A&A 379, L17-L20 (2001)
DOI: 10.1051/0004-6361:20011345
VLT-ISAAC 3-5
m spectroscopy as a new tool for
investigating H2 emission in protostellar jets
T. Giannini - B. Nisini - F. Vitali - D. Lorenzetti
Osservatorio Astronomico di Roma, via Frascati 33, 00040
Monte Porzio, Italy
Received 17 September 2001 / Accepted 26 September 2001
Abstract
We report 3-5
m IR spectroscopy obtained with VLT-ISAAC on the
IRS17 molecular hydrogen jet in the Vela-D Molecular Cloud. Together with H2emission lines from the v = 1 rovibrational state, the spectra show several
pure rotational lines of the fundamental state with excitation temperature up
to
22000 K. We show how theoretical rotation diagrams indicate these
lines as unique both to probe the presence of collisionally excited gas
in NLTE conditions and to infer the gas density.
Key words: stars: formation - infrared: ISM: lines - ISM: jets and
outflows - ISM: individual objects: Vela clouds
A large number of molecular jets has been so far investigated in the near
infrared with the current ground-based instrumentation through large field
(
10 arcmin) imaging and intermediate resolution
spectroscopy (
)
(e.g. Eislöffel 1997). In particular,
molecular hydrogen imaging of the v=1-0 S(1) at 2.122
m is extensively
used for identifying knots of molecular emission, while the spectroscopy of
the H2 rovibrational lines lying in the 1.6-2.5
m range is largely
effective both to probe the molecular gas at thousands of Kelvin and to infer
the prevailing excitation mechanism (fluorescence, C-ontinuos or J-ump shocks,
see e.g. Black & van Dishoeck 1987; Kaufman & Neufeld 1996; Hollenbach
& McKee 1989; Smith 1995). Recently, space-born spectroscopy evidenced the
advantages of observing in the mid-IR the ground state H2 pure rotational
transitions, emitted by levels with excitation energy between 0 and
10000 K. These appear of particular interest because, in addition to be
practically unaffected by extinction problems, they are characterized by
significantly different critical densities (spanning from
103 to
105 cm-3), which make them particurlarly suitable both to probe shock
components at different temperatures (from few hundreds to thousands of
Kelvin, e.g. Benedettini et al. 2000; Nisini et al. 2000) and to trace
collisionally excited gas in NLTE conditions. Unfortunately, these
observations are severely limited by the unavoidably poor spatial resolution.
Now, VLT-ISAAC has opened a window in the thermal IR (3-5
m) investigable
with high to intermediate spectral resolution at an adequate plate scale for
sampling the individual knots within the molecular jets, thus offering the
opportunity to diagnose the local variations of the physical conditions by
using the unique capabilities of the pure rotational H2 lines.
In this paper we report one of the first
observations of 3-5
m long-slit spectroscopy of protostellar jets. Our
target is the molecular hydrogen jet we have recently discovered in the Vela-D
Molecular Cloud, namely the IRS 17 jet (Lorenzetti et al. 2001, hereinafter
Paper V, following the numbering of previous papers on the same subject). It
results composed by a large number of individual bright knots extending up to a
distance of
0.3 pc from the central driving source. Previous infrared
spectroscopy in the 1.6-2.5
m range with NTT-SOFI has revealed it is a
quite rare example of pure molecular jet with a low excitation degree,
as implied by the lack of both [Fe II] lines and H2 transitions
coming from levels with v
3. For this reason such a jet appears as a
well tailored candidate to search for thermal H2 pure rotational lines and
to investigate their relative importance with respect to rovibrational
contributions. Moreover, being several bright knots quite well aligned along
the jet axis, they result easily accomodable within a single slit, giving the
further observative advantage to allow a multiple diagnostic along the jet in
a single exposure.
Figure 1 shows the H2 (2.122
m) continuum subtracted
image of the IRS 17 jet, which was obtained in a previous observing run with
NTT-SOFI (Paper V). It results in about 20 knots of emission emanated from the
central candidate driving source IRS17-40 (
44
47
76;
43
35.8
),
which is marked in the figure with a cross. Out of them, six knots, labelled
with the same identification as in Paper V (namely C2, C3, C5, G1, G2, G3)
have been spectroscopically investigated with ISAAC (LW arm).
The same knots had been observed with SOFI at low resolution (
)
between 1.6-2.5
m (Paper V). In this paper the intensities of the lines
lying in the SOFI domain have been used together with those derived from
the ISAAC observations.
