A&A 384, 225-241 (2002)
DOI: 10.1051/0004-6361:20020103
N. Schneider1,2,3 - R. Simon1,4 - C. Kramer1,2 - J. Stutzki1 - S. Bontemps3
1 - I.Physikalisches Institut, Universität zu Köln,
Zülpicher Straße 77, 50937 Köln, Germany
2 -
IRAM, BP 53, 38406
Saint Martin d'Hères, France
3 -
Observatoire de Bordeaux, BP 89, 33270 Floirac, France
4 -
Institute for Astrophysical Research, Boston University,
725 Commonwealth Avenue, Boston, MA 02215, USA
Received 7 September 2001 / Accepted 15 January 2002
Abstract
The molecular cloud associated with Sharpless 106 has been
studied in a variety of (sub)millimeter CO rotational lines on angular
resolution scales from 11'' to 80''. We used the KOSMA 3 m
telescope to obtain an extended 12CO J=32 map, from
which we calculate a total mass of 2000
and an average
density of
cm-3 for the molecular cloud. The peak
intensity region around the massive young star S106 IR was observed in
13CO J=6
5 and 3
2 with KOSMA and in isotopomeric
low-J CO lines with the IRAM 30 m telescope. A clump decomposition
made for several lines yields a common clump-mass spectral
index of
,
illustrating the self-similarity of the
detected structures for length-scales from 0.06 to 0.9 parsec.
All 12CO and 13CO line profiles within approximately 2'around S106 IR show blue wing emission and less prominent red wing
emission, partly affected by self-absorption in colder foreground
material. We attribute this high-velocity emission to the ionized
wind of S106 IR driving a shock into the inhomogeneous molecular
cloud. We do not find evidence for a smooth or fragmented disk around
S106 IR and/or an expanding ring in the observed CO emission
distribution.
The excitation conditions along a cut through the molecular cloud/H II region are
studied with an LTE analysis (and an Escape Probability model at the position of
S106 IR), using the observed CO line intensities and ratios. The kinetic
gas temperature is typically 40 K, the average density of the cloud in the core
region is
cm-3, and the local density within the clumps is
cm-3. The 13CO/C18O line and column density
ratios away from S106 IR reflect the natural isotopic abundance but towards the
optical lobes and the cavity walls, we see enhanced 13CO emission and
abundance with respect to C18O. This shows that selective
photo-dissociation is only important close to S106 IR and in a thin layer of the
cavity walls. In combination with the results from the excitation analysis we
conclude that the molecular line emission arises from two different gas phases:
(i) rather homogeneous, low- to medium-density, spatially extended clumps and
(ii) embedded, small (
0.2 pc), high-density clumps with a low volume
filling factor.
Key words: ISM: clouds - ISM: individual objects: S106 - ISM: molecules - ISM: kinematics and dynamics - ISM: jets and outflows - radio lines: ISM
The H II region S106 in Cygnus is a prominent bipolar
emission nebula associated with an extended molecular cloud. The
complex is most probably located at a distance of 600 pc (Staude et al. 1983), although larger distances of 2 to 2.5 kpc have
been suggested by Reifenstein et al. (1970) and Neckel (1990,
private communication). The two lobes of ionized gas seen in optical
and radio continuum emission have an angular extent of 3' in nearly
north-south direction and are separated by a dark bar of
projected size, devoid of optical and radio
continuum emission and perpendicular to the axis of symmetry of the
nebula. The bar was initially interpreted as a large-scale molecular
gas disk (Little et al. 1995; Bally & Scoville
1982). Stutzki et al. (1982), however, found that their NH3 observations
are inconsistent with a ring structure. Barsony et al. (1989) conclude from their molecular line data that
the emission arises from a clumpy molecular cloud and found no
indication for a disk-like structure.
The nebula is excited by a single O7-O9 star (Eiroa et al. 1979; Gehrz et al. 1982) referred to as
S106 IR. The star is deeply embedded in the
dark lane and drives an ionized wind with a velocity of 200
km s-1 (Br
observations of Simon & Fischer
1982; model of Hippelein & Münch 1981). The
magnitude of the visual extinction toward S106 IR was estimated between
12
and 21
,
depending on the assumed distance (Eiroa et al. 1979; Hodapp & Rayner 1991; van den Ancker et al. 1999).
The (sub)mm dust emission in S106 was observed by Mezger et al. (1987) and Richer et al. (1993). Their maps show two emission peaks approximately 15'' east and west of S106 IR, the latter referred to as S106 FIR. Since two clusters of H2O masers were detected at the position of S106 FIR (Stutzki et al. 1982; Furuya et al. 1999), indicating shocked material excited by a micro jet (10''length-scale), this source was interpreted by Richer et al. (1993) as a Class 0 young stellar object. The detection of molecular material entrained in the jet, however, remains elusive.
The molecular cloud associated with the H II region has been studied
at an angular resolution of typically 1' in the lower-J CO lines,
NH3, and CN (Lucas et al. 1978; Bally & Scoville
1982; Stutzki et al. 1982;
Churchwell & Bieging 1982). The molecular line maps in
optically thick lines reveal an extended (approximately
or 3.5 pc
4.4 pc at 600 pc distance) cloud with peak emission
at the position of S106 IR, whereas maps in optically thin molecular
lines and mm- and submm continuum show two maxima of emission
separated by 3' east and west of S106 IR.
