A&A 426, L49-L52 (2004)
DOI: 10.1051/0004-6361:200400074
M. Guélin 1 - S. Muller 1,2 - J. Cernicharo 3 - M. C. McCarthy 4 - P. Thaddeus 4
1 - IRAM, 300 rue de la piscine, 38406 Saint-Martin-d'Hères,
France
2 - Institute of Astronomy and Astrophysics, Academia Sinica, 128
Section 2, PO Box 1-87, Nankang, Taipei 115, Taiwan
3 - Instituto de Estructura de la Materia, C/Serrano 121, 28006 Madrid, Spain
4 - Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge,
MA 02138, USA
Received 29 July 2004 / Accepted 6 September 2004
Abstract
Following discovery of the free radical SiCN in the
C-star envelope
IRC+10216, we report the detection in the same
source of its isomer SiNC. The microwave spectra of SiNC and SiCN
were studied in
the laboratory and their rotational transition frequencies are accurately
known. The ground fine structure state of SiNC,
,
gives rise to a
series of rotational transitions, spaced by 12.8 GHz, each with
-doubling.
Five weak lines are detected with the IRAM 30-m telescope at the
frequencies of the
(e),
(f),
(f) and
(e) and (f)
rotational transitions. Other SiNC lines
from these or adjacent rotational transitions
are found to be blended with stronger lines from known molecules.
The lines assigned to SiNC have a cusped shape, characteristic of species
confined to a hollow shell in the outer circumstellar envelope. They are
twice weaker than their SiCN counterparts, which have the same shape, and
presumably arise in the same region of the envelope. SiNC and SiCN have
about the same abundance in IRC+10216, 4
10-9 with
respect to H2.
This contrasts with HCN, HC3N and HC5N, for which the cyanide to
isocyanide abundance ratio is >100.
Key words: stars: circumstellar matter - stars: AGB and post-AGB - stars: individual: IRC+10216 - ISM: molecules - radio lines: stars
Although many refractory molecules are observed close to the central star of IRC+10216, others, such as SiC, SiC2 and MgNC, are only detected in the outer envelope and are thought to form in situ (Guélin et al. 1993, hereafter GLC). The formation of refractory molecules in a cold, tenuous medium is poorly understood: it may be the result of gas-phase reactions between molecules and radicals or ions, or of reactions on dust grains (see GLC and the review of Glassgold 1996). To clarify this question, the study of additional refractory molecules is highly desirable.
The detection of refractory species in space is hampered by their low abundances and the lack of accurate spectroscopic data. Four years ago, Apponi et al. (2000) observed in a laboratory discharge three Si-bearing isoelectronic radicals, SiCCH, SiCN and SiNC, and measured their microwave spectra. These measurements led almost at once to the detection of SiCN in IRC+10216 (GMC). In this Letter, we report the detection in this source of its isomeric rearrangement SiNC.
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Figure 1:
Spectra of four rotational transitions of SiNC observed with
the 30-m telescope. Most lines in IRC+10216 are cusped in shape and
have widths
of 29 km s-1, like the
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Like SiCN and SiCCH, SiNC is linear and has a regular
electronic ground state.
Its rotational spectrum consists of nearly harmonic
doublets each split
by 11-13 MHz, separated by twice the rotational constant: 12.8 GHz.
Each rotational transition is further split by magnetic hyperfine
structure, but for the large
J transitions studied here that is unresolved,
and the spectrum reduces to the
doublets, the two
components of which are denoted e and f.
By analogy with SiCN, which has a similar moment of inertia and dipole
moment
,
the rotational lines of SiNC in IRC+10216 are expected to peak in intensity
at wavelengths between 3 mm and 2 mm.
The present observations of SiNC were made with the IRAM 30-m telescope. Two dual-polarization SIS-mixer receivers were used to observe the 3-mm and 2-mm rotational transitions; the receivers were tuned to a single sideband, with rejections of the image (upper) sideband >25 dB at 3-mm and >13 dB at 2-mm. (The rejection level was measured against a frequency-modulated load and checked by recording the intensity of strong astronomical lines from the image sideband.) The system noise temperature was 100-200 K.
Data were taken in the balanced wobbler-switching mode, with a wobbling frequency of 0.5 Hz and a throw of 1.5-2'. Zero to third-order baselines were removed across the 0.5 GHz-wide band of the spectrometer. The channel resolution was 1 MHz. The telescope pointing and focus were checked by monitoring the intensity and shape of the strongest lines lying in the IF band and, every 1-2 h, by observing a nearby planet or the continuum source OJ287.
Four rotational transitions of SiNC in IRC+10216,
,
,
,
and
,
are shown in Fig. 1. The millimeter lines in
this source generally have sharp edges and a constant width of 29
km s-1, making them
fairly easy to identify (see e.g. Fig. 2 of GMC and CGK). The typical
cusped profile
of a line arising in the outer envelope of IRC+10216 is shown
in the insert in Fig. 1d, where the thick grey line represents the
line of C4H (133 862 MHz) at a scale 1/60.
In Fig. 1, we have marked by a short vertical line the laboratory-derived rest
frequencies of the SiNC transition components, and by two vertical
arrows the positions
predicted for the edges of the SiNC lines (these arrows are at
km s-1 from the center of the line). Both components of the
doublet, although weak, are detected. This can be better seen on
the insert
in Fig. 1d where we have shown the average profile of both doublet
components (scale
1/1) superimposed on the C4H line, scaled down by a factor of 60.
