2008A&A...483..471N


C.D.S. - SIMBAD4 rel 1.7 - 2020.08.04CEST22:34:20

2008A&A...483..471N - Astronomy and Astrophysics, volume 483, 471-484 (2008/5-4)

Multi-wavelength observations of a nearby multi-phase interstellar cloud.

NEHME C., GRY C., BOULANGER F., LE BOURLOT J., PINEAU DES FORETS G. and FALGARONE E.

Abstract (from CDS):

High-resolution spectroscopic observations (UV HST/STIS and optical) are used to characterize the physical state and velocity structure of the multiphase interstellar medium seen towards the nearby (170pc) star HD 102065. The star is located behind the tail of a cometary-shaped, infrared cirrus-cloud, in the area of interaction between the Sco-Cen OB association and the Local Bubble. We analyze interstellar components present along the line of sight by fitting multiple transitions from a group of species all at once. We identify four groups of species: (1) molecules (CO, CH, CH+), (2) atoms (CI, SI, FeI) with ionization potential lower than HI, (3) neutral and low-ionized states of atoms (MgI, MgII, MnII, PII, NiII, CII, NI and OI) with ionization potential larger than HI and (4) highly-ionized atoms (SiIII, CIV, SiIV). The absorption spectra are complemented by HI, CO and CII emission-line spectra, H2 column-densities derived from FUSE spectra, and IRAS images. Gas components of a wide range of temperatures and ionization states are detected along the line of sight. Most of the hydrogen column-density is in cold, diffuse, molecular gas at low LSR velocity. This gas is mixed with traces of warmer molecular gas traced by H2 in the J>2 levels, in which the observed CH+ must be formed. We also identify three distinct components of warm gas at negative velocities down to -20km/s. The temperature and gas excitation are shown to increase with increasing velocity shift from the bulk of the gas. Hot gas at temperatures of several 105 K is detected in the most negative velocity component in the highly-ionized specie. This hot gas is also detected in very strong lines of less-ionized species (MgII, SiII* and CII*) for which the bulk of the gas is cooler. We relate the observational results to evidence for dynamical impact of the Sco-Cen stellar association on the nearby interstellar medium. We propose a scenario where the infrared cirrus cloud has been hit a few 105yr ago by a supernova blast wave originating from the Lower Centaurus Crux group of the Sco-Cen association. The observations provide detailed information on the interplay between ISM phases in relation with the origin of the Local and Loop I bubbles.

Abstract Copyright:

Journal keyword(s): ISM: structure - ISM: clouds - ISM: kinematics and dynamics - ISM: individual objects : Chamaeleon clouds - ultraviolet: ISM - stars: individual: HD102065

Simbad objects: 15

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Number of rows : 15

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 HD 102065 pr* 11 43 36.9449447212 -80 29 00.508433432   6.67 6.61     B9IV 57 0
2 [DB2002b] G300.23-16.89 DNe 11 54 31 -79 27.8           ~ 41 1
3 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 690 0
4 V* T Cha Or* 11 57 13.5268556629 -79 21 31.521755129   10.00 11.86     K0e 234 1
5 * bet Cha V* 12 18 20.8245890 -79 18 44.070964 3.59 4.104 4.229     B4V 77 0
6 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 357 1
7 NAME Musca Cld 12 23 -71.3           ~ 157 0
8 NAME Coalsack Nebula DNe 12 31 19 -63 44.6           ~ 242 0
9 IRAS 12340-7958 * 12 37 39.7466355997 -80 15 13.713429632   16.11 14.39 13.63 9.81 ~ 101 0
10 NAME Cha III MoC 12 37.8 -80 15           ~ 124 2
11 NAME Loop I SR? 15 01 -38.7           ~ 329 2
12 NAME Upper Centaurus Lupus As* 15 24 -41.9           ~ 360 1
13 NAME Upper Sco Association As* 16 12 -23.4           ~ 1028 1
14 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1129 1
15 NAME Local Bubble ISM ~ ~           ~ 694 0

    Equat.    Gal    SGal    Ecl

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2020.08.04-22:34:20

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