The small scale molecular cloud structure in the environment of S106
IR was studied with higher angular resolution (typically 15'')
single-dish maps in CO and CS lines (Barsony et al. 1989;
Richer et al. 1993; Little et al. 1995), as well as
by means of interferometric observations in HCN (Bieging
1984), CS 2
1 (Barsony et al. 1989), and HCO+ 1
0 (Loushin et al. 1990). On this scale, a second
"bar'' or "lane'' of size
was detected and
sometimes interpreted as an edge-on disk of (cold) molecular gas,
responsible for collimating the ionized wind of S106 IR (Bally &
Scoville 1982; Bieging 1984; Mezger et al. 1987). Other authors, however, argue against a smooth
disk of molecular material and explain the bipolarity of the nebula by
either an asymmetric stellar wind (Felli et al. 1984; Barsony
et al. 1989) or the presence of a very small (30 AU) and
very dense (
cm-3) disk which collimates the
H II lobes and casts an equatorial shadow in the optical and infrared
seen as a narrow dark lane (Persson et al. 1988; Bally et al. 1998).
The intention of the present study is to understand the complex spatial and velocity structure observed in the molecular cloud. The S106 region with its signposts of (high mass) star formation - a bipolar H II region, a possible small or large scale disk or remnants thereof, and high velocity molecular line emission suggestive of outflow emission - makes it an ideal place to study the effects of a new born high-mass star on its parental molecular cloud. The present paper (Part I of a series) contains an analysis of low- and mid-J CO lines, including their emission distribution on different size-scales, the excitation conditions, and a comparison to IR data. In Part II, we investigate the influence of the FUV radiation from S106 IR on the surrounding cloud and present a detailed study of the Photon Dominated Region (PDR).
Following a description of the data acquisition and observational
parameters (Sect. 2), we present our CO observations (Sect. 3). In
Sect. 4, we give the results of a clump decomposition, discuss the
excitation conditions along a cut through the molecular cloud/H II region and perform an LTE and Escape Probablity analysis of the CO
data. Section 5 gives a summary of the paper.
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Points | Grid | HPBW |
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|
[GHz] | [K] | [km s-1] | [K] | |||||
KOSMA | ||||||||
12CO 3![]() |
345.796 | 1213 | 40'' | 80'' | 0.63 | 290 | 0.12 | 0.60 |
13CO 3![]() |
330.588 | 37 | 20'' | 80'' | 0.63 | 330 | 0.63 | 0.13 |
13CO 6![]() |
661.067 | 37 | 20'' | 38'' | 0.48 | 1140 | 0.23 | 2.50 |
IRAM | ||||||||
12CO 2![]() |
230.794 | 4560 | 5.5'' | 11'' | 0.45 | 980 | 0.10 | 0.84 |
13CO 2![]() |
220.399 | 4560 | 5.5'' | 11'' | 0.45 | 650 | 0.11 | 0.47 |
12CO 1![]() |
115.271 | 1035 | 11'' | 22'' | 0.70 | 417 | 0.10 | 0.23 |
13CO 1![]() |
110.201 | 1035 | 11'' | 22'' | 0.70 | 245 | 0.11 | 0.10 |
C18O 1![]() |
109.782 | 1035 | 11'' | 22'' | 0.70 | 269 | 0.11 | 0.11 |
All molecular line maps obtained within the framework of this study
are centered on the position of S106 IR at RA(B1950.0) =
and DEC(B1950.0) =
,
which will
be referred to as such or the (0, 0) position and marked by a star in
the figures throughout the paper. The technical and observing
parameters of the molecular line data are summarized in Table 1.
The 13CO 65 and 13CO 3
2 lines were observed
simultaneously in 1998 February at the Kölner Observatorium für
Submm-Astronomie (KOSMA) which operates a 3 m submm radiotelescope on
Gornergrat, Switzerland (Kramer et al. 1998b). The
observations were performed with a dual-channel SIS-receiver, built at
the Cologne Institute, operating at 325-365 GHz and 630-690 GHz
(Graf et al. 1998). Two acousto optical spectrometers of
the Cologne group were used as backends (Schieder et al.
1989).
The data were taken during a period of mean zenith opacity of 1.27 at
661 GHz and 0.25 at 330 GHz. The observations at 330 GHz were
corrected for sideband imbalance due to an atmospheric water line at
325 GHz as derived from an atmospheric model by Grossman
(1989). The spectra were calibrated to a main beam brightness
temperature scale (
).
Pointing was monitored simultaneously for both spectral channels using
continuum cross scans of Jupiter and found to be accurate to within
15''. The offset between the two beams was derived in the same
manner and found to be 20'' in elevation.
We observed in position-switching mode with an emission free reference
position at RA(B1950.0) =
and
DEC(B1950.0) =
.
The average noise temperature per
spectral channel of the 13CO 6
5 data is 2.5 K with 4 K for
the more noisy spectra at the northern and eastern border of the map
and 1.4 K for the data in the central part.
A large scale map in the 12CO J=32 line was taken in 1999
January using the recently implemented On-the-Fly (OTF) observing
mode at KOSMA (Kramer et al. 1999). An area of
was mapped on a fully sampled 40'' grid.
We performed scans at constant declination with a length of
10', two dumps per beam-size and a spectra dump time of 4 s. The
whole area was covered once in horizontal scans during 3 observing
shifts of 4 hours each. The area of peak CO emission was included in
each of the shifts, showing that the deviations in intensity between
the maps are less than 10%. The data were taken with the same
front- and backends used in 1998.
The pointing accuracy was of the order of 10'', derived from
continuum cross scans of Jupiter.
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Figure 1:
Contour lines of the KOSMA 12CO J=3![]() ![]() ![]() ![]() ![]() ![]() |
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In 1997 June, we observed the 12CO and 13CO J=21, and
the 12CO,13CO, and C18O J=1
0 lines with the IRAM
30 m telescope in its OTF mapping mode. The spectral lines were
recorded simultaneously under uniform weather conditions (atmospheric
opacity of 0.4 at 230 GHz) prevailing over several days. We used the
IRAM facility receivers and autocorrelator which was adapted in
spectral resolution and bandwidth so that all CO lines have a similar
velocity resolution of
0.1 kms-1. Pointing and focus were
checked every 2 hours. The pointing accuracy was found to be better
than 4'' and the receivers were aligned to within 2''.
