Issue |
A&A
Volume 499, Number 1, May III 2009
|
|
---|---|---|
Page(s) | 233 - 247 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/200911617 | |
Published online | 27 March 2009 |
Linking pre- and proto-stellar objects in the intermediate-/high-mass star forming
region IRAS 05345+3157
,
,![[*]](/icons/foot_motif.png)
F. Fontani1,2 - Q. Zhang3 - P. Caselli4 - T. L. Bourke3
1 - ISDC, Ch. d'Ecogia 16, 1290 Versoix, Switzerland
2 -
Observatoire de Genève, University of Geneva, Ch. de Maillettes 51, 1290 Sauverny, Switzerland
3 -
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
4 -
School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
Received 2 January 2009 / Accepted 25 February 2009
Abstract
Context. To better understand the initial conditions of the high-mass star formation process, it is crucial to study at high angular resolution the morphology, the kinematics, and the interactions of the coldest condensations associated with intermediate-/high-mass star forming regions.
Aims. This paper studies the cold condensations in the intermediate-/high-mass proto-cluster IRAS 05345+3157, focusing on the interaction with the other objects in the cluster.
Methods. We performed millimeter high-angular resolution observations, both in the continuum and several molecular lines, with the PdBI and the SMA. In a recent paper, we published part of these data. The main finding of that work was the detection of two cold and dense gaseous condensations, called N and S (masses 2 and
), characterised by high values of deuterium fractionation (
0.1 in both cores) obtained from the column density ratio N(N2D+)/N(). In this paper, we present a full report of the observations, and a complete analysis of the data obtained.
Results. The millimeter maps reveal the presence of 3 cores inside the interferometer primary beam, called C1-a, C1-b and C2. None of them are associated with cores N and S. C1-b is very likely associated with a newly formed early-B ZAMS star embedded inside a hot core, while C1-a is more likely associated with a class 0 intermediate-mass protostar. The nature of C2 is unclear. Both C1-a and C1-b are good candidates as driving sources of a powerful 12CO outflow, which strongly interacts with N, as demonstrated by the velocity gradient of the gas along this condensation. The ´´ linewidths are between 1 and 2 km s-1 in the region where the continuum cores are located, and smaller (
0.5-1.5 km s-1) towards N and S, indicating that the gas in the deuterated condensations is more quiescent than that associated with the continuum sources. This is consistent with the fact that they are still in the pre-stellar phase and hence the star formation process has not yet taken place there.
Conclusions. The study of the gas kinematics across the source indicates a tight interaction between deuterated condensations and the sources embedded in millimeter cores. For the nature of N and S, we propose two scenarios: they can be low-mass pre-stellar condensations or ``seeds'' of future high-mass star(s). However, from these data it is not possible to establish how the turbulence triggered by the neghbouring cluster of protostars can influence the evolution of the condensations.
Key words: stars: formation - ISM: molecules
1 Introduction
The initial conditions of star formation are still a
matter of debate. Studies have begun to unveil the chemical and physical
properties of starless low-mass cores on the verge of forming
low-mass stars (Kuiper et al. 1996; Caselli
et al. 2002a,b;
Tafalla et al. 2002, 2006),
demonstrating that in the dense and cold nuclei of these cores,
C-bearing molecular species such as CO and CS are strongly depleted
(e.g. Caselli et al. 2002b; Tafalla et al. 2002),
while N-bearing molecular ions such as N2D+ and ´´ (Caselli et al. 2002a,b; Crapsi et al. 2005) maintain
high abundances in the gas phase, and their column
density ratios reach values of 0.1 or more, much higher than
the cosmic [D/H] elemental abundance (
,
Oliveira et al. 2003).
The characterisation of the earliest stages of the formation process of high-mass
stars is more difficult than for low-mass objects, given their shorter evolutionary
timescales, larger distances, and strong interaction with their
environments. Nevertheless, significant progress has been made
by various authors who have performed extensive
studies aimed at the identification of massive protostellar candidates,
i.e. very young (<105 yr), massive (M>8 )
stellar
objects which have not yet ionised the surrounding medium
(Molinari et al. 1996;
Sridharan et al. 2002; Fontani et al. 2005).
On the other hand, the pre-protostellar stage, namely the
phase in which a cold starless core evolves towards the
onset of the formation of a high-mass protostar, has not yet
been investigated in great detail, even though in the last
few years an increasing effort has been devoted to this study (see e.g. Wang
et al. 2006; Zhang et al. 2009; Beuther & Sridharan 2007).
Many ultracompact (UC) H II regions are located in clusters (see e.g. Thompson et al. 2006), and it is common to find massive young stellar objects in different evolutionary stages in the same star forming region (Kurtz et al. 2000). Therefore, one expects to find even earlier phases of massive star formation in the vicinity of UC H II regions and/or other ``signposts'' of massive star formation activity. With this in mind, several authors have searched for cold and dense spots in the neighbourhood of luminous IRAS point sources (Fontani et al. 2006), UC H II regions (Pillai et al. 2007) and methanol masers (Hill et al. 2006). In particular, Fontani et al. (2006) searched for N2D+ emission in the gas associated with 10 luminous IRAS sources with the IRAM-30 m telescope, and detected deuterated gas in 7 out of the 10 sources observed.
The subject of the present work is one of the sources
studied by Fontani et al. (2006), which stands out
for its very interesting characteristics: it is a high-mass
(180
,
Fontani et al. 2006) dusty
clump, undetected in the MSX 8
m band, located
near the luminous IRAS point source 05345+3157 (
60
to the N-E). The region is located
at a distance of 1.8 kpc (Zhang et al. 2005),
and its surface density (
1.3 g cm-2) and
mass-to-luminosity ratio (
)
indicate that it is potentially a site of massive
star formation (see Fig. 1 of Chakrabarti & McKee 2005).
Hereafter, we will call our target i.
Previous interferometric studies have reavealed a clumpy
structure of the molecular gas in i (Molinari et al. 2002).
From IRAM-30 m data, Fontani et al. (2006) have measured
an average CO depletion factor (ratio between expected and
observed CO abundance) of
3 and an average
deuterium fractionation (the column density ratio between
a deuterated species and the corresponding one containing hydrogen)
of
0.01, three orders of magnitude higher than the cosmic
[D/H] abundance. These findings indicate for the
first time the possible presence of a high-mass pre-stellar core
(with
K and
cm-3), analogous
to those detected in several low-mass star forming regions.
However, the angular resolution was insufficient to determine
whether we are dealing with a single high-mass core or instead with
a sample of low-mass ones.
Therefore, we recently mapped i at high-angular resolution in
the (1-0) line with the IRAM Plateau de Bure Interferometer
(PdBI), and in the ´´ and N2D+ (3-2) lines with the Submillimeter Array (SMA),
in order to derive a detailed map of the deuterium fractionation in the
source.
Simultaneously, we obtained observations in the continuum at 96,
225 and
284 GHz with the two interferometers,
as well as in several lines of other molecules. The preliminary results of these observations,
focused mainly on the deuterium fractionation derived from the ´´ and N2D+ data, have been
published by Fontani et al. (2008, hereafter Paper I).
For completeness, in Fig. 1 we summarise the main
observational results of that work, by showing: (i) the 3 mm
continuum observed with PdBI, which reveals the presence of 4 cores,
one of which lies outside the interferometer primary beam;
(ii) the distribution of the intensity of the
(1-0) line, which is extended and has a complex structure;
(iii) the distribution of the N2D+ (3-2) line integrated emission,
concentrated in two condensations, called N and
S. The integrated emission of the (3-2) line (not shown in Fig. 1)
is compact, and is detected towards the strongest continuum peak only.
