Issue |
A&A
Volume 519, September 2010
|
|
---|---|---|
Article Number | A2 | |
Number of page(s) | 17 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/201014539 | |
Published online | 06 September 2010 |
Molecular gas chemistry in AGN
II. High-resolution imaging of SiO
emission in NGC 1068: shocks or XDR?![[*]](/icons/foot_motif.png)
S. García-Burillo1 - A. Usero1 - A. Fuente1 - J. Martín-Pintado2 - F. Boone3 - S. Aalto4 - M. Krips5 - R. Neri5 - E. Schinnerer6 - L. J. Tacconi7
1 - Observatorio Astronómico Nacional (OAN)-Observatorio de Madrid,
Alfonso XII 3, 28014-Madrid, Spain
2 - Centro de Astrobiología (CSIC-INTA), Ctra de Torrejón a Ajalvir, km
4, 28850 Torrejón de Ardoz, Madrid, Spain
3 - Observatoire de Paris, LERMA, 61 Av. de l'Observatoire, 75014
Paris, France
4 - Department of Radio and Space Science with Onsala Observatory,
Chalmers University of Technology, 439 94 Onsala, Sweden
5 - Institut de Radio Astronomie Millimétrique (IRAM), 300 rue de la
Piscine, Domaine Universitaire de Grenoble, 38406 St. Martin d'Hères,
France
6 - Max-Planck-Institut für Astronomie, Königstuhl 17, 69117
Heidelberg, Germany
7 - Max-Planck-Institut für extraterrestrische Physik, Postfach 1312,
85741 Garching, Germany
Received 30 March 2010 / Accepted 7 May 2010
Abstract
Context. This paper is part of a multi-species
survey of line emission from the molecular gas in the circum-nuclear
disk (CND) of the Seyfert 2 galaxy NGC 1068. Unlike in other
active galaxies, the intensely star-forming regions in
NGC 1068 and the CND can be resolved with current
instrumentation. This makes this galaxy an optimal test-bed to probe
the effects of AGN on the molecular medium at 100 pc scales.
Aims. Single-dish observations have provided
evidence that the abundance of silicon monoxide (SiO) in the CND of
NGC 1068 is enhanced by 3-4 orders of magnitude with respect
to the values typically measured in quiescent molecular gas in the
Galaxy. We aim at unveiling the mechanism(s) underlying the SiO
enhancement.
Methods. We have imaged the emission of the SiO(2-1)
(86.8 GHz) and CN(2-1) (226.8 GHz) lines in
NGC 1068 at 150 pc
and 60 pc spatial resolution with the IRAM Plateau de Bure
interferometer (PdBI). We have also obtained complementary IRAM
30 m observations of HNCO and methanol (CH3OH)
lines. These species are known as tracers of shocks in the Galaxy.
Results. SiO is detected in a disk of 400 pc
size around the AGN. SiO abundances in the CND of
are
about 1-2 orders of magnitude above those measured in the
starburst ring. The overall abundance of CN in the CND is high:
.
The abundances of SiO and CN are enhanced at the extreme velocities of
gas associated with non-circular motions close to the AGN (r<70 pc).
On average, HNCO/SiO and CH3OH/SiO line ratios
in the CND are similar to those measured in prototypical shocked
regions in our Galaxy. Yet the strength and abundance of CN in
NGC 1068 can be explained neither by shocks nor by
photon-dominated region (PDR) chemistry. Abundances measured for CN and
SiO and the correlation of CN/CO and SiO/CO ratios
with hard X-ray irradiation suggest that the CND of NGC 1068
has become a giant X-ray-dominated region (XDR).
Conclusions. The extreme properties of molecular gas
in the circum-nuclear molecular disk of NGC 1068 result from
the interplay between different processes directly linked to nuclear
activity. The results presented here highlight in particular the
footprint of shocks and X-ray irradiation on the properties of
molecular gas in this Seyfert. Whereas XDR chemistry offers a simple
explanation for CN and SiO in NGC 1068, the relevance of
shocks deserves further scrutiny. The inclusion of dust grain chemistry
would help solve the controversy regarding the abundances of other
molecular species, like HCN, which are under-predicted by XDR models.
Key words: galaxies: individual: NGC 1068 - galaxies: ISM - galaxies: kinematics and dynamics - galaxies: nuclei - galaxies: active - radio lines: ISM
1 Introduction
Nuclear activity and intense star formation can shape the excitation and chemistry of molecular gas in the circum-nuclear disks (CND) of galaxies. The effect of strong radiation fields (UV and X-rays) and the injection of mechanical energy (by gas outflows or jet-ISM interactions) on molecular gas properties are key ingredients in the feedback of activity. Molecular line observations can be used to study the nature of the dominant source of energy in galaxies hosting both active galactic nuclei (AGN) and intense star formation. Furthermore, nearby galaxies can serve as local templates of distant galaxies, where these phenomena can be deeply embedded.
Some of the tracers of the dense molecular gas phase, which
are commonly used in extragalactic research, can be heavily affected by
the feedback of AGN activity. In particular the lines of HCN (the most
widely observed tracer of the dense molecular medium) appear as over-luminous
in the CND of many Seyfert galaxies with respect to other tracers of
the dense molecular gas (Tacconi et al. 1994; Kohno
et al. 2001;
Usero et al. 2004,
hereafter U04; Krips et al. 2008).
Doubts have thus been cast on the universality of the conversion factor
between the luminosity of the HCN(1-0) line,
,
and the mass of dense molecular gas in active galaxies (Graciá-Carpio
et al. 2006,2008; García-Burillo
et al. 2006;
Krips et al. 2008).
X-rays can efficiently process large column densities of molecular gas
around AGNs, producing X-ray dominated regions (XDR). It has been
proposed that the abundances of certain ions, radicals and molecular
species, like HCN, can be enhanced in XDR (Lepp &
Dalgarno 1996;
Maloney et al. 1996;
Meijerink & Spaans 2005;
Meijerink et al. 2007).
However, it is still controversial whether pure gas-phase XDR models
are able to enhance HCN abundances in AGN to the level imposed by
observations.
The inclusion of dust grain chemistry, not taken into account
by gas-phase XDR schemes, could solve the HCN controversy in AGN by
enhancing the abundance of this molecule. Besides HCN, other molecular
species can also undergo significant changes in their abundances due to
dust grain processing. X-rays can evaporate small (10 Å)
silicate grains (Voit 1991).
This can increase the Si fraction in the gas phase and then
considerably enhance the abundance of SiO in X-ray irradiated molecular
gas (Martín-Pintado et al. 2000;
U04; García-Burillo et al. 2008;
Amo-Baladrón et al. 2009).
Furthermore, mechanical sputtering of dust grains in molecular shocks
is an additional source of dust grain chemistry. Large SiO abundances
have been found in the nuclei of a number of non-AGN galaxies where
interferometer maps have been the key to identifying large-scale
molecular shocks (García-Burillo et al. 2000,2001; Usero
et al. 2006).
To address the role of X-rays and shocks in shaping the chemistry of molecular gas in AGN requires a multi-species approach. Unlike SiO, other tracers of the dense molecular gas, like CN, are not expected to be highly abundant in shocks (Mitchell 1984; Fuente et al. 2005; Rodríguez-Fernández et al. 2010). However, there is a consensus supported by observations and theoretical models that the CN radical is a privileged tracer of highly ionized molecular gas, typical of photon or X-ray-dominated regions (PDR or XDR) (Boger & Sternberg 2005; Fuente et al. 1993,2008; Janssen et al. 1995; Lepp & Dalgarno 1996; Meijerink & Spaans 2005; Meijerink et al. 2007). Observations of tracers like SiO and CN can then be used to quantify the relevance of shocks and XDR chemistry in AGN. Furthermore the high-spatial resolution provided by interferometers is paramount to spatially distinguish between the different chemical environments (star formation vs AGN activity) that can coexist in a single galaxy.
