adsabs/AstroCLIMB huggingface dataset:
Paper: Free Core Nutation and Its Relation to the Spin-over Mode
Authors: Jérémy Rekier
Figure caption: Normalized kinetic energy of the mantle (in red) and core (in blue) as a function of the forcing frequency (A m/A = 1/10, e f = 1/10, e = 2/15, and ﹩\tilde{\phi }=1﹩).
Paper: Free Core Nutation and Its Relation to the Spin-over Mode
Authors: Jérémy Rekier
Figure caption: Normalized kinetic energy of the mantle (in red) and core (in blue) as a function of the forcing frequency (A m/A = 9/10, e f = 1/400, e = 1/300, and ﹩\tilde{\phi }=1﹩). Top: centered around ﹩{\omega }_{\mathrm{fcn}}﹩. Bottom: centered around ω cw.
Paper: Free Core Nutation and Its Relation to the Spin-over Mode
Authors: Jérémy Rekier
Figure caption: Normalized kinetic energy of the mantle (in red) and core (in blue) for the two-layer elastic planet as a function of the forcing frequency (﹩\tilde{\phi }=1﹩, other parameters are given in Table 1). Top: centered around ﹩{\bar{\omega }}_{\mathrm{fcn}}﹩. Bottom: centered around ﹩{\bar{\omega }}_{\mathrm{cw}}﹩.
Paper: Free Core Nutation and Its Relation to the Spin-over Mode
Authors: Jérémy Rekier
Figure caption: Period offset in the inertial frame, ΔT, as given by Equation (81) as a function of N fcn (other parameters are from Table 1). The inner shaded area (in blue) corresponds to the interval of ±10 days about T fcn, and the outer one (in yellow) to the interval of ±10% about ﹩\mathrm{Im}({K}_{\mathrm{cmb}})﹩. The vertical dashed line corresponds to Earth’s value.
Paper: Free Core Nutation and Its Relation to the Spin-over Mode
Authors: Jérémy Rekier
Figure caption: Normalized transfer function of a (rigid) two-layer planet with a large (heavy) liquid core and a comparatively small (light) mantle (A m/A = 1/10, e f = 1/10, and e = 2/15).
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: The map of the location of NASA's Curiosity's first 19 rock sampling sites. The samples have been analyzed by laboratory instruments inside the vehicle. On the left, 15 images of the drilled holes show the variation in color and grain size of cuttings and powders. Inset: MAHLI images of all full-depth drill holes taken at a standoff of 10 cm with the exception of Sebina, which was taken at a standoff of 25 cm. Image Credits: NASA/JPL-Caltech/MSSS/UA (PIA21254). The image does not represent all the drilled rocks. In 2021 September, a total of 33 similarly heterogeneous-appearing drill samples have been collected (MSL update to MEPAG VM #13, 2021).
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: Schematic representation of the Ma_MISS acquisition modes on the borehole wall. The ring images are acquired using the drill rotation, while the column images are taken using the vertical translation of the drill. The image of the borehole is adapted from https://photojournal.jpl.nasa.gov/catalog/PIA17594.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: Selection of spectra of minerals (top: phyllosilicates; bottom: silicates) acquired with the Ma_MISS breadboard at the IAPS INAF laboratory. Acquisitions have been carried out on mineral powders with the Ma_MISS breadboard laboratory model, and data were subsequently processed to simulate the Ma_MISS FM spectral sampling and resolution. The laboratory spectra are affected by gaps due to the low S/N occurring in the 1.0–1.1 μm and 1.7–1.8 μm ranges of the spectrometer (FieldSpec) used in the laboratory. The Ma_MISS instrument is not affected by these gaps.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: The laboratory model (breadboard) of the instrument includes all the subsystems: the illumination system (IL), consisting of the 5 W lamp and the illumination bundle; the optical head (OH); the sapphire window (SW); the signal fiber (SF) (signal link), which is a series of three optical fibers that carry the collected light from the optical head to the laboratory spectrometer (FieldSpec). Power Supply (PS) and Sample Holder (SH) and the test sample (T) are also illustrated in the diagram.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: Representation of the drill/scoop/trench depths planned and realized by previous Mars missions in comparison with ExoMars. ExoMars drill excavation depth is not to scale.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: Oxia Planum (335.6◦E, 18◦N) and ExoMars (2022) landing site ellipses.
