adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: Comparison between the solid body static gravity field and the atmosphere-induced one. The solid and dashed black lines represent the field and associated uncertainties measured by Magellan, the dash–dotted blue line represents the uncertainty attainable by VERITAS, and the red line represents the amplitude spectrum of the gravity anomalies due to atmospheric mass redistribution. To highlight the low-degree features of the atmospheric gravity field, we limit the figure to degree 50.
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: The tidal and loading Love numbers are shown in a three-dimensional phase space with the mantle viscosity shown as the color bar. Error bars are fixed at the average values found for the calculations made using the simulations from both X21 (circles) and D17 (crosses). The lengths of the error bars are taken from the expected VERITAS observational uncertainties calculated in Section 3.2 (black: Doppler only, and red: Doppler + tie points). The upper right panel is zoomed in on the average Re[k 2] and -Im[k 2] to emphasize the small observational error we expect for these measurements and how the observed values can be used to accurately discern from the large number of possible interior states.
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: Atmospheric pressure anomalies sampled over a Venus solar day. The subsolar point is at 0°, 90°, 180°, and 270° in longitude for quadrants a, b, c, and d, respectively.
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: The tidal and loading Love numbers are calculated for harmonic degrees l = 2 to l = 10 for the purely liquid core models of X21 (left panels) and those that include a solid inner core (right panels). We separate out the real portion of the tidal response (panels a and b), the imaginary portion (panels c and d), and the real portion of the loading (panels e and f). The mantle viscosity is shown as the scatter point color.
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: Graphical representation of Equation (15). ﹩{k}_{2}^{{\prime} }﹩ is shown vs. k 2 − h 2. Calculations were performed on the interior models from X21 (circles) and D17 (crosses). The diagonal dotted line represents the theoretical value ﹩{k}_{2}^{{\prime} }﹩ obtained from k 2 and h 2 under the assumption of Equation (11).
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: Degree-2 loading Love number amplitudes are shown as a function of the forcing period for three different rheological laws (Maxwell, black line; Andrade, blue line; and Sundberg–Cooper, green line). We report the expected accuracy of the two measurements of the loading Love numbers as the black error bars centered on the Andrade line (the red error bar represents the results expected from the Doppler and tie points combined analysis, while the black error bar represents the Doppler-only case). The vertical dashed magenta and black lines represent the loading and tidal forcing frequencies, respectively.
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: Tidal k 2 vs. loading ﹩{k}_{2}^{{\prime} }﹩ calculated using both the X21 (circles) and D17 (crosses) simulated interiors of Venus (for the definition of X21 and D17, see section 3.2). The mantle viscosity is shown as the scatter plot colors. Calculations were performed using the incompressible limit, K → ∞ (right data points) as well as allowing for compressibility and a finite bulk modulus (left data points).
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: Gravity anomalies due to pressure field perturbations. The color scale represents differences between the perturbed and unperturbed fields rescaled between −1 and 1. Panel (a) shows the gravity anomaly differences when perturbing the pressure anomaly grid, and panel (b) shows the gravity anomaly differences when perturbing the Fourier series expansion coefficients.
Paper: Constraining the Venus Interior Structure with Future VERITAS Measurements of the Gravitational Atmospheric Loading
Authors: Gael Cascioli, Joe P. Renaud, Erwan Mazarico, Daniele Durante, Luciano Iess, Sander Goossens, Suzanne Smrekar
Figure caption: The same phase space as shown in Figure 6, repeated here. The core-mantle-boundary radius is now shown as the color bar.
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: Maps of forecasted uncertainty σ  M  on the mass of Planet X at 400 au as a function of its location in the sky. Plots are in ecliptic coordinates with the vernal equinox at center. The Mollweide projection is used. The upper panel shows the nominal case using all observational constraints to date, including Juno/Cassini ranging and Mars ranging. “Old” data are the existing measurements without Juno, Cassini, or Mars ranging. In the middle panel, only the old data and the Juno/Cassini data are used (Mars ranging is omitted), as described in Section 5.3. In the lower panel, forecasted LSST observations of Jovian Trojans are included, which makes up some of the precision lost by omission of Mars (see Section 7.1).