NGC 1068 is the strongest nearby Seyfert 2 galaxy,
and as such is a prime candidate for studying the feeding and the
feedback of activity using molecular line observations. Tacconi
et al. (1994)
and Schinnerer et al. (2000,
hereafter S00) used the Plateau de Bure Interferometer (PdBI) to map
the emission of molecular gas in the central
kpc
disk at high-resolution (1-4
)
using HCN and CO lines. The CO maps spatially resolve
the distribution of molecular gas in the disk, showing a prominent
starburst ring (hereafter SB ring) of
1-1.5 kpc-radius,
which significantly contributes to the total CO luminosity of
NGC 1068 (see also Planesas et al. 1991; and
Baker 2000,
hereafter B00). Furthermore, CO emission is detected in a
central
pc
CND surrounding the AGN. In contrast to CO, emission from the HCN(1-0)
line, which is also spatially resolved in Tacconi et al.'s
maps, arises mainly
from the CND. Tacconi et al. (1994) derived a high
HCN/CO intensity ratio (
1) in the CND. This is about a
factor of 5-10 higher than the average ratio measured in the SB ring
(Usero et al., in prep.). Radiative transfer calculations
based on multi-line observations of HCN and CO showed that the
abundance of HCN relative to CO was significantly enhanced in
the CND: HCN/CO
10-3
(Sternberg et al. 1994).
Usero et al. (2004)
used the IRAM 30 m telescope to observe with low to moderate
spatial resolutions (10-30
)
the emission of eight molecular species in the CND of
NGC 1068. The global analysis of the survey, which includes
several lines of SiO, CN, HCO, H13CO+,
H12CO+, HOC+,
HCN, CS, and CO, indicated that the bulk of the molecular gas emission
in the CND of NGC 1068 could be interpreted as coming from a
giant XDR. More recently, Pérez-Beaupuits et al. (2007,2009) analyzed new
single-dish data obtained for several rotational lines of HCO+,
HNC, CN and HCN, and arrived at similar conclusions as U04. However,
the low spatial resolution of these single-dish observations are not
optimal to precisely distinguish the contributions of the starburst and
the CND in NGC 1068.
We here use the high-spatial resolution (1-3
)
afforded by PdBI to map the emission of the (v=0, J=2-1)
line of SiO and the N=2-1 transition of CN in the
central
kpc
disk of NGC 1068. The spatial resolution of the new
observations, one order of magnitude higher than that of the
30 m survey of U04, allows us to neatly separate the emission
of the SB ring from that of the CND. Furthermore, the SiO and CN PdBI
maps are used together with complementary single-dish data obtained in
CH3OH and HNCO lines to study the chemical differentiation
inside the CND through an analysis of line ratio maps. Line ratios are
interpreted with the help of one-phase large velocity gradient (LVG)
models. While the emission of the different lines and species analyzed
here likely comes from regions characterized by different physical
conditions, the adopted one-phase approach allows us to explore the
existence of overall trends in the chemical abundances of these species
with a minimum set of free parameters in the fit. We explore the
dependence of line ratios with the illumination of molecular gas by the
X-ray AGN source. We also explore the link between shock chemistry and
gas kinematics in the CND.
We describe in Sect. 2 the
observations, including high-resolution SiO, CN and CO maps
obtained with the PdBI, single-dish data obtained with the
30 m telescope as well as X-ray images taken by Chandra of
NGC 1068. Section 3 presents the
continuum maps derived at 86.8 GHz and 226.8 GHz. The
distribution and kinematics of molecular gas derived from SiO and CN
are described in Sects. 4 and 5. SiO and CN
abundances are discussed in Sect. 6. In
Sect. 7
we interpret the
line ratio maps in terms of two different chemical scenarios (shocks
and XDR). The main conclusions of this work are summarized in
Sect. 8.
We assume a distance to NGC 1068 of Mpc (Bland-Hawthorn
et al. 1997);
this implies a spatial scale of
70 pc/
.
2 Observations
2.1 Interferometric maps
Table 1: Observational parameters of the SiO and CN PdBI data.
Observations of NGC 1068 were carried out with the PdBI array (Guilloteau et al. 1992) between 2004 December and 2005 February. We used the BC configurations and six antennae in dual frequency mode. We simultaneously observed the (v=0, J=2-1) line of SiO (at 86.847 GHz) and the N=2-1 transition of CN. The CN(2-1) transition is split up into 18 hyperfine lines blended around three groups (J=5/2-3/2, J=3/2-1/2 and J=3/2-3/2). We observed the two strongest groups of lines at 226.9 GHz (J=5/2-3/2) and 226.7 GHz (J=3/2-1/2), hereafter referred to as high-frequency (HF) and low-frequency (LF) CN lines, respectively. During the observations the spectral correlator was split into two halves centered at 86.800 GHz and 226.767 GHz. This choice allowed us to cover the SiO line at 3 mm and the CN lines at 1 mm. The J=1-0 line of H13CO+ (at 86.754 GHz) is simultaneously covered by the 3 mm setup. Rest frequencies were corrected for the recession velocity initially assumed to be







The image reconstruction was done with the
standard IRAM/GILDAS software (Guilloteau & Lucas 2000). We used
natural weighting and no taper to generate the SiO line map with a size
of 64
and
0.25
/pixel
sampling; the corresponding synthesized beam is
,
.
We also used natural weighting to generate the CN map with a size of 32
and
0.12
/pixel
sampling; this enabled us to achieve a spatial resolution of
1'' (
,
). The conversion factors
between Jy beam-1 and K are
22 K Jy-1 beam at
86.8 GHz, and 21 K Jy-1 beam
at 226.8 GHz. The point source sensitivities were derived from
emission-free channels. They are 1.5 mJy beam-1
in 2.5 MHz-wide channels at 3 mm, and
7.6 mJy beam-1 in
6.25 MHz-wide channels at 1 mm. Images of the
continuum emission of the galaxy were obtained by averaging those
channels free of line emission at both frequency ranges. The
corresponding point source sensitivities for continuum images are
0.3 mJy beam-1 at
86.8 GHz and 0.7 mJy beam-1
at 226.8 GHz.
We use the 1.8
resolution
CO(1-0) interferometer maps of NGC 1068 obtained
with the PdBI by S00. We list in Table 1 the relevant
parameters for the SiO and CN PdBI observations presented here.
2.2 Single-dish spectra
New CH3OH and HNCO observations of the
nucleus of NGC 1068 were carried out in 2006 July
with the IRAM 30 m telescope at Pico de Veleta (Spain). We
observed the 2k-1k group
of transitions of CH3OH. This group is a blended
set of four lines. Hereafter we consider the frequency of the 20-10A+ line
(96.741 GHz) as velocity reference.
We observed the higher frequency group of transitions of methanol at
2 mm (denoted as 3k-2k),
a blended set of eight lines. The frequency of the 30-20A+ line
(145.103 GHz) is taken as velocity reference. We also observed
the 4
04-303
rotational transition of HNCO (hereafter designated as 4-3) at
87.925 GHz. The corresponding beam sizes of the telescope are 28
at
3 mm and 17
at
2 mm. The 3 mm and 2 mm SIS receivers of
the 30 m telescope were tuned to the redshifted frequencies of
the lines around
km s-1.
The velocity range covered was
for the 3 mm lines and
for the 2 mm lines. The wobbler switching mode was used to
obtain flat baselines with a maximum beam throw of 4
.
Typical system temperatures during the observations were 200 K
at 3 mm and
300 K
at 2 mm. All receivers were used in single side-band mode
(SSB), with a high rejection of the image band.
The calibration accuracy is better than 20
.
Pointing of the 30 m telescope was regularly checked every
1.5 h by observing a nearby continuum source; we found an
average rms pointing error of 2-3
during
the observations.
Throughout the paper line intensities are given in antenna
temperature scale, .
The
scale relates to the main beam temperature scale,
,
by the equation
,
where
and
are, respectively, the forward and beam efficiencies of the telescope
at a given frequency. For the IRAM 30 m telescope
(1.48) at 86 GHz (145 GHz).
![]() |
Figure 1:
Continuum maps obtained with the PdBI towards the nucleus of
NGC 1068 at 3 mm (grey scale contours: 3%, 5%, 10%,
15%, 25% to 85% in steps of 15% of the maximum =
39.8 mJy beam-1) and
1 mm (white contours: 20% to 95% in steps of 15% of the
maximum = 14.2 mJy beam-1).