Paper: Exploring the Shallow Subsurface of Mars with the Ma_MISS Spectrometer on the ExoMars Rover Rosalind Franklin
Authors: M. C. De Sanctis, F. Altieri, E. Ammannito, S. De Angelis, B. Ehlmann, M. Ferrari, A. Frigeri, S. Fonte, M. Formisano, M. Giardino, A. Apuzzo, J. Brossier, N. Costa, L. Rossi, G. Vizzini, G. V. Ciarletti, F. Westall
Figure caption: Schematic view of Ma_MISS instruments with the different parts in the rod/tip and on the drill box.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Results for planets with pure N2 atmosphere (left) and N2+CO2 atmosphere (right) under a rotation period of 5 Earth days. (a) and (b): zonal-mean zonal winds and the scaled E-P flux, the same as those in Figure 6. (c) and (d): the sum of heating rates from longwave radiation and turbulent thermal diffusion averaged over tidally locked longitude. AP is the antistellar point, and SP is the substellar point.
Paper: Atmospheric Overturning Circulation on Dry, Tidally Locked Rocky Planets Is Mainly Driven by Radiative Cooling
Authors: Shuang Wang, Jun Yang
Figure caption: Atmospheric overturning circulation diagram; the same as Figure 1 but for dry, slowly rotating, tidally locked rocky planets with atmospheres of pure N2 (a) and N2+CO2 (b).
Paper: Topographically Influenced Evolution of Large-scale Changes in Comet 67P/Churyumov–Gerasimenko's Imhotep Region
Authors: Abhinav S. Jindal, Samuel P. D. Birch, Alexander G. Hayes, Orkan M. Umurhan, Raphael Marschall, Jason M. Soderblom, Jean-Baptiste Vincent, Dennis Bodewits
Figure caption: Georeferenced images of the Imhotep region. (a) Preexisting scarps “h,” “m,” and “n” can be observed on 2015 May 24 before activity begins in the Imhotep region. (b) By 2015 June 5, new scarps “a,” “b,” and “c” emerge in the northern portions of the basin. (c) New scarps “d,” “e,” “f,” and “g” are observed on 2015 June 27. (d) New scarp “i” is observed on 2015 July 2. (e) New scarps “j” and “k” emerge on 2015 July 11. At the same time, the boundaries of the scarps in the northern portions of the basin appear more muted, indicating sediment deposition. (f) By August 1, scarp activity reaches the southern end of the basin, while deposition continues toward the north. New scarps “l” and “o” emerge during this time, while preexisting scarps “m” and “n” also begin their migration. (g) New scarp “p” is first observed on 2015 August 23. Deposition of material spreads across the basin during this time, with several scarps completely disappearing under newly deposited sediment. (h) After 2015 October 27, scarps “g” and “j” no longer migrate, whereas scarps “p” and “k” continue migrating until 2015 November 29 and December 6, respectively. (i) Scarps “g,” “j,” “k,” and “p” are still visible on 2016 January 23 and remain visible for the entirety of the Rosetta mission. These scarps likely act as seed points for the next cycle of erosion as the comet approaches perihelion again.
Paper: Topographically Influenced Evolution of Large-scale Changes in Comet 67P/Churyumov–Gerasimenko's Imhotep Region
Authors: Abhinav S. Jindal, Samuel P. D. Birch, Alexander G. Hayes, Orkan M. Umurhan, Raphael Marschall, Jason M. Soderblom, Jean-Baptiste Vincent, Dennis Bodewits
Figure caption: Overview of the Imhotep region. (a) The Imhotep region (highlighted in yellow) lies on the large lobe of 67P and has the equator (dashed green line) passing through its northern portion. (b) Imhotep consists of a central deposit of smooth terrains bounded by high-standing topography on all sides. (c) Shown is the topography surrounding Imhotep as viewed from the north of Imhotep. Source: ESA—European Space Agency (https://creativecommons.org/licenses/by-sa/3.0/igo), (d) Shown is a high-resolution view of two large boulders within the smooth terrain deposits. The granular nature of the deposit is evident by the speckle pattern in the smooth terrains at such resolutions (0.2 m pixel–1).
