U.S. Antarctic Program
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?
USAP Planning Timelines
• NSF & ASC put together support packages for science, construction & operations/maintenance
• Planning cycles range from 1-3 yrs, 3-5 yrs & 5-10. 10 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.
• Start with a little history…
1911- Roald Amundsen
Led Norwegians to the South Pole
Buried ~65 ft., now displaced
3000 ft. from the Geographic
South Pole
The first structure placed at South Pole
Construction of Surface Station
1970: Station Buried
1956 – IGY, U.S. Mandate: Establish Science Station
First Landing 31 Oct 1956
Dome Station
1974-2006
Design Criteria:
• 15 to 20 year life
• Maximum 33 males
• 250 KW Power Plant
• Limited Science
Construction at the Bottom of the World —
Challenges and Progress
1997
Change is coming…
Elevated Station (Total time ~15 to 20 yrs)
South Pole Elevated Station Layout
te
xt
te
xt
Fuel Storage Facility Logistics Arch
Garage Shops
Power Plant
A2
B2
B3
A1
A4
B1
B4
RF Building
SPTR-2
Ice Cube Lab
HF Antenna
Dark Sector
Lab
LO Facility
Cryogens Facility
Utility Tunnel
A1-Winter Quaters
A4-Winter QuatersA1-Food Service/
Dining
A3 Medical/PC Lab
B2-Science Lab
B3- Admin/communications
B4-GYM/ Multipurpose
B1-Quarters/ EM Power
Remote Facilities
Skynet
South Pole
Telescope
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 costs
@ $5.5M (Funded)
* Weather 2-year schedule delay, scope changes,
unforeseen events @ 9.3M (Funded)
C. Estimated to complete $145.5M (9% increase)
* Deferral of Cargo Facility, SPTR-1 upgrade,
Final closeout, & change requests @ $2.82M
SPSE/SM Project Budget 154-person station (summer) &
50-person (winter)
2000-Begin Elevated Station
Settlement Issues?
Elevated Test
Assembly Pod B-2
Structural Steel Construction
A1/A2 and Vertical Tower
Saddle Truss Steel Split in half to fit inside an LC-130…
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
Elevated Station Features
Kitchen
Dining Area
Communications
Medical Recreation
Berthing
LC-130 Logistics
SPSE and SPSM
24 million pounds (cargo&pax)
907 missions (13 yrs)
Dimensions of an LC-130
LC-130 Cargo Flights
Check out fuel flights…
New Power Plant Power Capacity Doubled to 1 Megawatt
Water & Sewer
Utilities
10’ x 6’ x 3000’ Snow Utilidor
•Water Well Life ~7 years
•Becomes a sewer bulb storing waste
•New Water Well Developed
•Repeat leapfrog process
Annual Consumption: ~1,100,000 gallons
South Pole
Information Technology and Communications
GOES/
Skynet
SPTR-2
RF
Building
South Pole Satellite Coverage
Geosynchronous satellites
with subpoints below 8° S
are visible at South Pole
8° S
TDRS F4 GOES-3
South Pole Satellite Visibility 17-18 Jan 09
-1
0
1
2
3
4
5
6
0:00 12:00 0:00 12:00 0:00
Time (GMT)
Ele
vati
on
An
gle
(d
eg
) F1
F3
F4
F5
F6
F7
GOES
South Pole Satellite Window
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
– 802.11b - 2.4 GHz
Science at South Pole
Solar Physics, Astrophysics,
and Cosmology
6 projects
Meteorology and
Climatology
3 projects
Geology and
Geophysics
3 projects
Aeronomy and
Space Physics
7 projects
Glaciology 1 projects
Science Support 2 projects
Clean Air Sector
Meteorology and
Climatology
3 projects
Quiet
Sector
Geology and
Geophysics
3 projects
Dark Sector
Solar Physics,
Astrophysics, and
Cosmology 6 projects
Glaciology 2 projects
Aeronomy and
Space Physics
7 projects
Downwind Sector
Science Support 2 projects
SPT
Biology & Medicine 1 project
SPT (Total time ~5 to 10 yrs)
South Pole Telescope
First light 17 Feb 2007
3
4
Lots of bright sources: SPT discovery of a new population of distant star- forming 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)
34
2011: This is zoom-in of an SPT sky map:~50 sq. degrees from 2500 sq. degrees SZ survey
The large scale noise-like features in this map are the Cosmic Microwave Background variations. CMB is the fossil light from the Big Bang, and the SPT has made the highest resolution measurements of this radiation.
SPT’s sensitivity and high angular resolution observations provide currently the most efficient constraints to the existing cosmological models.
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SPT 800 deg2
Keisler et al., 2011
SPT 200 deg2
Shirokoff et al.,2010
Am
plit
ud
e o
f C
MB
flu
ctu
atio
ns
larger ← angular size → smaller
• 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, high-
redshift 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)
Published SPT results and discoveries
Replace Azimuth Bearing on SPT
What was wrong?
Installation of new bearing
Almost There…
SPT polarization receiver deploying in 2011/12
SPT-Pol
observations
Three year
projection:
σ(Σmν) = 0.15 eV
r to 0.023 at 2σ
• 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 Co-moving shield construction
installation last year
Trusses
Shield Panels
Primary Mirror
AMANDA
• Avg. time to deep drill hole 41 hrs.
• Avg. hole depth 2452 m
• Avg. drilling rate 1.7 m/min.
• Avg. fuel per hole 5,520 gal.
• Drill thermal power output 4.7 MW
• Avg. string deployment time 8 hrs.
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
IceCube (Total time ~5 to 15 yrs)
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 reconstructed neutrino event
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.
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 2010.
The IceCube Lab
The Seasonal Equipment Site
A Digital Optical Module (DOM) is
prepared for deployment
IceCube 2009/2010
Averages
31 hrs Deep drilling
time
2450 m Hole Depth
1.9m/mi
n
Drilling Rate
4,200
gal
Fuel per hole
9.5 hrs String
deployment
IceCube Neutrino Observatory
IceCube Lab (ICL)
Field Camp Science (Total time ~1 to 5 yrs)
Field Camp Replacement Underway
Small Scale Science (Total time ~1 to 3 yrs)
BAS GPS
Biology at South Pole (1-2 yrs)
Snow Temperature Measurements
Enjoy Your Visit to the South Pole