The lowest contours correspond to |
Open with DEXTER |
![]() |
Figure 2:
a) (Upper panel) SiO
integrated intensity map (contour levels are 3 |
Open with DEXTER |
![]() |
Figure 3:
CN integrated intensity map. Contour levels are 3 |
Open with DEXTER |
3 Continuum maps
Figure 1 shows the continuum maps derived at 86.8 GHz and 226.8 GHz in the nucleus of NGC 1068. The morphology of the maps is similar to that described by Krips et al. (2006), who observed the continuum emission at the nearby frequencies 110 GHz and 230.5 GHz. The emission consists of a central component (AGN core), a NE elongation (jet), and a SW elongation (counter-jet). The counter-jet and the jet are only detected at 3 mm.
We used the GILDAS task UV-FIT to fit
the continuum visibilities at both frequencies with a set of three
point sources. Most of the flux comes from the compact source located
at the position of the VLBI radio core at (
,
,
0
).
The AGN core has a flux of 39.
.3 mJy
and 16.
.7 mJy
at 86.8 GHz and 226.8 GHz, respectively. The NE jet
component is fitted by a point source of 23.
.3 mJy at
86.8 GHz, located at (
,
,
3.4
).
The 3 mm counter-jet point source at (
,
,
)
has a flux of
mJy.
There are nevertheless hints of extended emission, mostly at
3 mm, which are not fully accounted for by the point source
fitting (Krips et al. 2006).
Taking into account the differences in frequency, spatial resolution
and fitting functions used, the solution described above agrees with
that found by Krips et al. (2006,
see their Table 1 for a detailed description).
4 Molecular gas distribution
4.1 SiO distribution
Figure 2
shows the SiO(2-1) intensity map obtained by integrating the emission
in velocity channels from v = 967 to
1307 km s-1. In this velocity
range the line emission is detected at significant 3
levels on scales larger than the beam inside the PdBI field of view. We
overlay the SiO(2-1) map on the CO(1-0) map of S00. The CO map
fairly represents the overall molecular gas distribution in
NGC 1068. Schinnerer et al. (2000) estimated that
the CO PdBI map recovers
80
of the total flux, based on the comparison between the CO flux
measured by the PdBI and the flux derived from the CO maps
obtained through the combination of the BIMA array and NRAO single-dish
data of Helfer & Blitz (1995).
For the sake of comparison, the spatial resolution of the CO(1-0) map
shown in Fig. 2,
originally
1.8
,
was degraded to that of the SiO data. In Fig. 2 we also compare
the SiO map to the morphology of the jet derived from the 3 mm
continuum data.
Unlike CO, most of the total SiO emission detected inside the
PdBI primary beam comes from a circum-nuclear molecular disk located
around the AGN, referred to as CND. The integrated flux of SiO in the
CND is 2 Jy km s-1.
This is
74
of the total flux detected by U04 at 28
spatial
resolution with the 30 m telescope towards the AGN.
U04 estimate that
75
of the SiO emission of their AGN spectrum comes from the CND itself,
with a residual
25
contribution from the SB ring. Taken together, these
estimates indicate that the PdBI recovers practically all of the SiO
flux in the CND. Little SiO emission is detected from the SB ring in
the PdBI map. A few SiO clumps with sizes
beam and intensities at the 3-4
level are distributed along the SB ring.
The overall distribution of SiO in the CND, spatially resolved
by the PdBI beam, shows an east-west elongation. The deconvolved full
size of the emission at a 4
level is
400 pc
along the east-west axis. The CND is marginally resolved along the
north-south axis; the corresponding deconvolved size is
150 pc.
These sizes are comparable with those derived from the higher
resolution 1-0 and 2-1 CO maps of the CND published by S00, as
well as with those derived from the CN(2-1) map described in
Sect. 4.2.
The SiO emission is slightly asymmetric around the AGN: the SiO
emission peak is at (
,
,
0
).
Instead, the CO map shows a maximum at (
,
,
0
)
(see Fig. 1 of S00). The latter corresponds to the E
CO knot, in the notation of S00. The E CO knot is
thus shifted
50 pc
east relative to the E SiO knot.
4.2 CN distribution
Both lines of CN (LF and HF, as defined in Sect. 2) are
detected in the CND of NGC 1068. As expected, none of the CN
lines are detected towards the SB ring, as this region is located well
beyond the edge of the primary beam of the PdBI at 226.8 GHz.
The HF/LF intensity ratio shows no significant spatial variation inside
the CND. The average ratio, 1.7,
closely agrees with the value expected in the limit of optically thin
emission (
).
For the remainder of this paper we will use the higher S/N
ratio maps of the HF line.
Figure 3
shows the intensity map of the HF line of CN(2-1) obtained towards the
CND of NGC 1068. We integrated the emission in velocity
channels from v = 955 to 1277 km s-1,
i.e., similar to the velocity range used to derive the SiO map. With
this choice we encompass all significant line emission and at the same
time avoid blending with the LF CN(2-1) line. At this spatial
resolution (1
)
the overall morphology of the CND traced by CN roughly resembles that
seen in CO lines. At close sight there are noticeable
differences between these tracers, though. The two CN knots, connected
by a bridge of emission on the northern side of the CND, lie at (
,
,
0
)
and (
,
,
).
As for SiO, the CN knot located east is significantly closer to the AGN
compared to the corresponding CO knot.
5 Molecular gas kinematics
5.1 Background from previous work
The overall kinematics of molecular gas in the disk of
NGC 1068 were modeled by S00 and B00. One of the scenarios
advanced by S00 invokes two embedded bars: an outer oval and a nuclear
bar of 17 kpc
and 2.5 kpc deprojected diameters, respectively. The two bars
are coupled through resonance overlapping, so that the corotation of
the nuclear bar coincides with the outer inner Lindblad resonance (ILR)
of the oval. The gas response inside
(350 pc), a region that encompasses the whole CND detected in
SiO and CN, would lie between the ILRs of the nuclear bar.
Schinnerer et al. (2000)
and B00 also proposed a nuclear warp model to alternatively account for
the anomalous kinematics of molecular gas in the CND. The non-coplanar
gas response in the nuclear region could have been caused by the
interaction of the molecular disk with the jet or with the associated
ionization cone. Baker's model proposes a warped molecular disk that
evolves from a low inclination (
)
at
to a highly-inclined disk (
)
at
.
This configuration naturally explains the steep velocity gradient (high
velocities) measured in the major axis position-velocity (p-v)
diagram of CO at small radii (
).
In particular, S00 favor a hybrid model where the gas response to the
bar is combined with a nuclear warp. Besides being able to reasonably
fit the gas kinematics, the main advantage of the hybrid solution over
the pure bar model is that the first explains the asymmetric excitation
of molecular gas evidenced by the remarkably different R=2-1/1-0
line ratios measured in the east and the west CO lobes.
Baker (2000)
argues that the east lobe with the higher R
corresponds to the directly X-ray illuminated surface of a warped disk,
whereas the west lobe corresponds to the back of the warped disk,
characterized by a lower R. The
illumination of the CND gas by X-rays may also explain the particular
chemistry of molecular clouds analyzed in Sect. 6.2.
The kinematics of molecular gas in the inner pc
region are also complex, as recently revealed by the 2.12
m H2
1-0 S(1) map of Müller-Sánchez et al. (2009). These data,
mostly sensitive to hot (
K) and moderately
dense (n(H
cm-3)
molecular gas, show a structure that bridges the CND and the central
engine. This connection is made through highly elliptical streamers
detected in H2 lines. Davies et al. (2008) used these data
to study the large-scale kinematics of molecular gas in the CND itself
and concluded that the whole CND is a lopsided ring in expansion (Krips
et al., in prep.). The scenario of an expanding ring, first
advanced by Galliano & Alloin (2002), could be
linked to the onset of a nuclear warp instability.
5.2 SiO kinematics
Figure 4a
shows the isovelocity contour map of the CND of NGC 1068
derived from SiO. Isovelocities were obtained using a 3
clipping on the data cube. The velocity centroid of SiO emission
towards the AGN is
km s-1
in HEL scale. Gas velocities are red (
)
on the northwest side of the CND, while blue velocities (
)
appear southeast. This picture is consistent with a spatially resolved
rotating molecular structure. The kinematic major axis is fitted to
to expand the maximum range of SiO radial velocities at the edge of the
CND (
).
This solution lies within the wide range of PA values derived from the
photometric fitting of the disk and, also, from the observed stellar
and gas kinematics (
,
Brinks et al. 1997;
Dehnen et al. 1997;
S00; B00; Emsellem et al. 2006;
Gerssen et al. 2006).
