A&A 371, 312-327 (2001)
DOI: 10.1051/0004-6361:20010356
ISOCAM 3-12
m imaging of five galactic compact
H13pt15ptII regions![[*]](/icons/foot_motif.gif)
A. Zavagno
1 -
V. Ducci1
Observatoire de Marseille, 2 place Le Verrier,
13248 Marseille Cedex 4, France
Received 23 September 1999 / Accepted 7 March 2001
Abstract
We present 3-12
m ISOCAM observations of the five Galactic compact
HII regions Sh 61, Sh 138, Sh 152, Sh 156 and Sh 186.
The unidentified infrared bands (UIBs) centred at 3.3, 6.2, 7.7, 8.6
and 11.2
m - and underlying continuum - are imaged using the
SW1, SW2, LW4, LW6 and LW8 filters.
Images are also obtained at 5.985, 6.911, 8.222, 10.520
and 12.000
m using the circular variable filter (CVF).
We show that the 5.985
m emission represents a true continuum
reference for the 6.2
m band, allowing a derivation of this
band's properties. Due to uncertainties in the continuum estimates,
only lower limits can be given for the 3.3, 7.7 and 11.3
m band
fluxes. These limits agree with previous results found in the literature.
The distribution of the bands coincide. The 3.3
m emission is
not observed in high extinction zones, suggesting a lower temperature
of the carriers and/or a higher abundance of larger molecules
in those zones.
The 6.2
m band emission peaks outside the
ionized zone, in the photodissociation region.
The 6.2
m band luminosity correlates with the far UV
field intensity, suggesting a UV excitation. We also find a correlation
between the spatial distribution of the 6.2
m band emission and
zones of strong 2.122
m H2 emission due
to ultraviolet fluorescence. This suggests that both emissions
are due to UV excitation. The 6.2
m emission is slightly closer to
the exciting star. This suggests that the band carriers
survive in the HI zone.
The 12
m emission traces the continuum emission from very small
grains, when present, and follows well the distribution of UIB
emission. This suggests a link between the two emission carriers.
The emission peak observed on the star in Sh 61 and Sh 156
indicates that the continuum from very small grains
dominates the emission in highly excited regions.
Key words: ISM: HII regions - Dust ISM: extinction - ISM: lines and bands
Compact HII regions are associated with young massive stars
and with a large amount of dust.
The presence of the unidentified infrared bands (UIBs) in the spectra of these
regions is well established (Jourdain de Muizon et al. 1990a;
Zavagno et al. 1992).
These emission bands are centred at 3.3, 6.2, 7.7, 8.6 and 11.2
m.
Duley & Williams (1981) were the
first to note that some UIB wavelengths are characteristic of
the bending and stretching modes of CC and CH bonds in aromatic
molecules. Since then, various carriers have been proposed for these bands
including the polycyclic aromatic hydrocarbons (PAHs; Léger & Puget
1984; Allamandolla et al. 1985) and
more amorphous materials containing aromatic
hydrocarbons (Sakata et al. 1984; Borghesi et al. 1987; Papoular et al. 1989).
The ISO mission has greatly enlarged our knowledge of mid-IR emission
properties over a wide range of UV environments. The
mid-IR spectrum was found to be insensitive to the radiation
field intensity up to 104 times the solar vicinity value (Boulanger et al. 2000).
The observed constancy of the band positions and profiles disagrees with
the laboratory spectra of PAH molecules that show important
variations (band intensity ratios) as a function of the state
of the molecule (ionisation state, hydrogenation degree). The mean PAH
ionisation is predicted to increase with the intensity of the
UV radiation field, leading to a drastic change in the band intensity
ratios. Uchida et al. (1998) first
pointed out another problem by publishing a "normal'' UIB spectrum
associated with the reflection nebula vdB 133 in which the UV flux is low.
Then, Pagani et al. (1999) found no correlation
between the mid-IR and far-UV emission in M 31.
The constancy of the UIB spectrum and the presence of UIB emission in
UV-poor environments pose problems for the carriers' identification
(Uchida et al. 2000).
The observed constancy of the UIB spectrum could indicate that
the carriers are aromatic hydrocarbon particles larger than
the molecules studied in the laboratory (Boulanger et al. 2000).
The observed correlation between the UIB distribution
and the far-infrared intensity (Onaka et al. 2000)
reinforces the idea of larger particles for the UIB carriers.
One way to constrain the nature of the UIB carriers is to look
at their properties as a function of the physical
environment (gas density, excitation conditions).
Considering a sample of objects in a similar
evolution stage should weaken the impact of dust evolution
(Cesarsky et al. 2000) in the interpretation.
