U.S. Antarctic Program

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Rosalind Tucker
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1 U.S. Antarctic Program

2 Installation & Maintenance of Science Facilities on the Antarctic Plateau How do we plan for replacing a station without impacting the science goals at South Pole? How do we build a 10-m telescope without impacting the building of a new station? How do we install a cubic kilometer neutrino detector without impacting the building a new station or a 10-m telescope?

3 USAP Planning Timelines NSF & ASC put together support packages for science, construction & operations/maintenance Planning cycles range from 1-3 yrs, 3-5 yrs & yrs is typical length of ASC contract in the USAP. Why So Long? It takes at least 2 yrs to get an idea into a federal budget, then another 1-3 yrs to plan, followed by 1-5 implementation/operation on the ice depending on project scope/budget/cost.

4 Start with a little history

5 1911- Roald Amundsen Led Norwegians to the South Pole The first structure placed at South Pole Buried ~65 ft., now displaced 3000 ft. from the Geographic South Pole

6 1956 IGY, U.S. Mandate: Establish Science Station Construction of Surface Station First Landing 31 Oct : Station Buried

7 Dome Station Design Criteria: 15 to 20 year life Maximum 33 males 250 KW Power Plant Limited Science

8 Construction at the Bottom of the World Challenges and Progress 1997 Change is coming

9 Elevated Station (Total time ~15 to 20 yrs)

10 t South Pole Elevated Station Layout Cryogens Facility Remote Facilities Garage Shops RF Building Skynet Dark Sector Lab Fuel Storage Facility Logistics Arch LO Facility HF Antenna South Pole Telescope Power Plant Utility Tunnel Ice Cube Lab SPTR-2 t e x t A1 A1-Winter Quaters A1-Food Service/ Dining A2 B2 B3 A4 A4-Winter Quaters A3 Medical/PC Lab t e x B1 B1-Quarters/ EM Power B2-Science Lab B4 B4-GYM/ Multipurpose B3- Admin/communications

11 SPSE/SM Project Budget 154-person station (summer) & 50-person (winter) I. SPSE Funding (Work completed within budget) $ 25.0M II. SPSM A. Initial Funding $127.9M B. Current Cost $142.7M (7% increase) * Added 40 beds, schedule delay & fuel $5.5M (Funded) * Weather 2-year schedule delay, scope changes, unforeseen 9.3M (Funded) C. Estimated to complete $145.5M (9% increase) * Deferral of Cargo Facility, SPTR-1 upgrade, Final closeout, & change $2.82M

12 2000-Begin Elevated Station Settlement Issues?

13 Elevated Test Assembly Pod B-2

14 Structural Steel Construction A1/A2 and Vertical Tower

15 Saddle Truss Steel Split in half to fit inside an LC-130

16 Year Round Work Plan Summer ~100 Days Exterior Work 3 Shifts: 9hrs per day 6 days a week Winter ~265 Days Interior Work 1 Shift: 9hrs per day 6 days a week

17 Elevated Station Features Kitchen Communications Berthing Dining Area Medical Recreation

18 LC-130 Logistics SPSE and SPSM 24 million pounds (cargo&pax) 907 missions (13 yrs) Dimensions of an LC-130

19 LC-130 Cargo Flights Check out fuel flights

20 New Power Plant Power Capacity Doubled to 1 Megawatt

21 Water & Sewer Utilities Water Well Life ~7 years Becomes a sewer bulb storing waste New Water Well Developed Repeat leapfrog process 10 x 6 x 3000 Snow Utilidor Annual Consumption: ~1,100,000 gallons

22 South Pole Information Technology and Communications SPTR-2 GOES/ Skynet RF Building

Elevation Angle (deg) South Pole Satellite Coverage South Pole Satellite Visibility 17-18 Jan 09 6 5 4 F1 F3 3 F4 F5 2 F6 8 S 1 0 F7

