adsabs/AstroCLIMB huggingface dataset:
Paper: Using SOFIA’s EXES to Search for C6H2 and C4N2 in Titan’s Atmosphere
Authors: Zachary C. McQueen, Conor A. Nixon, Curtis de Witt, Véronique Vuitton, Panayotis Lavvas, Juan Alday, Nicholas A. Teanby, Joseph Penn, Antoine Jolly, Patrick G. J. Irwin
Figure caption: Reference profiles of the atmospheric gas composition (left panel), vertical temperature profile (right panel, solid black trace), and haze profiles (gray dashed trace). Temperature and gas profiles are from the photochemical model detailed in V. Vuitton et al. (2019).
Paper: Influence of Magnetosonic Waves on the Venusian Ionosphere: The Role of Electron Landau Heating
Authors: Nigang Liu, Zhenpeng Su, Siyang Yi, Jiang Yu, Kun Li, Jun Cui
Figure caption: Overview of the magnetosonic wave event observed by PVO during Orbit 162 on 1979 May 15: (a) electron density Ne; (b) magnetic field strength (black line) and magnetic field components in the VSO coordinate system; (c) magnetic field components in MFA coordinate system; (d) wave power PB obtained from FFT of magnetic field during selected time intervals, with the vertical dashed line marking the oxygen ion gyrofrequency ﹩{f}_{{{\rm{O}}}^{+}}﹩ corresponding to B = 45 nT; (e) waveform of magnetosonic waves (black line) and magnetic field oscillations in the MFA coordinate system; and (f)–(g) maximally varying BL, intermediately varying BM, and normal BN magnetic field components in the minimum variance coordinate system during selected time intervals, with the determined wave normal angle Ψ marked. Note that the minimum variance analysis does not work for linearly polarized waves because the derived minimum and intermediate eigenvalues are too close to uniquely determine the polarization plane. The shaded regions in Figures 1(a)–(c) roughly mark the transition region.
Paper: Influence of Magnetosonic Waves on the Venusian Ionosphere: The Role of Electron Landau Heating
Authors: Nigang Liu, Zhenpeng Su, Siyang Yi, Jiang Yu, Kun Li, Jun Cui
Figure caption: Particle observations during the inbound and outbound segments at PVO Orbits 161 and 162: (a)–(b) electron density Ne; (c)–(d) total ion density Ni; and (e)–(f) electron temperature Te. All the data points are mapped by altitudes. The modeled calculations of electron density and temperature assume SZA = 65° for inbound and SZA = 35° for outbound. The solid and hollow circles in Figures 2(e)–(f) represent electron temperature data from OETP and ORPA, respectively.
Paper: Influence of Magnetosonic Waves on the Venusian Ionosphere: The Role of Electron Landau Heating
Authors: Nigang Liu, Zhenpeng Su, Siyang Yi, Jiang Yu, Kun Li, Jun Cui
Figure caption: Dispersion curves and corresponding minimum resonant energy ﹩{E}_{{\rm{\min }}}﹩ of compressional (solid lines) and noncompressional (dashed lines) waves in cold plasma: (a)–(b) wavenumber ﹩kc/{{\rm{\Omega }}}_{{{\rm{O}}}^{+}}﹩ and compressibility ﹩{P}_{{B}_{\parallel }}/{P}_{B}﹩ as functions of wave frequency ﹩\omega /{{\rm{\Omega }}}_{{{\rm{O}}}^{+}}﹩; (c)–(d) minimum Landau resonant energy ﹩{E}_{{\rm{\min }}}﹩ of e−; (e)–(f) minimum cyclotron resonant energy ﹩{E}_{{\rm{\min }}}﹩ of O+; and (g)–(h) minimum cyclotron resonant energy ﹩{E}_{{\rm{\min }}}﹩ of H+. The orange solid dots mark the observed magnetosonic wave with wave frequency ﹩f=1.3{f}_{{{\rm{O}}}^{+}}﹩ and normal angle Ψ = 85°.
Paper: Influence of Magnetosonic Waves on the Venusian Ionosphere: The Role of Electron Landau Heating
Authors: Nigang Liu, Zhenpeng Su, Siyang Yi, Jiang Yu, Kun Li, Jun Cui
Figure caption: BO calculation results of compressional waves in hot plasma: (a)–(b) comparison of the dependence of wavenumber ﹩kc/{{\rm{\Omega }}}_{{{\rm{O}}}^{+}}﹩ on wave frequency ﹩\omega /{{\rm{\Omega }}}_{{{\rm{O}}}^{+}}﹩ in cold plasma (solid lines) and hot plasma (hollow dots); (c)–(d) normalized electron Landau damping rate ﹩\gamma /{{\rm{\Omega }}}_{{{\rm{O}}}^{+}}﹩ as a function of wave frequency ﹩\omega /{{\rm{\Omega }}}_{{{\rm{O}}}^{+}}﹩ and wave normal angle Ψ; and (e)–(f) wave energy density ﹩4{\mu }_{0}W/{B}_{{\rm{W}}}^{2}﹩ as a function of wave frequency ﹩\omega /{{\rm{\Omega }}}_{{{\rm{O}}}^{+}}﹩ and wave normal angle Ψ.