In order to study the properties of the mid-IR emission
as a function of physical conditions,
we have carried out an observational programme of
direct imaging between 3 and 12
m using ISOCAM (Cesarsky
et al. 1996a) in a sample of five Galactic compact HII
regions. These regions display different properties mainly related
to the spectral type of their main exciting star.
We report here the first results centred on the distribution of
the observed emissions.
Section 2 presents the sample of compact HII regions
together with the ISOCAM observations and the data reduction procedure.
The observed emissions are presented
in Sect. 3 and discussed in Sect. 4. The conclusions are summarized
in Sect. 5.
Five Galactic compact HII regions have been selected for
this programme on the basis of the following criteria:
- high 12
m brightness (IRAS 12
m flux
10 Jy);
- presence of the 7.7, 8.6 and 11.3
m bands in
IRAS low resolution spectra, together with the absence of silicate
absorption at 10 and 18
m;
- known spectral type for the main exciting star;
- small optical size (diameter
3
in the optical).
![\begin{figure}
\par\includegraphics[width=18cm,height=22cm,clip]{fig1.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg8.gif) |
Figure 1:
DSS R-band images for the five sources. The inscribed rectangles
show the areas observed with ISOCAM.
Radio emission is superimposed as contours (see text).
The white dot represents the position of
the main exciting star. North is up, east is left |
The main properties of the sources are summarized in Table 1.
Columns 1 and 2 give the names of the sources in the Sharpless catalogue
(1959) sources and
of the associated IRAS sources.
The spectral type of the main exciting star is given in Col. 3.
The distance is given in Col. 4. The total and far UV
(FUV; 91-240 nm) luminosities, both calculated from the models of
Schaerer & de Koter (1997) for the given spectral type,
are given in Cols. 5 and 6. Note that these values represent
lower limits, as the main exciting star is often found associated with a
dense cluster in such regions (Smutko & Larkin 1999).
The FUV luminosity is given to derive the FUV radiation field intensity,
at a given position, in units of the local interstellar
radiation field,
.
A value of
corresponds to a FUV radiation field
of
1.6 10 -3erg s-1 cm-2 between 91.2 and 240 nm
(Habing 1968).
The luminosity emitted in the 12, 25, 60 and 100
m IRAS
bands (
)
was computed by summing the observed
flux densities in the individual IRAS bandpasses using the formula
,
where D is the distance to the source,
is the IRAS bandwidth,
and
the observed flux density. This luminosity is given in Col. 7.
The coordinates of the CAM field centre are given in Col. 8.
References for the spectral type and distance are given
in footnotes.
Figure 1 presents R-band images of the five sources
extracted from the Digitized Sky Survey (DSS-II).
The field observed with ISOCAM is shown.
When available, the radio emission has been superimposed on
the optical images.
The radio emission at 6 cm is taken from Felli & Harten
(1981) for Sh 138 and Sh 186 and from Birkinshaw (1978) for
Sh 156. That for Sh 152 at 11 cm is from the observations of Scott
published in Cox et al. (1987). We give hereafter some
information about the morphology of the regions.
We will see that the distribution of the mid-IR emission is linked with it.
Sh 61 is a compact HII region ionized by a pre-main-sequence Be star
(AS 310) associated with a dense star cluster (Testi et al. 1998).
AS 310 is a binary system and high angular resolution observations in the
near-IR (Ageorges et al. 1997) revealed four more sources
located within
5
of the binary. A 30
mass of gas is associated with
this source (1.3mm observations of Henning et al. 1994).
The near-IR study in the JHK bands and in the H2 2.122
m and
Br
2.166
m lines by Smutko & Larkin (1999) reveal the
presence of a bright H2 region on the northern edge of the nebula
(see their Fig. 1).
Ground based spectroscopy reveals the presence of the
3.3
m band (Brooke et al. 1993).
Despite the spectral type given for the main exciting star we will see
that its mid-IR emission presents extreme properties. The distance is well
determined (Georgelin, private communication) and the spectral type,
determined using optical spectroscopy, is reliable.
Sh 138 is a compact HII region associated with a dense cluster
(Deharveng et al. 1999).
The core of the associated molecular cloud (Johansson et al.
1994) is
located 10
south-east of the main exciting star. In this zone,
radio emission (see Fig. 1) is observed without associated H
emission. The sharp decrease of the optical emission in this direction
suggests the presence of dust.
Sh 152 (Heydari-Malayeri & Testor 1981; Cox et al. 1987) has a well-defined
interface between the ionized and neutral media.
Two peaks of emission (called
and
in
Heydari-Malayeri & Testor
1981) are observed in this region. [OIII] 500.7 nm and
HeI 587.5 nm emissions coincide with those peaks.
