Note: Allocated times include question time
and discussion.
Thursday 28 June 2001
0930
– 1000 Coffee.
Opening
1000 – 1020 Welcome
The Hon. Sir Guy Green, AC, KBE, Governor of Tasmania.
1020 – 1050 Opening Address: Antarctica
– where international collaboration comes naturally.
A.
Ferrari
Istituto
Nazionale di Astrofisica, Italy
1050 – 1120 Present status of the French-Italian
station at Dome C.
M.
Candidi (1) and A. Lori (2)
(1)
IFSI/CNR
(2)
PNRA/ENEA
The
completion of the structure of the base has allowed the
announcement of the planned opening for winter over in 2003;
the layout of the facilities and the logistics capabilities
for transfer of equipment and personnel will be presented.
1120
– 1150 Coffee break
Site testing I
1150 – 1210 Concordiastro
E.
Fossat
Universite'
de Nice, France
Site
qualification in visible light and astroseismology are the
first two goals of the Concordiastro program, which intends
to demonstrate that the Dome C site is certainly also outstanding
for the visible wavelength range and at least for some given
specific scientific targets.
1210
– 1230 JACARA site-testing in Antarctica: past, present
and future.
M.C.B.
Ashley, M.G. Burton, J.W.V. Storey
UNSW,
Australia
The
Joint Australian Centre for Astrophysical Research in Antarctica
(JACARA) has been site-testing at the US Amundsen-Scott
South Pole Station since 1994, and at Dome C since 2000.
During this time we have built and operated instruments
that measure the sky emission in the UV, optical, near-IR,
mid-IR, and sub-millimetre regimes. Our work has included
micro-thermal measurements of the atmosphere, acoustic radar
(SODAR), differential image motion monitors, and CCD-imaging
cloud monitors. JACARA also participated in key aspects
of the SPIREX/Abu 60-cm infrared telescope at South Pole
Station. The results from this program will be summarised,
and the future directions will be discussed.
1230
– 1400 Lunch
Site testing II
1400 – 1415 Submm Astronomy from Dome
Concordia
G.
Dall'Oglio
Università
di Roma 3, Italy
We
describe measurements carried out in Antarctica during the
1998/99 US-Italian Antarctic Expedition. Atmospheric noise
was monitored in three atmospheric windows between wavelengths
of 1 and 3 mm for ten days at the Italian-French base, Dome
Concordia. Measurements of the temporal and spatial power
spectrum of atmospheric fluctuations were performed. We
do not observe the expected Kolmogorov spectrum for these
fluctuations and conclude that Dome C is a good site for
millimetric astronomy measurements.
Plans
for future activities are also presented
1415 – 1430 Submillimetre Site Testing
at Dome C
P.G.
Calisse (1), M.C.B. Ashley (1), M.G. Burton (1), J.R. Everett
(1), M.A. Phillips (1),
J.W.V.
Storey (1), S. Radford (2), J. Peterson (3)
(1)
University of New South Wales, Australia
(2)
NRAO, USA
(3)
Carnegie Mellon University, USA
We
present the first 350 um site testing data from Dome C,
acquired with a submillimre tipper last summer. A comparison
with similar data from other sites and with data under acquisition
with the same instrument this winter at the South Pole will
follow.
1430
– 1445 Near- and Mid- Infrared Sky brightness at the
South Pole
J.S.
Lawrence, M.C.B. Ashley, M.G. Burton, P.G. Calisse, A. Phillips,
J.R. Everett, and
J.W.V.
Storey
UNSW,
Australia
Measurements
taken with the Infrared Photometer Spectrometer (IRPS) have
indicated that the near infrared sky over the South Pole
is much darker than at latitude sites. Data from the Mid-Infrared
Sky Monitor (MISM) has indicated that similar advantages
are obtained at mid-infrared wavelengths. Currently the
Near Infrared Sky Monitor (NISM) is collecting data from
the South Pole; it will be deployed, with the MISM, to Dome
C in 2002. A review of the operation of these three instruments
and data collected to date will be given.
1445 – 1500 Submillimeter Site Testing
at South Pole
J.
Peterson
University
of Carnegie-Mellon, USA
Identical
sky brightness photometers have been operated at the South
Pole, Atacama, and Mauna Kea for several years. Results
comparing the statistics of brightness and its variations
will be presented. These monitors are functionally equivalent
to the new submillmeter photometer which has recently been
tested at Dome C. The comparison of data from these four
instruments
will allow objective site comparison.