Paper: OSSOS XXV: Large Populations and Scattering–Sticking in the Distant Trans-Neptunian Resonances
Authors: B. L. Crompvoets, S. M. Lawler, K. Volk, Y.-T. Chen, 英同 陳, B. Gladman, L. Peltier, M. Alexandersen, M. T. Bannister, S. Gwyn, J. J. Kavelaars, J.-M. Petit
Figure caption: Measured and predicted populations, as a ratio to the 8:3 population (as in Tables 5 and 6). Black squares with error bars are our 95% confidence limits on our measured population ratios from OSSOS++, green circles are population predictions from Neptune migration models dynamically classified in Lawler et al. (2019), green squares are population predictions from a Nice Model simulation dynamically classified in Pike et al. (2017), and magenta triangles are scattering–sticking population predictions from Yu et al. (2018).
Paper: OSSOS XXV: Large Populations and Scattering–Sticking in the Distant Trans-Neptunian Resonances
Authors: B. L. Crompvoets, S. M. Lawler, K. Volk, Y.-T. Chen, 英同 陳, B. Gladman, L. Peltier, M. Alexandersen, M. T. Bannister, S. Gwyn, J. J. Kavelaars, J.-M. Petit
Figure caption: Top three panels: toy models of 7:2 (a = 69 au), 11:4 (a = 59 au), and 12:7 (a = 43 au) resonances demonstrate the equilibrium configurations of the resonances with respect to Neptune (blue point). Bottom three panels: the 7:2, 11:4, and 12:7 resonances with realistic orbital distributions, where libration amplitude can be large and thus the pericenter location oscillates about the equilibrium configuration. Depending on which resonance one looks at, its pericenter location (and thus the most likely location to detect TNOs) differs. For these toy models, pericenter occurs at Neptune’s semimajor axis.
Paper: OSSOS XXV: Large Populations and Scattering–Sticking in the Distant Trans-Neptunian Resonances
Authors: B. L. Crompvoets, S. M. Lawler, K. Volk, Y.-T. Chen, 英同 陳, B. Gladman, L. Peltier, M. Alexandersen, M. T. Bannister, S. Gwyn, J. J. Kavelaars, J.-M. Petit
Figure caption: The best n:2 parameterized orbital model (see Table 2), shown as cumulative plots in pericenter distance (left) and inclination (right). Red markers indicate real OSSOS++ TNOs in n:2 resonances (excluding the 5:2 as discussed in the text), the gray dotted line is the intrinsic underlying model distribution, and the black line is the distribution of simulated detections. The blue box highlights the range of possible model values: the real TNOs must fall within this range for the model to be valid. These distributions are not rejectable with AD values of 0.78 and 0.87.
Paper: OSSOS XXV: Large Populations and Scattering–Sticking in the Distant Trans-Neptunian Resonances
Authors: B. L. Crompvoets, S. M. Lawler, K. Volk, Y.-T. Chen, 英同 陳, B. Gladman, L. Peltier, M. Alexandersen, M. T. Bannister, S. Gwyn, J. J. Kavelaars, J.-M. Petit
Figure caption: All three models are compared through a histogram detailing the variance of their inclination in the 11:4 resonance. Although in each case the distribution is determined by sin(i) times a Gaussian (Equation (4)), the width of that Gaussian differs in each case as per the given model. The current model (blue) has a population of N = 3900, Unified Distribution (peach) has a population of N = 2800, and Minimized Population Distribution (green) has a population of N = 1400.
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: Context for the DAVINCI mission within a framework of past orbital missions and with connections to future missions. Key science themes are highlighted with connections to questions left over from past missions, and with new connections to contemporary and future missions and the era of exoplanet science. DAVINCI is viewed as a gateway for Venus as a future astrobiology target in the context of how habitability is both established and lost in our solar system and beyond (e.g., Limaye et al. 2021).
