Results 181 to 190 of about 52,995 (203)

The Interstellar Reddening and Metallicity of NGC 330

Symposium - International Astronomical Union, 1991
A reddening of E(B-V) = 0.12 ± 0.02 has been determined for NGC 330 in the Small Magellanic Cloud (SMC) from spectrophotometry of B stars in the cluster. This high reddening helps explain many of the anomalous low metallicity estimates for the cluster. Preliminary analysis of Coudé spectra of K giants in the cluster indicates a high value of 3.5 to 4.5
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The interstellar reddening in front of globular clusters.

Publications of the Astronomical Society of the Pacific, 1975
We have observed 187 field stars in galactic fields containing globular clusters. For 15 of the 28 fields, we derive color excesses that should be essentially the same as for the globular clusters. Three additional cases deserve further work. The remaining ten fields are at low galactic latitude.
D. L. Crawford, J. V. Barnes
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On interstellar reddening law in the Taurus dark clouds

Astrophysics and Space Science, 1982
The interstellar reddening law in the Taurus dark clouds is investigated from visual, infrared, and ground based ultraviolet photometric observations of heavily reddened stars HD 29647, HDE 283701, and HDE 283812. The star HD 29647 located in the center of a very dense dark cloud Khavtassi 278 shows a reddening law which is anomalous in the wavelengths
V. Straižys, W. Z. Wisniewski, M. J. Lebofsky   +2 more
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Interstellar reddening in the direction of the globular cluster M71

Astrophysics and Space Science, 1984
Interstellar reddening as a function of distance in the direction of the globular cluster M71 is determined by two-dimensional quantification of 96 foreground stars observed in the Vilnius photometric system. In concentric areas with the radii 30′ and 10′ centered on the cluster the reddening shows the same variations ranging fromEB-V=0.12 to 0.32. The
R. Janulis, V. Straižys
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Interstellar Reddening at High Galactic Latitudes

Symposium - International Astronomical Union, 1973
Measures in the Strömgren four-color and Hβ systems provide an accurate way to determine color excesses of early-type stars. Fourteen areas at high galactic latitude have now been searched for faint A stars which are then measured photoelectrically to obtain the color excesses.
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Bandwidth effects on interstellar reddening and on theR-ratio

Astrophysics and Space Science, 1985
The energy distributions of 85 stars were combined with the transmittance ofB andV tilters and with an interstellar reddening law in order to investigate the effects of the bandwidth on the colour excess and on the ratioR=Av/E(B-V). Since these depend both on the stellar spectral type and on the quantity of absorbing matter, corrective formulae are ...
B. Cester, C. Marsi
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Interstellar reddening and distance of Nova Cygni 1978

Nature, 1979
THE interstellar feature of KI (λ7699 A) has been observed in the direction of Nova Cygni 1978 with an equivalent width of Wλ≃116 mA and has been used here to deduce a colour excess of E(B−V) = 0.38 ± 0.08 mag. The distance–reddening law to the nova is derived from a sample of stars in the nearby field surrounding the nova.
MARK H. SLOVAK, STEVEN S. VOGT
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Studies of interstellar reddening

2018
The wavelength dependence of interstellar obscuration, in magnitudes against reciprocal wavelength, is known to be well represented, over the visible part of the spectrum, by two straight lines intersecting at or near the broad interstellar absorption band at 4430A. The existing measures, obtained principally from low dispersion objective prism spectra,
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Interstellar reddening in the galaxy

2019
Objective prism spectra obtained with the 16/24/60-inch Schmidt telescope have been used for an investigation of the wavelength dependence of interstellar absorption in the spectral range from 8000A to 3450A, in a region of 30 square degrees in Cygnus centred on (20ʰ15ᵐ, 38 °).
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The absorption feature at 2200 � in the interstellar reddening curve

Astrophysics and Space Science, 1972
The profile of the absorption feature at 2200 A has been calculated for model grains of graphite, graphite core-dirty ice mantle and silicate. They are compared with the observed profile obtained by Bless and Savage from a number of early type stars. We have also shown that it is unlikely that the radiation damage of silicates in Interstellar Space can
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