Icy Satellites – Status and Science C. J. Hansen, A. Hendrix 6 January 2005 Icy Satellite Science Objectives UVIS Icy Satellite Science Objectives are to Investigate: • Surface age and evolution – UV albedo maps • Surface composition and chemistry – Reflection spectra • Tenuous atmospheres / exospheres – Emission spectra, occultations Since our last meeting… Cassini has had moderate-distance flybys: – – – – Iapetus Tethys Dione Iapetus Oct. 20 Oct. 28 Dec. 15 Dec. 31 1.2 x 106 km 255,000 km ~75,000 km 124,000 km Phoebe • The Phoebe data set is complete (Cassini won’t be close to Phoebe ever again) • All three science objectives can be addressed with our data set – Considerable progress has been made in all three areas • Results have been presented at COSPAR, DPS, and AGU • High level results documented in UVIS team Science paper • Next on our list is a dedicated Phoebe paper (to submit to Icarus, Amanda Hendrix will be first author) • Most important finding: Evidence of water ice on Phoebe’s surface makes the outer solar system the most likely place of Phoebe’s origin Example: Phoebe UV Albedo Map Similar geometry Time: C/A-01:22 Range: 31,300 km Phase angle: 83° Lat/Long: 21°S, 349°W Blue/green=reflected solar Red=background Ly-a (IPH) Composition: Phoebe’s Disk-Integrated FUV reflectance spectrum H2O, CO2 frosts contribute to Phoebe’s FUV spectrum; other (dark) materials unknown at this time - similar to C ring non-ice material ISS_000PH_HIRESC Note brightness difference between high and low latitudes Phoebe’s spectral variations with latitude No Emissions Detected above Background A gas (oxygen) detection threshold of <2 x 1013 cm-2 is based on a minimum 2-sigma detectable level of 10 counts above background, instrument sensitivity at 130.4 nm of 3.4 cts/kR-sec, integration time of ~ 10 hours, and solar wind values for the electron density and temperature at Saturn. Phoebe UVIS Results - so far • Average FUV spectrum – Consistent with presence of CO2, H2O frosts – Phoebe is VERY dark <1650 Å; blocks IPH • Lack of emission features – No Chiron-like activity – Dissociative excitation of sublimated / sputtered H2O by solar wind is not a significant process (in contrast to Europa) • Latitudinal variation in reflectance spectrum – More H2O frost in S. polar region than at mid-latitudes Iapetus • Distant Iapetus observations collected for longitudinal, phase coverage – (Most of the mission is required to fill in complete coverage) – Some observations were lost due to s/c pointing errors • Close Iapetus flyby on December 31 – 124,000 km distance • Big science question – Why is one hemisphere of Iapetus so much darker than the other? – Geometric albedo range (visible): 0.02 – 0.6 – Competing hypotheses: endogenic vs. exogenic origin • We can weigh in on this by comparing our spectra of both sides of Iapetus to Phoebe and Hyperion Main Models for Albedo Dichotomy Model Pros Cons Refs Geologic resurfacing Infill of dark crater floors; clean edge (?) Hemispheric pattern Smith et al. 1982 Accretion from Phoebe Hemispheric pattern Color Soter 1974 As above + volatization Hemispheric pattern; color? The math Cruikshank et al. 1983; Squyres et al., 1984; Bell et al. 1985; Buratti and Mosher, 1995 Accretion from Titan or Hyperion Pattern and spectra Low albedo Matthews 1992; Vilas et al. 1996; Jarvis et al. 2000; Owen et al. 2001 Meteoritic erosion Hemispheric pattern Low density (1.2gm/cc) Cook and Franklin 1970; Wilson and Sagan, 1995, 1996 Accretion of D-type material from outer retrograde satellites Sufficient source; Phoebe not red Cruikshank et al. 1983; Buratti et al. 2002, 2004; Black et al., 2004 (general exogenic) Hemispheric pattern and spectra Iapetus: October 15, 2004 Range=1,222,000 km Radius=730 km Need much less H2O, more dark material to fit this Iapetus spectrum, compared to Phoebe a=88° Iapetus UVIS Results - so far (October) • FUV spectrum of southern hemisphere region • Distant, sub-pixel observation • Both dark, light terrains in pixel • Reflected solar features do not appear as in Phoebe spectrum • May be due to lower spatial resolution, small size of body • May have overall slightly bluer spectrum than Phoebe; less steep at longer wavelengths • Less H2O • More dark material • Must wait for closer Iapetus observations to