We note that SiO isovelocities are twisted to larger position angles (
)
at smaller radii (
),
which already suggests non-circular and/or non-coplanar motions in the
CND. A similar isovelocity twist is seen in other molecular tracers, as
pointed out by B00. Outside the CND, the large-scale stellar and gas
kinematics indicate that the major axis of the disk is oriented
east-west (Emsellem et al. 2006).
We therefore adopt below PA = 90
as the best guess for the major axis orientation.
Figure 4b
shows the SiO p-v diagram
along the major axis. The p-v diagram
is mostly symmetric for the lowest contour levels around the position
of the AGN (
),
and with respect to a radial velocity
(HEL
km s-1.
We therefore adopt the first as the dynamical center and the second as
the systemic velocity
of the galaxy. This value of
agrees well with all previous determinations of the galaxy's receding
velocity (
km s-1,
e.g., de Vaucouleurs et al. 1991; Huchra
et al. 1999).
The highest contour levels of the p-v plot
are shifted east, however; this reflects the overall east-west
asymmetry of the CND described in Sect. 4.1.
The steep velocity gradient (high velocities)
measured along the major axis at
can be interpreted at face value as a signature of rotation for a
highly inclined disk. Figure 4b
nevertheless confirms non-circular motions in the CND: SiO emission is
detected at regions of the p-v
diagram which are forbidden by circular rotation:
emission in quadrants I and II of Fig. 4b can be
interpreted by gas which is in apparent counter-rotation and/or moving
radially outward. In either case, this can be taken as evidence that
gas orbits must be either elongated, if they lie in a common plane, or,
alternatively, non-coplanar
.
Note that the detection of SiO gas in these regions cannot be explained
by beam smearing effects: the deconvolved size of the emission for the
velocity channels with the largest excursions into I
and II (
1155 km s-1
and 1125 km s-1, respectively)
is
1.5
the beam size at
.
Similar features are detected in the 0.7
resolution
CO(2-1) map of S00 (Fig. 4 of S00).
As discussed in Sect. 5.3, CN
emission is also associated with forbidden
velocities.
In the extended ILR region of the CND it is expected that the
gas flow would trace the gradual transition from the x1
orbits of the nuclear bar (between corotation and the outer ILR) to the
x2 orbits (between the ILRs)
(e.g., Athanassoula 1992;
Buta & Combes 1996).
Orbits of the x2 family
would thus account for most of the CO and SiO emission
detected at high velocities at
in the major axis p-v diagrams
of Fig. 5a.
Contrary to SiO emission, which is mainly restricted to the CND,
CO emission is detected over the SB ring (
),
but also in a region that connects the CND with the SB ring. A
significant percentage of the CO emission on these
intermediate scales (
3-8
)
is detected at low velocities, i.e., at velocities
significantly below the terminal limit imposed by the rotation curve at
these radii (Fig. 5a).
This is the kinematic signature of the gas response to the stellar
potential, characterized in this region by the crowding of x1
orbits at the leading edges of the bar (S00; B00). As expected, the
x1
+ x2 orbit combination
produces a double-peaked line-of-sight velocity distribution in the
CO p-v diagram that
shows the characteristic figure-of-eight trend as a
function of radius where high velocities lie at
small radii (Kuijken & Merrifield 1995; García-Burillo
& Guélin 1995).
![]() |
Figure 4:
a) (Upper panel)
SiO isovelocities contoured over false-color velocity maps. Velocities
span the range [1050 km s-1,
1225 km s-1] in steps of
25 km s-1. The velocity scale
is HEL. The AGN position is marked with a star. The position of the
kinematic major axis derived from SiO at
|
Open with DEXTER |
![]() |
Figure 5:
a) (Upper panel)
Position-velocity diagram of CO(1-0) (contours; data from S00 degraded
to the resolution of SiO) and SiO(2-1) (color scale; this work) along
|
Open with DEXTER |
In the light of the published dynamical models of NGC 1068
(S00; B00), we conclude that most of the SiO emission in the CND is
associated with a region identified as the extended ILR region of the
galaxy. Non-coplanar motions have alternatively been proposed to fit
the CND kinematics. Nonetheless in either case (nuclear bar or nuclear
warp) the high velocity emission detected in SiO is physically
associated with gas lying at small radii (
).
![]() |
Figure 6:
Same as Fig. 4
showing in a) (Upper panel)
CN isovelocities, derived from the high frequency (HF) 2-1 transition
of CN, contoured over false-color velocity maps. Velocities span the
range [1025 km s-1,
1200 km s-1] in steps of
25 km s-1. Similarly, we show
in b) (Lower panel)
the p-v diagram of CN along the
major axis at |
Open with DEXTER |
5.3 CN kinematics
Figure 6a
shows the isovelocity contour map of the CND of NGC 1068
derived from CN. Isovelocities were obtained with a 3
clipping on the data. Compared to SiO, the higher spatial resolution of
the CN maps provides a sharper but more complex picture of the gas
dynamics in the CND. The rotating pattern of the CN emitting gas is
highly perturbed. The overall kinematics suggest an east-west
orientation of the major axis. However, at close sight the PA of the
major axis changes from 90
to 180
over the spatial extent of the E CN knot. In addition, isovelocities
show an irregular pattern at the W CN knot. In spite of the more
complex kinematics revealed by the higher resolution CN map on smaller
scales, we will nevertheless assume below the same overall orientation
and kinematic parameters determined from SiO. As argued in
Sect. 5.2,
this is a reasonable guess compatible with previous determinations
based on the observed stellar and gas kinematics.
Figure 6b
shows the CN p-v diagram along
.
At this spatial resolution the p-v
diagram shows a strong east-west asymmetry: most of the gas emission
appears associated to the E knot. Similarly to SiO, CN emission is
detected at regions of the p-v
diagram which are forbidden by circular rotation.
For CN, forbidden velocities appear mostly at quadrant I (see
Fig. 6b).
Due to the higher spatial resolution, the velocity gradient measured
along the major axis is
a
factor of two steeper in CN than in SiO. Otherwise the two molecular
tracers of the CND share the same kinematic features, such as the
existence of high velocity emission at small radii
(for CN
;
see Fig. 6b),
likely connected to x2
orbits. Like SiO, CN shows no detectable emission at low
velocities on intermediate scales (
;
see Fig. 5b).
6 Molecular abundances
In Sect. 6.1 we use the average SiO/CO and SiO/H13CO+ intensity ratios measured in the CND and the SB ring to derive the global abundance of SiO in the two regions with a one-phase LVG radiative transfer model. We further analyze in Sect. 6.2 the SiO/CO and CN/CO intensity ratio patterns inside the CND, as derived from the high-resolution PdBI maps. We discuss how these patterns can be interpreted in terms of different physical/chemical properties of molecular gas in the CND.
6.1 SiO abundances in the CND and the SB ring
We estimated the average SiO/CO velocity-integrated intensity
ratios (
)
measured in the CND and the SB ring regions defined as follows. Based
on the CO distribution shown in Fig. 2a, we delimit the
SB ring as the region between
and
with SiO intensities >2.5
levels to derive integrated values. Similarly, the CND region is
defined by a 2.5
clipping on the integrated intensities of the SiO map of Fig. 2b. Intensity
units used to derive line ratios are K km s-1
with K in
scale. The
ratios are thus equivalent to brightness temperature ratios, because
the line widths for SiO and CO are comparable at this spatial
resolution.
The maximum ratio in the SB ring corrected by the different
primary beam attenuation factors is
,
a ratio estimated from the average spectrum of the clumps detected in
SiO. This is a factor of
20
lower than the corresponding ratio averaged over the CND, estimated as
.
The dichotomy between the CND and the SB ring is apparent from the
remarkably different
ratios measured in the two regions. The origin of this dichotomy could
be found in the different physical conditions or, alternatively, in the
different chemical properties of molecular gas in these two regions.
Below we use a radiative transfer code to fit the set of available line
ratios to distinguish the contribution of different factors.
6.1.1 LVG model results
To estimate the SiO abundances both in the CND and in the SB ring, we
adopted a one-phase LVG approach to model the radiative transfer of the
SiO emission. We used an LVG code to translate the SiO brightness
temperatures into the SiO column density per velocity width (
)
and the volume density of its collisional partner, H2
(n(H2)), in each cloud. We
fed into the LVG code the average SiO(2-1) brightness temperature (from
our PdBI observations) and the average SiO(3-2)/SiO(2-1)
velocity-integrated line ratio (from U04), hereafter
,
measured in each target region. Provided that the 3-2 and 2-1 SiO
emissions arise from the same clouds in each region,
remains independent of the unknown filling factor
.