Paper: Influence of Magnetosonic Waves on the Venusian Ionosphere: The Role of Electron Landau Heating
Authors: Nigang Liu, Zhenpeng Su, Siyang Yi, Jiang Yu, Kun Li, Jun Cui
Figure caption: Minimum resonant energies ﹩{E}_{{\rm{\min }}}﹩ of electron Landau resonance for magnetosonic waves at three different frequencies.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Model comparison for simulated observations of Venus (planet b) and EM (planet c): ﹩{{ \mathcal H }}_{PP}﹩ in dashed blue, ﹩{{ \mathcal H }}_{PPP}﹩ in solid orange, ﹩{{ \mathcal H }}_{PPP}﹩ in dotted–dashed green. Right: histograms showing the distribution of scatter for each planet. The dashed black line corresponds to a Gaussian with the same mean and variance as the injected noise. The red curve is a normal distribution with zero mean and a standard deviation of 0.5 minutes.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Simulated TTVs of two transiting terrestrial planets given in Table 1—Venus/b (top) and EM/c (bottom)—with a best-fit linear ephemeris removed, colored by source. Left panels: the gray curve is the sum of all the perturbations, calculated from the median values of the posterior sampling of the best-fit three-planet model. Right panels: same as the left panels, but here the solid gray line was created from the median posteriors in our best-fit four-planet model.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Likelihood as a function of mass ratio and period of a third perturbing planet. Each curve corresponds to a value in 10 grid points of the mass ratio, where γ = log10(mp/M⊙). The log-likelihood was computed over 200 logarithmic steps in P = [1.5, 22] yr, while optimizing over the orbital phase.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Top-down view of SS orbits computed from JPL ephemerides over 15 yr; the x–y axes represent the projected coordinates of the international celestial reference frame (P. Charlot et al. 2020) used by the JPL ephemeris. We indicate a projection of the direction near which the mid-transits of Venus (triangles) and EM (circles) can be seen.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Schematic of the simulated MTS (i), along with the configurations considered in this work (ii–iv). We treat EM as planet c, with a location provided by the JPL ephemerides of the EMB.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Measured planet mass as a function of orbital period for multiplanetary systems with Np planets, listed by discovery method: transit (green circles), RVs (blue squares), TTVs (purple triangles), and others (yellow circles; NASA Exoplanet Science Institute 2020). The retrieved mass measurements in this work—for Venus, EM, Mars, and Jupiter—are taken from the right panel of Figure 10: the four-planet model with a 10 s noise injected (i.e., a total timing uncertainty of 19.3 s). Data accessed on 2024 December 29.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: 1D posterior histograms for planet parameters fit in at least two of our configurations for our fiducial case—i.e., those common between our two-, three-, and four-planet models discussed in Section 3.2—compared to the truth (dashed vertical line) for Venus, EM, and Jupiter. The rows correspond to planets b/c/d; the parameter being plotted is indicated in the title of each panel.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: ΔBICs for our best-fit models from the fine grid search (Section 2.2.4), where positive values represent a preference for an additional planet. Values below the black contour line correspond to at least a 5σ detection of a third, massive planet (left) and a nearby terrestrial planet (right). Note the different scales of the color bars.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Period likelihood profiles for planets added in the ﹩{{ \mathcal H }}_{PPP}﹩ (dark-red curve) and ﹩{{ \mathcal H }}_{PPPP}﹩ (orange curve) models, along with the histograms of the posteriors, for our fiducial case. The vertical lines indicate the actual periods of Jupiter (left) and Mars (right).
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Recovered median and 1σ posterior mass vs. injected timing error for planets (b–e, respectively) around a Sun-like star: ﹩{{ \mathcal H }}_{PPP}﹩ (left) and ﹩{{ \mathcal H }}_{PPPP}﹩ (right) models. The true masses for Venus, EM, Jupiter, and Mars are plotted as dashed horizontal lines. Note the different scales for the axes.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Relative likelihood profiles for baselines simulated in this work, as indicated in the y-axis. Left: the three-planet search when σobs = 30 s. Right: the four-planet search when σobs = 10 s.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Same as in Figure 11, but here we plot the percent precision of the best three-planet model: planet b on the left, planet c in the middle, and planet d on the right. After fitting our fiducial simulation—transits with 30 s injected noise observed over 30 yr—with a third planet, there is a reduction from 20% to 8% error for c and from 11% to 4% error for b. Here empty bins show when the percent precision was greater than 100%.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Percent precision on mean mass ratio for planets b (left panel) and c (right panel) in the two-planet model, binned by white noise and observing baseline. Empty bins indicate where the chains did not find a solution, and we use the same color bar scaling for both panels.