1500
– 1530 Coffee
Site testing III
1530 – 1545 One night of seeing at
the South Pole
T.
Travouillon, M.G. Burton, M.C.B. Ashley, J.W.V. Storey
UNSW,
Australia
The
seeing conditions at the South Pole have already been the
subject of studies for its unique altitude distribution.
Most of the turbulence at the origin of the seeing is located
within a boundary layer 300m high above which the free atmosphere
is very stable. Up to now, no continuous measurements of
the turbulence have been made and we therefore could not
easily follow the evolution of the turbulence through out
the whole six month night. Using a Doppler SODAR we have
been able to sample the first kilometre of the atmosphere
almost continuously between February and November 2000.
It has enabled us to follow the time evolution of the boundary
layer as well as to assess its relationship with temperature
and wind velocity. The mean seeing at ground level was measured
to be 1.73" with a strong dependence on weather conditions
(standard deviation of 1.07").
The
importance of the concentration of turbulence in the lower
300m advantages the application of image correction. The
coherence time of the turbulence within the first 1000m
of atmosphere beats any other site in the world with a mean
40 milliseconds .The isoplanatic patch size also takes advantage
of the localisation of the turbulence and on average would
be as large as 119.88".
The
results presented here show how compatible the Antarctic
continent is with an adaptive optic system and how simple
meteorological measurements can predict the seeing conditions.
1545
– 1600 Characterisation of surface turbulence at Dome
Concordia
P.G.
Calisse (1), M. Nardino (2)
(1)
UNSW, Australia
(2)
CNR, Italy
Micrometeorological
observations of the surface turbulence have been carried
out during the Antarctic summer at Dome Concordia (3306
a.s.l.) in 1997. The parameterisation of the surface turbulence
is described by the similarity theory and the results obtained
by comparing the experimental findings and the relationships
reported in literature are explained. Moreover, in order
to characterise the surface around the measurement point,
it has been obtained the surface roughness length for each
wind direction sector.
The Present Status of
Antarctic Astronomy
1600 – 1630 CARA: 15 years of Astrophysics
at the South Pole
R.
Pernic
University
of Chicago
(to
be presented by J. Peterson
Univ.
of Carnegie Mellon, USA)
The
astrophysics effort at the South Pole from 1986 to the present
will be discussed. The emphasis will be on the practical
aspects of operation in the summer and winter.
1630 – 1645 The South Pole Thermal
IR Experiment
J.M.
Rathborne, M.G. Burton, M.C.B. Ashley and J.W.V. Storey
UNSW,
Australia
The
Antarctic plateau offers superior conditions on Earth for
observational astronomy. The cold, dry and thin atmosphere
is extremely stable, improving the sensitivity of infrared
(IR) and millimetre observations considerably over the best
temperate latitude sites. These unique conditions can be
utilised, in particular, to observe processes occurring
deep in molecular clouds in our galaxy. Continuum IR emission
and many molecular transitions from these processes are
normally `blocked' by the high precipitable water vapour
content and thermal background emission from the Earth's
atmosphere at temperate sites. The implementation of a thermal
IR imager on the Antarctic plateau would enable us to observe
these processes and uncover the deepest objects and intense
interactions occurring in star forming molecular cloud complexes.
The
60cm SPIREX/Abu telescope, located at the South Pole, was
the first prototype for the implementation of thermal IR
imager in Antarctica. Observations over two winter seasons
achieved remarkable high resolution, wide field images of
the star forming regions in the Carina nebula and NGC 6334.
These images reveal information crucial to understanding
star formation, and combined with ground- and space-based
observations of other wavelength regimes, allow us to obtain
a more complete picture of the star formation process. The
SPIREX project was a collaboration between the Joint Australian
Centre for Astrophysical Research in Antarctica (JACARA),
the Center for Astrophysical Research in Antarctica (CARA)
and the National Optical Astronomy Observatories (NOAO).
1645 – 1700 Polarimetry of the Cosmic
Microwave Background from the Antarctic Plateau
G.
Sironi, G. Boella, M. Gervasi, E. Battistelli, M. Zannoni,
A. Passerini
University
of Milano-Bicocca, Italy
Detection
of linear polarization at level of a part on a million,
or less, associated to the anisotropy of the Cosmic Microwave
Background will confirm the cosmological origin of the observed
anisotropy and provide information on the thermal history
of the Universe between the recombination epoch and now.
In particular the presence of polarization can help in deciding
if the evolution of the Universe included a reionization
epoch.