The dust is concentrated in a layer located south-west of the
main exciting star (see Fig. 2b in Cox et al. 1987).
A bright
shell-shaped H2 region is observed at the edge of the ionized zone (see
Fig. 8 in Smutko & Larkin).
Sh 156 is a bright HII region with a horseshoe shape
(Heydari-Malayeri et al. 1980).
The radio emission peak is slightly displaced to the north-west of the
H
emission peak (cf. Cox et al. 1987) indicating the
presence of dust in this zone.
Strong [OIII] 500.7 nm emission
(Heydari-Malayeri et al. 1980) confirms the high excitation
degree of this nebula.
Sh 186 is a compact, low density region (Hunter 1992).
The radio and optical emissions coincide well in this case.
Near-IR measurements revealed the presence of heated dust
(Felli & Harten 1981) but IRAS measurements indicate a weak
infrared emission (Jourdain de Muizon et al. 1990a;
Zavagno et al. 1992).
The 3-12
m ISOCAM observations were made with
the 3
0 pixel size and the small field mirror.
The field covered is 87

87
for Sh 61, Sh 152 and Sh 186 and
174

87
for Sh 138 and Sh 156 (see Fig. 1).
Observations using the SW1 (3.05-4.1
m), SW2
(3.2-3.4
m),
LW4 (5.5-6.5
m), LW6 (7-8.5
m) and LW8 (10.7-12
m)
filters were obtained to look at the distributions of
the 3.3, 6.2, 7.7 and 11.2
m emission bands and continuum.
Five CVF observations were made at 5.985, 6.911, 8.222, 10.520 and
12.000
m with a FWHM that varies between 0.156 and 0.295
m.
The elementary observing time was 2.1s and the gain was set to 2. The same exposure
time was used for all the regions and the number of elementary frames varies between
60 for LW filters to 210 for SW filters. About 120 images were taken for each
continuum measurement using the CVF. The data were
processed with the off-line pipeline version 7 (OLP V7) and
were analysed using CAM Interactive Analysis (CIA, Ott et al.
1997) version 3.
The standard procedure was applied: dark correction, deglitching, stabilisation,
flat field correction and calibration (see Stark et al. 1999
for details). The stabilisation was done using the models developed
by Tiphène et al. (2000) and Coulais & Abergel (1998)
for the SW and LW CAM detectors, respectively. The results of this procedure are robust
because the observed sources are bright (12
m IRAS
flux between 10 and 40 Jy) and a large number of elementary frames were taken,
allowing the detector to reach stabilisation at the end of an observation.
The final fluxes are given in janskys and the uncertainties are less than 8%.
The images were recentred using the USNO-A2.0
catalogue (Monet et al. 1998). We used the stars that are seen both in
the visible (on DSS images) and at 3
m (SW1 images).
Then the long wavelength infrared emissions (LW and CVF images) are recentred to
coincide with the SW emission. The position shift is, at most, of 2 pixels (6
).
We describe, hereafter, the observed emissions.
When speaking about the UIB and underlying continuum
emissions we consider that a continuum emission is
associated with the bands.
Uchida et al. (2000) discussed this problem.
The derived band and continuum
fluxes are quite sensitive to how one fits the UIBs,
i.e. using Gaussian or Lorentzian profiles, and chooses the continuum. In
particular, Boulanger et al. (1998) fit the bands of NGC 7023
with a Lorentzian
profile, so the apparent continuum is due to the wings of the band. Note that in this case there is little continuum contribution
from very small grains after fitting the UIBs with
Lorentzians. An alternative is to consider that there is a continuum
associated with the bands and linked with the band carriers.
In this case the continuum is estimated from measurements outside
the band (see Uchida et al. 2000). Tran (1998) has shown that
the UIB fluxes derived for NGC 7023 using Gaussian or Lorentzian fit
are well correlated, differing only by a multiplicative constant.
Because of this, comparisons must be made between results derived
with the same method. The band integration limits are also important
(Uchida et al. 2000).
The SW1 filter (3.05-4.1
m) contains both the
3.3
m emission band and the satellite bands observed between 3.35 and
3.8
m (see Jourdain de Muizon et al.
1990b). The contribution of these bands to the SW1 emission
is less than 10%. Near the exciting star, hydrogen recombination lines
(Pf
at 3.296
m and Br
at 4.05
m) are present
but become negligible outside the ionized zone (see Fig. 1 in
Verstraete et al. 1996).
The SW2 filter (3.2-3.4
m) is centred on the
3.3
m band. We used the SW1 emission to estimate the
3.3
m band continuum.
We designate the SW1 and the SW2 width by
and
.