In Paper I we derived the masses of N and S,
which are
9 and
2.5
,
respectively. Also,
from the N2D+/´´ column density ratio we
obtained a deuterium fractionation of
0.1 in both
condensations, which is the typical value
derived in low-mass pre-stellar cores.
![]() |
Figure 1:
Summary of the main findings of Paper I: the dashed
contours represent the intensity of the (1-0) line
integrated between -21.2 and -14.5 km s-1, corresponding
to the main group of the hyperfine components of this line,
observed with the PdBI (see also Fig. 2 of Paper I). Levels range from
the 3 |
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In this work we present a full report of the observations presented in Paper I, and a complete analysis of the data obtained. In Sect. 2 we describe the observations and the data reduction, while the results are presented in Sect. 3. In Sect. 4 we derive the main physical parameters, which are then discussed in Sect. 5. The main findings of this work are summarised in Sect. 6.
Table 1: Molecular transitions observed with the SMA and the PdBI.
2 Observations and data reduction
![]() |
Figure 2:
Top left panel: map of the 284 GHz continuum (grey scale)
obtained with the Submillimeter Array. The first level is the
3 |
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2.1 Submillimeter Array observations
Observations of N2D+ (3-2) (at 231321 MHz) and (3-2) (at 279511.7 MHz)
towards i were carried out with the SMA (Ho et al. 2004) in the compact
configuration on 30 January and 21 February 2007, respectively.
The correlator was configured to observe
the continuum emission and several other molecular
lines simultaneously (see Table 1). The phase centre was the nominal
position of the sub-mm peak detected with the JCMT (Fontani et al. 2006),
namely RA(J2000) =
and Dec(J2000) = 32
00
06
,
and the local
standard of rest velocity
is -18.4 km s-1.
For gain calibrations, observations of i were alternated
with the quasars 3C 111 and J0530+135. Quasar 3C 279 and Callisto
were used for passband and flux calibration, respectively.
The SMA data were calibrated with the MIR package (Qi 2005),
and imaged with MIRIAD (Sault et al. 1995).
Channel maps were created with natural weighting, attaining a
resolution of: 3
7
3
0 for the N2D+ (3-2)
channel map; 3
0
2
8 for the 225 GHz continuum image;
2
7
2
0 for the (3-2) channel map;
1
9
1
2 for the 284 GHz continuum image.
At the assumed distance of 1.8 kpc, these values translate
into spatial resolutions of
0.025 and
0.01 pc at
225 GHz and 284 GHz, respectively (i.e. 5000 and 2000 AU,
respectively).
The 3
level in the 225 and 284 GHz continuum images is
0.006 and 0.018 Jy beam-1, respectively.
The spectral resolution in velocity for the N2D+ and (3-2)
was 0.53 and
0.44 km s-1, respectively.
All the lines observed are listed in Table 1:
in Cols. 1 and 2 we give the transitions observed and the line
rest frequency, respectively; Col. 3 gives the spectral resolution;
Col. 4 reports on the detection (Y) or
non-detection (N) of the transition, and the 3
level
in the channel maps of the detected transitions is given
in Col. 5.
2.2 Plateau de Bure Interferometer observations
We observed the (1-0) line at 93173.7725 MHz towards i with the
PdBI on 11 and 20 August 2006, in the D
configuration, and on 3 April 2007 in the C configuration.
In Table 1, the spectral resolution in velocity is given.
We used the same phase reference and
velocities as for
the SMA observations. The nearby point sources 0507+179 and 0552+398 were
used as phase calibrators, while bandpass and flux scale were
calibrated from observations of 3C 345 and MWC 349,
respectively. For continuum measurements, we placed two
320 MHz correlator units in the band when making the observations in
D configuration, and six 320 MHz correlator units in C configuration.
The ´´ lines were excluded in averaging these units to produce the
final continuum image (at
96095 MHz). The synthesised beam size of
the ´´ channel map was 3
2
3
4, while that of the
continuum was 3
1
3
2, which translates into a
spatial resolution of
0.03 pc.
The 3
level in the continuum image is
Jy beam-1.
We stress that the observations of the (1-0) and N2D+ (3-2) lines have
approximately the same angular resolution.
The data were reduced with the GILDAS software,
developed at IRAM and the Observatoire de Grenoble.
2.3 Combining SMA and NRAO data for 12CO (2-1)
The problem of the missing short spacing information on the SMA
data of the 12CO (2-1) line can be solved combining the SMA data
with the peviously published 12CO (2-1) map from the NRAO-12 m telescope (Zhang et al. 2005). For observing details on the single-dish observations
we refer to the paper by Zhang et al. (2005). The single-dish
data were converted to visibilities in the MIRIAD package with the
task UVMODEL. The interferometer and single-dish data were then
processed together. The synthesised beam of the combined data
is 2.87
3.60
(PA
42
).
For more details on the method adopted
see e.g. Zhang et al. (2007).
2.4 Data reduction
The (1-0), (3-2), and N2D+ (3-2) rotational transitions have hyperfine structures. To take this into account, we fitted the lines using METHOD HFS of the CLASS program, which is part of the GAG software developed at IRAM and the Observatoire de Grenoble. This method assumes that all the hyperfine components have the same excitation temperature and width, and that their separation is fixed to the laboratory value. The method also provides an estimate of the total optical depth of the lines, based on the intensity ratio of the different hyperfine components. For the rest frequencies of the ´´ and N2D+ lines, we used the laboratory values given in Crapsi et al. (2005). We have not applied the corrections given in Pagani et al. (2008), since these are well below the spectral resolution of our observations.
![]() |
Figure 3:
Left panel: map of the 284 GHz continuum (solid white contours)
obtained with the Submillimeter Array,
superimposed on the Spitzer MIPS image of i at 70 |
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3 Results
3.1 Continuum maps
The 284 and 225 GHz continuum images obtained with the SMA are shown in the top and bottom left panels of Fig. 2, respectively. For a complete comparison among the three continuum maps, in Fig. 2 we also show the continuum emission at 96 GHz, already presented in Fig. 1.
At 284 GHz, three main compact cores are detected inside the
SMA primary beam (44
), two of them close to the
map centre and the other one is
10
S-E of the map centre.
We will call the central condensations C1-a and C1-b, respectively,
because they are located at the position of source C1 in the 96 GHz image,
while the eastern one exactly matches the emission peak of the core C2. Among the other 96 GHz
continuum sources shown in Fig. 1, we clearly detect C3 outside the
interferometer primary beam (not shown in Fig. 2), while C4 is undetected.
At 225 GHz, the continuum sources C1-a and C1-b are blended
into C1 as in the 96 GHz image (Fig. 1), and C2 is clearly detected
as well. As for the 284 GHz image, C4 is
undetected while C3 is detected but not shown because outside the
primary beam, corresponding to the interferometer field
of view.
There is a faint emission 18
to the NE of C1-a and
C1-b, but we decided not to consider this as a real source because it
is detected at 6
in this image only, and quite close to the edge
of the interferometer primary beam.
Because C3 and C4 are outside and on the edge of the primary beam, respectively, we decided not to discuss these sources further in the following.
Spitzer Post-Basic Calibrated Data (PBCD) at 24 and 70 m were
obtained from the Spitzer Archive. The data were taken in
Photometry/Super Resolution mode as part of program 20635 (R. Klein, PI).