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: A possible history of water on Venus (e.g., Way et al. 2016; Way & Del Genio 2020), compared to Earth's history. Venus's epoch of surface liquid water may have persisted for over 2 billion years, and DAVINCI measurements can help constrain this hypothesis. Evidence also suggests volcanic activity on Venus persists to this day (e.g., Smrekar et al. 2010), and DAVINCI noble gas measurements will help constrain the history of Venus's volcanism.
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: DAVINCI measurements of krypton and its first ever measurements of xenon will resolve questions of differences in the noble gas inventories at Earth (blue curve with triangles), Mars (red curve with circles), and Venus (teal curve with squares, with the Pioneer Venus and Venera range indicated as the filled teal region). For comparison, solar values (orange line with half-circles) and carbonaceous chondrite values (brown curve with squares) are also shown. These differences may imply variation in the materials that formed each planet as well as subsequent events during planetary evolution. Figure after Baines et al. (2013).
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: DAVINCI measurements of gas mixing ratios could constrain the surface mineralogy and chemical state of the near-surface atmosphere. This diagram shows stability fields of iron-bearing minerals at Venus's surface conditions. The red quadrangle corresponds to putative gas chemical equilibrium at mixing ratios of CO2 and SO2 of 0.965 and 130–185 ppm, respectively. Measuring CO, OCS, SO2, and CO2 will determine whether atmospheric gases equilibrate with each other and what minerals are stable. The figure is modified from Zolotov (2015).
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: DAVINCI detailed measurements will reveal the composition of the Venusian atmosphere below ∼70 km, providing necessary context to understand key chemical cycles, such as the putative sulfur (S) cycle shown here. SO2 is the third most abundant gas in the Venusian atmosphere after CO2 and N2, so measurements of it and other S-bearing gases are important anchors for chemical and physical models of Venus’s atmosphere. Boxes outlined in blue designate key species targeted by the DAVINCI descent sphere analytical instruments (Section 2.3).
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: Representative altitude-sampled measurements of selected key species for VMS (high-cadence colored points in left panel) and VTLS (lower-cadence gray triangular points in right panel) in the lower atmosphere. Averaging of VMS values (left panel) can achieve smaller uncertainties without significant loss of vertical structure information, as illustrated with the black points with reduced error bars. Possible gradients near the surface are indicated with dashed lines at altitudes <10 km in the VMS (left) panel. Additional VTLS measurements beyond the DAVINCI reference mission scenario may be possible, as suggested by the notional white VTLS points in the deepest part of the atmosphere (right panel).
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: Summary of descent sphere vertical descent timeline in the Venusian atmosphere with select science topics pursued at each altitude band.
Paper: Revealing the Mysteries of Venus: The DAVINCI Mission
Authors: James B. Garvin, Stephanie A. Getty, Giada N. Arney, Natasha M. Johnson, Erika Kohler, Kenneth O. Schwer, Michael Sekerak, Arlin Bartels, Richard S. Saylor, Vincent E. Elliott, Colby S. Goodloe, Matthew B. Garrison, Valeria Cottini, Noam Izenberg, Ralph Lorenz, Charles A. Malespin, Michael Ravine, Christopher R. Webster, David H. Atkinson, Shahid Aslam, Sushil Atreya, Brent J. Bos, William B. Brinckerhoff, Bruce Campbell, David Crisp, Justin R. Filiberto, Francois Forget, Martha Gilmore, Nicolas Gorius, David Grinspoon, Amy E. Hofmann, Stephen R. Kane, Walter Kiefer, Sebastien Lebonnois, Paul R. Mahaffy, Alexander Pavlov, Melissa Trainer, Kevin J. Zahnle, Mikhail Zolotov
Figure caption: DAVINCI delivers high-priority science using five descent sphere (DS)-based instruments, and two remote-sensing instruments on the carrier relay imaging spacecraft (CRIS), all with robust flight heritage. See Table 2 for instrument details for the in situ DS in comparison with previous in situ missions (Pioneer Venus Large Probe).