constraints on companion mass and separation consistent with the measured acceleration of the host star. For nonaccelerating stars, such as HD 193664 (right panel), we adopt a 3σ upper limit above which companions can be ruled out with 99.7% confidence (gray region). Dashed lines correspond to boundaries between stars and brown dwarfs (≈75 MJup) and brown dwarfs and giant planets (≈13 MJup). Conservative and optimistic HZ limits are displayed as dark and light yellow rectangles, respectively; we detail the HZ limit calculations in Section 2.2.
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: Fraction of parameter space (in companion mass and separation) that the HGCA method is sensitive to, to within at least 99.7% confidence. Each panel is calculated in different mass ranges—stellar (m2 > 75 MJup), brown dwarf (13 MJup < m2 < 75 MJup), and giant planet (5 MJup < m2 < 13 MJup)—and semimajor axis ranges—CHZ and 1–20 au—for all nonaccelerating targets. Hipparcos-Gaia accelerations are sensitive to most stellar companions orbiting within the CHZ, with typical sensitivities of 50%–90%. For brown dwarfs, the sensitivity range spans 0%–70%, and for planets it is typically less than 30%. On solar system scales (1–20 au), the HGCA method is almost 100% sensitive to stellar companions, while the sensitivity range for brown dwarfs typically spans 60%–100%. For planets, the sensitivity on solar system scales ranges from 0% to 100%.
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: Average sensitivity of HGCA astrometric acceleration method to companions across mass and separation space, calculated from nonsignificant accelerations. 90%, 50%, and 10% contours are shown. All known companions of HWO targets in the HGCA are plotted. Red circles and stars represent planets and stars, respectively, that account for their host star’s acceleration; white circles and stars represent planets and stars that do not account for the acceleration.
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: Left: significance of acceleration (s) for all HWO targets in the HGCA. Middle: of the 54 accelerating HWO targets, 37 have companions that are consistent with the acceleration and 17 have unknown accelerators. Right: of the 37 accelerations that are consistent with a known source, 22 accelerations are caused by a stellar companion, one is caused by a white dwarf, four are caused by a binary, eight are caused by a planet, and two have ambiguous accelerators.
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: HZ limits in physical (top) and angular (bottom) separation for all HWO targets following the prescription from R. K. Kopparapu et al. (2014). These display the separations that HWO will need to resolve. Optimistic bounds, defined by “recent Venus” and “early Mars” empirical constraints, are shown on the far left and right, respectively. Conservative bounds, defined by “runaway greenhouse” and “maximum greenhouse” calculations, are shown on the center left and right, respectively.
Paper: Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory
Authors: Katie E. Painter, Brendan P. Bowler, Kyle Franson, Juliette C. Becker, Jennifer A. Burt
Figure caption: Top: HGCA acceleration measurements for HWO preliminary targets. Bottom: significance of HGCA acceleration measurements for HWO targets, calculated from χ2 values for constant-proper-motion model fits (see Section 2 for details). We adopt a cutoff for significance at 2σ. The significant (>2σ) accelerations are shown in red in both the top and bottom panels.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: The scatter points mark the velocity offsets resulting from a Gaussian fit to the binned CCF time series in WASP-189 b’s literature rest frame (vsys and Kp listed in Table 1). Three bins are used pre-eclipse and post-eclipse. The scatter points’ colors correspond to different spectral templates: only-iron (at equilibrium chemical abundance), fiducial without titanium (our highest S/N template), and fiducial without iron and titanium. The purple line indicates our best alternative orbital fit compared to the literature, for the spectral template with the highest S/N, where the purple shaded region indicates orbital fits consistent within ΔS/N = S/Npeak − S/Nvelocity offset = 1. This is compared against predictions by a GCM (red dashed line) for the velocity offset of iron lines in another typical UHJ, but with the slope scaled to the rotational velocity of WASP-189 b. This GCM included the effect of rotation and winds, and assumed no drag. Our alternative orbital fit is consistent with the literature, and its additional slope is consistent with 3D effects.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Left panel: the left portion shows a comparison between the P-T profile from F. Yan et al. (2020), who used HARPS-N emission spectroscopy, and the the P-T profile constrained by A. G. Sreejith et al. (2023), who used CUTE NUV transit observations. The right portion shows the emission contribution function for the fiducial spectral template using the CUTE P-T profile. A strong neutral iron emission line core is indicated. Right panel: similar to the S/N maps of Figure 6, but shown for the fiducial spectral template that uses the P-T profile from CUTE and with chemical profiles computed using FASTCHEM. This spectral template is detected at S/N = 9.9.