Observations at 24 microns were obtained on 7 October 2005 (AORKEY
14944768), with an integration time of 99 s, and at 70 microns on 2 April
2006 (AORKEY 14945024) with an integration time of 76 s (using the Fine
Scale mode). At present no IRAC observations have been made.
The left and right panels of Fig. 3 show the
Spitzer MIPS continuum images at 70
m and 24
m. In both
images, two peaks roughly coincident with the
submillimeter continuum sources C1 and C3 are detected. At 70
m,
an extended emission is detected towards C2, S and the southern portion
of N, but we believe that it is just due to the low angular resolution of
the map (
18
), which do not allow us
to disentangle the contibution of the different sources.
The 24
m continuum emission shows two peaks spatially coincident
with the 70
m ones, but they are both more centrally peaked than at
70
m, and have smaller extensions, probably due to the better angular resolution
(
6
at 24
m). A faint emission is detected towards C2, at the edge
of the main emission peak.
No emission is detected towards N and S at this wavelength.
![]() |
Figure 4:
Integrated intensity of the hyperfine component F1 F =
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3.2 Molecular line emission
In Paper I we have shown and discussed the distribution of the integrated intensity of the N2D+ and ´´ lines (see also Fig. 1). However, as said in Sect. 2.1, several transitions of other species have been observed and detected simultaneously as the N2D+ and ´´ ones. In this section, we complete the analysis started in Paper I and show a full report of the observations obtained.
Table 2: Line parameters for calculations of the 12CO (2-1) outflow.
3.2.1 Integrated emission map of the optically thin component of the N2H+ (1-0) line
The integrated intensity of the main group of hyperfine components
of the (1-0) line is shown in Fig. 1.
As already discussed in Sect. 1, the emission is extended and presents
several bumps which are not resolved into separate emission peaks.
This may be the real shape of the emission in this tracer, or
it can be due to other reasons, such as an insufficient angular resolution, or
opacity effects. To better understand this, in Fig. 4 we
show the distribution of the integrated intensity of the
hyperfine component
only, which is
well separated from the other components and it is expected to be optically
thin: from the fitting procedure described in Sect. 2.4,
we obtain an optical depth for this component of
.
Figure 4
shows that the extension of the integrated
intensity of this component is similar to that shown in Fig. 1,
but in this case we do detect five emission peaks. This suggests that, since the
angular resolution is the same, the lack of well separated
intensity peaks in Fig. 1 is probably due to optical depth effects.
The main emission peak is
located 4
north of C2, while the others are
located about
5
east of C1, and
5
south
of C2, respectively, and two fainter peaks (detected at
)
are seen towards core N. None of the millimeter sources
coincide with the five ´´ emission peaks. These results indicate
that the source can host other dense cores which are not detected
in the millimeter continuum observations, probably because they are
too cold.
3.2.2 Integrated emission map of the 12CO (2-1) line wings
Single-dish observations of the source in the 12CO (2-1)
line have been performed by Zhang et al. (2005), with
a 29
angular resolution. They detected a massive outflow
in the non-Gaussian line wings, the orientation of which is approximately in
the WE direction, but the angular
resolution was not sufficient to detect either the outflow center
and the detailed morphology of the outflow itself.
The observations reported in this work significantly improve
the angular resolution of the previous ones, allowing us
to better determine the outflow shape and identify its origin.
In Fig. 5, we show the map of the integrated intensity in the 12CO (2-1) line wings, derived from channel maps obtained combining SMA and NRAO data, as described in Sect. 2.3. The blue- and red-shifted emissions have been averaged in the velocity intervals (-46.4, -26) km s-1 and (-9.2, 6.4) km s-1, respectively. The outflow axis is predominantly oriented in the WE direction, with redshifted gas in the east and blueshifted gas in the west. The lobes are clearly separated and have approximately a biconical shape. The outflow center is near the position of the continuum source C1, and the exciting source can be either C1-a and C1-b. The source coincident with the most western peak of the (1-0) line integrated emission can also contribute to the observed emission, but is less likely to contribute than the continuum sources, due to the fact that there are no other signs of protostellar activity associated with it. The blueshifted gas shows a fainter secondary peak to the north of the map. From geometrical considerations, this northern blue-shifted emission might be driven by a source within N, rather than C1-a or C1-b. However, as we will further discuss later, the sources embedded within N are probably in the pre-stellar phase, i.e. prior to the main accretion phase in which the outflow is expected to form, so that this solution seems to us very unlikely.
The outflow length, from end-to-end, is approximately 35
(if we do not consider the secondary peaks of the blueshifted
emission), corresponding to
0.28 pc at a distance of 1.8 kpc.
The semi-opening angle is between about 30 and 40
,
and the
spatial separation of the lobes suggests that the inclination angle
with respect to the line of sight is likely to be very close
to the plane of the sky (see also Cabrit & Bertout 1986).
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Figure 5:
Top panel: red- and blue-shifted integrated emission
of the 12CO (2-1) line (combined SMA + NRAO data), superimposed on the 96 GHz
continuum map observed with the PdBI (grey-scale). Both red and blue contours
start from 0.25 Jy beam-1 (
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In Table 2 we give the line parameters for the
calculation of the outflow properties, namely:
the velocity range of the blue- and red-wings,
and
(Cols. 1 and 2, respectively), the
integrated intensity of 12CO (2-1) in the wings,
(blue) and (red)
(Cols. 3 and 4; T is the main beam brigthness temperature), and the maximum
velocity of the wings,
and
(Cols. 5 and 6), defined as the difference
between the maximum velocity of the blue- and red-wings and the
systemic velocity (i.e. -18.4 km s-1). The values listed in Cols. 3 and 4
are averaged values over the blue and the red lobes,
respectively.
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Figure 6:
Integrated maps of all the molecular lines listed
in Table 1, detected towards
i with the SMA. For all transitions, the emission has been averaged over all the
channels with signal. In each panel, the transition is indicated in the
top left corner, the grey scale represents the 94 GHz continuum, and
the position of the mm cores is indicated by the white crosses.
For 13CO, C18O, CH3OH (8-1,8-70,7) and SO, the contours start
from the 3 |
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3.2.3 Integrated intensity of other lines
In Fig. 6 we show the distribution of the integrated intensity of all the detected transitions listed in Table 1, averaged over the channels with signal, except for 12CO (2-1) that has been already discussed.
The integrated intensity of the 13CO (2-1) line peaks at the position of C1, but it shows an elongated shape towards the north-east, suggesting that some of the emission comes from the outflow. On the other hand, the C18O (2-1) line emission is less extended and it seems to arise from a common gaseous envelope in which C1-a and C1-b are embedded. No significant emission of this line is detected towards the 12CO outflow lobes. A similar distribution is seen in the integrated emission of 13CS (5-4) and, slightly less, in CH3OH (80,3-71,3), showing that these transitions trace the same gas.
The integrated intensity of the two high excitation lines
OCS (19-18) and CH3CN (12-11) clearly
shows the presence of a compact hot core centered on source C1-b.
In both tracers, the hot core is unresolved, so that its diameter has an
upper limit of approximately 3
,
i.e.
0.026 pc at the given
distance. The hot-core nature of this condensation is confirmed
by the gas temperature of
200 K that we will derive in Sect. 4.1.
For the CH3OH (8-1,8-70,7) and SO (5 6 - 45) line, the emission looks clumpy, with a main spot corresponding to the position of C1, and another prominent spot coincident with the red-shifted 12CO emission, and several fainter spots north and west of C1 which do not coincide with any of the other tracers observed. The strong emission of SO (5 6 - 45) in the red lobe of the 12CO outflow is consistent with previous studies, in which it has been found that SO abundance is enhanced in outflows (Bachiller et al. 2001; Viti et al. 2003), and it has been clearly detected in other massive outflows studied at high-angular reoslution (see e.g. the case study of AFGL 5142, Zhang et al. 2007).
