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