Paper: Modeling the Solar System. I. Characterization Limits from Analytic Timing Variations
Authors: Bethlee M. Lindor, Eric Agol
Figure caption: Power-law relations for ﹩{\sigma }_{{m}_{p}}﹩−σtot derived from the posteriors of the three-planet model: planets b (left), c (middle), and d (right). For the x-axis, the injected timing noise has been added in quadrature to the mean of the posterior systematic error to obtain the total timing precision.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: (a) The trajectories of the Galileo (triangles) and JUICE (circles) orbits in Phi-Omega (GphiO or PO) transformed from cartesian to spherical coordinates. (b) The position of Ganymede at the times of the six flybys closest approach wrt Jupiter in Jupiter’s magnetic dipole spherical coordinates (dip). The black line represents Ganymede’s trajectory for one Jupiter rotation.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: The background inducing field of Jupiter over one complete rotation at the position of Ganymede (black line) in PO Cartesian coordinates. The triangles and circles represent the closest approach for Galileo and JUICE orbits, respectively.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: Comparison between the predicted induced (left) and quadrupole (right) field signals for the Galileo flybys. The quadrupole field is estimated using the model of M. G. Kivelson et al. (2002), while the induced field is estimated assuming a perfect conductor and using Jupiter’s internal and external field models of S. Sharan et al. (2022a) and J. E. P. Connerney et al. (2020), respectively.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: Standard deviation of the difference between the amplitudes of the induced field signals estimated at different ocean depths and the modeled quadrupole signals for the Galileo flybys. Using Equation (4), the bottom x-axis represents the amplitude ratio of the inducing and induced fields with no phase difference, while the top x-axis represents the corresponding ocean depth.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: The (a) internal dynamo (spherical coordinates) and (b) external magnetodisk (cylindrical coordinates) fields of Jupiter observed at the positions of Ganymede using the models of S. Sharan et al. (2022a) and J. E. P. Connerney et al. (2020), respectively. The periodicity of the fields is easily noticeable.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: The dipole field prediction for the JUICE flybys at Ganymede and their amplitude comparison using the dipole plus induction model of M. G. Kivelson et al. (2002) in PO Cartesian coordinates.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: The quadrupole field prediction for the JUICE flybys at Ganymede and their amplitude comparison using the quadrupole model of M. G. Kivelson et al. (2002) in PO Cartesian coordinates.
Paper: Viability of the Early JUICE Flyby Trajectories to Confirm Ocean Existence at Ganymede
Authors: Shivangi Sharan, Michele K. Dougherty, Adam Masters, Ciaran Jones, Matthew Acevski
Figure caption: The induction field prediction for the JUICE flybys at Ganymede and their amplitude comparison using the background periodic field of Jupiter in PO Cartesian coordinates.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The 53Mn–53Cr isochron for EC-1 with mineral separates explicitly from the groundmass (1-CPX-1, 1-CPX-2, 1-SP, and 1-PY). This isochron gives almost identical results to the isochron with all mineral separates and the whole rock for EC-1 (Figure 1).
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The BSE image of ilmenite and chromite in the EC-2 fragment. Chr: chromite; Ilm: ilmenite; Pl: plagioclase; Py: pyroxene.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The BSE image of the EC-1 fragment. Pl: plagioclase; Px: pyroxene.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The BSE image of groundmass pyroxene, ilmenite, and chromite in EC-1 fragment. Notice the lamellae of high Ca-pyroxene (medium gray) and low Ca-pyroxene (light gray) in the groundmass. Pl: plagioclase; Px: pyroxene; Ilm: ilmenite; Chr: chromite.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The BSE image of pyroxene xenocryst (Px-1) in the EC-1 fragment. The position of the chemical profile across the groundmass pyroxene and xenocryst is implied by the white line.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The BSE image of the K-feldspar lamellae and silica phase in EC-1 fragment. Pl: plagioclase; Px: pyroxene; Ilm: ilmenite; K-Feld: K-feldspar.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The BSE image of the exsolution structure of pyroxene in the EC-2 fragment. Px: pyroxene; Pl: plagioclase.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: The BSE image of the EC-2 fragment with xenocryst (pyroxene) and groundmass (plagioclase and pyroxene).