On the other hand, the CH3OH (8-1,8-70,7) line is believed
to be a Class I methanol maser line, and it has been detected
at low-angular resolution in several high-mass star forming regions (see
e.g. Slysh et al. 2002). Recently, the SMA has imaged
several masers in this line towards the source DR21(OH) (Bourke, priv.
comm.).
Class I methanol masers are often located offset from the position of hot cores
or HII regions, where Class II and other masers, such as those of water and OH,
are found. They are believed to be collisionally excited, probably where a
powerful outflow impacts the surrounding quiescent material (see e.g. Sandell
et al. 2003). However, high angular
resolution observations have shown that in some cases they
can be found in close proximity to HII regions and water masers (Kurtz
et al. 2004).
The map shown in Fig. 6 clearly shows
that the (8
-1,8-70,7) line comes from both the hot core and
the red lobe of the outflow, indicating that it is generated
by shocked gas, and the spatial extent is similar to that of SO, even
though the SO emission is more prominent in the outflow
than that of CH3OH. To better understand the nature
of the CH3OH (8-1,8-70,7) line, in Fig. 7 we
show the spectra of this line
towards two positions at an offset of (-3
,
-2
)
and
(+5
,
-1.5
)
from the map centre. These two positions correspond
to the main emission peaks of the averaged map, and roughly coincide
with C1 and with the inner part of the red lobe of the 12CO
outflow, respectively (see Fig. 6). We clearly see that
the line in the outflow is much narrower than the one observed towards
core C1 (
5 km s-1 and
1 km s-1, respectively). The broad line
seen towards C1 is likely thermal, while the narrow
one observed towards the red lobe of the 12CO outflow could come from a
single maser spot, even though the flux density is not very high (
0.08 Jy) and could also be thermal as well.
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Figure 7: Spectra of the CH3OH(8-1,8-70,7) line obtained towards the positions of the two main emission peaks seen in the averaged map of this line (Fig. 6). The offsets (in arcsec) are indicated in the top-right corner, and correspond to the peak position of C1 and the ``base'' of the red lobe of the 12CO outflow. |
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Finally, to better highlight the emission of 13CO and SO in the outflow, in Fig. 8 we show the integrated intensity maps of the blue- and red-shifted emission of the 13CO (2-1) and SO (5 6 - 45) lines. The blue-shifted emission of 13CO seems to trace the cavity created by the blue lobe of the 12CO outflow, while the red-shifted emission follows the inner part of the 12CO red lobe (see upper panel of Fig. 8). For SO (5 6 - 45), we find a similar result for the red-shifted emission, while the blue-shifted emission of this line does not follow that of 12CO, but it arises mostly from core C1 and from the 12CO red lobe. This strange feature could be explained by the presence of another outflow not detected in 12CO, centered roughly in between core N and core C1. A northern bump in the blue-shifted emission is also detected, located at the position of the northern blue-shifted emission seen in Fig. 5.
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Figure 8:
Top panel: red- and blue-shifted integrated emission
of the 13CO (2-1) line observed with SMA, superimposed on the 96 GHz
continuum map observed with the PdBI (grey-scale). For this latter
we use the same contours
as in Fig. 5. The integration ranges in velocity are (-15.88; -8.14)
and (-23.06; -20.85) km s-1. The red contours start from 0.16 Jy beam-1 (
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4 Derivation of the physical parameters
4.1 Temperature of core C1-b from CH 3CN
Figure 9 shows the CH3CN (12-11) spectrum at the peak position
of the emission map shown in Fig. 6. CH3CN is a symmetric-top molecule
whose rotational levels are described by two quantum numbers: J, associated with the total angular
momentum, and K, its projection on the symmetry axis. Such a structure entails that for each radiative
transition,
,
lines with
can be seen (for a detailed description see
Townes & Schawlow 1975). In our observations the bandwidth covers up to the K=7 component
for the (12-11) transition. However, we detected only lines up to K=4, for which the energy of
the upper level is 184 K.
In order to compute the line parameters, we performed Gaussian fits to the observed spectrum assuming that all
the K components arise from the same gas. Hence, they have the same LSR velocity and line width.
We fixed the line separation in the spectrum to the laboratory value
and derive a line width by fitting the spectrum of all the K components. Then, under
the assumption of LTE conditions, we compute the CH3CN spectrum using the gas temperature,
the CH3CN density, the source size as input parameters, and a line width fixed to the observed
value (Qiu 2009, private communication). This approach does not assume optically thin emission
in CH3CN, as does in the Boltzmann analysis (see e.g. Kuiper et al. 1984; Bergin et al. 1994).
The best fit to the CH3CN spectrum shown in Fig. 9 yields a range of
kinetic temperatures from 150-250 K. These values are comparable to typical temperatures found
in hot molecular cores surrounding a newly formed massive star
(see e.g. Kurtz et al. 2000).
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Figure 9: Spectrum of the CH3CN (12-11) line at the peak position, obtained with the SMA. The red line represents the best fit to the components K=0 to K=4, performed as explained in Sect. 4.1. |
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4.2 Physical parameters from dust emission
Table 3:
Peak position, angular and linear diameter, integrated flux density, mass, H2 volume
and column density of the millimeter condensations C1 (resolved into C1-a and C1-b in the 284 GHz image) and
C2. The masses are computed for ,
and assuming T = 30 K. The H2 volume and
column densities are calculated assuming a spherical source with diameter equal to the deconvolved
3
level.
The physical parameters derived from the millimeter continuum images
presented in Sect. 3.1 are listed in Table 3:
the position of the emission peak, in RA (J2000) and Dec (J2000),
of C1 (resolved into C1-a and C1-b at 284 GHz) and C2
are listed in Cols. 2 and 3, respectively; the deconvolved angular ()
and linear (D) diameters are given in Cols. 4 and 5.
Assuming that the emission has a Gaussian profile, we
derived the angular diameter of the sources deconvolving
the observed FWHM with a Gaussian corresponding to the
synthesised beam of the interferometer.
The observed FWHM was measured as the geometrical mean of major
and minor axes of the contour at half of the intensity peak.
The linear diameters were computed using a source distance of
1.8 kpc (Zhang et al. 2005).
In Cols. 6 of Table 3 we also give the flux density,
,
derived integrating over the
3
level in each core. Column 7 shows the gas masses obtained
from
:
assuming constant gas-to-dust ratio, optically thin and
isothermal conditions, the total gas+dust mass is given by:
In Eq. (1), d is the distance,











In Cols. 8 and 9 of Table 3, we also list the average H2 volume and
column densities. The H2 average volume densities were computed assuming
spherical cores, then the column densities were derived by multiplying the
volume densities for the core diameters. We have used
as angular diameters those obtained deconvolving the 3
levels in the continuum
images, and not those listed in Table 3 because the continuum fluxes were
derived integrating the emission within the 3
contours. All volume densities are of the
order of 106 cm-3, while the column
densities are of the order of 1023 cm-2, which are typical values found
in cores associated with intermediate-/high-mass forming stars, and are higher
than the critical value of 1 g cm-2 required to form a massive star at the core centre
(Krumholz et al. 2008), assuming that the gas is totally made up of H2.
