&lt;title&gt;Precision Radial Velocities And Residual Problems With Reticon Arrays&lt;/title&gt;

Campbell, B.; Walker, G. A. H.; Johnson, R.; Lester, T.; Yang, Sean; Auman, J. R.

doi:10.1117/12.965863

Cited by 7 publications

(5 citation statements)

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“…The heliocentric systemic velocity of NGC 5882 derived from our modeling is 12^4 km s~1, which is comparable to values found by previous authors : 9.8 (Bianchi 1992) and 7.7 km s~1 (Campbell et al 1981). However, Acker (1978) quotes 21 km s~1 for this object.…”

Section: Kinematicssupporting

confidence: 79%

Knots in the Outer Shells of the Planetary Nebulae IC 2553 and NGC 5882

Corradi

Gonçalves

Villaver

et al. 2000

ApJ

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We present images and high-resolution spectra of the planetary nebulae IC 2553 and NGC 5882. Spatiokinematic modeling of the nebulae shows that they are composed of a markedly elongated inner shell and of a less aspherical outer shell expanding at a considerably higher velocity than the inner one. Embedded in the outer shells of both nebulae are found several low-ionization knots. In IC 2553, the knots show a point-symmetric distribution with respect to the central star : one possible explanation for their formation is that they are the survivors of preexisting point-symmetric condensations in the asymptotic giant branch wind, a fact that would imply a quite peculiar mass-loss geometry from the giant progenitor. In the case of NGC 5882, the lack of symmetry in the distribution of the observed lowionization structures makes it possible that they are the result of in situ instabilities. Subject headings : ISM : jets and outÑows È ISM : kinematics and dynamics È planetary nebulae : individual (IC 2553, NGC 5882)

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Section: Kinematicssupporting

confidence: 79%

Knots in the Outer Shells of the Planetary Nebulae IC 2553 and NGC 5882

Corradi

Gonçalves

Villaver

et al. 2000

ApJ

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“…This result has been achieved even though we have made no attempt to correct for variable high-frequency components to the dispersion relation (cf. Campbell et al 1981). While the sample is small, this does suggest that nightto-night systematic errors are probably less than random errors for individual spectra.…”

Section: Observations Of Procyon With the Hf Techniquementioning

confidence: 86%

Precision radial velocities

Campbell

1983

PASP

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A number of techniques for determining stellar radial velocities with a precision better than 100 m s -1 are now becoming available. These will find application in a variety of programs, including the study of low-amplitude pulsating stars, or searches for stellar oscillations, starspots, or extra-solar planetary systems. Oscillations or spot effects will very likely limit the ultimate precision for planet search programs to about 1ms -1 .Three types of precision velocity techniques have been proposed, using for wavelength reference either telluric lines, Fabry-Perot fringes, or lines generated in an absorption cell. We have used the latter technique, with a hydrogen fluoride cell, to obtain time series observations of Procyon on three nights. The internal error in these velocities is 10 m s 1 , and the mean night-to-night difference is about 6 m s -1 . These results suggest that the HF technique has good long-term stability, and therefore can be applied to the search for sub-stellar mass companions to solar-type stars.

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“…The principal advantages of the diode arrays for optical spectroscopy are their geometrical stability and their very high quantum efficiencies at visible and near-infrared wavelengths because of the lack of an electrode structure over the photosensitive junction. Campbell et al (1981) have reported radial-velocity measurements accurate to ± 15 m s" 1 at a dispersion of 10 Â mm -1 , an accuracy corresponding to ~ 2 X 10" 2 of a 15-micronwide diode. However, measurements to this level of accuracy require an accurate determination of the high frequency structure of the spatial linearity of the diodes along the array.…”

Section: A Silicon Diode Arraysmentioning

confidence: 98%