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Michael H. Wong Abstract Science Programs Requirements for PDX A Dedicated Space Telescope for Time-Domain Solar System Science Máté Ádámkovics Gordon Bjoraker Leigh N. Fletcher Erich Karkoschka Julianne I. Moses Joachim Saur Nathan J. Strange Michael H. Wong UC Berkeley NASA GSFC JPL Univ. Arizona LPI Univ. Cologne JPL mikewong@ astro.berkeley.edu STScI (Instruments Division) Sushil K. Atreya John R. Casani Richard G. French Jian-Yang Li Keith Noll Kunio Sayanagi Anne Verbiscer UC Berkeley (Astronomy Department) Univ. Mich. JPL Wellesley Univ. Maryland STScI Caltech Univ. Virginia Don Banfield John T. Clarke William Grundy Franck Marchis Glenn S. Orton Nick Schneider Padmavati A. Yanamandra-Fisher Cornell Boston Univ. Lowell SETI/UC Berkeley JPL CU JPL Jim Bell Imke de Pater Amanda R. Hendrix Melissa A. McGrath Kathy A. Rages Eric H. Smith Cornell UC Berkeley JPL NASA MSFC SETI Lockheed Martin Susan Benecchi Scott G. Edgington Daniel Hestroffer William J. Merline Kurt Retherford Lawrence A. Sromovsky STScI JPL Obs. Paris Meudon SwRI SWRI UW-Madison Abstract Requirements for PDX Resolution / sensitivity / volume trades Time-variable phenomena with scales ranging from minutes to The chief requirements for time-domain solar system science are angular resolution, For most space telescope missions, photometric sensitivity is a major requirement. For time-domain solar system decades have led to a large fraction of recent advances in many sampling interval, and campaign duration. Although many ground- and space-based astronomy, a trade can be studied between sensitivity and payload volume, since relatively bright solar system aspects of solar system science. We present the scientific telescopes satisfy the angular resolution requirement, only a dedicated solar system targets are less demanding of sensitivity. A sparse-aperture configuration enables this trade to favor smaller motivation for a dedicated space observatory for solar system mission could achieve the time domain requirements. payload volume, maximizing the total aperture (and thus resolving power) for a given payload size. science. We call the observatory the Planetary Dynamics Explorer (PDX). This facility will ideally conduct repeated imaging and spectroscopic observations over a period of 10 years or more. It Angular resolution will execute a selection of long-term projects with interleaved Studies of planetary dynamics require the resolution of small distant objects such as scheduling, resulting in the acquisition of data sets with cloud features, volcanic plumes, and fragments of small solar system bodies. With a consistent calibration, long baselines, and optimized sampling nominal 3-m aperture, PDX will achieve an angular resolution of about 40 mas at optical intervals. wavelengths. This resolution is comparable to that provided by HST and the best current A sparse aperture telescope would be an ideal configuration for ground-based telescopes, which have demonstrated a wealth of time-domain science the mission, trading decreased sensitivity for reduced payload opportunities (see below). In the coming decades, extremely high resolution will be mass, while preserving spatial resolution. Ultraviolet capability is afforded by very large ground-based telescopes, but PDX will not attempt to compete essential, especially once the Hubble Space Telescope retires. with those efforts, instead specifying a 40 mas resolution based on the minimum requirement to image dynamically relevant features in the solar system. Specific investigations will include volcanism and cryovolcanism (on targets such as Io, Titan, Venus, Mars, and Enceladus); seasonal weather cycles; zonal flow, vortices, and storm evolution Sampling interval on the giant planets; mutual events and orbit determination of multiple small solar system bodies; auroral, solar wind, and Observing programs will be scheduled to ensure that each program acquires data at its magnetospheric interactions; variability in thin atmospheres; and desired sampling interval, which will typically range from hours to days. Occultation cometary evolution. The mission will produce a wealth of data light curves will push the short-interval limits with millisecond-range sampling products—such as long time-lapse movies of planetary intervals. atmospheres—with outreach potential as well as scientific value. Existing and planned ground- and space-based facilities are not Campaign duration suitable for these time-domain optimized planetary dynamics Campaign durations lasting from the entire mission lifetime to single visits will be Figure 1. Sparse aperture telescope examples. Top left: Illustration of the MIDAS multiple telescope array for studies for numerous reasons, including: oversubscription by accommodated, providing new opportunities as compared with semester- or cycle-based astrophysical users, field-of-regard limitations, sensitive detector spaceborne remote sensing (Smith et al. 2005).Middle and bottom left: The Star-9 prototype distributed aperture scheduling at other observatories. In particular, campaigns lasting the full mission telescope on its optical testbed at Lockheed Martin (Rieboldt et al. 2005, Kendrick et al. 2006). Right: Optical path saturation limits that preclude bright planetary targets, and lifetime will enable high-return high-risk science such as cryovolcanic activity searches. of the Star-9 system (Kendrick et al. 2005). © 2006 Lockheed Martin Corporation. Images from Kendrick et al. limited mission duration. (2006), courtesy of Lockheed Martin Corporation. Science programs PDX will provide an ideal platform for a range of time-domain research programs. Table 1. Examples of Investigation Category Data type (wavelength regime) Sampling scales Campaign duration A selection of general observer programs will be solicited from the broader solar time-domain solar Atmopheric dynamics: winds and transport Atmospheres Imaging (O) Hours, days Years system research community. Programs will be prioritized based on their scientific system science in- impact derived from the effective use of the resolution, sampling rate, and vestigations that Variable atmos. structure & composition Atmospheres Imaging, spectroscopy (UV, O, IR) Hours, days Days, years could be explored campaign duration opportunities uniquely provided by the PDX observatory. A set using PDX. Note that Occultations Atmospheres Photometry, spectroscopy (UV, O, IR) Milliseconds Hours of observing programs with complementary temporal requirements will be chosen since most investiga- to maximize the facility duty cycle. Monitoring programs will be able to trigger tions requiring spec- Aurorae, magnetospheres Atmospheres/space science Imaging, spectroscopy (UV) Minutes, hours Years, hours shorter-interval target of opportunity observations under the appropriate troscopic data also Volcanic trace gases Atmospheres/geology/astrobiology Spectroscopy, imaging (IR) Days Years conditions. require spatially re- solved spectra, an Volcanic plumes Geology Imaging, spectroscopy (O, IR) Days, hours Years PDX will make its greatest contributions in the areas of planetary atmospheres, integral field spec- active geology, and small solar system bodies. A sample of candidate trometer might be an Cryovolcanism Geology/astrobiology Imaging, spectroscopy (UV, O, IR) Days Years investigations is given in this section; many more investigations could be ideal spectroscopic Mutual events, lightcurves Small bodies Photometry (O) Milliseconds, minutes Hours, months pursued, but these give at least a sense of the demands on sampling interval and instrument choice. Cometary evolution Small bodies Imaging, spectroscopy (UV, O, IR) Hours Days campaign duration that are important for time-domain solar system science. A. B. 2000 Longitude (Sys III) C. 245 240 235 230 100 −25 Figure 2. Examples of time- Figure 3. Left: Spectral imaging observations of TItan using domain science at Jupiter. HST Surface Troposphere Stratosphere Strat. Subtracted VLT/SINFONI with ~45 mas effective resolution show that ob- ) 50 ACS/HRC images of Jupiter servations at 1-day intervals can reveal significant cloud –1 −30 from 2006 at ~50 mas effective variation. Much higher spatial resolution Cassini ISS data 0 resolution (A) were used to pro- showed even more rapid change at hour timescales, but it is −35 vide velocity profiles along the not clear that PDX could spatially resolve the rapid changes. White Oval BA (2000) White Oval BA (2000) Velocity (m s −50 Red Oval BA (2006) Red Oval BA (2006) east-west (B) and north-south 2007 Jan 28 Below: Schaller et al. (2006) used observations taken at day- Latitude (planetographic) (C) scale intervals to demonstrate changes in cloud activity, −40 axes of Oval BA (Asay- −100 Davis et al. 2009). Differences which they relate to a large convective event in 2004 and to 295 290 285 280 −100 −50 0 50 100 150 seasonal effects. The 2002 vertical line is southern solstice; –1 between 2000 and 2006 veloc- 2006 Longitude (Sys III) Velocity (m s ) ity profiles near 30° south lati- the 2005 vertical line is the date when Titan’s region of maxi- tude are attributed to transient 2007 Jan 29 mum insolation moved north from the south pole. interactions (of unknown times- D. E. F. G. cale) between the vortex and its 200 200 180 northward jet. Wind measure- 180 Plumes 180 160 160 160 140 ments require sampling inter- 140 140 vals on hour timescales. Zonal 120 25 March 2007 Jan 30 120 120 100 wind profiles before (D; black), ) 100 100 5 June –1 80 during (D; grey), and after (E) 80 80 (m s 60 u 60 60 the eruptions of massive power- 40 40 40 ful convective plumes (G) re- 20 20 20 vealed significant changes in 0 0 0 the zonal winds (F) as derived 2007 Jan 31 –20 –20 –20 u(25 March) – u(5 June) from HST WFPC2 imaging data 0.04 0.06 0.08 0.10 0.010 0.015 0.020 0.025 0.004 0.006 0.008 0.010 –40 –40 –40 15 20 25 30 15 20 25 30 15 20 25 30 I/F I/F I/F Planetographic latitude (degrees) (Sánchez-Lavega et al. 2008). References Figure 4. Images of Io at Figure 5. Although taken at dif- Asay-Davis, X., Marcus, P.S., Wong, M.H., de Pater, I., Sánchez-Lavega, A., G.S. Orton, R. Hueso, E. ~50 mas resolution demonstrate ferent wavelengths, these 1986 2009. Jupiter’s evolving Great Red Spot: Velocity García-Melendo, S. Pérez-Hoyos, A.
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