The mass of C2, estimated to be 11.8, 4.7 and 2.9
at 96, 225 and 284 GHz, indicates that the core probably hosts an
intermediate-mass object. The mass of C1 is 27 and 11.8
from the 96 and
225 GHz continuum emission, and when it is resolved in two components, C1-a and
C1-b, in the 284 GHz image, the masses of the components are 3.8 and 5.2
,
respectively. These values are typical of cores associated with intermediate-mass
protostellar objects (see e.g. Beltràn et al. 2008).
For C1-b, adopting the temperature of 200 K from CH3CN, we even obtain 0.6
.
However, as we will discuss in Sect. 5.1, the source embedded in core C1-b
is likely an early-B newly formed star. Therefore, the gas mass
derived from the millimeter continuum represents for this source the mass of the
circumstellar material only, and not that of the central star.
Additionally, for all sources these mass estimates, especially
those derived from the 284 GHz continuum, are
very uncertain because they are affected by several problems. First, both the
assumed dust temperature and
are very uncertain:
is expected to be between 1 and 2 in high-mass star forming regions
(see e.g. Hill et al. 2006, and references therein),
while the dust temperature can vary considerably from a source
to another (see e.g. Molinari et al. 2000; Sridharan
et al. 2002).
For example, assuming the gas temperature derived
from NH3 observations, that is T=17 K (Jijina et al. 1999),
with
we get 7.9 and 10.9
for C1-a and C1-b, respectively,
and 8.8 and 12.2 assuming T=17 K and
(Mathis &
Wiffen 1989).
Second, the 284 GHz image is more affected than the others by
the problem of the missing flux, so that the core masses derived
from this image are representative of the circumstellar material very close
to the central object only, while those
from the 225 and 96 GHz continuum are more representative of the whole
envelope. To estimate the amount of
flux filtered out beacuse of missing short spacing information, we have compared
the flux measured with the single-dish SCUBA map at 850
m
(Fontani et al. 2006) to that measured in the 284 GHz map:
the peak flux of the single-dish map is
2.0 Jy beam-1. Assuming
a spectral index of 4, the peak intensity at 1 mm (i.e. 284 GHz) is 1.04 Jy beam-1.
After smoothing the interferometric map at the SCUBA angular resolution of
14
,
the flux density in the area corresponding to the
SCUBA beam is 0.11 Jy beam-1, which means that we are recovering
only
11% of the total flux.
Therefore, the masses derived from the 284 GHz continuum maps have to be
considered as lower limits for the circumstellar masses. On the other hand,
at 96 GHz, the expected flux is 0.011 Jy beam-1 while the value measured
from the PdBI map is 0.0075 Jy beam-1, so that at this frequency we recover
of 68
of the total flux.
4.3 Physical parameters from N 2H+ and N 2D+
4.3.1 Deuterium fractionation
For completeness, in Table 4, we give
the physical parameters derived in Paper I for
condensations N and S from ´´ and N2D+: the
´´ and N2D+ total column densities (N() and
N(N2D+), Cols. 2 and 3); the deuterium fractionation, (
,
Col. 4); the linear
diameter (L, Col. 5); the mass derived from N() (
,
Col. 6). The uncertainties computed following
the standard propagation of the errors are given between parentheses.
For more details on the
methods used as well as in the assumptions made, see
Sect. 3.1 of Paper I.
As already discussed, in both condensations,
is 0.11,
which is comparable to the values of
found in low-mass
pre-stellar cores
by Crapsi et al. (2005), following the same method.
These values are also comparable to those derived by
Pillai et al. (2007) in infrared-dark clouds from deuterated
ammonia. However, their observations are related to the very
cold, pc-scale molecular envelope, and not to compact sub-pc
scale cores.
Table 4: Physical parameters derived in Paper I for condensations N and S from ´´ and N2D+.
We could not derive the column densities of N and S from the
(3-2) line because this is undetected towards the two
molecular condensations, as shown in Fig. 1 of Paper I.
Such a different distribution of the integrated intensity
with respect to that of the (1-0) line is
probably due to the extended emission being
filtered out differently by the two interferometers. To compute the
amount of the missing flux, we have compared our interferometric
spectra with the single-dish spectra obtained with the IRAM-30 m telescope
(see Fontani et al. 2006). We have resampled the single-dish
spectra of (1-0) and (3-2) to the same resolution in velocity
as the interferometric spectra.
The superposition of the spectra is shown in Fig. 10:
in the (1-0) line, the flux measured by the PdBI is 2 times
less than that measured with the IRAM-30 m telescope, while in the
(3-2) line the flux measured with the SMA is only
one fifth of that measured with the 30 m antenna. This indicates
that the extended emission is much more resolved in
the SMA map of the (3-2) line than in the PdBI map of the (1-0) line.
![]() |
Figure 10:
Flux density comparison between IRAM-30 m spectra
and interferometric spectra obtained in the (1-0) ( top panel)
and (3-2) ( bottom panel) lines. The interferometric flux density
of the (1-0) line, measured with the PdBI, has been multiplied by a
factor of 2, while that of the (3-2) line, measured with the SMA,
by a factor of 5. Both PdBI and SMA spectra have been obtained
integrating the maps in Figs. 1 and 2 of Paper I
over the 3 |
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4.3.2 Velocity field
![]() |
Figure 11:
Left panel: map of the (1-0) line width, |
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From the molecular lines observed one can derive information about the
velocity field in the source. In particular, the peak velocity,
,
of the lines gives information on ordered
motion of the gas (rotation, inward or outward motion), while the line
widths,
provide information on the gas turbulent motion.
In this section, we show the results obtained from the (1-0) line,
for which the spectra are not affected by central dips as are those of
12CO and its isotopologues. Also, this tracer is fairly well detected
towards both the continuum cores and the deuterated ones, so that
it allows us to investigate both ordered and turbulent motion across
the whole source.
To derive
and
,
we adopted the following procedure:
from the channel maps of the (1-0) line, we extracted a spectrum from each
pixel inside the 3
level of the integrated emission (pixel
size
1
),
and then fitted these spectra as described in Sect. 2.4.
In Fig. 11 we show the maps of
(left panel),
and
(right panel) of the (1-0) line.
From the left panel, one can
see that the line widths are clearly broader than
1 km s-1 in the region where the continuum cores C1 and C2 and
the (1-0) main peaks are located.
On the other hand, the gas is more
quiescent around this central region, and towards the position
of N and S (
between
0.4 and 1 km s-1). These
results indicate that in the continuum cores, as well as in the ´´
main peaks, the star formation process is actively taking place,
while in the deuterated cores the gas is more quiescent
because they are still in the pre-stellar phase. Interestingly,
the plot in the right panel of Fig. 11 indicates
that in the region where the turbulence is higher
the gas is also red-shifted with respect to the systemic
velocity, while no clear trend is seen in
the other regions of the source, in which the gas velocity is
quite close to the systemic one.
This is probably caused by the interaction with the
red lobe of the 12CO outflow, which is expanding in that
portion of the cluster.
In Sect. 5.2, we will discuss in more detail
this interaction, and how
and
vary in the deuterated cores N
and S, by also using the N2D+ (3-2) line.
4.4 Outflow parameters from 12CO line wings
Table 5: Physical parameters of the 12CO outflow.
In Table 5, the characteristics of the flow are given.
Column 1 lists the computed parameters which are: the H2 column density of the
blue- and red-lobe,
and
;
the total mass,
;
the momentum,
;
the energy, E; the dynamical timescale,
;
the mass entrainment rate,
;
the
mechanical force,
;
the mechanical luminosity,
.