The difference, in intensity, between the
SW1 and SW2 emission gives an estimate of the continuum
emission through a filter of equivalent width
(
). This value is then normalised
to the SW2 filter width and subtracted from the total SW2 emission.
The continuum is clearly overestimated in the ionized zones due to the
presence of hydrogen recombination lines but the agreement found
between our derived values and previous results (see Sect. 4.1)
indicates that the continuum estimate is correct outside the
ionized zones.
The 6.2
m band
emission is obtained by subtracting the
5.985
m CVF emission from the LW4 emission.
The 6.911
m emission is affected by the
[ArII] emission line at 6.983
m in the ionized region
due to the low ionisation potential (15.7 eV) of argon
(see Fig. 1 in Roelfsema et al. 1996). This emission traces
well the ionized region (Cesarsky et al. 2000b).
The LW6 filter (7-8.5
m) includes the 7.7
m band and part
of the 8.6
m band.
At 8.222
m, the wings of these two bands create part
of the measured emission and part may be due to small grains
(see Chap. 2 in Tran 1998). We used a linear
interpolation between the 6.911 and 8.222
m to estimate
the continuum associated with the 7.7
m band.
The 7.7
m band emission is obtained by subtracting this continuum
from the LW6 emission.
[SIV] emission at 10.52
m requires a high ionisation
potential (35 eV) and, if present, should peak near the
ionizing star.
The LW8 filter (10.7-12
m) includes the 11.04 and
11.2
m bands, the emission "plateau'' (Allamandola et al.
1989) together with the short wavelength part of the
strong rising continuum observed in compact
HII regions (see Fig. 3 in Roelfsema et al. 1998).
This continuum probably corresponds to emission from very
small grains (Tran 1998). The exact nature of this grain
population, suggested by Désert et al. (1990) to
explain the 25
m emission excess observed by IRAS,
remains unclear. The contribution of very small grains' emission
to the 6-12
m continuum depends on the peak wavelength
of the small grains' emission
(the shorter the peak wavelength, the higher its contribution to the
6-12
m continuum). The 12
m measurement can be used to
study this continuum emission, if present. The 11.3
m band
emission is obtained by subtracting a continuum estimated
using a linear interpolation between the two surrounding CVF measurements at 10.5 and 12
m.
![\begin{figure}
\par\includegraphics[width=18cm,height=22cm,clip]{fig2a.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg34.gif) |
Figure 2:
ISOCAM 3-12 m emissions superimposed (white contours)
on the R-band images, for the five sources. The range of levels
is given in Table 2 for the filters and in Table 3 for the CVF, both
in mJy/pixel. North is up, east is left |
![\begin{figure}
\par\includegraphics[width=17cm,clip]{fig2b.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg35.gif) |
Figure 2:
continued |
![\begin{figure}
\par\includegraphics[width=17.5cm,clip]{fig2c.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg36.gif) |
Figure 2:
continued |
![\begin{figure}
\par\includegraphics[width=17cm,clip]{fig2d.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg37.gif) |
Figure 2:
continued |
![\begin{figure}
\par\includegraphics[width=17.5cm,clip]{fig2e.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg38.gif) |
Figure 2:
continued |
Table 2:
Range of levels in Fig. 2 (in mJy/pixel) for the filters
Source |
SW1 |
SW2 |
LW4 |
LW6 |
LW8 |
|
Half-maximum filter coverage in m |
|
3.05-4.1 |
3.2-3.4 |
5.5-6.5 |
7-8.5 |
10.7-12 |
|
Levels in mJy/pixel |
Sh 61 |
10-49 |
15-70 |
40-225 |
70-537 |
80-835 |
Sh 138 |
10-56 |
15-58 |
40-194 |
40-504 |
40-472 |
Sh 152 |
5-22 |
10-25 |
30-113 |
40-292 |
40-232 |
Sh 156 |
5-45* |
7-40* |
20-197* |
30-550* |
40-780* |
Sh 186 |
0.4-1.1* |
2-6* |
10-40 |
10-92 |
10-79 |
*Not regularly spaced levels.
Figure 2 presents, for each source, the distribution of emissions
observed with ISOCAM. These emissions are superimposed (contours)
on the R-band images. Tables 2 and 3 give the range of levels
in Fig. 2 for the filters and for the CVF, respectively.
Table 3:
Range of levels in Fig. 2 (in mJy/pixel) for the CVF
Source |
CVF central wavelength in m |
|
5.985 |
6.911 |
8.222 |
10.520 |
12.000 |
|
Levels in mJy/pixel |
Sh 61 |
20-89 |
35-221 |
90-398 |
50-836 |
60-670 |
Sh 138 |
30-222 |
30-276 |
50-403 |
40-309 |
40-475 |
Sh 152 |
18-47 |
30-170 |
30-217 |
30-116 |
40-245 |
Sh 156 |
20-220 |
25-230* |
50-370 |
20-661* |
30-780* |
Sh 186 |
13-32* |
8-47 |
15-70 |
10-31 |
15-72 |
* Not regularly spaced levels.