To further constrain the model, the gas kinetic temperature was fixed
at 50 K, as obtained by Tacconi et al. (1994) from
multi-transition CO observations of the CND. This assumption
is not critical, because the results barely depend on the gas
temperature below, e.g., 100 K. Quite likely, 100 K
is a comfortable upper limit to the average temperature of the
SiO-emitting gas in a PdBI beam.
The output of the LVG code is summarized in Fig. 7. Because the
filling factors are unknown the possible solutions for the CND (SB
ring) clouds would lie over the corresponding
isocontour, anywhere to the right of the intersect with the CND (SB
ring) SiO(2-1) isocontour (i.e., the lower
,
the higher
in a cloud). The loci of possible solutions become two-dimensional
bands once we also consider the uncertainties in
.
The measured
ratios correspond to typical gas densities of
105 cm-3
in the CND, while they are about five times lower in the SB ring.
We searched for a reasonable estimate of the SiO abundance
with respect to H2 (X(SiO
)
in the SB ring and the CND. For this we used ancillary
CO observations of NGC 1068 to infer the H2
column density. A full radiative transfer approach (e.g., LVG) is
impossible though in the SB ring, because multi-transition
CO observations are not available in this region.
Alternatively, we used the standard conversion between the CO(1-0)
integrated intensities and the H2 column
densities (
)
given by the so called
factor in the two target regions. The
conversion factor is on the order of
cm-2/(km s-1)
in the Milky Way (Strong et al. 1988), a value which
roughly holds true for most nearby galaxies. We adopted the Galactic
value for the SB ring. It is known though that a lower
has been found in galaxy centers, where molecular clouds are subject to
abnormal conditions (e.g., they are unlikely to be virialized). In
particular,
in the CND of NGC 1068, could be
5 times lower than
the standard value, according to the estimates of U04, a result which
agrees with the findings obtained in the nuclear disks of other spiral
galaxies (e.g., García-Burillo et al. 1993).
Under these assumptions, we proceeded as follows to estimate X(SiO) in the SB ring and the CND:
- each target region is characterized by fixed
and
values
, assumed to be independent of the filling factor, and by a certain
;
- The measured
allows us to calculate the SiO(2-1) brightness temperature as a function of
from the diagram in Fig. 7;
-
is proportional to the product of
and the SiO(2-1) brightness temperature. Thus, ultimately, X(SiO) can be expressed in terms of a certain function of
parameterized by
,
ratios and
;
- the range of values for
can be constrained. The lower limit to
corresponds to
. On the other hand, for
arbitrarily low, the CO(1-0) brightness temperatures in a cloud would rise above the assumed kinetic temperature (50 K), which cannot occur if CO is collisionally excited. This sets an upper limit to
.







![]() |
Figure 7:
LVG results for SiO, assuming a kinetic temperature of
|
Open with DEXTER |
![]() |
Figure 8:
SiO abundances estimated from the LVG model as a function of the SiO
column density per velocity width (
|
Open with DEXTER |
![]() |
Figure 9:
a) ( Upper left panel) SiO(2-1)/CO(1-0)
velocity-integrated intensity ratio (
|
Open with DEXTER |
6.1.2 SiO/H13CO+ ratios
The results of the radiative transfer model described above can be compared to an alternative estimate of the abundance of SiO in the CND, based on the observed SiO/H13CO+ line ratio. The H13CO+(1-0) line, observed simultaneously with the SiO(2-1) line, was also detected in the CND of NGC 1068. Compared to SiO, the H13CO+ line is about a factor of three weaker. This ratio is significantly higher than that derived by U04, who reported a value about 1 from a 30 m spectrum of the CND. The disagreement between the PdBI and the 30 m results is an indication that compared to SiO the contamination from the SB ring in H13CO+ is more severe, and cannot be accurately estimated with the lower resolution 30 m map.
Given the weakness of H13CO+
in the CND, we omitted any discussion of the 2D morphology of the
emission of this line.
We nevertheless used H13CO+
to independently estimate the abundance of SiO in the CND with a LVG
code to fit the global SiO(2-1)/H13CO+(1-0)
intensity ratio measured in the nucleus of NGC 1068. The value
of X(SiO) can be derived assuming a plausible range
of physical conditions for the gas. This relies on two basic
assumptions (see also the discussion in Garcia-Burillo et al. 2000; and Usero
et al. 2006).
First, because SiO and H13CO+
have similar dipole moments and the observed transitions have
comparable upper state energies, it is plausible to assume similar
physical conditions for the two species. In our case we took the CND
values estimated by U04 from the multi-line 30 m survey of
NGC 1068: n(H2
cm-3
and
K. As a second
assumption we took a standard abundance for H13CO
and
derived X(SiO) from the SiO/H13CO+
column density ratio fitted by LVG. In our case this corresponds to a
typical abundance of the main isotope X(H12CO
+ ) =10-8, and to an
isotopic ratio [12C]/[13C
,
similar to the values found in the CND of our Galaxy (Wannier 1980).
The derived abundance of SiO in the CND is
.
This estimate is comfortingly close to the lower limit of the X(SiO)
value derived from the LVG modeling of the SiO/CO ratios
described above. This agreement confirms that the one-phase LVG
approach adopted in Sect. 6.1.1
provides a reasonable estimate of the SiO molecular abundances in
NGC 1068, in spite of the inherent limitations of this
simplified description of the molecular ISM in this model.
We thus conclude that the dichotomy between the CND and the SB
ring, regarding the measured
and
ratios, cannot be attributed to a comparatively higher volume density
of SiO gas in the CND, but mainly to a significant enhancement of the
SiO abundance in this region.
![]() |
Figure 10: a) ( Upper panel) SiO abundance as a function of gas density in the high velocity gas at the position of the AGN (solid line) and in the low velocity at the edge of the CND (dashed line). The abundances are derived from the mean SiO and CO brightness temperatures within the respective velocity windows as defined in text. The SiO abundance in the two regions can be the same only within the grey area. b) ( Lower panel) Same as a) but particularized for the density and abundance ranges for CN. |
Open with DEXTER |
6.2 Chemical differentiation in the CND
6.2.1 SiO abundances
Figure 9a
shows the SiO(2-1)/CO(1-0) velocity-integrated intensity ratio (
)
in the CND, derived with a spatial resolution corresponding to that of
SiO. The changes in
are more significant along the major axis, where the spatial resolution
is the highest.
changes by about a factor of three inside the CND: it goes from a peak
value of
in a region close to the AGN
to a minimum of
at the eastern boundary of the
CND (
);
reaches a secondary maximum (
)
at the western edge of the CND (
).
This range of values confirms and significantly expands the differences
in the SiO/CO ratios between the east (
0.07) and the west (
0.10) lobes
of the CND, identified by U04 as coming from the blue and the red
velocity components of the line profiles respectively. Figure 9b shows
the SiO/CO ratio displayed here as a function of velocity and
position across the major axis of the galaxy. The differences in the
SiO/CO ratios, which go from
0.05 to
0.5, expand out to about one
order of magnitude depending on the velocity channel and position along
the major axis. Line ratios follow a regular pattern, where the highest
ratios are associated with high velocities. In
particular, the SiO/CO ratio is
at
km s-1
towards the AGN and the western secondary maximum. By contrast, the
corresponding average ratios at low velocities (
km s-1)
are about a factor of 6-7 lower (
)
at the edges of the CND (
3
).
The dichotomy between the SiO/CO ratios measured at high
and low velocities can be interpreted in terms of
different physical conditions (i.e., different n(H2)),
or alternatively as a signature of chemical differentiation (i.e.,
different X(SiO)) in the CND. Figure 10a shows the
range of possible LVG solutions that fit the CND ratios. We explored
two extreme solutions: in the first case, a common X(SiO)
is assumed, whereas in the second case, we adopted a common n(H2).
While physical conditions and chemical abundances in the gas are to
some extent interconnected we could investigate which is the main
driving cause of the reported changes in the line ratios by exploring
the two extreme cases described above. We
restricted H2 densities to lie within a range of
values around the average density derived from the fit of the
ratio measured in the CND (n(H
cm-3).
