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Infrared Imaging with COAST
John Stephen Young
St John's College, Cambridge
and
Cavendish Astrophysics
A dissertation submitted for the degree of
Doctor of Philosophy in the University of Cambridge
26 March 1999
See below to download the thesis, or to use
the bibliography with hyperlinks.
The first optical/IR aperture synthesis image from separated
telescopes was made at visible wavelengths, in
1995 (Baldwin et al. 1996), using the Cambridge Optical
Aperture Synthesis Telescope (COAST). COAST is the first optical
interferometer specifically designed to produce images, by measuring
closure phase as well as visibility amplitude.
COAST was designed to work at visible wavelengths. The aim of this
project was to add the capability of imaging at near-infrared
wavelengths, following on from the work of Beckett. The
project was made possible by the arrival of new detector technology,
discussed in Chapter 2.
This work describes the problems encountered in modifying COAST to
operate as an imaging telescope in the near-infrared, and the
solutions employed in overcoming these problems. Many of the solutions
have more general applications in interferometry.
The effectiveness of the solutions is clearly demonstrated by the
number of astronomical results obtained with the working COAST IR
system. These results, described in Chapters 5-8, include
high-quality images of Capella and Betelgeuse, and a large number of
diameter measurements of Mira variables. The astrophysical
implications of these results, combined with high angular resolution
observations at visible wavelengths, are also discussed.
Chapter 2 is a brief review of the principles of operation
of modern infrared array detectors, required in order to follow the
discussion in later chapters.
Chapter 3 describes the optical systems of a typical stellar
interferometer, with particular emphasis on beam-combining schemes
which could be used at infrared wavelengths. The relative merits of
the different schemes when a noisy detector is used are discussed.
The pupil plane beam combiner chosen for IR operation at COAST is
described, as are the fundamental problems in aligning such a
system. Possible solutions to these problems are discussed,
including the methods finally adopted at COAST. These procedures
have been used at COAST to accurately align the four-way IR beam
combiner and maintain its alignment throughout the observing
season.
Chapter 4 discusses the readout mode used for the NICMOS3
camera at COAST to sample pupil plane fringes at up to 2.5 kHz. The
functionality of the software used to control the NICMOS array and
store fringe data is described.
Chapter 5 describes the procedures used when observing with
COAST in the infrared, illustrated by observations of the binary
star Capella. I discuss the methods for extracting visibility
amplitudes and closure phases from the raw data, and subsequently
using them to reconstruct an image of the astronomical target.
Chapter 6 is concerned with contemporaneous high resolution
imaging of the M-type supergiant star Betelgeuse in a number of
wavebands from 0.7-1.3 micron, performed with COAST, and with the
William Herschel Telescope by the technique of non-redundant
masking. The implications for the possible origin of the
"hotspots" frequently detected on Betelgeuse are discussed.
Chapter 7 presents the results of a programme to
monitor the angular diameter of the Mira variable star
chi Cygni. This programme was carried out with COAST and the
William Herschel Telescope, over a period of 17 months.
Chapter 8 describes a programme to make near-continuum
(1.3 micron) diameter measurements of a sample of Mira variables
with COAST, and the implications of the measurements for the
effective temperatures, physical diameters and pulsation modes of
the sample stars.
Chapter 9 is a summary of the most important ideas from each
chapter. Developments planned for the IR instrumentation at COAST
are discussed, with suggestions for future astronomical programmes.
The thesis is available as a PDF file (2.4Mb), a single PostScript file (6.7 Mb), or as a number
of smaller PostScript files, one for each chapter:
Please note that the thesis is formatted for A4 paper.
Below is a version of the bibliography with links to the text of
most of the cited articles.
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Mon. Not. R. astr. Soc., 287, 955-960, 1997.
- W. Wamsteker.
Standard stars and calibration for JHKLM photometry.
Astron. Astrophys., 97, 329-333, 1981.
- G. Weigelt,
Y. Balega, K.-H. Hofmann, and M. Scholz.
First diffraction-limited speckle masking observations of the Mira
variable R Cas with the 6m SAO telescope.
Astron. Astrophys., 316, L21-L24, 1996.
- P. A. Whitelock,
J. W. Menzies, M. W. Feast, F. Marang, B. S. Carter, G. Roberts, R. M.
Catchpole, and J. Chapman.
High-mass-loss AGB stars in the South Galactic Cap.
Mon. Not. R. astr. Soc., 267, 711-742, 1994.
- R. W. Wilson, J. E.
Baldwin, D. F. Buscher, and P. J. Warner.
High-resolution imaging of Betelgeuse and Mira.
Mon. Not. R. astr. Soc., 257, 369-376, 1992.
- R. W. Wilson, V. S.
Dhillon, and C. A. Haniff.
The changing face of Betelgeuse.
Mon. Not. R. astr. Soc., 291, 819-826, 1997.
(PostScript)
- B. Wirnitzer.
Bispectral analysis at low light levels and astronomical speckle masking.
J. Opt. Soc. Am. A, 2, 14-21, 1985.
- G. Woan and
P. J. Duffett-Smith.
Determination of closure phase in noisy conditions.
Astron. Astrophys., 198, 375-378, 1988.
- P. R. Wood.
Pulsation and evolution of Mira variables.
In M. O. Mennessier and A. Omont, editors, From Miras to Planetary
Nebulae: Which Path for Stellar Evolution, pages 67-84,
Gif-sur-Yvette, 1990. Editions Frontières.
- S. P. Wyatt and J. H. Cahn.
Kinematics and ages of Mira variables in the greater solar
neighborhood.
Astrophys. J., 275, 225-239, 1983.
- A. Ya'ari and
Y. Tuchman.
Long-term nonlinear thermal effects in the pulsation of Mira
variables.
Astrophys. J., 456, 350-355, 1996.
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John Young
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