The OTF mapping was started with a horizontal coverage (scans in RA)
of an
large area with 6 dumps per beam-size and a dump
time of 2 s. We then proceeded to cover the same area with
vertical scans to obtain complete, but independent, maps of the whole
region and to reduce smearing effects and fluctuations in the
intensity calibration. The final maps in each molecular line are the
weighted average of all data obtained. The 1
0 maps show no
obvious scanning effects or calibration problems, in contrast to the
higher angular resolution maps of the 2
1 line, where we see
slight scanning effects in the form of low intensity horizontal and
vertical stripes.
Since the observed molecular cloud region is extended, the
contribution from the 170'' error beam of the IRAM 30 m telescope at
high frequencies, with a fraction of 0.31 of the total intensity on
the Moon (Garcia-Burillo et al. 1993; Greve et al. 1998), cannot be neglected. The IRAM 21 spectra were
therefore reduced in intensity by 25%, a value which is somewhat
arbitrary since the absolute error beam contribution varies for each
position observed. A more sophisticated procedure would be to correct
for the error beam contribution by using molecular line maps obtained
at smaller telescopes, as described in Schneider et al. (1998).
Figure 1 shows the line integrated (-8 to 6 km s-1) 12CO 32 map at 80'' resolution, overlaid on a
2
m image from 2MASS
. The CO emission
distribution is similar to that of the slightly smaller 12CO
1
0 map (50'' angular resolution) by Bally & Scoville
(1982).
The molecular gas with a typical main beam brightness temperature in
the CO 3
2 line above 10 K extends on a size-scale of at least
(
pc). From Fig. 1, the
cloud can be divided into a well defined high intensity core around
the young star S106 IR (
to 30 K) and a more
diffuse, lower intensity (
K) region to the
southwest.
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Figure 2:
Channel maps of the "On-the-Fly'' observations of the 12CO 3![]() ![]() |
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The channel maps of Fig. 2 reveal the velocity
structure of the cloud and isolate individual cloud fragments: At low
velocities (-6 to -2 kms-1), the typical double-peak
structure, which was also seen in the 13CO 10 map (50''resolution like the 12CO 1
0 map) of Bally & Scoville
(1982), is apparent. With increasing velocity, the emission
merges into one peak slightly shifted to the southwest of S106 IR and
a second, pronounced peak (associated with S106 South) establishes
roughly 4' further south to the main peak but disappears at higher
velocities (emission between -2.3 and 1 kms-1). Between -3and 4 kms-1, the lower intensity emission of the extended
molecular cloud is detected southeast of S106 IR, forming "streamers''
of molecular gas and giving the cloud a cometary shaped structure.
The primary star formation site in S106 is located within a radius of
1
7 around S106 IR and contains
160 IR sources (Hodapp &
Rayner 1991). It is coincident with the prominent peak in
CO emission already discussed in Sect. 3.1.1. The second, weaker CO peak
south of S106 IR harbours a small IR cluster and nebulosity (S106
south) evident in the 2MASS image at 2
m: weak
extended emission is apparent 5
south of S106 IR (see
Fig. 1). Since this newly recognized nebula also corresponds to a
slight enhancement in the stellar density distribution of the
brightest 2MASS 2
m sources (sources with
)); e.g., Bontemps (2001),
Knödlseder (2000), we interpret the nebula as a signpost for a
secondary site of star formation in S106. A couple of (most likely)
young stars seen by 2MASS are the brightest members of a probable
embedded cluster referred to here as S106 South. Finally we note that two
mid-IR sources observed by MSX (Price et al. 1998) are also
found in S106 South: MSX5C_G076.3045-00.6721 and
MSX5C_G076.3116-00.6582. They are detected at a 1 to 2 Jy level
between 8 and 15
m and both have a counterpart in the 2MASS point
source catalog. Their IR colors (calculated between 2 and 15
m)
are typical of Class I young stellar objects as defined by Lada
(1987), and their mid-IR fluxes at 600 pc are similar to the flux
of the brightest protostar of the
Ophiuchi cloud (EL29;
Bontemps et al. 2001) suggesting they are as luminous as
EL29, i.e. of the order of 20 to 30
.
![]() |
Figure 3:
The 13CO J=6![]() ![]() |
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The central area (31') around S106 IR (see Fig. 1) was
mapped in 13CO 6
5 and is shown in Fig. 3,
overlaid on a map of [C II] 158
m emission obtained at the KAO
(Schneider et al. 1999a,
1999b; Paper II). The 13CO 6
5 emission extends
outside the mapped region in all directions except to the
east. It closely follows the [C II] emission distribution showing that
this mid-J CO line traces the warm molecular component of PDRs.
The peak intensity of around 13 K, which is equivalent to a
Rayleigh-Jeans corrected temperature of 26 K, is found at offset
(60'', 0), a region with significant [C II] emission, whereas in the
outskirts of the PDR (at 80'', 0), indicated by a strong gradient of
decreasing [C II] intensity, the CO line intensity is reduced to about
6 K. The CO intensity also drops (to 8 K) at the central position
(0, 0) but increases again to 11 K at (-40'', 0).
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Figure 4:
Comparison of isotopomeric CO spectra at the same angular resolution
of 80'' (the 6![]() ![]() |
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Figure 5:
Maps of the line integrated CO 1![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 4 shows 12CO and 13CO 32, and
13CO 6
5 spectra at the position of S106 IR. All CO lines are
strongest at the velocity of the ambient cloud (-1.5 kms-1).
