269
EVOLUTION OF THE DUST PROPERTIES IN A TRANSLUCENT CLOUD
B. Stepnik1,2 A. Abergel1, J.-P. Bernard1, F. Boulanger1, L. Cambrsy3,4, M. Giard2, A. Jones1,
G. Lagache1, J.-M. Lamarre1, C. Meny2, F. Pajot1, F. Le Peintre1, I. Ristorcelli2, G. Serra2, and
J.-P. Torre5
1
Institut d Astrophysique Spatiale (IAS), Bt. 121, Universit Paris XI, F-91405 Orsay, France
2
Centre d Etude Spatial des Rayonnements (CESR), 9 av. Colonel Roche, BP 4346, F-31028 Toulouse, France
3
Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Mail Code 100-22, CA 91125, USA
4
Dpartement de Recherche Spatial (DESPA), Observatoire de Paris, F-92195 Meudon, France
5
Service d Aronomie du CNRS (SA), BP 3, F-91371 VerriŁres Le Buisson, France
Abstract grains. IRAS data show that the colour of the dust emis-
sion in the ISM varies from place to place within the same
The balloon borne experiment PRONAOS/SPM has
molecular complex (Boulanger et al. 1990). In particular,
measured the submillimeter emission from 200 to 600 m
the colour ratio I60m/I100m can decrease dramatically
with an angular resolution of 2-3.5 of a quiescent translu-
from diffuse to molecular regions (Laureijs et al. 1991).
cent filament (AV <"4) in the Taurus molecular complex.
This phenomenon is also observed in the Taurus molecu-
In order to analyse these data, we have developed a model
lar cloud (Abergel et al. 1994). The extended and diffuse
for the emission of the filament usingan independent tracer
part of the Taurus complex has an uniform IRAS colour
of the total column density (star count method on 2MASS
ratio I60m/I100m=0.15. The dense and cold parts of the
stars) and a radiative transfer code. We first use in the
complex are filamentary structures (Abergel et al. 1994,
model the optical properties of the dust from the standard
Lagache et al. 1998), which present a deficit of 70-100%
model of Desert et al. (1990). The computed brightness
of its IRAS colour ratio I60m/I100m.
profile fails to reproduce the data inside the filament. The
The physical properties of this cold dust is still not
agreement between data and model can only be obtained
characterised because IRAS and COBE data do not com-
by changing the dust properties inside the filament. We
bine the angular resolution and the spectral coverage re-
have removed all particles not in thermal equilibrium from
quired to analyse the thermal emission of individual clouds.
the densest part of the filament (typically nH <"104 cm-3),
However, PRONAOS/SPM, in combination with IRAS,
and multiplied the submillimeter emissivity by a signifi-
constrains both the temperature and the emissivity spec-
cant factor (<"3). This suggests that grain-grain coagula-
tral index of large grains at an angular resolution of 2-3.5 .
tion into fluffy aggregates occur inside the filament.
These data allow us to better understand the origin and
the nature of the cold dust in the ISM. This paper presents
Key words: ISM: dust property, continuum emission Mis-
observations and analysis of one of these Taurus filaments.
sions: PRONAOS, FIRST Object: Taurus complex
2. Observations
2.1. PRONAOS/SPM instrument
The observations have been performed with the PRONAOS
1. Introduction
experiment ( PROgramme National d AstrOnomie Sub-
It is now well established that the interstellar dust is made
millimtrique ). PRONAOS is a stratospheric balloon-
of several components differing in their chemical composi- borne which carry a two-meter telescope. SPM ( Spectro-
tion, structure and size. The smallest interstellar dust par- PhotomŁtre Multibande , see Lamarre et al. 1994), the fo-
ticles (sizes 15 nm) essentially emitting at wavelengths
cal instrument, is a single beam multi-band photometer.
below 150 m, are transiently heated in the InterStellar ra- This instrument simultaneously performs measurements
diation Field (ISRF). The largest interstellar dust grains
in four wide spectral bands, centred at 200, 260, 360 and
are in thermal equilibrium with the radiation field and
580 m. The atmospheric residual emission is reduced us-
their emission peaks around 100 m (Desert et al. 1990).
ing an oscillating mirror, which ensures a beam switch-
They have an average temperature of about 17.5 K in the
ing on the sky at a constant elevation. For this reason,
diffuse atomic medium (Boulanger et al. 1996), with an
PRONAOS/SPM is sensitive to emission gradients.
emissivity similar to the value of the model of Draine &
The photometric calibration is provided by ground mea-
Lee (1984). However, this simple description does not take
surements, two in flight black bodies, and planet observa-
into account spatial variations of dust properties at small
tions. The final accuracy of this calibration is better than
scale in our galaxy.
