Results 191 to 200 of about 1,020 (216)
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Interstellar reddening of del Cep.
Publications of the Astronomical Society of the Pacific, 1976K A Feltz
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A New, Large-scale Map of Interstellar Reddening Derived from H i Emission [PDF]
Astrophysical Journal, 2017 We present a new map of interstellar reddening, covering the 39% of the sky with low HI column densities (N_(HI) < 4 × 10^(20) cm^(−2) or E(B−V) ≈ 45mmag) at 16.′1 resolution, based on all-sky observations of Galactic HI emission by the HI4PI Survey.
D Lenz +2 more
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Interstellar reddening information system
Astronomische Nachrichten, 2013AbstractWe describe an electronic bibliographic information system, based on a card catalog, containing some 2500 references (publications of 1930–2009) on interstellar extinction. We have classified the articles according to their content. We present here a list of articles devoted to two categories: maps of total extinction and variation of ...
V.I. Burnashev +2 more
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The Interstellar Reddening and Metallicity of NGC 330
Symposium - International Astronomical Union, 1991A 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, 1975We 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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Bandwidth effects on interstellar reddening and on theR-ratio
Astrophysics and Space Science, 1985The 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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On interstellar reddening law in the Taurus dark clouds
Astrophysics and Space Science, 1982The 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 +2 more
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Interstellar reddening in the direction of the globular cluster M71
Astrophysics and Space Science, 1984Interstellar 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, 1973Measures 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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Interstellar reddening and distance of Nova Cygni 1978
Nature, 1979THE 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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