1. ALMA Science Workshop, May 2004 Solar System Science with the ALMA Mark Gurwell Harvard-Smithsonian Center for Astrophysics ALMA Science Workshop, May 2004

2. (alternate title for cosmologists) The Really Really Really Really Really Low Z Universe with the ALMA Mark Gurwell Harvard-Smithsonian Center for Astrophysics ALMA Science Workshop, May 2004

3. ALMA - What’s It Good For? We can use it to study pretty much everything out there:  Planetary and satellite atmospheres (DRSP Theme 4.1)  Solid surfaces of planets, rings, satellites, KBOs and other minor bodies (DRSP Theme 4.2)  Cometary comae and nuclei (DRSP theme 4.3) ALMA Science Workshop, May 2004

4. Synergy/’the competition’ Need synergy with, to complement, and/or to exceed current and future observatories, e.g. ALMA Science Workshop, May 2004 SMA IRAMJCMT OVRO (E) V L A BIMABIMA HST/NGST MRO

5. ALMA Sensitivity I - Point Source Sensitivity in 60 s* Frequency (GHz) 90 230 345 650 ALMA Science Workshop, May 2004 Continuum (mJy) 0.031 0.060 0.14 1.9 1 km s -1 (mJy) 5.1 6.1 11 120 Charon (mJy) 0.15 0.95 2.02 6.25 *From http://www.alma.nrao.edu/info/sensitivities/index.html

6. ALMA Sensitivity II- High Resolution Thanks to Karl Menten for this plot! ALMA Science Workshop, May 2004 D (AU) 0.3 1 5 10 30 50 100 25 mas (km) 5.4 18 91 181 544 907 1813

7. Before the DRSP details: What are we interested in? A non-exhaustive list How are the denizens of the solar system alike? How are they different? How do they ‘work’? What evolution have they undergone? Are there conditions for life elsewhere? How unique is our solar system? ALMA Science Workshop, May 2004 Now, on to the Details…

8. 4.1.1 Planetary Atmospheres - Atmospheric Structure and Dynamics ALMA Science Workshop, May 2004 SMA Mars CO 2-1 MapJCMT Venus Wind Measurement ALMA will measure vertical thermal structure and directly characterize winds on Mars and Venus on size scales of 100 km or less. Courtesy Todd Clancy

9. 4.1.2 Planetary Atmospheres - Mars 3D Water Cycle ALMA Science Workshop, May 2004 Clancy et al 1990 VLA 22 GHz Water MapOVRO 226 GHz HDO Map ALMA can match HST resolution with sensitivity to mm/sub mm transitions to study atmospheric temperature and water distribution in 3D

10. 4.1.3 Planetary Atmospheres - Chemistry and Trace Species Detection ALMA Science Workshop, May 2004 JCMT data, Courtesy Todd Clancy ALMA will have sensitivity and spatial resolution to seek, find, and map the distribution of trace atmospheric species on Mars, Venus and other planets

11. 4.1.5 Planetary Atmospheres - Tropospheres of Giant Planets ALMA Science Workshop, May 2004 (top) Phosphine 3-2 on Jupiter (CSO FTS, Weisstein and Serabyn) (left) 3.6 cm tropospheric emission during SL/9 impact (Grossman et al.) ALMA’s continuum sensitivity (8 GHz bandwidth) will allow detection of thermal gradients, belt/zone structure and very broad absorption lines from giant planet tropospheres

12. 4.1.6 Planetary Atmospheres - Titan’s Atmospheric Chemistry/Dynamics ALMA Science Workshop, May 2004 SMA 850 micron unresolved observations Titan is cool! And with ALMA we will be able to study its atmosphere with unprecedented detail, including direct measure of winds and 3D structure of temperature and molecular abundances on scales of a few hundred km OVRO 1.2 mm low res maps of nitriles Gurwell (2004)

13. 4.1.7 and 4.2.3 Planetary Atmospheres and Surfaces - Io’s Volcanism ALMA can map thermal emission from the surface showing location and temperature of hot spots, and can map molecules in volcanic plumes ALMA Science Workshop, May 2004 Galileo images courtesy NASA/JPL-Caltech. Io: 3630 km diameter = 1” at 5 AU 500 km plume = 140 mas

14. 4.2.2 and 4.2.5 Planetary Surfaces - Mapping Mercury and Asteroids ALMA will map temperature in the upper centimeter of the surfaces of terrestrial planets, moons, and minor bodies, providing understanding of surface material characteristics ALMA Science Workshop, May 2004 VLA image courtesy Bryan ButlerSMT data courtesy Amy Lovell

15. 4.2.1 and 4.2.3 Planetary Surfaces - Mapping Pluto and Charon ALMA Science Workshop, May 2004 Pluto is 100 mas and Charon is 50 mas at current distance from sun. ALMA will map the thermal emission from Pluto and Charon with up to 40 resolution elements, measuring temperature and/or emissivity variations that may change with time

16. 4.2.x Planetary Surfaces - Sizes, Temperatures, and Albedos of Distant Bodies ALMA Science Workshop, May 2004 ALMA will measure the temperatures of numerous KBOs in a matter of minutes, and modestly resolve the largest objects in the outer solar Kuiper Belt (and beyond?!) Shamelessly taken from Mike Brown’s website

17. 4.3 Comets ALMA Science Workshop, May 2004 Blake et al 2000 (OVRO) Hale-Bopp ALMA will study the molecular gas streaming from comets with great detail, informing our understanding of comet composition and coma chemistry

18. 4.3 Comets II ALMA Science Workshop, May 2004 SMA observations by Qi et al

19. Beyond… ALMA Science Workshop, May 2004 More shameless pilfering by moi from Mike Brown!

20. 4.4 Extrasolar Planets ALMA Science Workshop, May 2004 Alpha centauri unit It’s the same guy! Coincidence? Hmmm… What if… Special thanks to David Wilner as cocreator of L&O: ACU

21. 4.1.1 Extrasolar Planets - Direct Detection of Jupiters around Nearby Stars I ALMA Science Workshop, May 2004 1600 K 800 K 400 K Jupiter Saturn

22. 4.1.1 Extrasolar Planets - Direct Detection of Jupiters around Nearby Stars II ALMA Science Workshop, May 2004 1600 K 800 K 400 K Jupiter Saturn

23. And even further beyond… Ahh, but Neal covered this earlier… ALMA Science Workshop, May 2004 Courtesy David Wilner

24. Concluding Remarks Important Considerations: High Fidelity Imaging Imaging Scales from 10mas to degrees Bandpass Fidelity Over Large Bandwidth Long Baselines/High Resolution 1% Amplitude Calibration is Good Tracking of ‘Fast’, and Close, Objects Radar in the future? ALMA Science Workshop, May 2004

25. Concluding Remarks ALMA will be an incredibly sensitive instrument for continuum and line observations of solar system objects. With resolution comparable to or exceeding nearly all other observatories save robotic missions, it will have a major impact in solar system studies ALMA Science Workshop, May 2004

26. Acknowledgements Thanks to R. Todd Clancy, Amy Lovell, Karl Menten, Charlie Qi, Bryan Butler (without his knowledge, perhaps) and David Wilner for valuable contributions to this presentation. ALMA Science Workshop, May 2004