Big Telescope Projects in SESE Past, Present, & Future
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1 Big Telescope Projects in SESE Past, Present, & Future Rogier Windhorst (ASU) on behalf of SESE faculty ; ; ? Talk at the SESE Retreat, Th/Fr Aug , 2014, ASU, Tempe, AZ
2 (How) can SESE play in the big telescope league in the next 30 years? We need to think of large projects that will knock it out of the ball-park...
3 Past Present SESE astro faculty grants increased steadily since SESE started in True, even when corrected for growth in astro faculty since 2006 (next pg). Return-on-investment ROI=Σ(expend/startup) 2.6 (range [ ]).
4 Past Present Note: Current year (FY14) only lists half the Expenditures. Grants also increased for astro faculty at ASU before SESE started in Return-on-investment ROI=Σ(expend/startup) 16.5 (range 5 173[ ]). Access to new facilities is key to move beyond any funding plateau.
5 True relative size: Hubble, James Webb, & Giant Magellan Telescope 18 B$ ( ); 9 B$ ( ); 1 B$ ( ).
6 True relative size: Hubble, James Webb, and ATLAST B$ ( ); 9 B$ ( ); B$ ( ?).
7 Potential GMT+ATLAST synergy with SESE Solar System research: Left: Hubble maps Mars global dust-storm in 2001, in support of Mars Global Surveyor. Middle: Hubble sees Jupiter s Great Red Spot decline over two decades. Right: Hubble sees Saturn s Aurora change, in support of Cassini Mission. GMT & ATLAST will monitor global weather of solar system planets on many decades timescales at > 10 Hubble s resolution!
8 GMT, ATLAST will study Jupiter s weather at > 10 Hubble s resolution. Long orbital periods require data on many-decade time-scales (slide courtesy of Dr. J. Norwood).
![[LEFT]: April 1997 Galileo probe image of Jupiter s Moon Io.](/docs-images/81/83605279/images/9-1.jpg "[RIGHT]: Keck images of Aug. 2013 outbursts of Io s craters Rarog etal.")
9 GMT, ATLAST will study volcanic eruptions on solar system moons on decade s time-scales at > 3 10 Keck s resolution. [LEFT]: April 1997 Galileo probe image of Jupiter s Moon Io. [RIGHT]: Keck images of Aug outbursts of Io s craters Rarog etal.. (slides courtesy of NASA and Dr. I. de Pater).
10 GMT, ATLAST will study ring systems at > 10 Hubble s resolution. (slide courtesy of Dr. H. Hammel, I. de Pater et al.).
11 GMT, ATLAST will study Titan s Nitrogen-Methane atmosphere weather at > 10 Hubble s resolution (at near mid-ir wavelengths for GMT in accessible atmospheric windows). (slide courtesy of Dr. J. Lunine).
12 GMT, ATLAST multi-decade weather monitoring especially powerful for outer planets. (slide courtesy of Dr. H. Hammel). [Uranus went from Summer in 1986 (Voyager) to Fall in 2007].
13 GMT, ATLAST will study Uranus weather at > 10 Hubble s resolution. (slide courtesy of Dr. H. Hammel et al.).
14 GMT, ATLAST will study Uranus weather at > 3 10 Keck s resolution. (slide courtesy of Dr. H. Hammel et al.).
15 GMT, ATLAST will study Uranus weather at > 3 10 Keck s resolution. (slide courtesy of Dr. I. de Pater & H. Hammel et al.).
16 GMT, ATLAST will study Neptune s weather at > 3 10 Keck s resolution. (slide courtesy of Dr. H. Hammel et al.).
17 GMT+ATLAST synergy with SESE astrobiology, exoplanets, element production Top: Hubble NICMOS near-ir imaging of exoplanet system around the (very carefully subtracted!) star HR Bottom: AZ Large Binocular Telescope (LBT) Adaptive Optics imaging of HR 8799: Direct imaging of exoplanets & orbits around nearby star! GMT & ATLAST will find planets much closer in for more distant stars!