The line profiles are non-Gaussian, indicating a composite
of several velocity components overlapping along the line-of-sight
and/or highly turbulent gas. As we will see in Sect. 3.2, the line
profiles turn out to be even more complex in the higher angular
resolution IRAM observations. Although some of this fine structure is
blended in the KOSMA data, we can still
identify two major components at -1.5 kms-1 and 2 kms-1.
The typical line widths of these components are rather narrow (2 km
s-1) making shock heating of the corresponding gas unlikely. A
two component Gaussian fit to the 12CO 3
2 line reveals
strong excess blue wing emission extending approximately between -5and -10 kms-1. This finding confirms the detection of blue wing
emission by other authors, e.g., in the [C I] 492 GHz line and the
C18O J=3
2 and 2
1 lines by Little et al. (1995). The fit reveals that there is also some, less
prominent, excess redshifted emission at positive velocities between 2
and 6 kms-1. We can identify this red wing emission also in the
13CO 3
2 spectra which is not as obvious in 13CO 6
5
(there, some redshifted emission appears between approximately
1 and 3 kms-1).
In contrast, the blue wing emission (down to -10 kms-1) is
strong in all tracers. The fact that we see this high-velocity
emission even in the 13CO 65 line indicates that it arises
in high column density and warm gas.
The molecular cloud core around S106 IR and the extended PDR region,
an area of
(indicated in Fig. 1), was
observed in the 12CO, 13CO, and C18O 1
0, and
12CO and 13CO 2
1 lines at the IRAM 30 m telescope.
Figure 5 shows grey scale plots of the line integrated
emission of these lines.
The molecular gas is concentrated within two major emission regions
50'' east and 100'' west of S106 IR already visible in the
12CO 32 map (Fig. 2). In between, the lobes of the ionized
gas in the H II region are clearly outlined by a lack of molecular
line emission north and south of S106 IR. The transition zones
between molecular cloud and H II region are marked by a strong CO
emission gradient. We see sharp borders, i.e. edge-on PDRs, running
northeast to southwest in the 13CO and C18O 1
0 maps on
both sides of the cavity.
The stronger eastern CO peak, referred to as "East Clump''
(Little et al. 1995), connects to the western part of the cloud via a
bridge of emission crossing the (sub)mm continuum source S106 FIR
(15'' west of S106 IR). S106 FIR is not resolved as an individual
peak due to beam dilution and is best visible in the 13CO 2
1 map.
There are significant morphological differences between the maps which
mainly reflect differences in excitation and optical depth. 12CO
and 13CO 10 and 13CO 2
1 have an emission maximum
at the edge of the East Clump and trace the temperature profile in the
cloud core with a maximum close to the embedded star S106 IR. The
transitions of the rarer isotopomers 13CO and C18O show more
contrast than the 12CO maps and uncover the column density
distribution of the bulk of the colder material in the cloud away from
S106 IR. These optically thinner lines show a more north-south
oriented distribution and the East Clump in C18O even breaks up
into several distinct clumps along the cavity walls.
Figure 6 shows channel maps of the 12CO and
13CO 21 emission which impressively reveal the complex
spatial and velocity structure of the molecular cloud.
We distinguish five velocity intervals, reflecting the main
dynamical features of the molecular gas:
-9 to -4 kms-1
This blueshifted high-velocity emission, already apparent in the
lower angular resolution CO spectra (see Sect. 3.1), is resolved to be
confined to a small region around S106 IR, coincident with the edge of
the East Clump. More diffuse and extended emission is also
visible approximately 120'' west and 150'' southeast of S106 IR.
-3.5 to -2 kms-1
The high-velocity peak emission at S106 IR starts to merge with the
bulk emission of the cloud. In this velocity range, the "dark lane'' is best visible, evident as a narrow tongue of emission close to
S106 IR in approximately east-west direction.
-1.5 to +0.5 kms-1
This velocity interval represents the bulk emission of the
molecular cloud. The prominent double-peak morphology of the cloud
is evident, with an emission distribution elongated north-south along
both sides of the cavity walls of the optical lobes. Again, the H II region is nicely outlined by a lack of molecular emission. The
two peak emission regions east and west of S106 IR are linked via a
bridge of weaker emission crossing S106 IR, best seen at -1.5 to
-0.5 kms-1. At the tips of the southern and northern
optical lobe, CO emission traces swept-up material at the end of the
north-south flow from S106 IR. This gas is not blue- or redshifted
from the velocity of the ambient cloud since the inclination angle of
the two optical lobes is small,
with respect to the plane
of the sky, and within the range of the aperture angle of the lobes
(
,
Solf & Carsenty 1982).
The observed morphology and kinematics are thus fully consistent with the picture of a cavity created by S106 IR whose radiation and ionized wind sweep-up material from the cavity walls marked by the two lobes of the H II region and at the extreme ends of the flow.
+1 to +2 kms-1
The double-peak structure of the cloud breaks down and the emission
merges into a more diffuse extended plateau at S106 IR where the
molecular emission traces the redshifted component of the stellar wind
hitting the backside of the cavity walls.
+2 to +6 kms-1
At these redshifted velocities, we identify two emission regions
(mainly in 12CO). The first is centered on S106 IR (at 2.5 km
s-1), before shifting north for v=4 to 6 kms-1. The
second appears at 3.5 kms-1, approximately 120'' west of S106
IR, but disappears at 5.0 kms-1. The CO emission distribution
in this velocity range appears not as strong and confined as in the
blueshifted counterpart probably because the densest part of the East
clump is located at the near, blueshifted side of S106 IR.
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Figure 6:
Channel maps of 12CO 2![]() ![]() ![]() ![]() |
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Figure 7:
Isotopomeric CO 1![]() ![]() ![]() |
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The variety in the CO emission distribution is not only due to the complex kinematics of the molecular gas, but also influenced by self-absorption effects, as the following analysis of the spectral line profiles illustrates.