The H2 column densities in both the blue and red lobe,
and
,
have been derived from the
12CO (2-1) line integrated emission in the wings according to the
standard relations (see e.g. Rohlfs & Wilson 2004):
In Eq. (2),







All the other parameters given in Table 5 have been
derived according to Zhang et al. (2005),
taking into account correction for the flow
inclination angle, ,
with respect to the line-of-sight. The
parameters are given for no correction for the
inclination angle (Col. 2), for
(the mean inclination
angle given by Cabrit & Bertout 1986, Col. 3), and for
an extreme value of
(Col. 4). Since the outflow orientation
appears to be close to the plane of the sky, we will consider the values computed
for
and
as lower and upper limits.
In this range, the flow parameters (outflow mass, momentum,
energy, mechanical force and mechanical luminosity) are
consistent with the results obtained for outflows associated with
intermediate-/high-mass YSOs observed at high angular resolution (e.g. Molinari et al. 2002; Beuther et al. 2004, 2006).
We will further discuss the nature of the exciting source of the CO outflow in Sect. 5.1.
5 Discussion
5.1 Nature of the continuum sources
The maps shown in Sect. 3.1 and the parameters derived in Sect. 4 allow us to discuss the nature of the millimeter continuum cores C1-b, C1-a and C2.
C1-b probably hosts a very young early-B ZAMS star. This is indicated by
several pieces of evidence:
first, Molinari et al. (2002) have detected towards i a cm-continuum source whose position roughly
corresponds to that of C1-b, and the Lyman continuum derived from
their observations suggests that the embedded object is a newly
formed B2-B3 ZAMS star. Second, the source is embedded in a
hot core, as demonstrated by the kinetic temperature derived
from CH3CN (12-11) in Sect. 4.1, and by the presence of
other high-excitation lines (see Fig. 6),
and it lies where the main peak of the mid-infrared 24 m continuum emission
is detected (see Fig. 3). Third, it is close to the center of the outflow
lobes detected in 12CO (2-1) (Fig. 5), even though
a significant contribution to the observed blue- and
red-shifted emission can arise from C1-a and, less likely, from another source
not seen in the continuum image, located at the position of the
western emission peak of (see Fig. 5). As discussed in Sect. 4.2,
even though the masses derived form the millimeter continuum are 5.2 and 0.6
,
these measurements represent the mass of the circumstellar gas
only, and thus they do not contrast with the previous findings.
The source embedded in C1-a is probably a very young intermediate-mass protostar. This is indicated by: the core location at the centre of the 12CO outflow lobes, which suggests that the object embedded in the core is one of the main sources driving the powerful outflow; the core gas mass listed in Table 3; the non-detection of the core in the centimeter continuum (Molinari et al. 2002), indicating an evolutionary stage prior to the formation of an HII region. Based on these findings, we believe that the source embedded in C1-a is an intermediate-mass protostar still in the main accretion phase (i.e. a Class 0 object).
![]() |
Figure 12:
Left panels: map of the peak velocity (
|
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![]() |
Figure 13: Same as Fig. 12 for core S. |
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The nature of the source embedded in C2 is unclear. The core mass
(see Table 3) and the non-detection in the 24 m
image suggest that it can be an intermediate-mass embedded protostar.
The source is not associated with a detectable outflow, which however could be
an indication that the embedded source is extremely young. Interestingly, one can notice
from Fig. 4 that C2 is in the middle of a filamentary structure
extended in the N-S direction which also contains the deuterated cores N and S,
and four of the five peaks of the (1-0) integrated emission. This may
indicate that this portion of the source hosts the youngest low- and intermediate-mass
objects of the proto-cluster, and it is consistent with theoretical models
that predict that filamentary structures are common morphologies of molecular
clouds in several classes of dynamical formation models (e.g. van Loo
2007).
5.1.1 A proto-Trapezium system?
From the positions given in Table 3, we derive that
the projected linear separation among the three continuum sources
goes from 0.014 pc between C1-a and C1-b, to
0.07 pc
between C1-a and C2, i.e. from
2800 to 14 000 AU, at the given distance.
Looking at the 284 and 225 GHz images in Fig. 2, one could also suggest
the possible presence of a fourth continuum unresolved source to the NW of C1-a.
This is suggested by the elongated shape of C1-a in this direction, while
the synthesised beam of the SMA at 284 GHz is elongated in the NE-SW direction.
Assuming spherical symmetry, the stellar density
in this region is thus
proto-stars pc-3,
while it is
proto-stars pc-3 assuming the three
resolved sources only. These values are consistent with the stellar density measured in the
Trapezium cluster in Orion, estimated to be
of the order of 104 stars pc-3, and derived assuming the lower-mass stars
in the cluster as well. This suggests that the stellar density of
proto-stars pc-3is a lower limit, and that perhaps the three young intermediate-/high-mass (proto-)stars embedded
in C1-a, C1-b and C2 (plus possibly the unresolved one to the NW of C1-a)
represents a Trapezium-like system in the making.
Similar multiple systems of forming intermediate-/high-mass stars have been discovered recently through high-angular resolution observations (see e.g. Beuther et al. 2007b; Rodon et al. 2008), although these systems are denser than the one in i (more than 105 stars pc-3). Neverthless, these stellar densities are much lower than the value of 108 stars pc-3 needed for the formation of high-mass stars through merging of several lower-mass stars at the center of rich clusters (see e.g. Bonnell et al. 1998), but comparable to the value sufficient to produce binary induced mergers (Bonnell & Bate 2005).
5.2 Nature of the deuterated cores
In Paper I, we discussed the nature of the deuterated cores
based on the dust continuum emission and the deuterium
fractionation derived from the column density ratio N(N2D+)/N().
We derived the mass of the cores following
two approaches: one from the virial theorem, and the other assuming
an average abundance of . For completeness,
in Col. 6 of Table 4 we list the main results
obtained from the second approach in Paper I.
These values, together with a
(Col. 4 of
Table 4),
suggested that both cores are in the pre-stellar phase
but at present they are not massive.
On the other hand, as discussed in Sect. 3.3 of Paper I,
the average spectra of the (1-0) and N2D+ (3-2) lines
in both N and S show lines broader than those typically
observed in low-mass pre-stellar cores.
We proposed two possible scenarios for the nature of the two N2D+ condensations: (i) they are quiescent low-mass starless cores, and therefore they are going to form low-mass stars (in particular, N is likely to harbor several unresolved cores); (ii) they are condensations still in dynamic evolution and may be changing their mass and shape, undergoing either fragmentation or accretion from the parental cloud. In particular, the second scenario is suggested by the predictions of the ``competitive accretion models'', which predict formation of massive stars in a clustered environment through dynamical interaction among several ``seeds'' of forming (proto-)stars (see e.g. Zinnecker & Yorke 2007, for a review).
To better understand the nature of the two condensations, a detailed analysis of the gas kinematics is certainly very helpful. For this reason, here we investigate in more detail the gas kinematics in N and S by using as diagnostics the peak velocity and widths of the (1-0) and N2D+ (3-2) lines, following the same approach described in Sect. 4.3.2.
5.2.1 Condensation N
In the two left panels of Fig. 12 we show the maps of
and
,
respectively, obtained for N from the (1-0) line.
The same plots derived from N2D+ (3-2) are shown in the two right panels.
One can see in the first place that the velocity field in this
core is quite complex. The line width of the (1-0) line are slighly larger
in the southern region of the core, while that of the N2D+ (3-2) looks
larger in the northern and, less prominently, in the south-eastern portion of the core.
