Inversion of Fabry-Perot CCD images: use in Doppler shift measurements

1989 ◽  
Vol 28 (16) ◽  
pp. 3382 ◽  
Author(s):  
Vincent J. Abreu ◽  
Wilbert R. Skinner
Keyword(s):  
Doppler Shift ◽  
Fabry Perot

Fabry-Perot Velocimetry Techniques: Is Doppler Shift Affected By Surface Normal Direction?

1984 ◽  
Author(s):  
David R. Goosman ◽  
Alan M. Frank, ◽  
Henry H. Chau ◽  
Norval L. Parker
Keyword(s):  
Doppler Shift ◽  
Normal Direction ◽  
Surface Normal ◽  
Fabry Perot

The LPL Radial Accelerometer

1984 ◽  
Vol 88 ◽  
pp. 63-86 ◽  
Author(s):  
R.S. McMillan ◽  
P.H. Smith ◽  
J.E. Frecker ◽  
W.J. Merline ◽  
M.L. Perry
Keyword(s):  
Optical Fiber ◽  
Radial Velocity ◽  
Doppler Shift ◽  
Focal Plane ◽  
Incident Light ◽  
The Sun ◽  
Stellar Spectrum ◽  
Entrance Aperture ◽  
Fabry Perot ◽  
Interference Order

AbstractWe have begun to observe radial velocities of stars with an optical spectrometer designed for unusually high accuracy. Light from a star image in the focal plane of a telescope is fed to the entrance aperture of the spectrometer by a single optical fiber. Wavelengths are calibrated by transmission of collimated light through a tilt-tunable Fabry-Perot interferometer. The scrambling of incident light rays by the optical fiber and the intrinsic stability of the Fabry-Perot etalon provide immunity to the sources of systematic errors that plague conventional radial velocity meters. The spectrum is dispersed by an echelle grating crossed with another plane reflection grating. Several echelle orders in the vicinity of 4250-4600 Å are imaged in a two-dimensional format on a charge-coupled (CCD) array of detectors. About 350 distinct points on the profile of the stellar spectrum are sampled by successive orders of interferometrie transmission through the etalon. In the vicinity of 4300 Å each interference order is 47 milliangstroms wide and the sample points are 0.64 Å apart, resulting in distinct , widely-spaced monochromatic images of the entrance aperture to be formed in the focal plane of the camera. Changes in Doppler shift cause changes in the relative intensities of these images, according to the slope of the spectral profile at each point sampled. The instrument is being operated as a null-measurement accelerometer, sensitive only to changes in radial velocity, which simplifies operation and enhances sensitivity. With an argon-filled, iron hollow cathode emission line lamp, the interferometer can be calibrated to two parts in 100 million; this corresponds to ± 6 meters/sec in Doppler shift. Calibrations of the interferometer show variations of ± 27 meters/sec on a time scale of months; observations of stars are corrected for such changes. The internal repeatability of observations of the differential Doppler shift of light from the integrated disk of the Sun is ± 6 meters/sec. The corresponding result from about 70 observations of Arcturus (Kl IIIb; B=1.19) is ± 40 meters/sec internal repeatability for each exposure of 20 square-meter seconds. The external repeatability (day-to-day differential accuracy) of nightly averages of stellar observations is ± 20 meters/second. Since the internal precision on the sun and the argon lamp is much better than it is with short exposures on Arcturus, the quality of our observations of stars is limited by the rate of detected photons. This justifies averaging a number of short exposures of a star to approach “laboratory” precision.

scholarly journals Laser Doppler shift measuring method based on phase modulater and Fabry-Perot interferometer

2013 ◽  
Vol 62 (18) ◽  
pp. 184206
Author(s):  
Du Jun ◽  
Zhao Wei-Jiang ◽  
Qu Yan-Chen ◽  
Chen Zhen-Lei ◽  
Geng Li-Jie
Keyword(s):  
Doppler Shift ◽  
Measuring Method ◽  
Laser Doppler ◽  
Fabry Perot

A Fabry-Perot Interferometer For Accurate Measurement Of Temporal Changes In Stellar Doppler Shift.