Figure 7 displays spectra selected along a cut at
constant Declination through S106 IR. In all 12CO spectra, we
see broad blue wing emission approximately between -10 and -5 km
s-1, which is strongest at the positions of S106 IR (0, 0) and the
East clump (20'', 0). This high-velocity wing is also seen in
13CO 21 and 1
0 at position (0, 0) and, less prominent,
at (20'', 0). The ratio of the integrated line intensity of 12CO
and 13CO 2
1 in this velocity range is 8 for the (0, 0)
position and 12 towards (20'', 0), indicating that the 13CO
emission is optically thin.
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Figure 8:
Blue and red wing emission and self-absorption in
the red wing component. Positions where the 12CO
2![]() ![]() ![]() ![]() |
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The redshifted counterpart of the blue wing emission is less
pronounced but nevertheless visible in all 12CO 21 spectra
at velocities higher than 3 kms-1. Around 3 kms-1, the 12CO
spectra show a dip in intensity that gets filled in with emission in
the corresponding 13CO spectra, causing the 12CO/13CO
ratio to drop to values around 1 or lower for this velocity range. The
lack of 12CO emission is hence due to self-absorption of the
optically thick 12CO line in cold foreground material, presumably
associated with the extended molecular cloud. Figure 8
shows the blue- and redshifted emission distributions and the
positions where the 12CO/13CO ratio is lower than unity. We
see significant self-absorption in the western part of the region (an
area of
centered on the position -120'', 0)
which explains, at least partly, why prominent red wing emission in
S106 was not previously detected.
The 12CO spectra close to S106 IR, at (0, 0), (20'', 0) and
(-20'', 0), reveal a dip in the line center at -1 kms-1.
Since the 13CO and C18O 10 lines peak at the velocity
of the dip, the optically thick 12CO is hence clearly also
self-absorbed at velocities around -1 kms-1. The two velocity
components at -1 kms-1 and +2 kms-1 in the C18O
1
0 and 13CO 2
1 spectra at S106 IR and the East Clump
are due to a true line splitting, as opposed to self-absorption, which
confirms the finding of Little et al. (1995).
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Figure 9:
Position-velocity channel maps of 12CO and
13CO 1![]() ![]() |
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In order to identify other velocity signatures, e.g., rotation, we display the data cubes as position-velocity channel maps in Fig. 9. First, the most prominent features already introduced in the preceeding sections are again clearly visible: the typical double-peak structure of the molecular cloud with peak 12CO and 13CO emission east and west of S106 IR as well as the prominent "East Clump''. Its close correlation with the highly blueshifted emission suggests that the parts of the East Clump closest to S106 IR are being dispersed by the stellar wind. We also see the blue and red high-velocity wing emission, which show the highest degree of apparent confinement around S106 IR (panels corresponding to 0'' and 20'' offset in declination). The region of self-absorption in the red wing of the 12CO line discussed in the previous section is nicely outlined by the contours of the 13CO emission in the panels with Declination offsets -45'' to 65''.
There is no signature of systematic rotation of the cloud or of a
smooth disk in the position-velocity plots. Instead, the velocities
increase from west and east towards the center. The eastern
gradient is strongest at high southern Declination offsets (lower
panels) with +0.8 kms-1/0.1 pc, the gradient in the west
is smaller (approximately +0.3 kms-1/0.1 pc). North of S106 IR
(DEC offsets >20''), the structure is less tilted and any gradients
are rather small if evident at all. The velocity distribution is also
not compatible with that of an expanding cavity (which was suggested
by Little et al. 1995).
From the high angular resolution isotopomeric, multiline CO data presented in the previous section, we gained new insight on the small scale molecular cloud structure. This enables us to propose a scenario that explains the origin of the observed high-velocity emission distribution.
We attribute the dynamics of the molecular gas to the impact of the
ionized wind of S106 IR, driving a shock into an inhomogeneous
molecular cloud. In order to illustrate this and to discuss the most
promiment features of S106, we selected images of four velocity planes
of the 13CO 21 emission and overlaid them in
Fig. 10 on a JHK picture of S106 taken with the
Subaru
telescope.
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Figure 10:
Four different velocity planes of the 13CO 2![]() |
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Panel a shows highly localized blue wing emission centered just east of S106 IR, panel d the more diffuse red counterpart 20''north-west and southeast of S106 IR. The fact that the blueshifted emission is much more pronounced indicates that the blueshifted part of the ionized wind drives into a denser region/dense clump on the near side of the molecular cloud, leading to larger masses of swept-up material. This emission region is part of the East Clump, which wraps around S106 IR (with the denser part just east of S106 IR and less dense material in front and behind S106 IR). The high velocity emission hence marks where the ionized stellar wind hits the edge of the clump east of S106 IR in the fore- and background.
The dark lane, seen in panel b, appears to be a continuation of the East Clump to higher RA offsets, while the clump containing S106 FIR is linked with a bridge of emission to the East Clump, separating the optical lobes (also visible in Fig. 6 or Fig. 9). The CO emission distribution clearly shows that there is no smooth disk (see also Sect. 3), as it was already excluded by the observations of Barsony et al. (1989), and that the molecular gas is rather clumpy. The bipolar shape of the H II region then can be due to (i) an asymmetric stellar wind (Felli et al. 1984; Persson et al. 1988) or (ii) a very small circumstellar disk that extends within several AU of S106 IR (Bally et al. 1998).
The clumps could be the remnants of a toroid or disk, as it was suggested by Little et al. (1995), but there is no clear evidence for this assumption as reasoned from the position-velocity channel maps of Fig. 9. Moreover, the observed CO emission distribution can be explained exclusively by that of a clumpy molecular cloud. The impact of the H II region on the molecular cloud structure is clearly visible in panel c: east and west of S106 IR, the hot, ionized gas of the optical and radio lobes sweeps up the surrounding molecular gas and we see therefore a sharp gradient between the cavities and the molecular cloud.