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer
Authors: Barbara A. Cohen, Simeon J. Barber, Aleksandra J. Gawronska, Feargus A. J. Abernethy, Natalie M. Curran, Phillip A. Driggers, William M. Farrell, David J. Heather, Christopher Howe, Peter F. Landsberg, Veneranda López-Días, Andrew D. Morse, Thomas Morse, Michael J. Poston, Parvathy Prem, Roland Trautner, Orenthal J. Tucker, Tristram J. Warren, Stefano Boccelli
Figure caption: Peregrine Deck D and PITMS operational temperatures throughout the mission. The PITMS ITMS temperature channel (archived in the PDS) is used here as the operating temperature, though the temperature throughout the instrument is not constant (for example, there may be hot spots near the filament). Though PITMS operated in four sessions, only housekeeping data from the first session were used to assess instrument health, and no mass spectra were downlinked.
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer
Authors: Barbara A. Cohen, Simeon J. Barber, Aleksandra J. Gawronska, Feargus A. J. Abernethy, Natalie M. Curran, Phillip A. Driggers, William M. Farrell, David J. Heather, Christopher Howe, Peter F. Landsberg, Veneranda López-Días, Andrew D. Morse, Thomas Morse, Michael J. Poston, Parvathy Prem, Roland Trautner, Orenthal J. Tucker, Tristram J. Warren, Stefano Boccelli
Figure caption: Representative PITMS spectra before and after dust cover opening showing the full range of data and the decrease in both counts and noise when the dust cover was opened.
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer
Authors: Barbara A. Cohen, Simeon J. Barber, Aleksandra J. Gawronska, Feargus A. J. Abernethy, Natalie M. Curran, Phillip A. Driggers, William M. Farrell, David J. Heather, Christopher Howe, Peter F. Landsberg, Veneranda López-Días, Andrew D. Morse, Thomas Morse, Michael J. Poston, Parvathy Prem, Roland Trautner, Orenthal J. Tucker, Tristram J. Warren, Stefano Boccelli
Figure caption: PITMS mounted to the Peregrine lander Deck D (left) in the Astrobotic clean room and (right) during remove-before-flight activities (with B.A.C. for scale). The Iris rover (N. Potter 2023) is mounted to the underside of Deck D. The PITMS aperture opens to the +X direction of the spacecraft.
Paper: The Peregrine Ion Trap Mass Spectrometer (PITMS): Results from a CLPS-delivered Mass Spectrometer
Authors: Barbara A. Cohen, Simeon J. Barber, Aleksandra J. Gawronska, Feargus A. J. Abernethy, Natalie M. Curran, Phillip A. Driggers, William M. Farrell, David J. Heather, Christopher Howe, Peter F. Landsberg, Veneranda López-Días, Andrew D. Morse, Thomas Morse, Michael J. Poston, Parvathy Prem, Roland Trautner, Orenthal J. Tucker, Tristram J. Warren, Stefano Boccelli
Figure caption: Views of the PITMS instrument mounted to the Peregrine deck. The EMS is shrouded in MLI inside the white-painted wrapper.
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: Breakdown of the VERITAS Doppler Allan deviation (ADEV), at SPE = 15°. The deviation from the white noise slope (black dashed line, reported only for comparison and not associated with any intervening noise source) is mostly due to plasma noise, under extreme conditions (no dual frequency calibrations and solar maximum). The result from BepiColombo at 60 s (end-to-end, blue dot) is also shown for comparison (P. Cappuccio et al. 2020).
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: Expected VERITAS maps of the gravity field degree strength on Venus. Panel (A) reports the results for the nominal mission (four Venusian cycles), while panel (B) reports the results for the extended mission (six Venusian cycles). A Kaula’s constant ﹩K=1.2\times {10}^{-5}﹩ has been used to compute the maps. Hammer projection centered at 0﹩{\rm{^\circ }}﹩ longitude.
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: VERITAS Doppler error budget @ τ = 10 s. See Table 1 for definitions of legend.
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: Amplitude spectra of Venus simulated gravity field, and of Magellan and VERITAS gravity field uncertainties. For the VERITAS mission, results for the nominal mission (four Venusian cycles) and the extended mission (six Venusian cycles) are presented. The VERITAS results are exclusively derived from Doppler observables, and no uncertainty on the thermal tides model is considered.
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: Gravity anomaly uncertainty maps (cumulative error) on Venus’s surface. Panel (A) reports the gravity anomaly uncertainty at degree 95; it clearly indicates that the 7 mGal requirement across 90% of the planet is met. Panel (B) shows the gravity anomaly uncertainty at degree 230. Hammer projection centered at 0﹩{\rm{^\circ }}﹩ longitude.