We
present the Mk-3 model of our correlation polarimeter, an
improved version of a system which has been already used
for observation of the region of sky around the South Celestial
Pole from Antarctica (in 1994 at Baia Terra Nova and in
1998 at Dome C).
1830 – 1930 Reception
at Government House, Hobart, at the invitation of The
Hon. Sir Guy Green, AC, KBE, Governor of Tasmania.
2000
Conference dinner at the Royal Yacht Club, Hobart
Friday 29 June 2001
New Instrumentation for
Antarctica I
0900 – 0920 The DASI 2000 campaign
J.
Carlstrom
University
of Chicago, USA
No
abstract available.
0920 – 0935 Science with Antarctic
Infrared and Sub-millimetre Telescopes
M.G.
Burton, J.W.V. Storey, M.C.B. Ashley
UNSW,
Australia
A
wealth of data has now established that the Antarctic plateau
provides the best ground-based site for a wide range of
programs in observational astronomy, particularly at infrared
and sub-millimetre wavelengths. The reduced sky background
means that at thermal infrared wavelengths a 2-m class telescope
has similar sensitivity to an 8-m telescope at temperate
sites. Moreover, it is considerably easier to undertake
wide-field imaging with the smaller telescope. These type
of considerations lead to the following focus areas for
Antarctic telescopes, whereby they could contribute to scientific
investigations not readily undertaken elsewhere:
*
Wide-field thermal infrared imaging
*
Continuous observations, particularly at 2.4 microns
*
Precision photometry
*
Mid-infrared interferometry
Examples
of the kind of science programs that could then be performed
include:
*
Star formation and the galactic ecology
*
Proto-galaxies and the earliest star formation
*
Micro-lensing towards the Galactic Centre
*
Exo-solar planets
*
Stellar seismology and tomography
This
talk will describe these focus areas and outline some of
the scientific possibilities that Antarctic telescopes make
available.
0935 – 0955 The Douglas Mawson Telescope
J.W.V.
Storey, M.G. Burton, M.C.B. Ashley
UNSW,
Australia
The
Douglas Mawson Telescope (DMT) is proposed as a 2-metre
diameter astronomical telescope to be located at Concordia
Station, Dome C, Antarctica. The high, dry, cold atmosphere
of Antarctica allows a modest facility to have a mid-infrared
sensitivity rivalling that of the largest telescopes at
other sites. With unprecedented wavelength coverage, the
DMT offers Australian astronomers a unique new capability.
Capable of operating at optical, infrared and submillimetre
wavelengths, the DMT will be a general purpose facility
able to host state-of-the-art instrumentation developed
collaboratively by the partners.
0955 – 1010 Optical Design for Antarctic
2 metre Telescope with Near IR Imager
P.
Gillingham
Anglo
Australian Observatory, Australia
A
preliminary study has been made of the performance to be
expected from a Ritchey Chrétien telescope with a 2 metre
diameter primary mirror imaging directly onto an array in
the K' and L infrared windows. With baffling inside the
dewar and Narcissus mirrors outside the dewar, extraneous
sky radiation can be kept low enough not to significantly
reduce sensitivity. With a single element field flattening
lens, near diffraction limited performance is attainable
across a 30 arcmin diameter field; for the smaller field
appropriate to a 2k square detector array, no field flattening
is needed.
1010 – 1030 AIRO: The Antarctic Infrared
Observatory
J.
Jackson
Boston
University, USA
The
Antarctic Infrared Observatory (AIRO) is a proposed 1.8
meter telescope deployed to the South Pole. Because the
mean annual temperature is -50 C, the thermal background
at the South Pole is 20-50 times smaller than at temperate
sites. This enormous advantage in thermal background translates
directly into increased sensitivity and observing speed.
AIRO's first instrument, AIROCAM, will make unique wide
field images in the largely unexplored 2.3 to 5.6 micron
waveband. Both the infrastructure and the technology are
in place now to field AIRO at the South Pole. The large
field of view and excellent sensitivity of AIRO are optimally
suited for the first deep, wide field surveys in the 2.3
to 5.6 micron waveband. With this unique capability, AIRO
will make important observations of high-redshift galaxies,
protoplanetary disks, brown dwarfs, evolved stars, and star-forming
regions. AIRO can also relentlessly monitor rapid time-variable
sources such as gravitational microlenses without interruption
for long periods of time. All important aspects of AIRO:
the telescope, camera, data pipeline, and time allocation,
have been prototyped and thoroughly tested at the South
Pole. Upgrades to mid-infrared, spectroscopic, or polarimetric
instruments can be implemented rapidly and relatively cheaply.