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Differences in signal-to-noise ratio (ΔS/N) are measured between the complete fiducial spectral template and templates omitting one opacity source at a time. Large positive ΔS/N > 1 values indicate a significant detection of the excluded opacity source (e.g., Fe), whereas near-zero values suggest that excluding or including the opacity source has little effect, indicating insignificant detection.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Cross-correlation function time series for the fiducial spectral template showing that the exoplanet’s Doppler signature is visible on both nights. Top rows: CCF value in the barycentric rest frame (left) or WASP-189 b’s literature rest frame (right; assuming the literature values of Kp and vsys listed in Table 1). The planet’s expected radial velocity trail (RV) is drawn as a white dotted line. Pre-eclipse, post-eclipse, and eclipsed phases are indicated. Bottom row: mean values of the CCF in each rest frame for a subset of orbital phases as shown in the legend.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Detection S/N as a function of number of removed principal components. The blue line shows the detection S/N for the observed data without model injection, while the orange lines show the injected data for four different velocity offsets. The dashed green line indicates a detection threshold of S/N > 5.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Similar to Figure 6, but instead shown for each night: for the fiducial case, neutral iron (assuming equilibrium chemical abundances), and the fiducial model without iron.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Left: zoom of the fiducial spectral template with and without H− around 1.1977 μm, showing a titanium and an iron emission line. The effect on both lines is negligible. Right: similar to Figure 6, but for the fiducial spectral template with H− opacity included, which is detected at a comparable S/N = 9.7.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Average normalized spectrum obtained for each spectral order and observing night. The nights have been offset in wavelength for visual purposes. The first night is shown in green and the second night is shown in wine red.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Similar to Figure 6, but shown for all the atmospheric species that have insignificant presence or absence.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: The distribution of discovered input populations as a function of observation arc (top) and discovery time (bottom). Populations that are more distant and therefore move less over the 10 yr survey have longer observation arcs, and their members tend to be discovered early. Conversely, small (and therefore nearby and fast-moving when detected) NEOs tend to be seen only for one apparition and behave more like a transient population, though there is a sizable sample of d ≤ 10 m NEOs with long arcs. All slow-moving populations have highly concentrated observation arcs, a result of LSST’s cadence. The Jupiter Trojan population, which is concentrated on the sky into an L4 and L5 cloud, has highly concentrated discovery times including a particularly large discovery spike in the first year of the survey when the larger L4 cloud is first observed. This makes the Trojans’ observation arc distribution dependent on LSST’s survey start date, unlike uniformly distributed populations.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: A heatmap of the sky coverage of the LSST baseline v3.4 cadence (P. Yoachim et al. 2024a), at the completion of the 10 yr LSST survey. The main survey area—the so-called “wide, fast, deep“ (WFD) region—results in a relatively uniform number of visits over approximately 19,600 deg2 of the sky shown in magenta. The DDFs fields, having >10,000 of revisits are shown in yellow. The mini-surveys (including the northern Ecliptic spur, the Galactic plane, and the southern polar cap) generally have fewer visits than the WFD area, and are shown in purple. Note that a ∼15° band around the ecliptic is covered in full to maximize LSST’s solar system discovery and science potential.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: The differential number density and cumulative number of NEOs (top and bottom panels, respectively). The size distribution of the input population is shown in blue, the discovered sample is shown in green, the subsample with well-measured grizy colors is in black, and the well-measured light-curve subsample is given in gray. NEOMOD3 sizes are given in increments of 0.1 m, which results in a spiky histogram of very small NEOs, even with very large sample sizes. Note that discovered objects are a subset of simulated objects, and well-measured color/light-curve objects are a subset of discovered objects.