23 Elevation Angle (deg) South Pole Satellite Coverage South Pole Satellite Visibility Jan F1 F3 3 F4 F5 2 F6 8 S 1 0 F7 GOES -1 0:00 12:00 0:00 12:00 0:00 Geosynchronous satellites with subpoints below 8 S are visible at South Pole TDRS F4 Time (GMT) GOES-3

24 South Pole Satellite Window

25 Other South Pole Communication Systems High Frequency Radio Operational use (flight ops, weather, cargo, etc.) Land Mobile UHF Radio Construction, station operations, emergency response, science Air-to-Ground VHF Radio Aircraft communications Wireless Local Area Network Summer only b GHz

Science at South Pole Geology Solar Physics, and Astrophysics, Aeronomy and Glaciology 1 projects Geophysics and Cosmology Space Physics Meteorology and 3 projects 6 projects 7 projects Science

26 Science at South Pole Geology Solar Physics, and Astrophysics, Aeronomy and Glaciology 1 projects Geophysics and Cosmology Space Physics Meteorology and 3 projects 6 projects 7 projects Science Support Climatology 2 projects 3 projects Solar Physics, Astrophysics, and Cosmology 6 projects SPT Aeronomy and Space Physics 7 projects Clean Air Sector Dark Sector Biology & Medicine 1 project Science Support 2 projects Quiet Sector Meteorology Glaciology and 2 projects Climatology Downwind Sector 3 projects Geology and Geophysics 3 projects

27 SPT (Total time ~5 to 10 yrs)

28 South Pole Telescope First light 17 Feb 2007

11: This is zoom-in of an SPT sky map:~50 sq. grees from 2500 sq. degrees SZ survey e large scale noise-like features in this map are the osmic Microwave Background variations.

29 11: This is zoom-in of an SPT sky map:~50 sq. grees from 2500 sq. degrees SZ survey e large scale noise-like features in this map are the osmic Microwave Background variations. CMB is the ssil light from the Big Bang, and the SPT has made the ghest resolution measurements of this radiation. Lots of bright sources: SPT discovery of a new population of distant starforming galaxies. High signal to noise SZ galaxy cluster detections as shadows against the CMB. (Note that SZ-effect is independent of distance, i.e., redshift) 3 34

30 Amplitude of CMB fluctuations PT s sensitivity and high angular resolution bservations provide currently the most efficient onstraints to the existing cosmological models. SPT 800 deg 2 Keisler et al., 2011 SPT 200 deg 2 Shirokoff et al.,2010 larger angular size smaller 35

31 Published SPT results and discoveries First clusters discovered via their SZ signature Staniszewski et al., ApJ, 701, 32, 2009 Cluster spatial profiles measured to the virial radius Plagge et la., ApJ, 716, 1118, 2010 First detection of secondary CMB anisotropy and cosmological implications Lueker et al., ApJ, 719, 1045, 2010 Shirokoff et al., ApJ, 736, 61, 2011 First mm-wave detection of Cosmic Infrared Background (CIB) anisotropy Hall et al., ApJ, 718, 632, 2010 Discovery of high-redshift, strongly lensed dusty galaxies Vieira et al., ApJ, 719, 763, 2010 First cosmological constraints from an SZ cluster survey Vanderlinde et al., ApJ, 722, 1180, 2010 Redshift estimation, optical and x-ray properties of SPT SZ-selected clusters High et al., ApJ, 723, 1736, 2010 Zenteno e tal., ApJ, 734, 3, 2011 Andersson et al., ApJ,738, 48, 2011 Discovery of the two most massive z>1 clusters Brodwin et al., ApJ, 721, 90, 2010 Foley et al., ApJ, 731, 96, 2011 Testing ΛCDM with massive, highredshift clusters Foley et al., ApJ, 731, 96, 2011 Williamson et al., ApJ, 738, 139, 2011 Most sensitive measurement of the CMB power spectrum damping tail - improved cosmological constraints; inflation tests, number of neutrinos Keisler et al., ApJ, 2011 (in press) First public data release of SPT maps and tools Schaffer et al., ApJ, 2011 (in press)

