Far-infrared and molecular line observations of Lynds 183 - Studies of cold gas and dust

@article{Juvela2002FarinfraredAM,
  title={Far-infrared and molecular line observations of Lynds 183 - Studies of cold gas and dust},
  author={M. Juvela and K. Mattila and K. Lehtinen and D. Lemke and R. Laureijs and T. Prusti},
  journal={Astronomy and Astrophysics},
  year={2002},
  volume={382},
  pages={583-599}
}
We have mapped the dark cloud L183 in the far-infrared at 100 m and 200 m with the ISOPHOT photometer aboard the ISO satellite. The observations make it possible for the rst time to study the distribution and properties of the large dust grains in L183 without confusion from smaller grains. The observations show clear colour temperature variations which are likely to be caused by changes in the emission properties of the dust particles. In the cloud core the far-infrared colour temperature… Expand
ISO far-infrared observations of the high-latitude cloud L1642 - II. Correlated variations of far-infrared emissivity and temperature of “classical large” dust particles
Aims. Our aim is to compare the infrared properties of big, “classical” dust grains with visual extinction in the cloud L1642. In particular, we study the differences in grain emissivity betweenExpand
New insights into the dust properties of the Taurus molecular cloud TMC-2 and its surroundings
We present ISOPHOT observations at 120 and 200 μm of a 31 x 57 arcmin 2 region, with optical extinction Av ranging between 0.5 and 11 mag, that encloses the Taurus molecular cloud TMC-2. TheExpand
ISO observations of 3–200 μm emission by three dust populations in an isolated local translucent cloud
We present isophot spectrophotometry of three positions within the isolated high-latitude cirrus cloud G 300.2−16.8, spanning from the near- to far-infrared (NIR to FIR). The positions exhibitExpand
Direct evidence of dust growth in L183 from MIR light scattering
Theoretical arguments suggest that dust grains should grow in the dense cold parts of molecular clouds. Evidence of larger grains has so far been gathered in near/mid infrared extinction andExpand
A cold globule with a Class 0/I embedded source
Infrared observations of the dark cloud DC 303.8-14.2 and the embedded point source IRAS 13036-7644 have been made with the ISOPHOT instrument aboard ISO at 7.7 μm, 60 μm, 100 μm and 200 μm. We haveExpand
FUSE observations of molecular hydrogen on the line of sight towards HD 141569A
We present an analysis of the Far Ultraviolet Spectroscopic Explorer (FUSE) spectrum of HD 141569A, a transitional object known to possess a circumstellar disk. We observe two components of gas atExpand
Ice and Dust in the Prestellar Dark Cloud Lynds 183: Preplanetary Matter at the Lowest Temperatures
Dust grains are nucleation centers and catalysts for the growth of icy mantles in quiescent interstellar clouds, the products of which may accumulate into preplanetary matter when new stars and solarExpand
Photoelectric Heating and [C II] Cooling of High Galactic Latitude Translucent Clouds*
The (2P3/2 → 2P1/2) transition of singly ionized carbon, [C II], is the primary coolant of diffuse interstellar gas. We describe observations of [C II] emission toward nine high Galactic latitudeExpand
Far infrared observations of pre-protostellar sources in Lynds 183
Using ISOPHOT maps at 100 and 200  μ m and raster scans at 100, 120, 150 and 200  μ m we have detected four unresolved far-infrared sources in the high latitude molecular cloud L 183. Two of theExpand
Spectroscopic study of ‘CO’ and its isotopic mm/submillimeter lines from dark cloud Lynds 183
We have made spectral line analysis of CO and its isotopic lines from dark cloud Lynds 183 (L183). Our dataset incorporates 12CO(1-0), 13CO(1-0) and 13CO(2-1) lines using NRAO-12 m and 12CO(3-2),Expand
...
1
2
3
4
...

References

SHOWING 1-10 OF 56 REFERENCES
Correlation between Gas and Dust in Molecular Clouds: L977
We report observations of the J=(1-0) C18O molecular emission line toward the L977 molecular cloud. To study the correlation between C18O emission and dust extinction we constructed a GaussianExpand
IRAS DETECTION OF VERY COLD DUST IN THE LYNDS-134 CLOUD COMPLEX
We have analyzed IRAS maps at 60 and 100-mu-m of the complex of dark clouds containing L134, L183 and L1780. Regions were found that are bright at 100-mu-m but not detected at 60-mu-m. These regionsExpand
Radio wavelength observations of the L134N molecular core
A detailed study of the L134N dense molecular core through radio astronomical observations of spectral lines at millimeter and centimeter wavelengths is presented. The prototypical dark cloud wasExpand
Far-infrared dust opacity and visible extinction in the Polaris Flare
We present an extinction map of the Polaris molecular cirrus cloud derived from star counts and compare it with the Schlegel et al. ([CITE]) extinction map derived from the far-infrared dust opacity.Expand
ISOPHOT Far-Infrared Survey of Nearby Molecular Clouds
We present results of a far-infrared molecular cloud mapping program which utilizes the PHT-P photometer and PHT-C cameras of the ISOPHOT instrument. ISO has enabled us to study the emission of veryExpand
CO DEPLETION IN THE STARLESS CLOUD CORE L1544
We present evidence for CO depletion toward the starless cloud core L1544. A comparison between C17O and the 1.3 mm continuum dust emission shows that CO is depleted by a factor of ~10 at the dustExpand
The physics and chemistry of the L134N molecular core
The dark cloud L134N is studied in detail via millimeter- and centimeter-wavelength emission-line spectra. A high-density core of molecular gas exists in L134N which has a kinetic temperature ofExpand
A survey of interstellar H I from L-alpha absorption measurements. II
The Copernicus satellite surveyed the spectral region near L alpha to obtain column densities of interstellar HI toward 100 stars. The distance to 10 stars exceeds 2 kpc and 34 stars lie beyond 1Expand
Probing the structure of molecular cloud cores: observations and modelling of C i and C18O in HH24–26
We describe observations of the (CO)-O-18 J = 2 --> 1, 3 --> 2 and C I P-3(1) --> P-3(0) lines towards the HH24-26 molecular cloud core. The (CO)-O-18 traces the north-south molecular ridge, but theExpand
A source model for the L134N molecular cloud
The dark molecular cloud L134N is observed at millimeter wavelengths in the CS (J = 3-2), OCS (J = 7-6), and HDO (1 sub 11-1 sub 10) transitions. The CS (J = 3-2) transition was observed at fourExpand
...
1
2
3
4
5
...