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: Fraction of the sky for which the σ  M  of a Planet X at 400 au is below the value on the x-axis. This is shown for the nominal scenario (solid), one restricted to already published ranging, and another extrapolating ranging data through 2034.
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: Each curve plots the fraction of the sky (y-axis) for which the uncertainty σ  M  on Planet X at 400 au is at or below the value on the x-axis. The solid curves are for cases without LSST Trojan data, and are labeled by the subsets of the observational data they use. All curves make use of the “old” observations. The dashed curves add the use of LSST Trojan observations to the scenario of the solid curve of matching color. The leftmost “KBO floor” curve plots the constraints that would be attained if the only limitation were confusion with the uncertain tidal field produced by the members of the Kuiper Belt. This floor is up to an order of magnitude below constraints with the best data expected in the next decade. The two vertical lines mark the σ  M  values that are needed for a definitive 5σ detection of Planet X if it has a mass of 5 M ⊕ and is at a distance of 800 au (left) or 400 au (right). Ideally, we would be able to detect the former at 100% of locations on the sky.
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: The fraction of the sky with uncertainty σ  M  on Planet X’s mass below a given level is shown for observation scenarios including LSST observations of Trojans. At the right end, we see the relatively small degradation in the combination of Trojans with old data that results from marginalizing over parameters of systematic-error models (as we move from the yellow to the dark curve on its right). At left, are shown scenarios in which we combine all of the proposed observational data, and arbitrarily reduce all uncertainties on the Trojans by factors of 5 (green) and 20 (magenta) from the actual forecast (black). It takes a 20-fold reduction for the Trojans to make a substantial improvement in the Planet X constraints, and gain the ability to detect a 5 M ⊕ Planet X at 5σ significance over a significant portion of the sky if it is at a distance of 800 au. At far left, below the 800 au signal, is the floor set by stochastic KBO quadrupoles.
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: As we increase the measurement errors on the Juno/Cassini ranging (red) or Mars ranging (blue), the forecasted uncertainties σ  M  on Planet X’s mass at 400 au are degraded. The solid lines show the median value of σ  M  and the hatched regions bound the 5%–95% percentiles of σ  M  across the sky. The full power of the Juno/Cassini data are more critical to the Planet X constraints than that of the Mars ranging.
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: Cumulative information from predicted LSST observations of the Trojans as a function of the magnitude of the faintest Trojan considered. Top axis shows the object radius of objects with an albedo of 0.04. Trojans fainter than H = 14.5 (vertical dashed line) do not add significant information; this is roughly the point at which their astrometry becomes limited by background noise.
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: If the body at right with radius R is illuminated along the horizontal axis, and the photocenter displacement when viewed (in red) at an illumination angle of ϕ is k ϕ R, the naive use of the photocenter instead of the barycenter is equivalent to a shift of the body toward the Sun by kR, at the location of the black dot.
Paper: Can the Gravitational Effect of Planet X be Detected in Current-era Tracking of the Known Major and Minor Planets?
Authors: Daniel C. H. Gomes, Zachary Murray, Rafael C. H. Gomes, Matthew J. Holman, Gary M. Bernstein
Figure caption: A map of σ  M , the lower limit on achievable M  X  uncertainty for Planet X at 400 au, set by ignorance of the Kuiper Belt’s tidal field. Note the change in color scale from Figure 1.
Paper: ASSIST: An Ephemeris-quality Test-particle Integrator
Authors: Matthew J. Holman, Arya Akmal, Davide Farnocchia, Hanno Rein, Matthew J. Payne, Robert Weryk, Daniel Tamayo, David M. Hernandez
Figure caption: Top: numerically and analytically calculated variational equations for the x-component of asteroid (3666) Holman. The two curves have been intentionally offset by 10−7 au to make them distinguishable on this scale. Bottom: difference between the numerically and analytically calculated results, for all Cartesian components. The magnitude of the difference grows quadratically in time, as expected.