33 What was wrong?

34 Installation of new bearing

35 Almost There

SPT polarization receiver deploying in 2011/12 Testing Inflation

signatures from inflationary (primordial) gravitational waves

SPUD) Measuring neutrino masses by determining intermediate scale

Dark Energy constraints by increasing sensitivity of SPT SZ survey

36 SPT polarization receiver deploying in 2011/12 Testing Inflation by searching for the CMB large angular scale B-mode polarization signatures from inflationary (primordial) gravitational waves generated in first instants of the Universe (complements BICEP & SPUD) Measuring neutrino masses by determining intermediate scale B-mode polarization induced by large scale structures Improving Dark Energy constraints by increasing sensitivity of SPT SZ survey SPT-Pol observations Three year projection: σ(σmν) = 0.15 ev r to at 2σ

37 SPT Co-moving shield construction installation last year Shield Panels Trusses Primary Mirror

IceCube (Total time ~5 to 15 yrs) 1996/2000

2005/2006 Season - First String 2009/2010

38 IceCube (Total time ~5 to 15 yrs) 1996/2000 Seasons - AMANDA 2008/2009 Season - 18 Strings 2005/2006 Season - First String 2009/2010 Season - 19 Strings 2006/2007 Season - 8 Strings 2010/2011 Season - 20 Strings 2007/2008 Season - 13 Strings 2011/2012 Season 7 Strings AMANDA Avg. time to deep drill hole Avg. hole depth Avg. drilling rate Avg. fuel per hole Drill thermal power output Avg. string deployment time 41 hrs m 1.7 m/min. 5,520 gal. 4.7 MW 8 hrs.

IceCube Neutrino Observatory IceCube is made up of strings of sensors called Digital Optical Modules, or DOMs,

DOMs send data on time and intensity of the detected light flashes generated by secondary particles to the

IceTop, a surface array of ice Cherenkov detectors, can measure high energy cosmic rays in coincidence with the

39 IceCube Neutrino Observatory IceCube is made up of strings of sensors called Digital Optical Modules, or DOMs, that detect the faint blue Cherenkov light released when a neutrino interacts with a nucleus in the ice. DOMs send data on time and intensity of the detected light flashes generated by secondary particles to the IceCube Lab on the surface. IceTop, a surface array of ice Cherenkov detectors, can measure high energy cosmic rays in coincidence with the deep detector. A skymap of high energy muon events that point back in the same direction as their parent neutrinos, allowing IceCube to identify astrophysical neutrino sources. A reconstructed neutrino event

IceCube Neutrino Observatory IceCube transforms a billion ton,

for neutrino interactions coming from violent astronomical events

Detector construction using a hot water drill began in December

IceCube 2009/2010 Averages 31 hrs Deep drilling time 2450 m Hole

40 IceCube Neutrino Observatory IceCube transforms a billion ton, natural ultra-transparent Antarctic ice block into an astronomical telescope. Building on the success of its predecessor AMANDA, IceCube looks for neutrino interactions coming from violent astronomical events like exploding stars and black holes. Detector construction using a hot water drill began in December 2004 and completed in December IceCube 2009/2010 Averages 31 hrs Deep drilling time 2450 m Hole Depth 1.9m/mi n 4,200 gal Drilling Rate Fuel per hole 9.5 hrs String deployment The IceCube Lab The Seasonal Equipment Site A Digital Optical Module (DOM) is prepared for deployment

41 IceCube Lab (ICL)

42 Field Camp Science (Total time ~1 to 5 yrs) Field Camp Replacement Underway

43 Small Scale Science (Total time ~1 to 3 yrs) BAS GPS

44 Biology at South Pole (1-2 yrs)

45 Snow Temperature Measurements

46 Enjoy Your Visit to the South Pole

Astrophysics from Antarctica: overview of recent science

Astrophysics from Antarctica: overview of recent science Michael Burton University of New South Wales SCAR Astronomy and Astrophysics from Antarctica 2 nd Workshop Siena, Italy 24-26 July, 2013 Outline