Zodiacal dust properties as deduced by inversion of iras observations

Levasseur-Regourd, Anny-Chantal; Dumont, René

doi:10.1007/bfb0118786

Cited by 9 publications

(18 citation statements)

References 7 publications

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“…This gives us further confidence that we have no serious source of systematic error in the calibration of our sky brightness values. (We do note, however, that Levasseur-Regourd and Dumont (1980) found 108 S 10 (V) for the zodiacal light at our mean ecliptic coordinates.) Garstang's (1989) Eqs.…”

Section: Discussioncontrasting

confidence: 49%

Optical Night-Sky Brightness at Mauna Kea over the Course of a Complete Sunspot Cycle

Krisciunas¹

1997

PASP

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ABSTRACT. We have produced a database of V band and B band night-sky brightness measurements rather evenly spread out over the course of a whole sunspot cycle from September 1985 to August 1996. Almost all the data were obtained at the 2800-m level of Mauna Kea using the same telescope, same photomultiplier tube, filters, and diaphragm, thus minimizing various sources of systematic error and allowing an estimate of the sources of random error. The yearly V band averages of observed sky brightness ranged from 21.287 to 21.906 magnitudes per square arcsecond. The color of the sky is B -V = 0.930 and does not change discemibly over the course of the sunspot cycle. After correcting the V band data to the zenith, we find that the airglow component varied a factor of 4.5 over the course of the solar cycle. Once the 11 -yr solar cycle effect is removed from the data, the most significant contribution to the scatter of individual data points appears to be the short-term variations on time scales of tens of minutes like those observed by the Whole Earth Telescope Project.

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Section: Discussioncontrasting

confidence: 49%

Optical Night-Sky Brightness at Mauna Kea over the Course of a Complete Sunspot Cycle

Krisciunas¹

1997

PASP

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“…For each target, it is assumed that the observation occurs at the time of the year when the zodiacal background is minimal, which is about 40 days before or after opposition for most targets. The resulting zodiacal background, derived from Levasseur-Regourd & Dumont (1980), is a function of ecliptic latitude, and ranges from m V ¼ 23:28 (ecliptic poles) to m V ¼ 22:24 (ecliptic equator).…”

Section: Zodiacal Lightmentioning

confidence: 99%

Theoretical Limits on Extrasolar Terrestrial Planet Detection with Coronagraphs

Guyon¹,

Pluzhnik²,

Kuchner³

et al. 2006

ASTROPHYS J SUPPL S

308

269

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Many high-contrast coronagraph designs have recently been proposed. In this paper, their suitability for direct imaging of extrasolar terrestrial planets is reviewed. We also develop a linear algebra based model of coronagraphy that can both explain the behavior of existing coronagraphs and quantify the coronagraphic performance limit imposed by fundamental physics. We find that the maximum theoretical throughput of a coronagraph is equal to 1 minus the nonaberrated noncoronagraphic PSF of the telescope. We describe how a coronagraph reaching this fundamental limit may be designed, and how much improvement over the best existing coronagraph design is still possible. Both the analytical model and numerical simulations of existing designs also show that this theoretical limit rapidly degrades as the source size is increased: the ''highest performance'' coronagraphs, those with the highest throughput and smallest inner working angle (IWA), are the most sensitive to stellar angular diameter. This unfortunately rules out the possibility of using a small IWA (

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“…First, the images were divided by a normalized median combination of 16 twilight exposures to remove the basic instrumental response. Significant structure was left because of the color difference between the blue twilight sky and the yellow zodiacal light dominating the '' dark '' sky near the Pleiades (Levasseur-Regourd & Dumont 1980;Schoening 1992). As a second correction, each field was divided by a 3 -clipped median average of 13 dark-sky fields taken away from the cluster during nights 1 and 2.…”

Section: Initial Reductionmentioning

confidence: 99%

The Pleiades Reflection Nebula. I. Ultraviolet, Optical, and Far‐Infrared Imaging Photometry

Gibson

Nordsieck²

2003

ApJ

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We present new wide-field optical and ultraviolet images of the Pleiades reflection nebula that allow a more thorough evaluation of the dust scattering than any prior data set. Vacuum-UV images were taken at 1650 and 2200 Å during the first flight of the Wide-Field Imaging Survey Polarimeter (WISP), a sounding rocketborne telescope. WISP captured the brighter parts of the nebula at both wavelengths, with 3 sensitivities of 22.5 and 23.4 UV mag arcsec À2 , respectively. The 5=0 Â 1=7 WISP field was also mapped at 4400 Å with a mosaic of 40 Burrell Schmidt CCD frames using a broadband B J filter. The Schmidt mosaic shows extensive and intricate nebulosity down to a 5 sensitivity limit of 27.6 B mag arcsec À2 , including features undetected by photographic surveys. We explore the intensity and color behavior of the nebula in our UV and optical images and far-infrared IRAS data. We find that the photometric structure near bright stars is more complex than previous studies have implied, but general trends are still apparent. The color gradients around the stars are caused by phase function effects rather than internal reddening. The greater concentration of scattered light versus thermal emission indicates that most of the observed scattering is from foreground dust. A somewhat greater concentration of UV versus optical light suggests grain scattering is more forward-directed at shorter wavelengths. The UV nebula is much fainter than expected from the stellar photometry and interstellar reddening. Explaining this UV faintness requires either more reddening than is measured or significant alterations to current dust property estimates.

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Zodiacal dust properties as deduced by inversion of iras observations

Cited by 9 publications

References 7 publications

Optical Night-Sky Brightness at Mauna Kea over the Course of a Complete Sunspot Cycle

Optical Night-Sky Brightness at Mauna Kea over the Course of a Complete Sunspot Cycle

Theoretical Limits on Extrasolar Terrestrial Planet Detection with Coronagraphs

The Pleiades Reflection Nebula. I. Ultraviolet, Optical, and Far‐Infrared Imaging Photometry

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