With these restrictions, Fig. 10a shows that
we need
one
order of magnitude increase in n(H2)
to fit the progression of
values
observed from low velocities (at larger radii) to high
velocities (at smaller radii). Alternatively, the scenario of
a common n(H2) but different
X(SiO), suggests a much wider range of solutions for
the CND. In this case, X(SiO) would need to be
about a factor of 5-6 higher at high velocities.
Although a tenfold increase of n(H2)
cannot be formally excluded based on these data
,
we note that this solution implies that the change should occur on
scales of
200-300 pc
(
the CND
radius). This is at odds with the significantly smaller differences
(about a factor of 2-5) that exist between the average
densities of SiO gas detected in the SB ring and the CND, two regions
more than 1 kpc apart. Therefore we can interpret the spatial
variations of
in the CND as the likely signature of chemical differentiation. In this
scenario, the abundance of SiO is significantly enhanced at high
velocities (i.e., at small radii
;
see Sect. 5.2).
This interpretation is supported by the correlation found between
and the X-ray irradiation of the CND discussed in Sect. 7.2.
6.2.2 CN abundances
Figure 9c
shows the CN(2-1)/CO(1-0) velocity-integrated intensity ratio (
)
derived in the CND with a spatial resolution corresponding to that of
the CO map. The average
ratio in the CND is about 0.15. The changes in
shown in Fig. 9c
are significant along the major axis.
changes by about a factor of three inside the CND. Similarly to the
SiO/CO ratio, the maximum CN/CO value (
0.3
0.03)
corresponds to a region very close to the AGN.
decreases to
at the edge of the CND.
Figure 9d
shows the CN/CO ratio here displayed as a function of velocity
and position across the major axis of the galaxy. Similarly to the case
of SiO discussed above, an inspection of Fig. 9d shows
that the differences in the measured CN/CO ratios are boosted
to reach about one order of magnitude depending on the velocity channel
and position along the major axis. Line ratios follow a regular
pattern, with the highest ratios associated with high
velocities. Towards the AGN the highest CN/CO values
(
)
correspond to the high velocity component of the
emission. This is in clear contrast with the corresponding values
measured at low velocities (
).
Following the scheme of Sect. 6.2.1 we explored
two families of LVG solutions that fit the range of
CN/CO ratios of the CND assuming a common X(CN)
or a common n(H2). For
simplicity we restricted H2 densities to lie
within the same range values explored for SiO. Pérez-Beaupuits
et al. (2009),
based on a multi-transition CN analysis, have derived a more restricted
density range (n(H
cm-3),
which nevertheless lies within the range explored here.
In the first scenario we need about an order of magnitude increase in n(H2)
to fit the progression of ratios from low-velocities
to high-velocities (see Fig. 10b). The
corresponding range of solutions in the second scenario requires about
a factor of 5-6 increase in X(CN). For
reasons similar to those described in Sect. 6.2.1 we favor an
interpretation of the spatial variations of
in the CND in terms of chemical differentiation. The abundance of CN
would be significantly enhanced at high velocities
(i.e., at small radii
;
see Sect. 5.3).
This interpretation is also supported by the correlation found between
and the X-ray irradiation of the CND discussed in Sect. 7.2.
7 Molecular gas chemistry in the CND of NGC 1068
Below we consider the pros and cons of two different scenarios, shocks and XDR chemistry, regarding their ability to explain the molecular abundances measured in the CND of NGC 1068 for SiO and CN. Complementary information provided by other molecular tracers is a key for this discussion. Furthermore, we use the information extracted from the observed kinematics of the gas and the relation of the derived molecular abundances with the X ray irradiation in the CND.
7.1 Shock chemistry
To explore the prevalence of shock chemistry in the CND of NGC 1068 we used the IRAM 30 m telescope to observe a set of lines of two molecular tracers of shocks: CH3OH and HNCO. We discuss below the line ratios derived for CH3OH, HNCO, SiO and CN in NGC 1068, and compare these with the ratios derived in galactic and extragalactic templates of shock chemistry. We also analyze the potential drivers of shocks in the CND.
7.1.1 Tracers of shocks: CH3OH and HNCO
On theoretical grounds, high abundances of methanol can only be
produced in gas-phase via evaporation and/or disruption of icy mantles.
Fast shocks (
km s-1)
can destroy
the grain cores, liberating refractory elements like Si to the gas
phase (Caselli et al. 1997;
Schilke et al. 1997).
By contrast, slow shocks (
km s-1)
are able to process the icy grain mantles, but not the grain cores
(Millar et al. 1991;
Charnley et al. 1995).
The different location of
Si-bearing material (cores) and solid-phase CH3OH
(mantles) in dust grains implies that SiO and CH3OH
are good
tracers of fast and slow
shocks, respectively. It is expected that the disruption of dust grains
by slow shocks can inject grain mantle material
into the molecular ISM without destroying the molecules (Bergin
et al. 1998;
Martín-Pintado et al. 2001).
In particular, the abundance of methanol is seen to be enhanced in
shocks associated with molecular outflows by more than two orders of
magnitude over the values typically derived in cold molecular clouds
(e.g., Bachiller & Pérez-Gutiérrez 1997;
Pérez-Gutiérrez 1999).
In external galaxies Meier & Turner (2005) associate
over-luminous methanol lines to shocks in IC 342. The close
association between SiO and CH3OH emission in
IC 342 discussed by Usero et al. (2006) corroborates
this picture.
Although it is still debated which is the main production mechanism of HNCO, models involving dust grain chemistry seem to be the most successful at increasing the abundances of HNCO in the gas phase. There is also supporting observational evidence that HNCO is related to shocks. In particular, Zinchenko et al. (2000) finds a good correlation between HNCO and SiO lines in dense cores of our Galaxy. Martín et al. (2008) have presented evidence of enhanced HNCO in molecular clouds suspected to suffer shocks in the Galactic Center. On larger scales, Meier & Turner (2005) interpret the large abundance of HNCO measured in the nuclear spiral structure of IC 342 as due to molecular shocks. In a later study Martín et al. (2009) observed several lines of HNCO in a sample of nearby starbursts and AGNs, concluding that molecular shocks can enhance the abundance of HNCO in galaxies. More recently, Rodríguez-Fernández et al. (2010) have reported a significant enhancement of HNCO in the bipolar outflow L1157, related to the shock chemistry at work in this prototypical young stellar object.
![]() |
Figure 11:
Spectra obtained with the IRAM 30 m telescope in selected
molecular line tracers of shock chemistry. We show in a) (
Upper panel) the spectra of the 2-1 line of CH3OH.
Intensity scale is in |
Open with DEXTER |
Table 2: Line ratios measured in prototypical regions.
7.1.2 Tracers of shocks in NGC 1068
Figure 11
shows the spectra obtained in the 3-2 and 2-1 line of CH3OH
and in the 4-3 line of HNCO towards the CND of
NGC 1068 with the IRAM 30 m telescope. Emission is
detected in the three lines at significant levels (S/N
ratio 7-12).
Within the errors the three line profiles appear centered
around
.
Yet the 3-2 line of methanol is a factor of 2 narrower than
the other two lines. This difference cannot be attributed to the
1.5
smaller beam of the CH3OH(3-2) line (
17
),
as the maximum spread of velocities is already reached on the scales of
the CND. By contrast this result reflects the lower excitation of
methanol lines at high-velocities (likely arising
in the inner CND, as shown by the SiO and CN interferometer maps). This
supports the view that there is no significant increase of molecular
densities at small radii on the scales of the CND (Sects. 6.2.1 and 6.2.2).
Table 2
shows the average CH3OH(2-1)/SiO(2-1), CH3OH(3-2)/SiO(3-2),
HNCO(4-3)/SiO(2-1), SiO(2-1)/ CN(2-1) and CN(2-1)/HCN(1-0) line ratios
in the CND of NGC 1068 in
scale. We corrected the line ratios from beam dilution when necessary
(single-dish observations) with the usual prescription for a point-like
source, which is applicable in this context for the CND. Line ratios
obtained in NGC 1068 are compared with results obtained in the
molecular lobes (known as B1 and B2) of the bipolar outflow L1157 (data
taken from Pérez-Gutiérrez 1999;
and Nisini et al. 2007).