10 % in absolute, and better than 5 % from channel to
IRAS and COBE data indicate that there are spa- channel.
tial variations in the emitting properties of the interstellar
Proc. Symposium The Promise of the Herschel Space Observatory 12 15 December 2000, Toledo, Spain
ESA SP-460, July 2001, eds. G.L. Pilbratt, J. Cernicharo, A.M. Heras, T. Prusti, & R. Harris
270 B. Stepnik et al.
a)
Figure 1. 100 m IRAS map of the Taurus filament. The
white box shows the region covered by the optical axis of b)
PRONAOS/SPM (without including the instrument beam
size). The PRONAOS/SPM beam sizes at each wavelength are
shown by the circles on the top left side of the figure. The 100
m IRAS contours are given from 11 to 23 MJy/sr with a step
of 2 MJy/sr.
2.2. Emission profiles
The Taurus cloud observations were carried out duringthe
second PRONAOS/SPM flight, on September 23rd 1996,
from New-Mexico (USA). We have observed a map of 3
50 centred at the position ą1950 =4h15m48s, 1950 =
25ć%12 01 (Fig. 1). To complement our data we have used
HIRES (Hig h RESolution processing ) IRAS imag es of the
cloud at 60 and 100 m.
Figure 2. Upper panel presents brightness profiles of the clouds.
Black lines in Fig. 2a present the brightness profiles of
Lower panel presents spectra of the central position of the fil-
the filament, averaged in a direction parallel to the long ament from which we have subtracted the emission of the sur-
rounding envelope (green dashed lines in upper panel). The data
axis of the cloud, and degraded to the angular resolution
are represented by the black continuous lines in upper panel
of the 580 m PRONAOS/SPM band (3.5 ). The emis-
and by the diamonds in lower panel, with the 1- error bars.
sion of the cloud can be separated into two components,
The standard model (see Sect. 3.3) is represented by red dashed
a bright filament and a surrounding envelope. We have
lines. The non-standard model (see sect. 3.4) is represented by
adjusted the surrounding envelope emission by a second
blue dashed lines.
order polynom (green dashed lines in Fig. 2a).
the large structure surrounding the filament is determined
2.3. Temperature profiles
using DIRBE data at 140 and 240 m.
We have modelled the cloud spectra using a single modi-
Table 1 presents these temperatures measurements.
fied black body spectrum:
-
fit
I = 250 m B(Tdust),
250 m
where 250 m is the dust emissivity at 250 m, the emis-
region offset Tdust
sivity spectral index, and Tdust the dust temperature. The
Filament 0 12.0+0.2 K
-0.1
temperatures of the filament and the envelope are mea-
Envelope 8 -25 14.8ą0.6 K
sured using PRONAOS/SPM data. The value observed
Outside 30 -1ć% 16.8ą0.7 K
are always compatible with 2. Therefore, in the follow-
Table 1. Values of the dust equilibrium temperature with the
ing, we set the value of to 2, according with the value
incident radiation field at different positions in the cloud.
proposed by Boulanger et al. (1996). The temperature of
Evolution of the Dust Properties in a Translucent Cloud 271
We have evidenced a significant temperature variation from
temperature of 12 K (see Sect. 2.3), while the computed
16.8ą0.7K outside the cloud to 12.0+0.2 K inside the fil-
-0.1 spectrum predicts 14.2 K. Moreover, at 60 m, the model
ament. Such a low temperature of 12 K is surprising for
presents an emission which is definitely not observed.
a translucent cloud (AV <"4). In order to understand its
In order to reproduce the observations, one solution
origin we have modelled the filament emission.
may be to change both the incident radiation field and
the AV profile inside the observational constraints. These
changes does not reproduce neither the observations. There-
3. Modelling the filament emission
fore, we conclude that it is the grain properties change
3.1. Density profile from star counts
inside the filament.
In order to model the submillimeter emission of our fila-
ment, we need an independent tracer of the total dust col-
3.4. Results using non-standard dust
umn density across the cloud. We have used the 2MASS
In a second step, we have investigated changes in the dust
J band star catalog, and applied the star counts method
properties inside the filament in order to reproduce our
developed by Cambresy (1999) to compute an AV map.
data. We have seen that the model predicts more emission
From the AV profile, we have computed the density pro-
at 60 m. The 60 m emission is mainly due to particles
file of the filament. We have decomposed the AV profile in
not in thermal equilibrium with the radiation field (VSGs
a large-scale component with a constant extinction value
for Very Small Grains). Therefore, we suggest that the
Alarge-scale (0.5) due to the diffuse medium surrounding
V
relative abundance of these particles strongly decreases in
the filament, and in the filament itself characterised by
the filament. Moreover, the model predicts less emission
an extinction depending on the distance from the centre,
r
in the submillimeter range that the one we have observed.
Afilament(r)= n0 ( )-2, withn0=5800 cm-3 and rc=2.3 .
V
rc
A straightforward explanation is to increase the emissivity
of grains at thermal equilibrium with the radiation field
3.2. Radiative transfer
(BGs for Big Grains). In order to reproduce the data we
have realised the following changes:
We have used the 3D radiative transfer code developed
by Bernard et al. (1992) and improved by Le Peintre et The BG emissivity is increased by a factor of 3.4+0.3.