1030
– 1100 Coffee
New Instrumentation for
Antarctica II
1100 – 1120 The future of the IRAIT
project in the international collaboration for Dome C
M.
Busso
Osservatorio
Astronomico di Torino, Italy
We
present the status of the Italian project IRAIT (Italian
Robotic Antarctic Infrared Telescope) and we outline its
future developments, as they emerge after the agreement
for establishing an international collaboration between
Italy, Australia and France for exploiting the unique opportunities
offered by the site of Dome C to infrared Astronomy. We
then review some of the main scientific motivations, showing
how Antarctic infrared astronomy, even with telescopes of
moderate size, will be complementary to what can be obtained
by other facilities, in the era of space-born experiments
and of large ground-based telescopes.
1120 – 1135 A Mid-Infrared Imaging
Survey with IRAIT of star forming regions
P.
Persi
Istituto
Astrofisica Spaziale CNR, Italy
We
present a detailed project that can be developed with a
mid-IR camera attached at the 80 cm infrared telescope (IRAIT)
at DOME C. The project include a survey at 10 and 20 micron
of several giant molecular clouds ( i.e. NGC 6334, NGC 3603)
and dark clouds (i.e. Chamaeleon I, II and III). The high
sensitivity and the moderate spatial resolution that can
be obtained with IRAIT in the mid-IR will allow to give
a complete census of the young stellar population in these
regions, and to define their initial mass function.
1135 – 1150 Wide-Field mid-IR imaging
from the ground
M.
Robberto
ESA
/ STScI, USA
I
will discuss the potential and the limits of mid-IR (5-25
micron) imaging with large telescopes from the ground, in
particular in what concerns wide-field imaging. The constrains
related to the variable background, small chopping amplitudes,
pupil rotation, etc. will be discussed using examples taken
at the UKIRT telescope. I will present a new reconstruction
method enabling to recover the negative counterparts present
on chopped and nodded images and mosaics. Coupled to the
proper observational strategy, the algorithm has recently
allowed obtaining spectacular 10 and 20 micron images of
the Orion nebula. Alternative methods for wide-field imaging
at these wavelengths will also be mentioned.
1150 – 1210 Large scale IR surveys:
present status and future prospects in Antarctica
N.
Epchtein
Observatoire
de la Cote d'Azur, France
I
will briefly summarize some of the main astrophysical results
obtained by the exploitation of the new near-IR surveys
DENIS and 2MASS. Some key areas of astrophysics such as
the quest of very low mass stars and brown dwarfs, the census
of galaxies in the ZOA, or of extremely red stellar populations
in the bulge and the Magellanic Clouds require an extension
of these major surveys towards the still essentially unexplored
range between 3 and 10 microns. The Antarctic Plateau is
the only place on Earth where such a long term exploration
can be envisaged. The feasibility of this project using
the facilities in project at Dome C will be discussed.
1210 – 1230 Thermal Infrared Astronomy
from the Antarctic Plateau
D.
Harper
University
of Chicago, USA
During
winter on the Antarctic Plateau, the atmosphere becomes
transparent in windows which are normally inaccessible except
from the stratosphere or space, and the extreme cold reduces
the thermal background, significantly increasing observational
sensitivity. The principal advantage of Antarctic telescopes
operating in the thermal infrared is that they can provide
much higher angular resolution data than airborne or space
telescopes. In this talk, we discuss the scientific requirements
for ground-based thermal infrared telescopes, compare Antarctic
Plateau sites with high altitude sites in the Atacama Desert,
and discuss the prospects for construction of large Antarctic
telescopes in the coming decade.
1230
– 1400 Lunch
New Instrumentation for
Antarctica III
1400 – 1415 Antarctic Astronomy at
Dome C. The mid-IR Instrumentation
M.
Ferrari Toniolo
IAS-CNR,
Italy
A
General review of the optimised design of a mid-IR camera,
in the light of theoretical results expected and of the
analysis of particular aspects due to the site of operation
is presented.
Particular
emphasis is put in the creation of a prototype following
an iterative process of optimisation with the progressive
knowledge of all the parameters involved in the instrument.
The
described Camera will be the basic instrument for the small,
medium and future very large Telescope that we plan to develop
for Dome C. Robotisation of the instrument and of the measure.
The
case of the Very Large Infrared Antarctic Telescope of the
future will be examined.
