2013ApJ...765..107L


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.10CET19:26:08

2013ApJ...765..107L - Astrophys. J., 765, 107 (2013/March-2)

Far-ultraviolet observations of the Taurus-Perseus-Auriga complex.

LIM T.-H., MIN K.-W. and SEON K.-I.

Abstract (from CDS):

We have constructed a far-ultraviolet (FUV) continuum map of the Taurus-Auriga-Perseus complex, one of the largest local associations of dark clouds, by merging the two data sets of Galaxy Evolution Explorer and FUV Imaging Spectrograph, which made observations at similar wavelengths. The FUV intensity varies significantly across the whole region, but the diffuse FUV continuum is dominated by dust scattering of stellar photons. A diffuse FUV background of ∼1000 CU is observed, part of which may be attributable to the scattered photons of foreground FUV light, located in front of the thick clouds. The fluorescent emission of molecular hydrogen constitutes ∼10% of the total FUV intensity throughout the region, generally proportional to the local continuum level. We have developed a Monte Carlo radiative transfer code and applied it to the present clouds complex to obtain the optical properties of dust grains and the geometrical structures of the clouds. The albedo and the phase function asymmetry factor were estimated to be 0.42+0.05–0.05, and 0.47+0.11 –0.27, respectively, in accordance with theoretical estimations as well as recent observations. The distance and thickness of the four prominent clouds in this complex were estimated using a single-slab model applied individually to each cloud. The results obtained were in good agreement with those from other observations of the Taurus cloud, as its geometrical structure is rather simple. For other clouds that were observed to have multiple components, the results gave distances and thicknesses encompassing all of the components of each cloud. The distance and thickness estimations were not crucially sensitive to the exact values of the albedo and the phase function asymmetry factor, while the locations of the bright field stars relative to the clouds as initial photon sources seem to be the most important factor in the process of fitting.

Abstract Copyright:

Journal keyword(s): dust, extinction - ISM: clouds - ISM: individual (Taurus, Auriga, and Perseus complex) - ISM: structure - ultraviolet: ISM

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 IC 43 GiG 00 42 22.065 +29 38 29.81   14.4       ~ 63 0
2 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3468 3
3 NGC 1333 SFR 03 28 55 +31 22.2   10.9       ~ 1187 1
4 NAME Tau-Aur-Per Region reg 03 33 +31.0           ~ 31 0
5 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1011 0
6 Ass Per OB 2 As* 03 42.2 +33 26           ~ 302 0
7 IC 348 OpC 03 44 34 +32 09.8           ~ 1206 1
8 Cl Melotte 22 OpC 03 47 00 +24 07.0           ~ 2914 0
9 NAME Eri Bubble HI 03 52 -02.0           ~ 80 0
10 NGC 1499 HII 04 03 18 +36 25.3           ~ 150 0
11 NAME Auriga reg 04 20 00.0 +38 05 00           ~ 164 0
12 NAME Kutner's Cloud MoC 04 32 44.6 +24 23 13           ~ 209 0
13 NAME Per B AGN 04 37 04.37510272 +29 40 13.8184969   21.7       ~ 459 2
14 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3335 0
15 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1330 0
16 IC 410 Cl* 05 22.0 +33 29           ~ 53 0
17 M 42 HII 05 35 17.3 -05 23 28           ~ 3664 0
18 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2944 0

    Equat.    Gal    SGal    Ecl

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2019.12.10-19:26:08

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