We see in Fig. 2 that 3-12
m emission is present in the five sources.
The brightest emissions are observed towards Sh 61 and Sh 156 whereas
Sh 186 shows only weak emissions.
Sh 138 and Sh 152 show intermediate fluxes, higher for Sh 138.
SW1 and SW2 emissions show different morphologies, the latter being enhanced
outside the ionized zone where emission from dust dominates.
The SW1 emission peaks on the main exciting
star, probably dominated by the star's continuum emission and hydrogen
recombination lines.
The SW emissions do not extend in regions of higher extinction
where longer wavelength emissions are observed. This is the case for Sh 138
where longer wavelength emissions are observed towards the molecular cloud, south-east of the main exciting star and for Sh 152 where the
northwestern extension is not observed at short wavelengths.
A similar result is found in the Galactic compact
HII region Sh 88B (Deharveng et al. 2000b) where the 3.3
m emission (Goetz et al. 2000) is not observed in high extinction
zones. In the PAH hypothesis, the maximum temperature reached by a molecule is
linked to its size. Small molecules can reach high temperatures and
emit preferentially at 3
m. The weaker UV field intensity in
high extinction zones leads to a lower temperature of the carriers that emit
at longer wavelengths. A higher abundance of larger molecules
in high extinction zones may also explain this result.
The SW2 emission, when compared to longer wavelength
emissions, is observed in lower extinction zones. In these zones, the short
and longer wavelength UIB emissions coincide at the ISO spatial resolution.
The emission peak in LW4 and LW6 is observed outside the ionized region,
towards the photodissociation region and coincides with zones of strong
2.122
m H2 emission for Sh 61, Sh 152, Sh 156 and
Sh 186, observed by Smutko & Larkin (1999). We discuss
the spatial coincidence between the 6.2
m band and zones of
strong H2 emission in Sect. 4.2. Except for Sh 61 where
the emission is probably seen face-on, the mid-IR emission surrounds the
ionized region. Weingartner & Draine (1999) proposed a model of grain
dynamics in photodissociation regions where the grains are pushed by the
radiation pressure and accumulate in the PDR and their destruction inside the ionized regions, leading to an enhanced
dust-to-gas ratio in this zone. The accumulation of band carriers in
the PDR could explain the observed shell-shaped mid-IR emission.
In Sh 61, Sh 138, and Sh 156 we observed a brightness enhancement of
the mid-IR emission at locations where young stars only detected in
the K-band are observed (see the images in Smutko & Larkin).
In Sh 138, the south-west extension observed in LW4 and LW6 also
corresponds to
a very red star observed in K (star 119 in Deharveng et al. 1999).
If those young stars are sufficiently hot, their FUV radiation
creates a local excitation of the dust, increasing the mid-IR emission.
If confirmed, this local dust excitation has to be taken into account.
The LW8 distribution outside the ionized region is similar to that of
the LW4 and LW6. Differences appear in Sh 61 and Sh 156 where the LW8 and
the 12
m emissions peak on the main exciting star.
In Sh 152, a similar trend, although less pronounced,
is observed in the dense ionized zone (the
component -
see Sect. 2.1).
Figure 3 presents the mean value of the flux observed in the
eight pixels around the exciting star
(i.e. in the ionized region) and near the mid-IR emission peak (i.e. outside
the ionized region - the mean flux observed in the eight pixels that surround the emission peak).
The mean background level, taken outside these emission zones,
is also shown for comparison.
The maximum flux uncertainty of 8% (see Sect. 2.2) is shown.
The uncertainty on the background fluxes, always smaller than the symbols,
is not shown.
![\begin{figure}
\par\includegraphics[width=18cm,clip]{fig3.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg39.gif) |
Figure 3:
Mean flux observed around the main exciting star (i.e. in the ionized zone;
filled circles), around the mid-IR emission peak (i.e. outside the ionized zone; open squares)
and on the background (filled triangles). The fluxes are given in mJy/pixel.
The thick black lines show the filter widths and
the error bars show the flux uncertainty |
In Sh 61 and Sh 156 the mid-IR emission is dominated
by emission near the star (filled circles in Fig. 3) whereas the emission
from dust in the PDR (open squares in Fig. 3) dominates in Sh 138, Sh 152 and Sh 186.
In Sh 61 and Sh 156, the strong rising shape of the flux density
is similar to the one observed towards highly excited
HII regions.