We also list the line ratios measured in the face-on barred galaxy
IC 342 when available (data taken from Hüttemeister
et al. 1997;
Meier & Turner 2005;
and Usero et al. 2006).
For L1157 we applied a correction for beam dilution assuming that the
sizes of molecular emission in B1 and B2 are 18
and
30
,
respectively.
As a result of this comparison we note the similarity between
the ratios derived from CH3OH, HNCO and
SiO lines in L1157 and NGC 1068.
At face value this indicates that most of the SiO emission in the CND
of NGC 1068 could be explained by fast
shocks similar to those identified in the young bipolar outflow L1157.
A comparison between the SiO/CN and CN/HCN ratios measured in L1157 and
NGC 1068 indicates a remarkable excess of CN emission in
NGC 1068, though. L1157 is the only outflow in which CN(2-1)
emission has been detected in the high velocity gas associated with the
bow shocks. But even for this extremely molecular-rich young outflow,
the SiO/CN intensity ratio is about a factor of 10 higher than in the
CND of NGC 1068. This CN excess questions the suitability of
the bipolar outflow template in NGC 1068. The age dating of
the most recent star-formation episode of the CND (>2-
yrs old, Davies
et al. 2010)
also questions the hypothesis that shocks in NGC 1068 can be
interpreted as stemming from an embedded population of young
stellar objects.
Alternatively, large-scale shocks produced by cloud-cloud
collisions, which are enhanced due to the complex orbital dynamics in
the ILR region of the CND, could be a viable mechanism to explain the
emission of SiO, CH3OH and HNCO in
NGC 1068. SiO maps show the existence of perturbed kinematics
of molecular gas in the CND (Sect. 5.2). The
prevalence of SiO emission at high and forbidden
velocities implies enhanced X(SiO) in gas
following non-circular orbits. Furthermore, the line ratios discussed
in Sect. 6.2.1
suggest an enhancement of SiO abundances at the extreme velocities
identified in the CND. A similar link between density waves and
large-scale molecular shocks has been proposed to explain the
enhancement of SiO in the circum-nuclear disks of our Galaxy
(Martín-Pintado et al. 1997;
Hüttemeister et al. 1998;
Rodríguez-Fernández et al. 2006)
and of the starburst galaxies IC 342 and NGC 253
(Usero et al. 2006;
García-Burillo et al. 2000).
Usero et al. (2006)
analyzed the large-scale molecular shocks produced in the ILR region of
IC 342. Shocks in this galaxy seem to arise during cloud-cloud
collisions at low velocities only after the kinetic energy associated
with the density wave driven streaming motions has partly dissipated
into turbulence. The comparison between IC 342 and
NGC 1068 indicates that CH3OH/SiO and
HNCO/SiO ratios are a
factor of two to three lower in NGC 1068. The detection of
over-luminous SiO lines in NGC 1068 could be the signature of
comparatively higher velocity shocks in this galaxy, possibly produced
by mechanisms unrelated to density waves. Other scenarios designed to
fit the CND kinematics, in particular those invoking a jet-ISM
interaction, which would give rise to a nuclear warp and, eventually,
to an expanding ring, could produce faster
molecular shocks in NGC 1068.
Gallimore et al. (1996)
analyzed the morphology and spectral index of the NGC 1068 jet
and concluded that the radio plasma may have been diverted at a shock
interface with the molecular ISM close to the AGN (knot C
at pc). Molecular
shocks in the CND could have propagated around the jet-ISM working
surface. The H2 line map published by Davies
et al. (2008;
see also Müller-Sánchez et al. 2009) reveals a
strongly perturbed velocity field at a region located just 0.5-1
(35-70 pc)
north of the AGN. The enhanced SiO abundances
derived at high velocities ``close'' to the AGN may well be the
signature of this jet-ISM interaction. Nevertheless, that SiO gas is
detected elsewhere in the CND suggests that shocks would be at work on
larger scales, either driven by an expanding ring or by the perturbed
kinematics at the ILR region. But whereas shock chemistry can explain
the strength and the line ratios of the different molecular shock
tracers detected in NGC 1068, it is not a valid explanation
for the measured CN abundances.
The discrepancies mentioned above motivate the search of a framework different to shock chemistry that would be able to simultaneously account for the high molecular abundances of SiO and CN measured in NGC 1068 (Sect. 7.2).
![]() |
Figure 12: a) ( Left panel) Chandra X-ray image of NGC 1068 (contours: 15, 30, 50, 100, 200, 400, 600, 1000, 2000 and 3000 counts) obtained in the 0.25-7.5 keV band by Young et al. (2001) is overlaid on the PdBI SiO map (color scale in units of Jy km s-1 beam-1). b) ( Middle panel) The X-ray image obtained in the 6-8 keV band by Ogle et al. (2003) (contours: 0.2, 0.5, 1, 2, 4, 8, 15, 25, 40, 80 and 100 counts) is overlaid on the SiO(2-1)/CO(1-0) brightness temperature ratio (color scale) at the SiO spatial resolution. c) ( Right panel) Same as b) but with the X-ray image obtained in the 6-8 keV band overlaid on the CN(2-1)/CO(1-0) ratio (color scale) at the CO spatial resolution. Ellipses show beams of SiO and CO as in Fig. 9. |
Open with DEXTER |
7.2 X-ray chemistry
We describe below the main properties of X-ray emission in NGC 1068, with a particular emphasis on the morphology, energetics and origin of hard X-ray emission in the CND (Sect. 7.2.1). We further discuss the observational evidence for X-ray chemistry in the nucleus of NGC 1068, and how the SiO and CN data specifically fit into this picture (Sect. 7.2.2).
7.2.1 X-ray emission in NGC 1068
We superpose in Fig. 12a the
subarcsec resolution X-ray image of NGC 1068 obtained in the
0.25-7.50 keV band with Chandra (contours) on the SiO map
(color scale). The X-ray image has been taken from the 3.2 s
frame time data published by Young et al. (2001). The
0.25-7.50 keV band image incorporates the contribution from
soft to hard X-rays and includes both continuum and line emission. The
morphology of the X-ray image reveals spatially resolved emission
distributed in a compact yet spatially resolved component located on
the AGN, and an elongated source that extends to the northeast,
similarly to the inner radio jet of the galaxy. The northeast
elongation of X-ray emission contrasts with the overall east-west
elongation seen in the CND molecular material detected in SiO and CN.
Lower level X-ray emission is detected outside the inner 12
field
of view (FOV) displayed in Fig. 12a. This
outer emission takes the shape of a complex spiral-like structure that
extends out to
(see Young et al. 2001
for a detailed description). The brightest region in X-ray emission
corresponds with the compact AGN source. The X-ray peak coincides with
the highest SiO/CO and CN/CO intensity ratios
measured in the CND (panels c and d). The contributions to the X-ray
luminosity in the 0.25-7.50 keV band are known to be multiple
(line and continuum emission, as well as emission from neutral and
ionized material), and therefore the link between the molecular line
ratios and the ``bolometric'' X-ray flux, if any, is not easily
interpretable. As argued below, by restricting the study to the hard
X-ray band the interpretation is facilitated.
Figure 12 (panels
b and c) shows the superposition of the hard X-ray image obtained in
the 6-8 keV band by Chandra (in contours) on the
SiO/CO and CN/CO ratio maps (color scale). The X-ray
map was obtained by applying an adaptive smoothing on the Chandra archive
NGC 1068 data available in this wave-band. This image is
virtually identical to the hard X-ray map originally published and
discussed by Ogle et al. (2003;
see also Young et al. 2001).
Emission in this band is dominated by the Fe I K
line, with a non-negligible contribution from Fe XXV and scattered
neutral and ionized continuum reflection (Ogle et al. 2003). An analysis of
the 4-10 keV continuum observed with ASCA in NGC 1068
led Iwasawa et al. (1997)
to conclude that most of the hard X-ray flux comes from reflection by
cold neutral gas. The strong emission detected in the
Fe I K
line in NGC 1068, a line generated by fluorescence in neutral
cold molecular clouds, corroborates this picture. Therefore the
6-8 keV band image allows us to directly probe to what extent
molecular gas in the CND of NGC 1068 is pervaded and processed
by X-rays, without a significant contamination from other sources to
the X-ray emission.