These latter were carried out in February 2001. We
performed long slit spectroscopy with a medium resolution grating (
with a 2
120 arcsec slit) in the wavelength range 2.7-5.1
m. The slit position angle (148
7), has been defined on the basis
of the SOFI image and fine tuned with the pre-imaging procedure at the VLT
telescope. We conducted our observations by chopping and nodding the targets
in different positions along the slit. The total integration time per grating
position is 660 s and 2200 s between 2.7-4.0
m and 4.4-5.1
m,
respectively. The data reduction and calibration were performed by using the
IRAF package. The spectra were flat-fielded and sky subtracted, while flux
calibration was obtained by observing the spectrophotometric standard star
H43125 (spectral type O9Ib), which was also used for removing atmospheric
absorption features. To ensure a correct inter-calibration between the ISAAC
and SOFI line fluxes, which are measured from the H2 2.122
m image and
are thus unaffected by slit aperture problems, we applied to the ISAAC derived
fluxes a further correction for taking into account the signal losses outside
the 2 arcsec slit. Since the size of the observed knots ranges between 5 and
10 arcsec2 (see Table 5 of Paper V), the estimated correction factors
result between 1 and 2. Wavelength calibration was obtained from the spectral
lines of a Xenon-Argon lamp; the associated uncertainty is comparable with the
spectral resolution element (2 pixels
5 Å). No significant shift
of the line centres from the rest wavelength has been detected.
As an example of our observations we show in Fig. 2 portions of the spectrum
of the brightest knot (G2), where several H2 0-0 lines have been
detected. These represent one of the first detections of pure H2 rotational
lines from the Earth. In addition, the spectra show several v=1-0 lines
belonging to the O series. No other line coming from species different from
H2 has been detected. The observed lines along with their spectral
identification and the excitation energy of the corresponding upper levels are
reported in Cols. 1-3 of Table 1. The line shapes are well represented by
gaussian profiles, which were fitted for computing the integrated line fluxes.
These latter with the associated 1
uncertainty, estimated by the rms
fluctuations of the adjacent baseline, are reported in Cols. 4-9 of Table 1.
Lines whose signal to noise ratio is between 2 and 3 are flagged. We note that
the line with the highest excitation energy (i.e. the 0-0 S(15)) was detected
only toward the G2 and G3 knots, which are those at the highest temperature
(T
2500 K, see Paper V).
![\begin{figure}
\par\includegraphics[width=6.5cm,clip]{Di175_f1.eps} %
\end{figure}](/articles/aa/full/2001/43/aadi175/Timg18.gif) |
Figure 1:
H2(2.122 m)-K (continuum subtracted) image of the IRS17
jet. The knots spectroscopically investigated with ISAAC are labelled
according to the identification code of Paper V, while the candidate exciting
source (IRS17-40) is marked with a cross. The slit orientation and
length are depicted as well. |
Open with DEXTER |
![\begin{figure}
\par\includegraphics[width=8cm,clip]{Di175_f2.eps} %
\end{figure}](/articles/aa/full/2001/43/aadi175/Timg19.gif) |
Figure 2:
Portions of the knot G2 spectrum where several H2 1-0 and 0-0
lines have been observed (indicated in the left upper corner of each panel). |
Open with DEXTER |
The line fluxes derived from our ISAAC observations have been combined with
those previously derived in the 1.6-2.5
m domain. In Paper V the SOFI
fluxes were used to construct rotation diagrams from which the
gas temperature and the visual extinction were simultaneously derived. These
data do not show any evidence of deviation from a linear
dependence, thus indicating that the traced gas is thermalised at
the derived temperature. Now, the newly detected lines offer the opportunity to
check the results of Paper V and to probe possible deviations from
LTE conditions.
Firstly, the fluxes of the lines detected with ISAAC were corrected for
the extinction by adopting the same
values derived from the SOFI
data, which range between 8 and 18 mag. Then, from
the so derived intrinsic fluxes, we calculated the data
points
to be just superimposed onto the rotation diagrams of Paper V. An
example of the obtained plots is depicted in Fig. 3, where the H2 rotation
diagrams relative to the G2 and C3 knots are shown. In each panel the dashed
line represents the LTE best fit to the population distribution at the
indicated temperature. As a general result we note that all the data points
relative to the ISAAC observations do not deviate from this straight line. We
will discuss in details the implications of this result in the next section.
Here we point out how the ISAAC lines allow to check the accuracy on the
visual extinction determination done in Paper V. Indeed, points corresponding
to extinction corrected lines emitted from the same upper level are expected
to be perfectly superimposed onto the rotation diagram. Such points are
represented in the investigated case by the pairs of lines: 1-0 S(1) and
1-0 O(5), 1-0 S(2) and 1-0 O(6), 1-0 S(3) and 1-0 O(7) (excited at 6950,
7583 and 8364 K, respectively), which generally overlap inside the error
bars in the rotation diagrams of Fig. 3. This circumstance, beside to testify
that a good estimate on the AV values has been obtained, assures
that a good inter-calibration exists between the SOFI and ISAAC data sets.