In the ionized zones where no emission from the 6.2
m band
is expected, the levels of the LW4 and 5.985
m emissions are similar,
indicating that we are measuring a continuum.
For Sh 61, the difference observed in Fig. 3 between LW4 and 5.985
m
flux levels in the ionized zone suggests that dust emission occurs.
A face-on configuration may explain this behaviour.
The 6.9111
m emission is always above the continuum level (as defined
by the 5.985
m flux) due to the [ArII] line.
Outside the ionized zones the 6.911
m measurement
can be used to estimate the 7.7
m band continuum.
The strong 8.222
m emission observed near the star
in Sh 61 and Sh 156 indicates that larger molecules
or small grains, that better survive in hard radiation
fields, may be responsible in part for this emission.
In the other regions, this emission follows well that of the
LW4 and LW6 emission, suggesting a common origin.
The 10.52
m emission peaks towards the main
exciting star in Sh 61 and Sh 156 (see Fig. 2).
This is also seen in Fig. 3 where the 10.52
m
flux is high in the ionized zone
(maximum flux level of 840 mJy observed in Sh 61 and of
780 mJy in Sh 156, on the star).
In Sh 152, an extension towards component
is observed
(see Fig. 2).
We used the 10.52 to 5.985
m ratio
as an indicator of a possible contamination by [SIV]
emission. In Sh 61 and Sh 156, the maximum value of this ratio
(
7) is found around the exciting star, suggesting
[SIV] emission.
The presence of [SIV] is confirmed by the
SWS spectra of Sh 156 (see Fig. 3e in Cox et al. 1999).
The possible presence of [SIV] in Sh 61,
incompatible with the spectral type of the main exciting star,
remains unclear. For Sh 61 and Sh 152 (component
)
we suggest that amorphous silicate grains
may be responsible for the observed emission (Cesarsky et al. 2000b).
The pre-main sequence nature of AS 310, the exciting star of Sh 61,
may explain this emission as a broad silicate emission is
observed towards T Tauri stars in the Chamaeleon I dark cloud
(see Gürtler et al. 1999). Extended red emission attributed
to nanosized silicon particles is observed towards component
in Sh 152 (Darbon et al. 2000) indicating the presence of these
grains.
The distribution and flux levels observed in Sh 138, Sh 152
(except towards the
component) and Sh 186
indicates that little or no [SIV] emission is present.
Sh 138 and Sh 152 should indeed only show
weak [SIV] emission, because only weak [OIII] 500.7 nm,
which requires a similar ionisation potential (35 eV), is observed in these
nebulae (Deharveng et al. 2000). In Sh 186, the low excitation prevents
such emission. Outside the ionized zones the flux level is low, and this
measurement can be used to estimate the 11.2
m band continuum.
In Sh 138 and Sh 186 the contribution of the long
wavelength continuum in the ionized zone is low at 12
m
(also revealed by the low 12
m to 5.985
m ratio, around
2 at maximum). The SWS spectrum of Sh 138 (Fig. 1e
in Roelfsema et al. 1996) confirms this fact.
This means that the contribution of the continuum attributed to very small
grains (VSGs) is small at 12
m.
We see in Fig. 2 that, in these two regions, the 12
m emission
follows that of the LW4, LW6 and LW8 emissions
quite well, suggesting a common origin for the carriers of both emissions.
In Sh 61, Sh 152 and Sh 156 the contribution of the VSG continuum
is large at 12
m and peak in highly excited region (see Fig. 2)
indicating that VSGs survive in hard radiation fields and dominate the emission.
In the following we derive the UIB fluxes considering that an underlying
continuum is associated with each band (see Sect. 2.3).
The 6.2
m band is well determined (see Sect. 3).
In the ionized zone the possible contamination by atomic lines
and continuum emission from very small grains prevent a reliable estimate
of the continuum underlying the 7.7 and 11.2
m bands.
For these two bands a mean value is
obtained using a value of the continuum estimated at
the band centre position with a linear
interpolation using the two surrounding CVF measurements (see Sect. 3).
The given
values probably represent a lower limit of the band fluxes as the continuum
estimates are upper limits.
For each band, the flux is integrated over a (87
)2 area.
This area, centred on the main exciting star, covers the whole emission band.
The integrated flux is then multiplied by the filter
width (in Hz). The results are given in Table 4.
Columns 1 and 2 give the name of the sources.
Columns 3 to 6 gives, respectively,
the fluxes of the 3.3, 6.2, 7.7 and 11.2
m bands.
The highest excitation region of our sample, Sh 156, has the highest
UIB fluxes, similar to those of Sh 61.
Sh 186 has the smallest values in agreement with its low IR luminosity.