For both species, the values range from
0.6 to
1.4 km s-1,
and are on average 3-4 times larger than those found in low-mass
pre-stellar cores (see e.g. Caselli et al. 2002a; for the case of
L1544, Crapsi et al. 2005). However, for the N2D+ (3-2) line, in the positions
where
km s-1, these values can be influenced by the
poor spectral resolution of
0.5 km s-1 (see Table 1).
Therefore, it is possible that linewidths smaller than
0.5 km s-1 are present but not observable with the adopted spectral resolution.
The peak velocity of both ´´ and N2D+ lines is between
and
km s-1, i.e. close to the systemic
velocity, but the gas in the southern region of the core looks slightly red-shifted
with respect to the northern one.
Also, from Fig. 5 one can notice that the red
lobe of the 12CO outflow, likely driven by C1-b, arises from a region
spatially coincident with the southern portion of core N, and possibly
interacts with it: the gas in the red-shifted lobe of the outflow probably
flows behind the core, undergoing drag on part
of the southern gas of N. In this way, one can
explain the observed red-shift of the ´´ and N2D+ lines in the
southern portion of N. This could also be interpreted as being due to
the presence of unresolved low-mass cores at a different velocity, and
the ´´ emission peaks shown in Fig. 4 are consistent with
this interpretation. In this case, the observed broad lines are just due to
the superposition of the different cores. However, this seems very
unlikely since the red-shifted gas in the southern portion of the
core is spatially coincident with the bulk of the red lobe of the
12CO outflow. We suggest that the observed red-shifted emission
and broad lines in the southern portion of N are both due to the interaction
with the ouflow.
5.2.2 Condensation S
In Fig. 13 we show the same maps as
in Fig. 12 for core S. The peak velocity of
both the (1-0) and N2D+ (3-2) lines look red-shifted towards
the north of the core (which appears to be more shifted to
the north-east in N2D+), suggestive of a rotation motion.
A disk-like structure has been observed in the low-mass pre-stellar
core L1544, and it is expected to be caused by the ambipolar
diffusion mechanism (Ciolek & Basu 2000; Caselli et al. 2002a).
However, L1544 also looks
flatter than what is seen in core S, which shows a spherical shape.
This can be due to a different orientation with respect to the line of sight
and to the worse angular resolution of our data, since Caselli
et al. (2002a) obtained observations with linear resolutions a factor of 3
better than ours. Interestingly,
of both ´´ and N2D+ are
larger towards the north-eastern part of the core, so that the
red-shifted gas also appears to be more turbulent. As for N,
this is suggestive of an interaction of the core with
the red lobe of the 12CO outflow, the southern edge of which
touches the upper side of core S (see the upper panel of Fig. 5).
In summary, the shape and the mass of this core indicate that it is a low-mass pre-stellar core, but the high turbulence and the red-shifted gas revealed in the northern part of the core (probably triggered by the neighbouring 12CO outflow) can influence the evolution of the core itself.
5.2.3 General conclusion on the nature of N and S
The main finding of the analysis performed above is that both cores are characterised by a probable interaction with the red lobe of the 12CO outflow. This can trigger turbulence in the cores themselves and can influence their evolution. In theoretical models of clustered star formation, turbulence (which in this case is generated by already formed protostars) can create density modifications across the cloud, generating several dense and cold ``seeds'', which subsequently can accrete backgound gas that was initially not associated with the ``accretion domain'' of the seed itself (see e.g. Bonnell et al. 2004; and McKee & Tan 2003). In this scenario, the two condensations can become more massive and form pre-stellar cores of higher mass. Alternatively, the interaction with the other cluster members, in particular with the powerful 12CO outflow, could also cause the fragmentation of the condensations.
5.3 Comparison with other star forming regions
5.3.1 Intermediate-/high-mass
The analysis made in Sects. 5.2 and 5.1 indicates that
in i there are objects with masses between 2 and
20
,
and in different evolutionary stages: pre-stellar core candidates, intermediate-mass
class 0 protostars, and a newly formed early-B ZAMS star. In recent years, many
star forming regions harboring intermediate- and high-mass young stellar objecs
have been investigated at high-angular resolution, and several of these regions
show a complex structure as seen in i. However, only in very few of them
has evidence of the presence of pre-stellar core candidates been found.
Among the studies performed so far, i appears to have the strongest similarities
with the high-mass protocluster associated with IRAS 20343+4129.
Palau et al. (2007) have observed this cluster with the SMA in the
sub-mm continuum and in 12CO (2-1). Since the synthesised beam and the
source distance are 3
and 1.4 kpc, respectively, their
observations have a linear resolution comparable to our ones. They found
two intermediate- to high-mass young stellar objects, one of which is driving a molecular
outflow, and the other one is driving an expanding cavity. Interestingly, the gas
at the edge of the cavity seems to be compressed into
several dense cores, detected in the millimeter continuum only.
Palau et al. (2007) propose that these are potential starless
cores representing a future generation of stars. In this scenario,
the formation of new stars in the cluster is caused by the interaction
between the highest mass objects (which are expected
to form first at cluster center), and the residual circumstellar (circum-cluster)
material as in i.
Leurini et al. (2007) have investigated
at high-angular resolution the high-mass star forming
region IRAS 05358+3543, and found 4 massive millimeter
cores. One of these seems to be
in the pre-stellar phase, being very cold ( K) and with a large
reservoir of material (
). However, the core does not show
any interaction with the other cluster members, and the
authors suggest that it could be also a very embedded massive protostar.
5.3.2 Low-mass
Several well-studied low-mass star forming regions show filamentary structures similar to that seen in i, and clustered star formation.
In the -Ophiuchi molecular cloud complex, the
large majority of low-mass millimeter cores associated with both pre- and
proto-stellar objects are found to be distributed in filaments (see
e.g. Nutter et al. 2006; André et al. 2007).
In particular, the structure of one of these filaments, Oph A, closely
resembles that of core N. André et al. (2007)
have used (1-0) to perform a detailed study of the kinematics in
Oph A, and their results are different from ours: first,
they derive an average line width (thermal +
non-thermal component) of
0.4 km s-1, which is yet more than
2 times smaller than that measured in our deuterated cores, even
though in the N2D+ lines we are limited by a spectral resolution of 0.5 km s-1,
and we are at the limit of our resolution towards some parts of the
deuterated cores.
Second, they do not find any evidence of interactions between
the different cores, so that there is not feedback from protostellar
activity. Similar morphologies have been obtained
observing (1-0) towards the Perseus molecular cloud by
Kirk et al. (2007), in which there seem to be a minimal
contribution of turbulence in the observed line widths.
These results clearly indicate that pre-stellar cores in low-mass star forming regions are commonly found in filaments similarly to what we have found in i, but they are much less turbulent and interact less with the other cluster members than those studied in this work. Therefore, as suggested in Sect. 5.2, in the condensations associated with i the nearby intermediate- and high-mass young objects likely play an important role in triggering turbulence and, eventually, in causing either the growth or the dispersion of the gas in these cores.
6 Summary and conclusions
We have presented a full report of the observations partially analysed by Fontani
et al. (2008, Paper I) towards the intermediate-/high-mass star forming region
IRAS 05345+3157. The observations were performed with the PdBI and SMA
in the following molecular transitions: (1-0) with PdBI, (3-2) and
N2D+ (3-2), both with the SMA. At the frequencies of these lines, we have
simultaneously observed the continuum emission, as well as other rotational
transitions such as 12CO (2-1), 13CO (2-1), C18O (2-1) and a few other high excitation
lines of less abundant species. In Paper I, the main finding presented was the
detection of two molecular condensations (called N and S) showing high values of deuterium
fractionation (0.1), derived from the column density ratio N(N2D+)/N().
