An anomalous ultraviolet extinction curve in the Taurus dark cloud

1980 ◽  
Vol 242 ◽  
pp. L83 ◽  
Author(s):  
T. P., Jr. Snow ◽  
C. G. Seab
Keyword(s):  
Extinction Curve ◽  
Dark Cloud ◽  
Ultraviolet Extinction

An ultraviolet extinction study of the rho Ophiuchi dark cloud

1980 ◽  
Vol 241 ◽  
pp. 173 ◽  
Author(s):  
C.-C. Wu ◽  
D. P. Gilra ◽  
R. J. van Duinen
Keyword(s):  
Dark Cloud ◽  
Ultraviolet Extinction ◽  
Rho Ophiuchi

The Ultraviolet Extinction Curve for Circumstellar Dust Formed in the Hydrogen‐poor Environment of V348 Sagittarii

1997 ◽  
Vol 476 (2) ◽  
pp. 865-869 ◽  
Author(s):  
John S. Drilling ◽  
James H. Hecht ◽  
Geoffrey C. Clayton ◽  
Janet Akyuz Mattei ◽  
Arlo U. Landolt ◽  
...  
Keyword(s):  
Extinction Curve ◽  
Circumstellar Dust ◽  
Ultraviolet Extinction

scholarly journals Ultraviolet photometry of stars from OSO II

1970 ◽  
Vol 36 ◽  
pp. 139-139
Author(s):  
Kenneth L. Hallam
Keyword(s):  
Wide Band ◽  
Extinction Curve ◽  
Magnitude Effect ◽  
Flux Measurements ◽  
Ultraviolet Extinction ◽  
Good Agreement

Ultraviolet stellar fluxes from 1500 to 3200 Å were from February through August 1965 on OSO II. A 15-cm diameter Gregorian telescope with a stepped grating spectrophotometer provided flux measurements in ten adjacent 180 Å wide band passes.By comparing fluxes of stars showing B-U color excesses smaller than 0.19 and larger than 0.26, an ultraviolet extinction curve has been derived, which agrees with others which have been published as far as the magnitude effect is concerned, but the shape differs somewhat, the slope at 1/λ = 3.8 μ−1 being somewhat greater than at 1/λ = 5.0 μ−1.If the stars' fluxes are corrected for reddening, it is found that there is a good agreement between observation and models for stars earlier than B3, but that many of the later type stars have a residual apparently intrinsic reddening.

A New Measurement of the Average Far‐Ultraviolet Extinction Curve

2002 ◽  
Vol 566 (1) ◽  
pp. 267-275 ◽  
Author(s):  
T. P. Sasseen ◽  
M. Hurwitz ◽  
W. V. Dixon ◽  
S. Airieau
Keyword(s):  
Extinction Curve ◽  
Ultraviolet Extinction ◽  
Far Ultraviolet

scholarly journals The Ultraviolet Extinction Curve of Intraclump Dust in Taurus (TMC‐1): Constraints on the 2175 A Bump Absorber

2004 ◽  
Vol 602 (1) ◽  
pp. 291-297 ◽  
Author(s):  
D. C. B. Whittet ◽  
S. S. Shenoy ◽  
Geoffrey C. Clayton ◽  
Karl D. Gordon
Keyword(s):  
Extinction Curve ◽  
Ultraviolet Extinction

Morphology and Energetics of the Molecular Gas within a Core and a Diffuse Region in the Filamentary Dark Cloud GF 9

2000 ◽  
Vol 120 (1) ◽  
pp. 393-406 ◽  
Author(s):  
David R. Ciardi ◽  
Charles E. Woodward ◽  
Dan P. Clemens ◽  
David E. Harker ◽  
Richard J. Rudy
Keyword(s):  
Molecular Gas ◽  
Dark Cloud ◽  
Diffuse Region

Polarimetric and photometric observations of CB54, with analysis of four other dark clouds

2021 ◽  
Vol 503 (4) ◽  
pp. 5274-5290
Author(s):  
A K Sen ◽  
V B Il’in ◽  
M S Prokopjeva ◽  
R Gupta
Keyword(s):  
Magnetic Field ◽  
Near Infrared ◽  
Galactic Plane ◽  
Photometric Data ◽  
Dust Particles ◽  
Dark Cloud ◽  
Dark Clouds ◽  
High Polarization ◽  
Field Parallel ◽  
Photometric Observations

ABSTRACT We present the results of our BVR-band photometric and R-band polarimetric observations of ∼40 stars in the periphery of the dark cloud CB54. From different photometric data, we estimate E(B − V) and E(J − H). After involving data from other sources, we discuss the extinction variations towards CB54. We reveal two main dust layers: a foreground, E(B − V) ≈ 0.1 mag, at ∼200 pc and an extended layer, $E(B-V) \gtrsim 0.3$ mag, at ∼1.5 kpc. CB54 belongs to the latter. Based on these results, we consider the reason for the random polarization map that we have observed for CB54. We find that the foreground is characterized by low polarization ($P \lesssim 0.5$ per cent) and a magnetic field parallel to the Galactic plane. The extended layer shows high polarization (P up to 5–7 per cent). We suggest that the field in this layer is nearly perpendicular to the Galactic plane and both layers are essentially inhomogeneous. This allows us to explain the randomness of polarization vectors around CB54 generally. The data – primarily observed by us in this work for CB54, by A. K. Sen and colleagues in previous works for three dark clouds CB3, CB25 and CB39, and by other authors for a region including the B1 cloud – are analysed to explore any correlation between polarization, the near-infrared, E(J − H), and optical, E(B − V), excesses, and the distance to the background stars. If polarization and extinction are caused by the same set of dust particles, we should expect good correlations. However, we find that, for all the clouds, the correlations are not strong.

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