The more diffuse and extended blue high-velocity wing (panel a) emission 150'' west and east of S106 IR most likely results from a dispersed wind "leaking'' through the gaps between individual molecular clumps. Panel d) shows red wing emission north and south of S106 IR, with the higher intensity contours closely following the optical/IR lobes, which results from molecular material swept-up from the walls on the far side of the ionized cavity (Richer et al. 1993).
Since the KOSMA 12CO 32 map provides the most complete
coverage of the large scale molecular cloud, we use it in the
following to estimate the total mass of the cloud complex. The
integrated line intensity of the map leads to an estimate of 2000
for the total mass and an average density of 1400 cm-3.
We adopted a distance of 600 pc and used the conversion factor
(X-factor) of
cm-2 K-1 (kms-1)-1 (Strong et al. 1988) for the conversion of
the 12CO line integrated intensity into H2 column densities.
Even though this conversion factor was determined for the 1
0
transition of CO, we adopt this value for the 3
2 line since the
ratio of the line integrated intensities 12CO 1
0/3
2,
using our KOSMA 12CO 3
2 data and data from Bally & Scoville
(1982), is typically 1 (at a few positions it increases up
to 1.4). Bally & Scoville determined a mass of 1200
from
their 13CO data, using a distance of 500 pc and not including the
lower intensity outer regions of the cloud.
We performed a clump identification on the spatially fully sampled
KOSMA 12CO 32 and IRAM 13CO 2
1, 13CO 1
0,
and C18O 1
0 data sets. The latter cover 7% of the KOSMA
12CO 3
2 map. We used the algorithm GAUSSCLUMPS, developed by
Stutzki & Güsten (1990) and discussed in Kramer et al.
(1998a), to decompose three-dimensional data (two spatial
axes and the velocity axis) into individual clumps, assuming Gaussian
density and velocity distributions. Only clumps which are
intrinsically (i.e., after deconvolution) larger than 50% of the
spectral and spatial resolution were considered. The clump masses
were calculated assuming optically thin emission and LTE (Local
Thermodynamic Equilibrium) for the 13CO and C18O lines (as
described in, e.g., Schneider et al. 1998 or Herbertz et al. 1991) and a distance of 600
pc. The values for the excitation temperatures
and
optical depths (for the optically thin lines) were taken from Sect. 4.3. (IRAM data) or determined from the KOSMA 3
2 map.
Figure 11 shows a log-log plot of the combined clump-mass spectrum obtained from the 4 molecular tracers. The clumps from the IRAM data are scaled to match the KOSMA histogram according to the procedure described in Schneider et al. (1998) and Heithausen et al. (1998). For all data sets, the number of clumps increases with decreasing mass until a turn over point, the completeness limit, is reached which results from finite angular resolution and limited Signal-to-Noise (S/N) ratio of the data.
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Figure 11:
Combined clump-mass spectrum derived from the KOSMA 12CO 3![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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The 12CO 32 clump-mass spectrum covers a mass range of 1 to
350
on a size-scale of clumps between 0.12 to 0.9 pc. In
contrast, the higher resolution IRAM maps are more sensitive to the
small scale structure and cover a mass interval from approximately 0.1
to 60
with clump sizes from 0.06 to 0.2 pc. Thus, due to the
lower angular resolution of the KOSMA map, the 12CO 3
2
emission is decomposed into larger, more massive clumps and a lower
number of small clumps. The turnover in the clump-mass spectra and
the lowest mass identified are different in the individual IRAM data
sets because (i) the 13CO 2
1 map has a factor 2 higher
angular resolution compared to the isotopomeric CO 1
0 maps, and
therefore traces the smallest structures and less massive clumps, and
(ii) the maps have different Signal-to-Noise ratios (the best quality
map is that of 13CO 1
0 with a peak S/N ratio of 110,
followed by 13CO 2
1 (S/N=67) and C18O 1
0
(S/N=25). Accordingly, a higher temperature threshold was used for the
C18O clump identification.
A fit to the power law function
,
in which
denotes the number of clumps within the mass interval
,
for
masses above the completeness limit yields the same value of the
clump-mass spectral index for each data set within the error
(typically 1 to 2%):
for 12CO 3
2,
for 13CO 2
1,
for 13CO 1
0, and
for C18O 1
0. The run of the power
law function with the rounded value of
is indicated as a
straight line in Fig. 10. The common clump-mass spectral index shows
that the structures are self-similar at least over a length-scale from
0.06 to 0.9 pc, the sizes of the smallest and largest clump. This
result is remarkable, considering that we used molecular lines with
different opacities, tracers of different excitation conditions and
because the spatial and kinematic structure of S106 is governed by the
interaction with the stellar wind.
The observed clump-mass distribution is typical for Giant Molecular Clouds and the clump-mass spectral index of 1.7 agrees with results from other molecular clouds, typically 1.4 to 1.9 (Kramer et al. 1998a; Simon et al. 2001), in a broad range of different interstellar clouds and using different molecular tracers.
In order to estimate the excitation conditions throughout the
S106 region including the interface of the molecular cloud to the
H II region, we perform a straight-forward LTE analysis,
using 12CO, 13CO, and C18O 10 data. We use these
lower frequency observations since they are less affected by the error
beam (see Sect. 2). The excitation temperature (
)
is
calculated by assuming an optically thick 12CO line and optically
thin 13CO and C18O 1
0 line (Little et
al. 1995). Since we assume LTE the excitation temperatures
for all isotopomers are equal. With the resulting opacities and the
line integrated 13CO and C18O intensities in K kms-1,
we derive the 13CO and C18O column density and H2 column
density as described in, e.g., Frerking et al. (1982) and
Dickman (1978).