1415 – 1430 IR Surveys for cosmology
in the NGST era
M.
Stiavelli
Space
Telescope Science Institute, USA
After
a brief introduction to the Next Generation Space Telescope
(NGST), the parameter space of ground based IR survey in
the era between the launch of SIRTF and that of NGST will
be discussed.
1430 – 1445 Using the DMT for Investigation
of Molecular Clouds
M.
Hunt
UNSW,
Australia
Observations
of molecular and atomic spectral-line transitions above
400-GHz with the DMT have the potential to shed new light
on the small-scale structure and physical conditions within
southern molecular clouds. Observations of the high J lines
of CO and other molecules will selectively find the high
density, high excitation gas surrounding newly formed stars,
and can be used to determine the physical conditions and
chemistry in these hot cores (Melnick et al. 2000). Observations
of gas-phase H2O and atomic C and O can be used to investigate
and model the interclump medium in dense molecular clouds
(Spaans & van Dishoeck 2001). Molecular clouds have
been found to be clumpy at all scales so far observed, and
the presence and nature of the interclump medium is predicted
to have a significant effect on the molecular abundances
and emergent line profiles. A survey of the millimetre and
submillimetre molecular line emission in southern dense
cores has been undertaken with the Mopra Telescope and the
SEST and will be used to select target molecular clouds
for investigation with the DMT at submillimetre wavelengths.
1445 – 1500 The Potential of the Antarctic
Plateau for Astrometric Interferometry
J.
Lloyd
University
of California, Berkeley, USA
Lower
boundary layer turbulence seriously degrades the seeing
at Antarctic Plateau sites from the superb free atmosphere
seeing. Despite the large gains available in the IR background
and transparency, the seeing removes much of the sensitivity
advantages Antarctic telescopes would have over mid-latitude
sites such as Mauna Kea or Paranal. The seeing at these
sites, while smaller in amplitude, is dominated by turbulence
at altitudes of 10-20km. The mean square error for an astrometric
measurement with a dual beam differential astrometric interferometer
in the very narrow angle regime is proportional to the integral
of h^2 C_n^2(h). Therefore, sites at which the turbulence
occurs only at low altitudes offer large gains in astrometric
precision. Science programs that would benefit greatly from
such an instrument include planet detection, microlensing
by dark matter candidates, studies of the mass and dynamics
of the galaxy, and fundamental astrophysical measurements
such as stellar properties and the cosmic distance scale.
1500 – 1530 Coffee
New Instrumentation for
Antarctica IV
1530
– 1545 MASTER: A Ttriple Heterodyne Receiver for Astronomy
in the Millimetre and Sub-Millimetre Domain
M.
Zannoni (1), E. Battistelli (1), G. Boella (1), M. Gervasi
(1), A. Passerini (1), G. Sironi (1), D. Andreone (2), L.
Brunetti (2), V. Lacquaniti (2), S. Maggi (2), R. Steni
(2), E. Natale (3), J. R. Thorpe (4)
(1)
Universita' degli Studi di Milano-Bicocca, Italy
(2)
Istituto Elettrotecnico Nazionale Galileo Ferraris, Italy
(3)
Oss. Astronfisico di Arcetri, Italy
(4)
University of Leeds, UK
A
system of three heterodyne receivers will be described.
The instrument is based on SIS (superconductor-insulator-superconductor)
tunnel junctions mixers which allow direct downconversion
from 94GHz, 225GHz and 345GHz to 1.5GHz, followed by IF
amplification.
This
instrument, coupled to a 2-4 meter dish and associated to
an Acusto Optical Spectrometer, can be used to study molecular
lines associated with astrophysical objects. Moreover the
three frequencies allow a complete study of the S-Z effect.
Current status of a 94GHz receiver, prototype of MASTER,
will also be described.
1545 – 1600 Optical coupling between
receivers and telescope: a study for MASTER
E.
Batistelli (1), G. Boella (1), M. Gervasi (1), A. Passerini
(1), G. Sironi (1), M. Zannoni (1),
E.
Natale (2)
(1)
Università di Milano-Bicocca, Italy
(2)
Osservatorio Astronomico di Arcetri, Italy
Optical
coupling between receivers and telescopes is one of the
key point forthe correct and sensible detection of Astrophysical
signals. At millimeter and sub-millimeter wavelengths, geometrical
optics doesn't hold anymore and a pure electromagnetic analysis
is difficult, time consuming and often impossible: our study
has thus been performed using gaussian beam (or quasioptical)
analysis which introduces wavelength corrections to geometrical
optics. It allows a deep control on the beam characteristics
in the optical system under test and permits to create an
ad hoc configurations for any system. A frequency independent
configuration has been studied for the optical coupling
between the 94GHz receiver prototype of MASTER and MITO
telescope on Italian Alps. An analogue configuration will
allow us to couple MASTER to any telescope.