-0.7
al. (2001). This model computes the distribution of grain The VSG abundance is decreased by a factor 0.1ą0.1.
temperature and the IR emission of an interstellar cloud. The BG and VSG properties are modified in the same
We assume that the incident radiation field is isotropic.
area 4 ą1 , which correspond to an AV treshold value
We adopt the average interstellar radiation field (ISRF) of 2.1ą0.5.
of Mathis et al. (1983) attenuated by the visual extinction
This simple cloud model in two dust phases separated by
Alarge-scale (see Sect. 3.1). In order to take the filamentary
an abrupt transition reproduces very well our data (see
V
shape of the cloud into account, we have assumed a cylin-
Fig. 2). We do not resolve the transition area with our
drical geometry in our calculation. The dust extinction
data. We conclude that we have evidenced the presence
and emission is computed using the Desert et al. (1990)
of non-standard dust inside the filament and the spatial
algorithm. It is a self-consistent model, which takes full ac-
correlation of the changes of the BG and VSG properites.
count of the transiently-heated small grains. Moreover, our
simulations are independent of the gas-to-dust ratio used,
4. Discussion
because star count measurements give the total quantity
of dust on the line of sight, and the radiative transfer code Several processes may affect the optical properties of dust
uses directly the dust density inside the cloud. in dense clouds: ice or molecular mantle formation on
grains, coagulation of grains (e.g. Draine 1985 ).
Preibisch et al. (1991) have shown that ice and carbon
3.3. Results using standard dust
mantles on BGs does not increase significantly the sub-
In a first step we have assumed constant optical proper- millimeter emissivity. Therefore, we conclude that mantle
ties of the dust through the cloud. We have used the stan- formation cannot be the main explanation for our obser-
dard dust composition adopted by Desert et al. (1990). vations.
Fig. 2 compares the model with the observations. The Dust coagulation is efficient for producing large fluffy
emission of the envelope is properly reproduced (offsets aggregates (Weidenschilling & Ruzmaikina 1994, Ossenkopf
greater than 7 ), but the filament emission (offsets smaller 1993). The optical properties of fluffy aggregates formed
than 7 ) is not well-reproduced by the model. Inside the by such a process have been computed by several authors
filament, at wavelengths longer than 100 m, the observed (Bazell & Dwek 1990, Stognienko et al. 1995). The submil-
emission shows an excess compared to the model, and the limeter emissivity of these aggregates strongly increases
grains are too warm inside the densest parts of the fil- with fluffiness. At 200 m this increase is typically a factor
ament. This is illustrated by comparing the spectra at of 1.5-3.5 for silicate aggregates and 3-20 for carbon ag-
the central position of the filament. We have observed a gregates (e.g. Stognienko et al. 1995). On the other hand,
272
the UV, visible and near-IR absorptivity are not signif- Cold equilibrium temperature of the BG with the ra-
icantly modified (Bazell & Dwek 1990), which implies a diation field (12 K), for a translucent cloud (AV <" 4).
decrease of the dust equilibrium temperature with the in-
Grain-grain coagulation processes can produce the relative
cident radiation field. Therefore, grain-grain coagulation
abundance and the grain optical properties measured for
can explain both the increase of the submillimeter emis-
this non-standard dust. Moreover, coagulation timescales
sivity, and the cold temperature observed. Dynamics sim-
(< 106 yr) are compatible with this scenario in the phys-
ulations (Weidenschilling & Ruzmaikina 1994, Ossenkopf
ical environment of this Taurus filament. Therefore, we
1993) have shown that, in the physics conditions of the
conclude that we have evidenced the signature of grain-
Taurus filament, the coagulation timescale is smaller than
grain coagulation into fluffy aggregates.
the cloud life times. Moreover, the smallest grains (VSGs)
FIRST would be the appropriate instrument to analyse
coagulate faster than the larger ones (Ossenkopf 1993).
the transitions zone between standard and non-standard
Therefore, grain-grain coagulation can explain the huge
dust in order to understand the physical processes in-
decrease of the VSG abundance observed even in a translu-
volved in the dust evolution that we have evidenced.
cent cloud.
Acknowledgements
Finally, we conclude that grain-grain coagulation into
We are indebted to the French space agency CNES who sup-
fluffy aggregates can produce strong variations of the rel-
ported the PRONAOS/SPM project. We are very grateful to
ative abundance and optical properties of dust observed
the PRONAOS/SPM technical team in CNRS and in CNES.
in our Taurus filament, and certainly occurs in the Taurus
This publication makes use of data products from the Two
filament.
Micron All Sky Survey. We thank the 2MASS team for their
Other observations have also evidence a change in the
work.
dust properties. Bernard et al. (1999) observed a low BG
equilibrium temperature toward a high latitude cirrus cloud
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