2003A&A...410..577A


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.07CET13:09:15

2003A&A...410..577A - Astronomy and Astrophysics, volume 410, 577-585 (2003/11-1)

ISOCAM and molecular observations of the edge of the Horsehead nebula.

ABERGEL A., TEYSSIER D., BERNARD J.P., BOULANGER F., COULAIS A., FOSSE D., FALGARONE E., GERIN M., PERAULT M., PUGET J.-L., NORDH L., OLOFSSON G., HULDTGREN M., KAAS A.A., ANDRE P., BONTEMPS S., CASALI M.M., CESARSKY C.J., COPET E., DAVIES J., MONTMERLE T., PERSI P. and SIBILLE F.

Abstract (from CDS):

We present ISOCAM observations (5-18µm) of the Horsehead nebula, together with observations of the (J=1-0) and (J=2-1) transitions of 12CO, 13CO and C18O taken at the IRAM 30-m telescope. The Horsehead nebula presents a typical photodissociation region illuminated by the O9.5 V system σ Ori. The ISOCAM emission is due to very small particles transiently heated to high temperature each time they absorb a UV photon. A very sharp filament (width: ∼10'' or ∼0.02pc) is detected by ISOCAM at the illuminated edge of the nebula. This filament is due to a combined effect of steep increase of the column density and extinction of incident radiation, on typical sizes below ∼0.01pc. Both the three-dimensional shape and the local density of the illuminated interface are strongly constrained. The dense material forming the edge of the Horsehead nebula appears illuminated edge-on by σ Ori, and the particles located beyond the border should not be affected by the incident radiation field. This structure may be due to dense filaments in the parental cloud which have shielded the material located in their shadow from the photo-dissociating radiations. The measurement of the penetration depth of the incident radiation from the infrared data (∼0.01pc) gives a density of a few 104cm–3 just behind the bright filament. This value is comparable to the estimate of the density beyond the edge and deduced from our molecular observations, and also to the density behind the ionization front calculated in the stationary case. The material behind the illuminated edge could also be non-homogeneous, with clump sizes significantly smaller than the observed penetration depth of ∼0.01pc. In that case no upper limit on the average density just behind the illuminated edge can be given.

Abstract Copyright:

Journal keyword(s): ISM: individual objects: Horsehead - ISM: dust, extinction - ISM: clouds - infrared: ISM - radio lines: ISM

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 743 0
2 * sig Ori Y*O 05 38 44.7665260139 -02 36 00.284709290 2.54 3.58 3.79 3.87 4.11 O9.5V 754 0
3 NAME Horsehead Nebula DNe 05 40 59.0 -02 27 30           ~ 457 0
4 IC 434 HII 05 41 -02.5           ~ 79 1
5 NGC 2023 RNe 05 41 37.9 -02 15 52           ~ 580 1
6 LDN 1630 DNe 05 45.5 -00 59           ~ 356 0
7 NGC 7023 RNe 21 01 36.9 +68 09 48           ~ 642 0

    Equat.    Gal    SGal    Ecl

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2021.03.07-13:09:15

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