In this work, the following main results have been obtained:
- The continuum emission at 96 and 225 GHz reveals two main cores, C1 and C2,
and C1 is resolved into two components in the image at 284 GHz,
called C1-a and C1-b. C1 is coincident with a prominent
mid-infrared emission detetcted in the Spitzer MIPS images at 24 and
70
m, which is only barely detected towards C2.
- The integrated intensity of the optically thin component of the (1-0) line shows an extended distribution with 5 emission peaks. Two of them fall inside condensation N, another one at the edge of condensation S, while none of them overlaps with the continuum sources.
- The integrated emission in the 12CO (2-1) line wings reveals the presence of a powerful bipolar outflow oriented roughly in the WE direction. From the outflow geometry, the sources C1-a and C1-b are the best candidates for powering the outflow. Assuming a unique source driving the outflow, its parameters are consistent with an engine which is a high-mass young stellar object.
- The (1-0) line widths are between 1 and 2 km s-1 in a region that spatially corresponds to that where the continuum cores are located, while they are significantly smaller (between 0.5 and 1.5 km s-1) in the deuterated cores.
- Based on previous observations and on the results
presented in this work, we can conclude that C1-b very likely harbors
a newly formed early-B star embedded inside a hot-core, and C1-a
harbors an intermediate-mass class 0 protostar. The nature of C2 is unclear
but it could be a very embedded intermediate-mass protostar. If we consider the
system of these three continuum sources and roughly assume a spherical
symmetry, we deduce a star density of
stars pc -3, consistent with the stellar density of the Trapezium cluster and much lower than the value required to form massive stars through collisions of low-mass ones.
- The nature of the deuterated cores has been discussed mainly using the information on the gas kinematics that one can derive from the lines of ´´ and N2D+. Core S is likely a single low-mass pre-stellar core, and the velocity of both the ´´ and N2D+ lines indicates a rotation motion roughly in the N-S direction. This motion and the high turbulence measured at the northern edge of the core is likely due to dynamical interaction with the red lobe of the 12CO powerful outflow. The nature of core N is less clear. Two scenarios are possible: it can be a filament of unresolved low-mass pre-stellar cores, similarly to Oph A, and in this case the high values of the ´´ and N2D+ line widths are due to the superposition of the several unresolved cores. Alternatively, it can be a single object still in dynamic evolution, which actively interacts with the red lobe of the 12CO outflow. In this case, the triggered trubulence can cause either the growth or the fragmentation of the core itself.
Acknowledgements
Many thanks to the anonymous referee for his/her useful comments and suggestions. It is a pleasure to thank the staff of the Smithsonian Astrophysical Observatory for the SMA observations. We also thank the IRAM staff and Riccardo Cesaroni for their help in the calibration of the PdBI data. F.F. is deeply grateful to Marc Audard, Carla Baldovin and Andres Carmona for useful discussion, and to Keping Qiu for fitting the CH3CN spectrum. P.C. thanks Jonathan Tan for useful discussions on protocluster dynamics. F.F. acknowledges support by Swiss National Science Foundation grant (PP002 - 110504). T.B. acknowledges support from US National Science Foundation grant (0708158).
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Footnotes
- ... IRAS 05345+3157
- Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
- ...
- The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica.
- ...
- The fits-files of the 93 GHz continuum image and of the ´´ (1-0) data-cubes are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/499/233
All Tables
Table 1: Molecular transitions observed with the SMA and the PdBI.
Table 2: Line parameters for calculations of the 12CO (2-1) outflow.
Table 3:
Peak position, angular and linear diameter, integrated flux density, mass, H2 volume
and column density of the millimeter condensations C1 (resolved into C1-a and C1-b in the 284 GHz image) and
C2. The masses are computed for ,
and assuming T = 30 K. The H2 volume and
column densities are calculated assuming a spherical source with diameter equal to the deconvolved
3
level.
Table 4: Physical parameters derived in Paper I for condensations N and S from ´´ and N2D+.
Table 5: Physical parameters of the 12CO outflow.
All Figures
![]() |
Figure 1:
Summary of the main findings of Paper I: the dashed
contours represent the intensity of the (1-0) line
integrated between -21.2 and -14.5 km s-1, corresponding
to the main group of the hyperfine components of this line,
observed with the PdBI (see also Fig. 2 of Paper I). Levels range from
the 3 |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
Top left panel: map of the 284 GHz continuum (grey scale)
obtained with the Submillimeter Array. The first level is the
3 |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Left panel: map of the 284 GHz continuum (solid white contours)
obtained with the Submillimeter Array,
superimposed on the Spitzer MIPS image of i at 70 |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Integrated intensity of the hyperfine component F1 F =
|
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Top panel: red- and blue-shifted integrated emission
of the 12CO (2-1) line (combined SMA + NRAO data), superimposed on the 96 GHz
continuum map observed with the PdBI (grey-scale). Both red and blue contours
start from 0.25 Jy beam-1 (
|
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Integrated maps of all the molecular lines listed
in Table 1, detected towards
i with the SMA. For all transitions, the emission has been averaged over all the
channels with signal. In each panel, the transition is indicated in the
top left corner, the grey scale represents the 94 GHz continuum, and
the position of the mm cores is indicated by the white crosses.
For 13CO, C18O, CH3OH (8-1,8-70,7) and SO, the contours start
from the 3 |
Open with DEXTER | |
In the text |
![]() |
Figure 7: Spectra of the CH3OH(8-1,8-70,7) line obtained towards the positions of the two main emission peaks seen in the averaged map of this line (Fig. 6). The offsets (in arcsec) are indicated in the top-right corner, and correspond to the peak position of C1 and the ``base'' of the red lobe of the 12CO outflow. |
Open with DEXTER | |
In the text |
![]() |
Figure 8:
Top panel: red- and blue-shifted integrated emission
of the 13CO (2-1) line observed with SMA, superimposed on the 96 GHz
continuum map observed with the PdBI (grey-scale). For this latter
we use the same contours
as in Fig. 5. The integration ranges in velocity are (-15.88; -8.14)
and (-23.06; -20.85) km s-1. The red contours start from 0.16 Jy beam-1 (
|
Open with DEXTER | |
In the text |
![]() |
Figure 9: Spectrum of the CH3CN (12-11) line at the peak position, obtained with the SMA. The red line represents the best fit to the components K=0 to K=4, performed as explained in Sect. 4.1. |
Open with DEXTER | |
In the text |
![]() |
Figure 10:
Flux density comparison between IRAM-30 m spectra
and interferometric spectra obtained in the (1-0) ( top panel)
and (3-2) ( bottom panel) lines. The interferometric flux density
of the (1-0) line, measured with the PdBI, has been multiplied by a
factor of 2, while that of the (3-2) line, measured with the SMA,
by a factor of 5. Both PdBI and SMA spectra have been obtained
integrating the maps in Figs. 1 and 2 of Paper I
over the 3 |
Open with DEXTER | |
In the text |
![]() |
Figure 11:
Left panel: map of the (1-0) line width, |
Open with DEXTER | |
In the text |
![]() |
Figure 12:
Left panels: map of the peak velocity (
|
Open with DEXTER | |
In the text |
![]() |
Figure 13: Same as Fig. 12 for core S. |
Open with DEXTER | |
In the text |
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