The correlation observed between
the 6.2 and 7.7
m band intensities in our sample (see also Fig. 18 in
Cohen et al. 1989) confirms a common origin for the carriers.
Ground-based data obtained for the 3.3
m band in Sh 61
(Brooke et al. 1993) give a flux of
13 10-18 W cm-2,
in very good agreement with our
determination. Sh 138 has been observed at 3.3
m by Jourdain de Muizon et al.
(1990b) and these authors also derive the 7.7
and 11.2
m band fluxes using IRAS data. Their results are,
respectively for the 3.3, 7.7 and
11.2
m bands, 4, 130 and
34 10-18 Wcm-2,
in good agreement with our values. The values we obtain for the
11.3
m band for Sh 138, Sh 156 and Sh 186 also agree well
with the results obtained by Zavagno et al.
(1992). No comparison can be made for the 7.7
m band due to
different integration band widths.
Using the fluxes given in Table 4, we derive band ratios.
Their values vary between
0.19 to 0.48 for [3.3]/[11.2], 0.27 to 0.6 for [6.2]/[7.7] and
2.8 to 4 for [7.7]/[11.2]. These values agree with the typical ones found
for HII regions by Cohen et al. (1989), i.e.
0.43 for [3.3]/[11.2],
0.58 for [6.2]/[7.7] and 3.3 for [7.7]/[11.2]. No correlation has been found between the ratio and the excitation conditions.
This is also the case for the sample studied by
Roelfsema et al. (1996).
For Sh 138 their value of the
[6.2]/[7.7] ratio agrees well with ours. The higher values they derived for the
[7.7]/[11.2] and [3.3]/[11.2] ratio come from different integration
band widths (see Lu 1998), especially a narrower integration
band for the 11.2
m feature. This again emphasizes the
importance of comparing results obtained by similar methods (see Sect. 2.3).
In order to look at the relation between the 6.2
m band flux
and the excitation conditions we derive a 6.2
m band luminosity, scaled
to a common distance, arbitrarily chosen to 2.5 kpc, the distance of Sh 61.
The derived values are 69
for Sh 186, 100
for Sh 61,
523
for Sh 152, 1045
for Sh 138 and 3740
for Sh 156 and show that the
6.2
m band correlates well with the intensity of the FUV field,
suggesting a FUV excitation. A PDR
model is needed to estimate accurately the FUV field intensity at
a given distance from the star. Nevertheless we derived the FUV field
intensity taking the value of
in Table 1 and considering that the decrease of the FUV
field with distance from the star is
only due to geometrical dilution, with an r-2 law (see Uchida et al. 2000). This crude estimate of the FUV field, at the distance
where the 6.2
m band peaks, gives a value of 104
.
This value agrees with the ones generally used in dense PDR models (Burton et al. 1990, see also Hollenbach & Tielens 1997).
A similar value of the FUV field intensity is
found for Sh 156 and Sh 186 at the 6.2
m band peak. This suggests that
similar excitation conditions prevail in these PDRs. The main observed
change is the distance between the exciting star and the 6.2
m band
peak. This distance increases with the spectral type of the star in
our sample rendering possible similar excitation condition in the PDR,
regardless the spectral type of the central exciting star.
The 6.2
m band distribution peaks in the PDR and this zone's
position corresponds to similar excitation conditions.
Figure 4 presents the 6.2
m band
distribution superimposed on the
H2/Br
images obtained and kindly provided by Smutko & Larkin
(1999) for Sh 61, Sh 152, Sh 156 and Sh 186.
![\begin{figure}
\par\includegraphics[width=15.7cm,clip]{fig4.eps}
\end{figure}](/articles/aa/full/2001/19/aa9270/Timg43.gif) |
Figure 4:
6.2 m band (contours) superimposed on the H2/Br
image obtained by Smutko & Larkin for Sh 61, Sh 152, Sh 156 and Sh 186. The black zones
are zones of strong H2 emission (in arbitrary units; see Sects. 3.2 and 4.1
in Smutko & Larkin).
Contour levels for the 6.2 m band are:
for Sh 61: 10-107 mJy/pix, for Sh 152: 4-59 mJy/pix, for Sh 156: 4-86 mJy/pix and for
Sh 186: 4-16 mJy/pix |
We only considered the 6.2
m band (see Sect. 3)
but the same result is found for the other bands as their
distributions coincide.
The zones of strong 2.122
m H2 emission are
represented as the black zones in Fig. 4
(see Sects. 3.2 and 4.1 in Smutko & Larkin for explanations).