1600 – 1615 MBI: a Bolometric Interferometer
for Dome C
L.
Piccirillo
Cardiff
University, UK
The
Millimeter-wave Bolometric Interferometer (MBI) is a novel
instrument under construction at Cardiff University. MBI
consists of 3 Cassegrain telescopes looking at three movable
flat mirrors. The beams from the telescopes are combined
in a cryogenic beam-combiner. The detectors are 3 arrays
of 3 by 3 spider web bolometers sensitive to intensity and
polarization. The maximum baseline of our first prototype
has been set to 4 meters giving a sub-arcmin resolution
at sub-millimeter wavelengths. We plan to take advantage
of the unique transparency of the Dome-C atmosphere to observe
at millimetric and sub-millimetric bands (2, 1, 0.85, 0.45
and 0.35 mm wavelengths)
1615 – 1630 A proposal for Solar Observations
at Dome C
P.
F. Moretti
Ossevatorio
Astronomico di Capodimonte, Italy
The
stability and thinness of the atmosphere, and the particular
weather conditions (very low wind and very dry air) make
the site of Dome C in Antarctica the best candidate on the
ground for obtaining high-spatial resolution observations
of the Sun for long periods of time. However, the effective
quality of the solar seeing at Dome C, i.e. the seeing during
the day and in the direction of Sun, is still to be assessed.
We
plan to install a 40 cm aperture telescope at Dome C, in
order to extract the characteristics of the solar seeing
at the site of the Concordia station, directly from both
high-resolution and full-disk solar images in different
spectral ranges. This contribution discusses the main points
of the project, i.e. the instrumentation, the constrains
of its Antarctic location, and the science that can be done
from the data. The telescope will be open to be used as
an international facility for solar observations.
1630 – 1645 The Geoelectric Circuit
and a need for Antarctic Plateau sites
G.
Burns
Australian
Antarctic Division, Australia
Global
thunderstorm activity maintains a variable potential difference
of the order of 250 kV between the quasi-equipotentials
of the lower reaches of the ionosphere and the Earth. Under
'fair-weather' conditions a downward current of ~3 pA/m2
and a geoelectric field of order 100-200 V/m can be measured
at ground level. The time constant of this global circuit
is ~20 minutes, thus by monitoring the 'fair-weather' field
it is possible to measure the globally integrated electrical
intensity of thunderstorm activity.
Meteorological
influences are a major hindrance to useful ground-based
measurements of the geoelectric circuit. Conditions suitable
for optical astronomy are generally advantageous for geoelectric
field measurements. The high altitude, clear skies and generally
low wind speeds of the polar plateau are ideal.
Additionally,
in polar regions, the interaction of the solar wind and
the Earth's magnetic field imposes an ionospheric convection
pattern of variable form and intensity, generally with a
dawn-to-dusk, cross-polar cap potential difference in the
range 20 to 60 kV.
Using
measurements made at Vostok, Antarctica (78.5S. 107E) we
have been able to statistically demonstrate the influence
of global thunderstorm activity and solar wind on the vertical
geoelectric field measured at ground level. In this talk
we will show how by additionally measuring the air-earth
current and making measurements at more than one Antarctic
polar plateau site, we will be able to separate these contributing
influences on individual days.
1645 – 1700 Possible Cosmic Ray Experiments
at Dome C
M.
Duldig
Australian
Antarctic Division, Australia
The
high altitude Dome C site offers excellent prospects for
cosmic ray observations at low to moderate energies. A neutron
monitor, based on the standard NM64 counter or on the new
Helium counter technology could be an important addition
to the worldwide monitor network. An in-ice high zenith
angle muon telescope could be installed using ice as the
absorber. The system would observe at depths greater than
the Mawson underground system and would thus be complimentary
to it. Design considerations and descriptions of the research
that could be addressed by both instruments will be presented.
1700
– 1730 Final Discussion and wrap-up.
1830 Wine tasting of fine Tasmanian wines, venue
TBA.
Saturday 30 June 2001
Tour of TIGER Ionospheric Radar.
Last update: 13 June 2001