make more definitive statements Sub-S/C location map CIRS_00BIA_FP3MAP001_PRIME Duration=00:57 AD=8.5 mrad Sub S/C=(29, 070), LT=14.4 =51o Disk map; Cassini Regio (subsolar point Ts≈125 K) (1) Iapetus Bright-Dark Comparison ISS_00CIA_GLOBMAPC001_PRIME (2004-366T14:00 UTC; 00:30 hrs) Trigger # Telemetry Rate number footprints number of images total Data Volume (predict) 2159 S&ER3 (24) 11 24 97 Mb 2+3x3 NAC clr mosaic 122500 km alt.; 740 m/pxl; d_IA=1950 pxl; 78 deg phase; sub-S/C lat/lon = +54/50; sun illuminates surface from left 2 NAC shutters per footprint (except #1 and2): 220 ms (bright) and 1.5 sec (dark terrain) WAC 4-color context (Vio, Grn, Ir1, Ir3) ISS_00CIA_COMPD001_VIMS (2004-366T19:00 UTC; 02:00 hrs) Trigger # Telemetry Rate number footprints number of images total Data Volume (predict) 1x1 NAC color mosaic 117500 km alt.; 705 m/pxl; d_IA=2050 pxl; 94 deg phase; sub-S/C lat/lon = +64/24; sun illuminates surface from left 10 NAC color frames + 3 polarizers Center of ftprt over dark terrain ==> long exp times selected Highest resolution color of BC flyby 2998 S&ER3 (24) 1 13 76 Mb More Iapetus in Nominal Tour Planned Cassini flybys at Iapetus (selection)* Date min. altitude best ISS pixel scale visible hemisphere** ----------------------------------------------------------------------------------------------------------------------------Jul 2004 2,500,000 km 15 km/pxl CR, southern bright terrain, SP Oct 2004 1,110,000 km 6.7 km/pxl anti-Saturn side (western CR), SP 31Dec04/ 01Jan05 117,500 km 710 m/pxl northern CR, high northern latitudes ----------------------------------------------------------------------------------------------------------------------------Nov 2005 416,000 km 2.5 km/pxl eastern and central CR, north. bright terrain Jan 2006 879,000 km 5.3 km/pxl eastern CR and trans. zone, "moat" partially Apr 2006 603,000 km 3.6 km/pxl leading side, SP Sep 2007 ~1,270 km# ~12 m/pxl CR (high phase), trailing side (low phase) ----------------------------------------------------------------------------------------------------------------------------*...Included are all flybys in 2004 and all flybys below 10 6 km altitude until June 2008. **...CR = Cassini Regio (dark material hemisphere); SP = south pole. #...10 Sep 2007: targeted flyby altitude not fixed yet; might be between ~1000 and ~1400 km. Dione • Close flyby on 15 December 2004 – Range: 72,912 km – Phase Angle: ~800 • UVIS was riding along on three observations – Collected first observation (GLOCOL) • Got FUV data but not EUV • Range: 159,395 km (7 pixels) • Phase: 340 – Partial collection of second observation (REGMAP), remainder lost due to error in how the SSR was configured • Next close Dione flyby is in Rev 16 (Oct. 2005) • Big science question for Dione post-Voyager was “What is the nature of the bright streaks?” The nature of Dione’s streaks • Voyager • Cassini UVIS Dione UV Albedo (GLOCOLOR) Dione REGMAP Tethys • Only fairly distant spectra so far, but significantly different than Phoebe • Upcoming, relatively close flybys: – – – – – – Rev 4; Rev 7; Rev 15; Rev 45; Rev 47; Rev 49; 82,975 km 64,990 km 33,295 km 97,131 km 16,166 km 48,324 km Tethys: October 28, 2004 Range=255,000 km Radius=530 km Tethys is ~10x brighter than Phoebe at similar phase angle Need much more H2O, less dark material to fit this Tethys spectrum, compared to Phoebe Model uses smaller H2O grain size a=50° Tethys UVIS Results - so far • 4 pixels on body • Reflected solar features do not appear as in Phoebe spectrum • May be due to larger amount of H2O ice - very dark • Tethys is ~10x brighter than Phoebe at similar phase angles • H2O is more dominant in Tethys spectrum than in Phoebe spectra – H2O grains may be smaller than on Phoebe - related to E-ring?? In the next 6 months… • First data from Mimas (range = 215,291 km) and Rhea (range = 144,171 km) in Rev 00C, right after completion of the Huygens Probe mission and playback (January 15) • We’ll get our first look at Enceladus in Rev 00C, at a range of 247,000 km (January 15) • Major upcoming close Enceladus flybys: – Rev 3; closest approach = 1179 km; February 17 • But this is right after T3 so major pointing uncertainties • We will get stellar occultation of lambda Sco – Rev 4; targeted flyby, closest approach = 500 km; March 9