We see that the 6.2
m band distribution coincides with zones
of strong 2.122
m H2 emission, whatever the spectral type of the
exciting star. This reinforces the finding of similar excitation conditions
in these PDRs. The 6.2
m emission seems to be slightly closer
to the star then the H2 emission. This is also observed in Orion
(see Fig. 9 in Cesarsky et al. 2000) and can be interpreted as
the survival of the carriers in the HI zone. Tran (1998) has shown that the intensity of the UIBs in NGC 7023 is strongly correlated with
the HI gas density. In Sh 61 the bright
H2 emission zone is found in the northern part of
the optical region where 6.2
m emission is also found.
In Sh 152 bright H2 emission surrounds the south part of the optical region
with a small extension to the south-east. This small extension also
corresponds to fainter 6.2
m emission. Larger scale LW6 emission (Copet
& Zavagno 1999) also follows perfectly the 2.12
m
H2 emission (Porras, private communication).
In Sh 156, an H2 extension is seen to the east and corresponds
to fainter 6.2
m
emission (see also Fig. 2). The 6.2
m band also
surrounds the ionized region in Sh 186 and corresponds well to zone of
strong H2 emission.
The good correlation between the 6.2
m band and the H2 strong
emitting
zones indicates that the 6.2
m band carriers are concentrated in
this part of the photodissociation region. The same result has been
found in the Rho Ophiuchi region where the H2 and UIB emissions
coincide (Habart et al. 2000) and in molecular clumps near the Keyhole
Nebula where 3.3
m and 2.12
m H2 emission exactly coincide
(Brooks et al. 2000). The correlation between both
emissions observed in the Rho Ophiuchi region, located at 135 pc,
indicates that the coincidence is not due to a lack of spatial
resolution of our ISOCAM data.
The spatial coincidence of the 6.2
m band
and the 2.12
m H2 emission due to fluorescence suggests that
H2 and UIB carriers are both excited by UV radiation.
The distribution of the 6.2
m band suggests that the dust has
been swept-up outside the ionized region and concentrates in the PDR.
The LW4 emission contrast between the emission peak and the ionized zone
is nearly the same in the five regions. Despite a small dynamic range
of excitation conditions, this result suggests that
the carriers are not more destroyed in the ionized zone of Sh 156 than in
that of Sh 186.
We obtained the distribution of the 3-12
m emission in
five Galactic compact HII regions using ISOCAM.
The main results can be summarized as follow:
- In the five regions, mid-IR emission is present. Considering that
a continuum or broad wings are associated with the UIBs, only the 6.2
m
emission band can be reliably derived using the 5.985
m CVF as a reference. We also obtain lower limits for the distribution and flux of the 3.3, 7.7 and
11.3
m bands. UIB fluxes agree
with previous results obtained by Brooke et al. (1993) and Jourdain de Muizon
et al. (1990b). The UIB ratios also agree
with those previously found for HII regions by
Cohen et al. (1989). Comparisons with other results
show that caution has to be taken when comparing UIB fluxes obtained using
different fitting methods and/or integration band widths;
- At the ISOCAM angular resolution, the 6.2, 7.7 and 11.3
m band
emissions are observed in the same zones, indicating a common origin
for the carriers. The 3.3
m band is not observed in high extinction
zones suggesting a lower temperature of the carriers and/or
a higher abundance of larger molecules in those zones;
- A crude estimate of the far UV field intensity at the location of
the 6.2
m band peak suggests that similar excitation conditions
prevail in the five PDRs;
- The 6.2
m emission peaks
in the photodissociation region. A good correlation between the
2.122
m H2 and 6.2
m emission zones is observed. This suggests
that UV excitation occurs for both emissions.
The correlation between the 6.2
m band luminosity and the FUV intensity
reinforces this idea. The 6.2
m emission is slightly closer
to the star then the H2 emission, as observed in Orion,
indicating that the carriers survive in the HI zone;
- The 12
m emission shows that the contribution of
continuum emission from very small grains is important in
high excitation regions and peaks on the exciting star. The similar
emission distributions suggest that 12
m and
UIB carriers may be linked.
Acknowledgements
J.-P. Baluteau, J. Caplan, S. Darbon, L. Deharveng,
C. Morisset, J.-P. Sivan and
J.-M. Perrin
are greatly thanked for many fruitful discussions. J. Larkin is deeply
thanked for his permission to use the data published in Smutko & Larkin as
well as M. Birkinshaw for the radio map of Sh 156.
The people in charge of the
ISOCAM data centre in Saclay are also thanked for their help regarding
the data reduction. D. Rouan is thanked for his help in using the
CAM-SW stabilisation programme. J. Lequeux is thanked for comments
that help to improve the paper.
This work benefited from the financial support of the GdR PCMI.
This research has made used of the Simbad astronomical database
operated in Strasbourg, France.
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