18 GMT, ATLAST will characterize the parameter space of Super-Earths. (slide courtesy of Dr. J. Patience; ASU).
19 GMT, ATLAST will find chemical building blocks of life in Exoplanet atmospheres. (slide courtesy of Dr. J. Patience; ASU).
20 GMT, ATLAST will characterize the atmospheres of (Super-) Earth-like Exoplanets. (slide courtesy of Dr. J. Patience; ASU).
21 GMT, ATLAST will characterize planetary debris disks before they form planets. (slide courtesy of Dr. J. Patience; ASU).
22 GMT, ATLAST will characterize chemical elements needed for (habitable) exoplanet formation. (slide courtesy of Dr. Timmes, Young, & Starrfield).
23 GMT, ATLAST will measure atomic and molecular composition of exoplanets and (proto-)planetary disks. (slide courtesy of Dr. Timmes, Young, & Starrfield).
24 GMT, ATLAST will measure chemical composition of asteroids, Kuiper Belt Objects, and of star-forming regions in our own and other galaxies. (slide courtesy of Dr. Timmes, Young, & Starrfield).
25 GMT, ATLAST provide most powerful, always-ready monitoring of the most explosive events in the universe. (slide courtesy of Dr. F. Timmes).
26 GMT, ATLAST will elucidate whether the core of Dark Energy (Supernovae as standard candles ; 2012 Nobel Prize) is observationally and theoretically correct. Powerful synergy with ASU supercomputer modeling. (slide courtesy of Dr. F. Timmes).
27 GMT, ATLAST will elucidate the nature of all types of exploding stars: the most energetic events in the Universe. (slide courtesy of Dr. F. Timmes).
28 GMT, ATLAST will measure the formation of the first stars in the (very small!) first globular clusters in the Universe. (slide courtesy of Dr. E. Scannapieco, M. Richardson).
29 Redshifts: o z=7 8, o z=9, O z= Hubble UltraDeep Field: What Webb will do in half a day. 592hr HUDF: FuvNuvUBViIzYJWH, AB < 31 ( 1 firefly from moon).
30 Panchromatic 13 filter Hubble UltraDeep Field: What ATLAST will do in half an hour! 592 hr HUDF: FuvNuvUBViIzYJWH, AB < 31 ( 1 firefly from moon).
31 List of Future Grants and Large Projects SMALL (0.1 1 M$): NSF AST, AAG, ATI (All SESE astro faculty). NASA Hubble, Herschel, Spitzer, Fermi, ADAP, ATP, Exoplanet, & EPO (all SESE astro faculty). DOE Low Energy Nuclear Physics (Krauss, Young). MEDIUM (1 10 M$): NASA Hubble (and Webb) Treasury projects, such as Malhotra s ; Windhorst JWST. NSF Physics Frontier Center (2013, 2016), such as Timmes 2014! NSF Science & Technology Centers (2014). NSF Sustainable Research Computing Center (2015); NSF HPC Acquisition (every 3 years; Timmes). NSF NSPIRE; NSF AISL STEM learning 2 M$ (400 k$/year; Bowman). NASA Astrobiology Institute (2017, 2020) Call 8 or 9 (Desch etal.). NASA Balloon program (5M$): BOBKAT CMB polarization (Mauskopf); HiTiDe outer planet monitoring (Scowen); GUSSTO sub-mm (Groppi). NASA APRA detector development: Groppi, Mauskopf, Scowen. LARGE ( M$): NSF MSIP (2013, 2016; 12 M$): Rhoads MMT Widefield IR Imager; Bowman s HERA radio experiment. MIDEX (2017; 350 M$): Scowen s ORION and HORUS mission concepts. Widefield Imager+Coronagraph: GMT (2016; 50 M$) & ATLAST (2020 s; 400 M$). GOAL 1: Overall package to increase SESE astro expenditures to 10 M$/yr. GOAL 2: ASU to partner in big telescope projects to enable major funding leaps forward.
32 Conclusion: To play in big league, ASU should consider joining big projects. Each of GMT and ATLAST facility nearly fills the whole Yankee ballpark... New paradigm: They are too large for an individual university to take on. We suggest to SESE faculty to discuss options with ASU administration.
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