J/A+A/592/A61 Isolated starless cores dust temperature (Lippok+, 2016)
Earliest phases of star formation (EPoS):
Dust temperature distributions in isolated starless cores.
Lippok N., Launhardt R., Henning T., Beuther H., Balog Z.,
Kainulainen J., Krause O., Linz H., Nielbock M., Ragan S.E.,
Robitaille T.P., Sadavoy S.I., Schmiedeke A.
<Astron. Astrophys. 592, A61 (2016)>
=2016A&A...592A..61L 2016A&A...592A..61L (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Extinction ; Bok globules
Keywords: stars: formation - stars: low-mass - ISM: clouds - ISM: structure -
dust, extinction - infrared: ISM
Abstract:
Constraining the temperature and density structure of dense molecular
cloud cores is fundamental for understanding the initial conditions of
star formation. We use Herschel observations of the thermal FIR dust
emission from nearby isolated molecular cloud cores and combine them
with ground-based submillimeter continuum data to derive observational
constraints on their temperature and density structure. The aim of
this study is to verify the validity of a ray-tracing inversion
technique developed to derive the dust temperature and density
structure of isolated starless cores directly from the dust emission
maps and to test if the resulting temperature and density profiles are
consistent with physical models. Using this ray-tracing inversion
technique, we derive the dust temperature and density structure of six
isolated starless cloud cores. We employ self-consistent radiative
transfer modeling to the derived density profiles, treating the ISRF
as the only heating source. The best-fit values of local strength of
the ISRF and the extinction by the outer envelope are derived by
comparing the self-consistently calculated temperature profiles with
those derived by the ray-tracing method. We find that all starless
cores are significantly colder inside than outside, with the core
temperatures showing a strong negative correlation with peak column
density. This suggests that their thermal structure is dominated by
external heating from the ISRF and shielding by dusty envelopes. The
temperature profiles derived with the ray-tracing inversion method can
be well-reproduced with self-consistent radiative transfer models.
Description:
Dust temperature maps for 6 Bok globules with starless cores are
presented. The following Bok globules have been observed: CB4, CB17,
CB26, CB27, B68, CB244
The midplane dust temperature [K] maps are provides as fits files.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
17 22 38.2 -23 49 34 B68 = Barnard 68
04 04 38 +56 56.2 CB17 = [CB88] 17
23 25 47 +74 17.6 CB244 = [CB88] 244
05 00 09 +52 04.9 CB26 = [CB88] 26
05 04 09.7 +32 43 09 CB27 = [CB88] 27
00 39 03 +52 51.5 CB4 = [CB88] 4
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 70 6 List of fits temperature maps
fits/* . 6 Individual fits temperature maps
--------------------------------------------------------------------------------
Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 22 I3 --- Nx Number of pixels along X-axis
24- 26 I3 --- Ny Number of pixels along Y-axis
28- 30 I3 Kibyte size Size of FITS file
32- 45 A14 --- FileName Name of FITS file, in subdirectory fits
47- 70 A24 --- Title Title of the FITS file
--------------------------------------------------------------------------------
Acknowledgements:
Ralf Launhardt, rl(at)mpia.de
(End) Patricia Vannier [CDS] 17-Jun-2016