Paper: ASSIST: An Ephemeris-quality Test-particle Integrator
Authors: Matthew J. Holman, Arya Akmal, Davide Farnocchia, Hanno Rein, Matthew J. Payne, Robert Weryk, Daniel Tamayo, David M. Hernandez
Figure caption: Left: the heliocentric equatorial trajectories of Earth (red) and Apophis (blue) from 2029 January 1 to 2030 January 1, encompassing the close approach on 2029 April 13. The x- and y-axes are ICRF coordinates. Right: the geocentric, equatorial position of Apophis near the time of the 2029 April 13 encounter (Earth’s physical size is shown as a circle). The deflection of the trajectory is clear.
Paper: ASSIST: An Ephemeris-quality Test-particle Integrator
Authors: Matthew J. Holman, Arya Akmal, Davide Farnocchia, Hanno Rein, Matthew J. Payne, Robert Weryk, Daniel Tamayo, David M. Hernandez
Figure caption: Left: the IAS15 step size as a function of time from the start of the integration (2029 January 1). The step size drops, reaching the prescribed minimum, at the time of the encounter. Right: divergence of two calculated trajectories as a function of time, differing by a small displacement in initial conditions. Note that the time axis in the left panel extends further.
Paper: ASSIST: An Ephemeris-quality Test-particle Integrator
Authors: Matthew J. Holman, Arya Akmal, Davide Farnocchia, Hanno Rein, Matthew J. Payne, Robert Weryk, Daniel Tamayo, David M. Hernandez
Figure caption: The magnitude of the accumulated error in integrating asteroid (3666) Holman for the indicated outgoing time and back to the initial time. The error grows approximately as t 3/2, as is shown by the dashed red line.
Paper: ASSIST: An Ephemeris-quality Test-particle Integrator
Authors: Matthew J. Holman, Arya Akmal, Davide Farnocchia, Hanno Rein, Matthew J. Payne, Robert Weryk, Daniel Tamayo, David M. Hernandez
Figure caption: The magnitude of the difference in the positions of Apophis integrated with ASSIST and with the JPL small-body code, as a function of time starting from 2029 January 1. The differences are less than ∼1 cm before the encounter, near day 102 in the figure, growing to ∼500 m by the end. Small differences in the calculated velocities near the close approach lead to a smoothly growing separation between the results as the integrations are continued. The discontinuities in the difference are due to adaptive step size changes.
Paper: ASSIST: An Ephemeris-quality Test-particle Integrator
Authors: Matthew J. Holman, Arya Akmal, Davide Farnocchia, Hanno Rein, Matthew J. Payne, Robert Weryk, Daniel Tamayo, David M. Hernandez
Figure caption: (5303) Parsijkij–Ceres close approach. Left: relative position. Right: magnitude of the separation vs. time.
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: Orientation of the STIS 52″ × 0.″5 slit relative to the Sun/comet vector for each of the six STIS observations, with the nucleus center defined as the origin. The sunward direction is to the left in the figure, indicated by the red arrow. Note that the offset pointings do not equally sample the radial distribution of emissions owing to the slit angle relative to the Sun/comet axis. The dotted–dashed and dashed lines indicate distances that are 2.″5 and 8″ from the nucleus center, respectively. Note that subtended slit lengths are different owing to changes in geocentric distance (Table 1).
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: OH column density measurements for 0″ and 8″ (top panel) and 2.″5 (bottom panel) offset STIS observations of 46P with a 7-pixel binning in the spatial direction. The derived ﹩{Q}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ from a vectorial model fit to the centered data in the top panel of Figure 4 is plotted with a solid line, and a 1σ error is overplotted as a transparent area. Note that for the 2.″5 pointings (odx607 and odx608) several of the points nearest to the nucleus (∼160–200 km) are approximately twice those of the centered observations at the same distance and are discussed in the text. The 2.″5 offset OH column density beyond 200 km is consistent with the centered data set as evidenced by the vectorial model fit displayed, which is effectively identical to the Q H2O fit to the centered OH data set in the top panel.
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: Enlarged COS G160M spectrum of 67P on 2021 October 18, with 11-pixel binning to display the S I intercombination multiplet centered at 1479 Å. We display a synthetic sulfur spectrum offset by −0.5 rayleigh Å–1 for both the allowed 3 D  o –3 P  o  and semiforbidden 5 D  o –3 P  o  intercombination transitions in cyan and magenta, respectively. The total synthetic spectrum from the sum of both multiplets is shown in black. We note that the allowed S I λ1483 blended feature is somewhat underpredicted with our derived g-factor at this atomic column density.