Offset |
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13CO/C18O | N(13CO) | N(13CO)/N(C18O) | N(H2) | ||
RA ('') | Dec ('') | (K) | line ratio | (1017 cm-2) | (1022 cm-2) | |||
80 | 0 | 40 | 0.6 | 4 | 0.8 | 4 | 3.8 | |
40 | 0 | East | 54 | 0.3 | 4 | 0.6 | 3 | 2.8 |
20 | 0 | 43 | 0.6 | 6 | 0.7 | 4 | 3.3 | |
0 | 0 | IR | >32 | <0.8 | 6 | <0.6 | 6 | <2.8 |
-20 | 0 | FIR | >29 | <0.5 | 8 | <0.4 | 8 | <1.9 |
-40 | 0 | 27 | 0.4 | 11 | 0.5 | 17 | 2.4 | |
-80 | 0 | 49 | 0.6 | 7 | 1.5 | 12 | 7.1 |
Table 2 gives an overview of the physical conditions of the bulk
emission of the molecular cloud (at a velocity of -1.0 kms-1)
along an east-west cut from +80'' to -80''. The results
especially at the positions of S106 IR and S106 FIR should be treated
with caution since the 12CO line shows self-absorption effects
around -1 kms-1. The excitation temperatures are therefore
lower limits and the opacities and column densities upper limits.
Keeping that in mind, we find that the maximum values for
(around 45 K) are in the eastern part of the molecular cloud. The
opacity of the 13CO line is generally smaller than 1 with a
minimum of 0.25 at (40'', 0) and a maximum of 0.8 at the position of
S106 IR. A direct comparison between S106 FIR, S106 IR, and the East
Clump shows that the 13CO line remains optically thin everywhere
at an excitation temperature of around 30 K for S106 IR and the East
Clump and a slightly higher value (40 K) for S106 FIR. Generally, the
derived values for excitation temperatures and column densities agree
well with the ones given by Little et al. (1995), obtained
from JCMT observations (not affected by any error beam pick-up). From
the average H2 column density of 3.4
1022 cm-2, we
derive an average density of 9.1
103 cm-3 of the cloud
core region (from its projected
400'' size in the CO maps and
assuming the same extent along the line-of-sight).
We determine the 13CO/C18O line and column density ratio in
order to look for systematic changes of this ratio along the cut. The
13CO/C18O ratio is expected to increase in regions of high
incident UV radiation due to effective self-shielding of the more
abundant species 13CO. If the cloud structure is clumpy on small
scales, this effect is even enhanced since small clumps have even less
shielding column for the C18O molecule to survive. The
13CO/C18O ratio is thus also correlated with the sizes of
the clumps. (See Zielinsky et al. 2000 for a detailed
discussion of these issues.) In our case, the 13CO/C18O
brightness ratio along the cut takes values between 4 and 11 which is
close to the natural isotopic abundance of 7. Since the
13CO column densities were determined including the line
opacities, the column density ratio is a more reliable tracer of
changes in the 13CO/C18O abundance ratio. We find values in
the range from 3 to 8 for the positions -20'' to 80'', and
significantly larger at -40'' and -80'' with ratios of 17 and 12, respectively. The low ratios observed towards the East Clump
suggest that the bulk of CO emission originates in rather large clumps
and that selective self-shielding is only important in a thin surface
layer of the clumps and close to the interface to the H II region.
To further analyze the correlation between changes in the
13CO/C18O ratio and the UV radiation, we show in
Fig. 12 an image of the 13CO/C18O 10
integrated intensity ratio for a 0.5 kms-1 wide channel centered on
v=-1 kms-1. The high ratios at the outer cloud boundaries are due to
noise in the C18O emission, but the low ratios toward the eastern
and western CO peaks indicate moderate optical depths for the
13CO line and no depletion (i.e., effective shielding) of the
C18O molecule.
The ratios are highest where CO is not depleted completely and the [C II] emission is intense: (1) towards the bridge of emission across S106 IR, (2) along the southwestern cavity wall of the H II region, following the tongue of [C II] emission seen in Fig. 3, and (3) towards the tip of the southern optical lobe. In these regions, we see a steep gradient of the ratio with distance away from the UV source and the H II region, supporting our assessment that the bulk of the emission originates from rather large, well shielded clumps and that selective self-shielding of 13CO is only important close to the H II region.
A more sophisticated approach to determine the physical parameters of
the molecular cloud or clump is to solve the radiative transfer
equation explicitly but using the approximation that the level
populations are independent of the position in the cloud. Then, the
probability of a photon to leave the cloud without being absorbed
depends on the geometry considered and on the value of the optical
depth. Here, we use an escape probability formalism for a
homogeneous, spherical cloud (Stutzki & Winnewisser 1985)
which computes line intensities, integrated intensities, rotational
temperatures, and optical depths in a user-defined data cube spanned
by the molecular column density N(CO), H2 density n(H2), and
kinetic temperature
.
The collision rates were taken from
Flower & Launay (1985).
We use the observed 13CO 65/13CO 3
2 and 13CO
2
1/13CO 1
0 line ratios (all data on or smoothed to an
angular resolution of 80'') to constrain a parameter space for
N(13CO),
), and
since the beam filling
factor cancels out to first order by using line ratios. We focus on
only one position (S106 IR) since the 80'' KOSMA beam comprises the
East Clump and S106 FIR. In addition, the variation of
and
in our LTE analysis across this area is not large, as it
was shown in Sect. 4.3, so that the results for S106 IR should yield a
good constraint on the excitation conditions in the molecular cloud
core.