Similarly, the high-frequency
components (f) of the
and
rotational
doublets are clearly detected (Figs. 1c and 1b). The low-frequency
components (e) of the
latter doublets are unfortunately
blended with much stronger lines of CP and NaCN and are not visible. Finally,
the (e) component of the
doublet is also
detected (Fig. 1a),
as is the low-frequency wing of the (f) component (see the thick grey
line near 82 960 MHz) -
the rest of which is blended with a strong line of C3H2.
Although the density of lines in IRC +10216 at the 2 mK level is fairly large, there is little doubt that the six lines in Fig. 1 are produced by SiNC. Rest frequencies of the components agree with the laboratory frequencies to within 1 MHz, or about 10% of a linewidth, and relative intensities agree well with those expected (see Table 1). We have searched for alternate assignments (in both the observed and the image receiver sidebands) in the standard catalogs of molecular transitions of astrophysical interest, as well as in a line catalog specifically assembled for IRC+10216 (see CGK). The transitions of known molecules that are likely to be present in Fig. 1, even at very weak levels, are indicated on the figure: none of them coincides to better than 4 MHz with our six SiNC lines. The density of lines that remain unidentified in IRC+10216 at the present sensitivity is typically two per 100 MHz (see GMC and Cernicharo et al. 2004), making it highly unlikely that the six SiNC lines in Fig. 1 are the result of chance coincidence.
Among the identified lines of other molecules in Fig. 1, we note the
lines of three 13C isotopomers of HC5N and the
-doublet of SiCN. The latter doublet has
already been reported by GMC,
but at a lower signal-to-noise.
The line at 82 905 MHz is identified by
Cernicharo et al. (2004) as the high-frequency
component of the
rotational transition of
the linear isomer of the HC4N radical.
In spite of the low
signal-to-noise, the SiNC lines of Fig. 1
appear to have the same cusped shape as the lines of SiCN
and of many carbon chain molecules and radicals (Fig. 2 of
GMC). Guélin et al. (1993, 2000)
have shown by interferometric observations that
the cusped lines in IRC+10216
are caused by the concentration of molecules in a thin shell of
radius 15
.
One of the best examples is the abundant SiCC molecule (Lucas et al. 1994).
Molecules in this thin shell
have mm-line intensities which agree with those expected for a Boltzmann
distribution of the rotational populations (see e.g. Kawaguchi et al.
1995 and CGK) - probably an indication of collisional
excitation and a fairly uniform shell. Rotational temperatures of molecules
with moments of inertia and dipole moments similar to those of SiNC
are all in the range 15-30 K. For SiCN, the
through
lines yield
K - possibly an underestimate since the lines are weak
and since the highest energy
lines that are observed originate from a level with
K.
For SiNC here, we derive
K, even
more uncertain because of the weakness of the lines (owing largely to
the 40% smaller dipole moment of SiNC relative to that of SiCN).
Assuming that the rotational temperature of SiNC is 18 K, we
derive a column density (twice the radial
column density accross the shell) of 2
1012 cm-2, about
equal to that of SiCN (GMC).
For both SiCN and SiNC, the population in the
ladder, which lies well above the
ground ladder, has been assumed to be negligible.
The column densities of SiNC and SiCN are similar to
that of MgCN (Ziurys et al. 1995) and are
20 times
smaller than those of SiC (Cernicharo et al. 1989) and
MgNC. On the assumption of a thin shell, the abundances of SiNC, SiCN and MgCN,
relative to H2, are
4
10-9.
Despite a dedicated search for its
rotational
transition, we have failed to detect SiCCH.
The 3
upper limit for the integrated intensity of this
line, 38 mK km s-1, yields an upper limit
to the SiCCH column density which is close to the value of the
detected lines of SiCN and SiNC (on the
assumption that
K).
This failure is hardly surprising: although MgNC and AlNC are readily
detected in IRC+10216, MgCCH and
AlCCH have not been found.
Table 1: Observed line parameters.
It has been argued by GMC
that SiCN may be formed in IRC+10216 by the radiative
association of Si+with HCN, leading to SiNCH+ and SiCNH+, followed by
dissociative recombination - a path similar to that proposed by
Glassgold et al. (1986) for the formation of SiC2.
The radiative association of Si+ with
HCN had been previously considered by Herbst et al. (1989) in their study of
silicon chemistry in interstellar clouds. These authors
derived a rather large reaction rate from laboratory measurements
in high pressure ternary conditions
(
cm3 mol-1 s-1).
The dissociative recombination of SiNCH+ would yield
SiNC. SiCN could also be formed from parallel reactions
of Si+ with HNC, but this isomer is 1000 times less abundant than
HCN in the outer envelope and is thus unlikely to play a significant role.
SiC2 and SiCN could also be formed through neutral gas phase reactions
involving free radicals. Recently Canossa et al. (2001) have measured in the
gas phase, the reaction:
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Neutral Si atoms may react also with HCN which is highly polar:
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Alternately, these silicon molecules could be synthesized on the surface of Si-rich grains. It is known that SiC, SiC2 and Si2C are abundant in certain stellar atmospheres, and that they condense quickly onto grains when they are expelled into space. The reaction of Si atoms with HCN on silicon substrates has been studied in the laboratory, and is found to proceed efficiently at 12 K, yielding both SiNC and SiCN (but with an unknown branching ratio: Maier et al. 1998). These molecules, once formed, may be released into the gas when the grains are exposed to interstellar UV radiation. According to GLC, the similarity of the spatial distributions of species as different as C4H, SiC2, MgNC, and, probably SiCN and SiNC, is better explained by grain chemistry than by gas phase reactions.