![\begin{figure}
\par\includegraphics[width=6.9cm,clip]{Di175_f3.eps} %
\end{figure}](/articles/aa/full/2001/43/aadi175/Timg57.gif) |
Figure 3:
H2 rotation diagrams for the knots G2 and C3. Filled and open
symbols indicate the lines observed with ISAAC and SOFI, respectively.
Triangles, squares and circles distinguish transitions coming from different
vibrational levels. In each panel the dashed line represents the best fit
through the line fluxes observed with SOFI (Paper V) at the temperature and
visual extinction indicated in the right upper corner. Vertical bars indicate
the lines coming from the same upper level (see text). |
Open with DEXTER |
We discuss here the found alignment onto a single straight line of all the
observative points. Such behaviour allows to rule out excitation by non
thermal processes, because in this latter case vibrational and
rotational temperatures should be different, and thus lines coming from various
vibrational states should lie onto straight lines with different slopes (see
e.g. Hora & Latter 1994).
Moreover, the presence of multiple gas components, which should result
in a smoothly curved line, rising toward higher excitation temperatures
,
is also rejected by our observations, which on the contrary
demonstrate that the H2 gas is thermalised at a single temperature
up to values of
22000 K.
This finding, together with the fact that the critical densities of
the involved levels span over three orders of magnitude (103-106 cm-3), suggests to use the observed lines to infer a stringent
lower limit to the gas density. To examine this possibility we developed a NLTE
model for the population of the first 51 levels of H2 (which correspond to a
maximum excitation temperature of about
25000 K), from which are
emitted transitions up to the vibrational state v=3. We adopted an abundance
ratio n(H)/n(H2)= 5
10-3, consistent with the predicted
value in dark clouds with AV larger than 4 mag (Hollenbach et al.
1991). Radiative decay rates are taken from Turner et al. (1977). The
collisional downward rates by impact of both atomic and molecular hydrogen for
each pair of levels are computed from the coefficients given by Draine et al.
(1983). Upward rates are computed using the principle of detailed balance. As
an example, the rotation diagrams obtained at temperature T=2400 K for
three different values of the gas density are reported in Fig. 4. Here is
evident how the v=1 and v=2 lines are still not thermalised for n=106 cm-3, while the v=3 lines reach the thermal equilibrium at densities
even larger than 107 cm-3.
The increasing underpopulation of levels with higher vibrational
state, although with similar excitation energy, has been explained
by Chang & Martin (1991) as due to the higher cross section which promotes
rotational more than vibrational excitation. Evidences of collisionally excited
gas in NLTE have been recognized in HH 7-11 (Everett 1997), where H2 lines
belonging to series from v=1 to v=3 have been detected. In this
case, however, NLTE signatures are blended with the effects caused to the
presence of different temperatures components. On the contrary, the
case presented here allows a straightforward intepretation. By comparing the
observative diagrams of Fig. 3 with the models of Fig. 4, and by
noting that the points relative to the 0-0 lines are well aligned with those
of the other transitions, we can infer a lower limit to the gas density of
107 cm-3. We remark that the v=3 transitions, although in
principle could be used as density indicators in analogy with the 0-0
lines, are predicted to be
100 times weaker than the 2.12
m
line.
The presence of a single temperature gas at
cm-3suggests a planar shock travelling in a medium with a high pre-shock density
as the most favourable excitation mechanism (Kaufman & Neufeld 1996). In
Paper V we noticed that such a mechanism could explain the SOFI observations
by assuming a shock velocity larger than 30 km s-1 and a pre-shock
density
105 cm-3. The lower limit to the post-shock density
derived here (>107 cm-3) indicates a shock compression factor
,
which is compatible with this kind of
shocks.
![\begin{figure}
\par\includegraphics[width=7.5cm,clip]{Di175_f4.eps}\end{figure}](/articles/aa/full/2001/43/aadi175/Timg62.gif) |
Figure 4:
Theoretical rotation diagrams for three density values
obtained with a NLTE model for the H2 excitation. Filled triangles,
filled squares, open circles and open triangles refer to transitions coming
from upper states with v=0, 1, 2, 3 respectively. The adopted
temperature is T = 2400 K, while the abundance ratio n(H)/n(H2) is
5 10-3. |
Open with DEXTER |
We have presented the VLT-ISAAC 3-5
m spectroscopy of the IRS 17 jet
in Vela-D Molecular Cloud. Along the investigated knots we observed
several H2 0-0 transitions with excitation energy up to
22000 K.
These have been used together with rovibrational lines previously observed in
the H-K bands to probe the gas physical conditions. The found alignment of all
the data points onto a single straight line demonstrates that the gas is
thermalised at a single temperature. Comparison with NLTE
models has allowed to put a lower limit to the gas density of 107 cm-3and the capability of the thermal 0-0 lines in probing collisionally
excited gas in NLTE conditions has been proved.
Finally, we remark that the presented observations point out
to a rare case of a pure planar shock, while usually bow morphologies are more
adequate to intepret the H2 data.
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Copyright ESO 2001