The 13CO 65/13CO 3
2 peak line ratio of 0.7
together with a 13CO 2
1/13CO 1
0 ratio of 1.2 is
only consistent with escape probability models of kinetic temperatures
between 40 and 100 K. We adopt an average excitation temperature of
40 K from the LTE analysis to derive a hydrogen density of
cm-3 and a 13CO column density of
cm-2 from the corresponding escape probability
model at
K. The corresponding H2 column density
then is
cm-2. This value is only a factor 2
larger than the H2 column density determined by the LTE analysis,
indicating that the beam is filled rather homogeneously. We can now
determine a typical clump size by
with
the local density of
cm-3 and the column density
given by the model. The typical diameter of a clump
then is 0.22 pc (1
2), which is rather large and implies a
predominantly homogeneous structure of the material in that
region. This finding supports the scenario of large clumps with high
area filling found from the comparison of the 13CO to C18O
line and column density ratios. The co-existence of very small, high
density clumps, however, is not excluded. In fact, the clump
decomposition of the IRAM CO data indicates substructure (Sect. 4.2)
below 0.22 pc. We therefore derive beam and volume filling factors in
the following section to address this issue.
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Figure 12:
Map of the 13CO/C18O 1![]() |
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The beam filling factor
is calculated from
with the observed main beam brightness temperature
of the respective transition (
)
and the temperature
which is obtained from the escape probability model,
given the kinetic temperature, column and volume densities (Beuther et
al. 2000).
varies between 40% for the 13CO
6
5 and 13CO 3
2 transitions, 50% for 13CO 2
1,
and 60% for 13CO 1
0. The volume filling factor of clumps
is a measure for the small scale structure in a cloud and is defined
as
.
In our case the average density is
cm-3, determined from the LTE analysis, and the local density is
cm-3 obtained from the Escape Probability
Model. The density of the interclump medium,
cannot be deduced in a straight-forward manner. Due to the
rather high local and average densities, however, the volume filling factor
remains 0.1 (10%) for a density regime of 50 to 600 cm-3 as a
realistic range for
.
Our value of 10% (typical values
are a few to 20%) implies a rather low volume filling and therefore
small scale structure of the molecular material. This result is not in
contradiction to the results obtained in Sects. 4.3 and 4.4
that the low-J CO emission arises from a predominantly homogeneous
medium (clumps on a size-scale larger than 0.2 pc (1'), with a
density around 104 cm-3 and a temperature of
K)
if we postulate the existence of embedded, small (
0.2 pc), high
density (
cm-3) and presumably warm clumps with
a low volume filling factor. In this picture, the observed 13CO 6
5
emission arises from these high density clumps, since the critical
density of the 6
5 transition is much larger than the density for
the large clumps, derived from the CO line analysis. In Part II of
the series, we will support this scenario of a two-component gas phase
by modelling the observed CO line intensities as well as [C II] and
[O I] fine structure lines to derive the temperature of the warm PDR
gas and the intensity of the incident UV flux.
We presented a spectroscopic study of the molecular cloud associated with S106 in mm and submm rotational transitions of CO isotopomers obtained with the KOSMA 3 m and IRAM 30 m radiotelescopes. The main results of this study are summarized below as follows.
1. The KOSMA 12CO 32 map reveals the large scale
distribution of molecular gas (
or
pc at
a distance of 600 pc). The total mass is 2000
and the average density
cm-3.
2. The IRAM 12CO and 13CO 21, and 12CO, 13CO
and C18O 1
0 observations focus on the molecular cloud core
around S106 IR (
). We identify two well defined emission
maxima east and west of S106 IR separated by 3', with the H II region outlined by a lack of emission. On a smaller scale, we distinguish
two dense molecular clumps east (East Clump) and west (S106 FIR, not
resolved) of S106 IR.
An analysis of the line profiles shows that there is self-absorption
in 12CO around S106 IR at -1 kms-1 (the velocity of the
bulk emission of the cloud) as well as at +3 kms-1, partly
hiding the redshifted (from 2 to 6 kms-1) counterpart of the
blue wing emission.
3. The high angular resolution position-velocity and velocity channel maps of CO clearly show that there is no smooth molecular disk on a size-scale of 6'. Our observations also do not support an expanding cavity. A fragmented toroid, however, cannot be completely excluded, but the CO emission distribution can be exclusively explained by a fragmented molecular cloud.
The emission distribution of the high-velocity gas can be explained by the ionized wind of S106 IR, driving a shock into the clumpy molecular cloud.
4. The 12CO 32 map and the 13CO and C18O
2
1 and 1
0 maps were decomposed into clumps.
We find a common clump-mass spectral index of
,
which indicates self-similarity of the detected
structures over length-scales from 0.06 to 0.9 parsec.
5. We discuss the excitation conditions along a cut through the
molecular cloud and S106 IR within the framework of an LTE and Escape
Probability analysis. We find that the kinetic gas temperature is
typically 40 K and that the 13CO lines are optically thin. The
average density of the cloud in the core region is
cm-3 and the local density
cm-3,
leading to a volume filling factor of 10%. Since the typical size-scale of
the clumps is 0.22 pc (1
2) and the observed 13CO/C18O
line and column density ratios reflect the natural isotopic abundance,
we derive the following scenario for the molcular cloud:
very small (
0.2 pc), high-density clumps with a small volume filling
factor coexist with rather homogeneous, low-density and spatially extended
clumps.
Acknowledgements
The KOSMA 3 m submillimeter telescope at the Gornergrat-Süd is operated by the University of Cologne in collaboration with Bonn University, and supported by special funding from the Land NRW. The observatory is administered by the International Foundation Gornergrat and Jungfraujoch.We thank the referee, Dr. R. Gehrz, for useful suggestions to clarify and improve the manuscript.