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: One-dimensional geometric albedo spectra extracted from an aperture of ± 20 pixels (40 pixels total) around the optocenter of the nucleus for coadded observations of 46P (magenta circles) and 67P (cyan circles), from recalibrated x2d files. For 46P the 4-pixel extraction subtends 400 km, while for 67P it is approximately 1000 km. Each spectrum has 7-pixel spectral binning and has been divided by the scaled solar spectrum and normalized to the average value between 2900 and 2930 Å. Note that the peaks seen at 2800 and 3080 Å are from OH (0,0) and (1,0) emissions, while the CS (0,0) band at 2580 Å marks the beginning of the noisier portion of the reflectance spectrum.
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: HST COS G160M spectrum of 67P from two coadded spectra on 2021 October 21, as extracted by the CALCOS pipeline-produced x1dsum file and with 31-pixel binning. Only the S I λ1479 multiplet feature is clearly detected.
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: OH column density profiles derived from HST STIS observations of 46P (top) and 67P (middle—2021 October 18; bottom—2021 December 11). A vectorial model for OH is shown with derived water production rates, ﹩{Q}_{{{\rm{H}}}_{2}{\rm{O}}}﹩, and 1σ error represented by the filled region. Both ﹩{Q}_{{{\rm{H}}}_{2}{\rm{O}}}﹩ and 1σ error bars are indicated in the plot legends. All error bars on OH column densities are 1σ and represent the combined instrumental and binning error.
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: One-dimensional STIS spectra extracted from an aperture of 30 pixels around the optocenter of the nucleus for coadded observations of 46P (top) and 67P (bottom), from recalibrated x2d files. A solar spectral fit to the data is shown to indicate the contribution from reflected sunlight from dust.
Paper: The Evolution of Activity and Chemical Composition in Rosetta’s Comet Targets across Multiple Apparitions: Complications for CS2 as the CS Parent in Comet Nuclei
Authors: John W. Noonan, Joel Wm. Parker, Walter M. Harris, Steven Bromley, Mohammad Saki, Youssef Moulane, Davide Farnocchia, Marco Micheli, Jian-Yang Li, 荐扬 李, Kathleen E. Mandt, Kumar Venkataramani, Dennis Bodewits
Figure caption: A scatter plot depicting the abundance ratios for CS2 and Af ρ relative to H2O detailed in Table 7. Leftward-pointing triangles are from the 1997 46P data set of Stern et al. (1998) and the revised CS2/H2O value from Feldman et al. (2004), the rightward-pointing triangle is from this work for 46P in 2019, the diamond reflects the 1982 67P data set of Feldman et al. (2004), and the circles are the 2021 67P abundances. Open symbols indicate pre-perihelion data points, and filled symbols represent post-perihelion measurements. Error bars are 1σ for the CS2/H2O relative abundances and are smaller than the markers for Af ρ/H2O.
Paper: A High Spatial and Spectral Resolution Study of Jupiter’s Mid-infrared Auroral Emissions and Their Response to a Solar Wind Compression
Authors: James A. Sinclair, Thomas K. Greathouse, Rohini S. Giles, John Lacy, Julianne Moses, Vincent Hue, Denis Grodent, Bertrand Bonfond, Chihiro Tao, Thibault Cavalié, Emma K. Dahl, Glenn S. Orton, Leigh N. Fletcher, Patrick G. J. Irwin
Figure caption: Predicted solar wind dynamical pressures at Jupiter in 2017 March using OMNI-measured conditions at Earth (Thatcher & Müller 2011) and two solar wind propagation models—mSWiM (Zieger & Hansen 2008) in black and the Tao et al. (2005) model in gray—to calculate the solar wind flow at Jupiter’s orbit. Dates/times are UTC. Red, blue, and green lines denote the time periods on March 17, 18, and 19, respectively, where the Gemini-TEXES spectra presented in this study were recorded. The Earth–Jupiter–Sun angles are shown near the top of the panel.