1986 ◽  
Author(s):  
R. S. McMillan ◽  
P. H. Smith ◽  
J. E. Frecker ◽  
W. J. Merline ◽  
M. L. Perry
Keyword(s):  
Doppler Shift ◽  
Temporal Changes ◽  
Fabry Perot

Detection at a distance of laser-generated ultrasound using a confocal Fabry–Perot interferometer

1986 ◽  
Vol 64 (9) ◽  
pp. 1320-1323 ◽  
Author(s):  
Jean-Pierre Monchalin
Keyword(s):  
Laser Pulse ◽  
Doppler Shift ◽  
Steel Plate ◽  
Solid Sample ◽  
Experimental Results ◽  
Fabry Perot ◽  
Frequency Stabilized Laser

A novel scheme to detect ultrasonic motion at the surface of a solid sample is presented. The surface of the sample is illuminated by a frequency-stabilized laser and the light scattered by the surface is received by a confocal Fabry–Perot interferometer, which demodulates the Doppler shift produced by ultrasound. Experimental results, obtained at a distance of 1.5 m from a machined but not polished steel plate, and excited by ultrasound produced by a laser pulse, are presented.

scholarly journals A long-term radial velocity program of high accuracy with a small telescope

1986 ◽  
Vol 118 ◽  
pp. 459-460
Author(s):  
R. S. McMillan ◽  
P. H. Smith ◽  
J. E. Frecker ◽  
W. J. Merline ◽  
M. L. Perry
Keyword(s):  
Radial Velocity ◽  
Doppler Shift ◽  
Incident Light ◽  
Systematic Errors ◽  
Stellar Spectrum ◽  
Differential Doppler ◽  
Fabry Perot ◽  
The Stability ◽  
Interference Order

We are making accurate observations of the change in Doppler shift of stellar absorption lines. The purpose is to detect the oscillatory reflex motion due to planets orbiting stars. The scrambling of incident light by an optical fiber and the stability of wavelength calibration by a Fabry-Perot etalon provide immunity to systematic errors. Selecting several echelle diffraction orders in the vicinity of 4250–4600 A, which are imaged on a CCD, about 350 points on the profile of the stellar spectrum are sampled by successive orders of interferometric transmission through the etalon. At 4300 A each interference order is 47 milliangstroms wide and the sample points are 0.64 A apart, causing distinct, widely-spaced monochromatic images of the entrance aperture to be formed in the focal plane of the camera. Changes in Doppler shift modify the relative intensities of these images, according to the slope of the spectral profile at each point sampled. To simplify operation and enhance sensitivity, the instrument is being operated as a null-measurement accelerometer, responding only to changes in radial velocity. With an argon emission line lamp the interferometer is calibrated to two parts in 100 million; this corresponds to ± 6 meters/sec in Doppler shift. These calibrations show instrumental variations of ± 27 meters/sec on a time scale of months; observations of stars are corrected for such changes. The internal repeatability of observations of the differential Doppler shift of Arcturus (K1 IIIb; B=1.19) is ± 6 meters/sec for each exposure of 600 square meter-seconds. These exposures are obtained in 15–20 minutes with a 0.9-meter telescope. The external repeatability (day-to-day differential accuracy) of nightly averages of stellar observations is ± 20 meters/second.

scholarly journals Astro-comb: revolutionizing precision spectroscopy in astrophysics

2008 ◽  
Vol 4 (S253) ◽  
pp. 499-501
Author(s):  
Claire E. Cramer ◽  
Chih-Hao Li ◽  
Andrew J. Benedick ◽  
Alexander G. Glenday ◽  
Franz X. Kärtner ◽  
...  
Keyword(s):  
Doppler Shift ◽  
Extrasolar Planets ◽  
Frequency Comb ◽  
Laser Frequency ◽  
Spectral Lines ◽  
Resolving Power ◽  
Long Term Stability ◽  
Fabry Perot ◽  
Line Spacing ◽  
Wide Line

AbstractSearches for extrasolar planets using the periodic Doppler shift of stellar spectral lines have recently achieved a precision better than 60cm/s. To find a 1-Earth mass planet in an Earth-like orbit, a precision of 5cm/s is necessary. The combination of a laser frequency comb with a Fabry-Perot filtering cavity has been suggested as a promising approach to achieve such Doppler shift resolution via improved spectrograph wavelength calibration. Here we report the fabrication of such a filtered laser comb with up to 40 GHz (~1 Angstrom) line spacing, generated from a 1 GHz repetition-rate source, without compromising long-term stability, reproducibility or spectral resolution. This wide-line-spacing comb (astro-comb) is well matched to the resolving power of high-resolution astrophysical spectrographs. The astrocomb should allow a precision as high as 1cm/s in astronomical readial velocity measurements.

Long-term stability of a Fabry-Perot interferometer used for measurement of stellar Doppler shift

1990 ◽  
Author(s):  
Robert S. McMillan ◽  
Peter H. Smith ◽  
Marcus L. Perry ◽  
T. L. Moore ◽  
William J. Merline
Keyword(s):  
Doppler Shift ◽  
Term Stability ◽  
Long Term Stability ◽  
Fabry Perot
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