![]() |
Figure 13: a) ( Left panel) The SiO(2-1)/CO(1-0) brightness temperature ratio versus the X-ray flux in the 6-8 keV band. The straight line represents the best fit to the points taking into account uncertainties visualized by the errorbars. The coefficient of determination of the regression is r2=0.6. b) ( Right panel) Same as a) but showing the CN(2-1)/CO(1-0) ratio. The coefficient of determination of the regression is r2=0.7. |
Open with DEXTER |



7.2.2 X-ray chemistry in NGC 1068
The CND of NGC 1068 has the basic ingredients to become a
giant XDR. First, the nucleus of this Seyfert 2 is a strong X-ray
emitter. The intrinsic luminosity in the hard X-ray band has been
estimated to be about 10
43-1044 erg s-1
(e.g., Iwasawa et al. 1997;
Maloney 1997;
Colbert et al. 2002).
Furthermore, the central engine of NGC 1068 is surrounded by a
massive (
)
circum-nuclear molecular disk of
200 pc radius. Thus,
most of the molecular mass of the CND lies at a radius of about
100 pc where the expected hard X-ray flux is about
10-100 erg cm-2 s-1.
This puts the molecular CND of NGC 1068 among the category of
strongly irradiated XDRs (Meijerink et al. 2007). As argued in
Sect. 7.2.1,
the hard X-ray image of NGC 1068 provides direct evidence that
molecular gas in the CND is pervaded by X-rays. We therefore expect
that the chemistry of molecular gas in the CND should show the
footprints of X-ray processing predicted on theoretical grounds. As
discussed below, there are specific predictions regarding SiO
and CN.
Gas-phase models that analyze the chemistry of X-ray
irradiated molecular gas foresee high abundances for CN, similar to
those measured in the CND of NGC 1068: X(CN a
few 10
-8-10-7
(Lepp & Dalgarno 1996;
Meijerink & Spaans 2005;
Meijerink et al. 2007).
The abundance of CN is enhanced in XDR mainly as a result of the higher
ionization degree of the gas. For similar reasons, there is a
theoretical basis supporting the enhancement of CN in PDR environments
(e.g.; Boger & Sternberg 2005; Fuente
et al. 1993,2008; Janssen
et al. 1995).
However, based on the age estimated for the most recent star formation
episode taking place in the CND(>2-
yrs old, Davies
et al. 2010),
and considering that the UV radiation from young massive stars should
dominate the feedback in a starburst, we can safely discard PDR
chemistry as the origin for the high abundances of CN in the CND of
NGC 1068. As argued in Sect. 7.1.2, shocks can
also be rejected as an explanation for CN abundances.
The recent gas-phase models of Meijerink et al. (2007) foresee a
significant enhancement of SiO in strongly irradiated (10-100 erg cm-2 s-1)
high density (
105 cm-3)
XDRs, i.e., in a regime similar to the XDR environment of
NGC 1068 where we measure X(SiO
a
few 10
-9-10-8.
In particular, Meijerink et al. (2007) predict that
the SiO(1-0)/CO(1-0) ratio can reach a value of
0.10 assuming a standard
depletion for silicon in gas phase. This closely agrees with the
average SiO(2-1)/CO(1-0) ratio observed in NGC 1068 (
0.08),
assuming that the typical SiO(2-1)/SiO(1-0) ratios should be
1. The
latter is an educated guess considering the physical conditions of SiO
gas in the CND.
In addition to the predictions of gas-phase chemistry,
Voit (1991)
has proposed that the abundance of silicon monoxide could also be
boosted due to dust grain processing by X-rays. These can evaporate
small (10 Å)
silicate grains and increase the Si fraction in gas phase, leading to a
considerable enhancement of SiO in X-ray irradiated molecular gas
(Martín-Pintado et al. 2000;
U04; García-Burillo et al. 2008;
Amo-Baladrón et al. 2009).
This scenario has been invoked by Martín-Pintado et al. (2000) and
Amo-Baladrón et al. (2009)
to account for the correlation between the abundance of SiO and the
equivalent width of the Fe K
fluorescence line in the Sgr A and Sgr B molecular cloud complexes of
the Galactic Center. For the Galactic Center, pure gas-phase XDR models
have difficulties in reproducing the observed SiO abundances, unless an
X-ray outburst is assumed to have taken place in Sgr A*
300 yr ago. By contrast, current gas-phase XDR models successfully
reproduce the SiO abundances derived in NGC 1068 without
resorting to dust grain chemistry. Nonetheless, the inclusion of dust
grain chemistry, likely linked to the mechanical heating of the
molecular ISM, would help solve the controversy regarding the
abundances of species like HCN and HNC, under-predicted by XDR schemes
(García-Burillo et al. 2008;
Loenen et al. 2008;
Pérez-Beaupuits et al. 2009).
Actually, while CN is overly produced in gas-phase XDR models, HCN is
under-produced with respect to the level required by observations in
AGNs. In addition to mechanical heating, the evaporation of dust grain
mantles in dense hot environments like those likely prevailing in the
nuclear disks of AGN, has been invoked as a mechanism responsible of
enhancing HCN abundances (Lintott & Viti 2006).
Other lines of evidence support the existence of an XDR in the
CND. The low HCO+/HOC+
ratios measured by U04 can be explained only if molecular clouds have
the high ionization degrees typical of XDR: X(e
.
Furthermore, the excitation of the 2.12
m H2 rovibrational
emission lines detected in the CND (Rotaciuc et al. 1991; Blietz
et al. 1994;
Galliano & Alloin 2002;
Müller-Sánchez et al. 2009)
has been interpreted to be dominated by X-ray emission (e.g., see
discussion in Maloney 1997;
and Galliano & Alloin 2002)
8 Summary and conclusions
We used the high spatial resolution and sensitivity capabilities of the
PdBI to map the emission of the (v=0, J=2-1)
line of SiO and the N=2-1 transition of CN in the
disk of the Seyfert 2 galaxy NGC 1068. The spatial resolution
of these observations (1-3
)
allowed us to separate the emission of the SB ring from that of the
CND. The PdBI SiO and CN data together with available PdBI
CO maps of the galaxy were complemented by single-dish data
obtained with the IRAM 30 m telescope in SiO, CH3OH and
HNCO lines to probe the physical and chemical properties of
molecular gas in the CND through an analysis of line ratios.
We summarize below the main results obtained in this work:
-
Unlike the CO lines, which show strong emission in the SB ring, most of the SiO emission detected inside the PdBI primary beam comes from a circum-nuclear molecular disk (CND) located around the AGN. The dichotomy between the CND and the SB ring is reflected in the remarkably different
ratios measured in the two regions. Large velocity gradient models implemented to fit line ratios indicate that the average abundance of SiO in the CND,
SiO
CND
, is about one to two orders of magnitude higher than that measured in the SB ring.
-
Similarly to CO, the SiO CND, of about 400 pc deconvolved size, shows an asymmetric double peak structure oriented east-west. The eastern knot corresponds to the SiO emission peak. However, CO and SiO emissions show differences at the scales of the CND. The SiO/CO velocity-integrated intensity ratio changes by about a factor of three inside the CND, reaching a peak ratio of
0.10-0.12 towards the AGN and the western knot.
-
The overall SiO kinematics in the CND are consistent with a rotating structure. But there is evidence that the CND rotating pattern is distorted by non-circular and/or non-coplanar motions. Compared to CO, SiO emission at small radii (
pc) stands out at extreme velocities that are not accounted for by circular rotation. The highest SiO/CO brightness temperature ratios in the CND are associated with the high velocities seen towards the AGN and the western knot. We interpret the spatial variations of the SiO/CO ratio in the CND as the likely signature of chemical differentiation. In this scenario the abundance of SiO is significantly enhanced at high velocities out to X(SiO
.
-
CN emission is also detected in a CND around the AGN. The size and morphology of the CND seen in CN are similar to those found in SiO. The overall abundance of CN in the CND is high:
CN
CND
. The CN/CO velocity-integrated intensity ratio changes by about a factor of three inside the CND and reaches a peak value of
0.30 towards the AGN. CN maps also show distorted kinematics that cannot be explained by circular rotation. The abundance of CN is significantly enhanced at high velocities, detected towards the AGN, out to X(CN
. The emission detected in CN at extreme velocities is physically associated with gas lying at small radii (
pc).
-
Different models have been proposed to account for the kinematics of molecular gas in the CND. Large-scale shocks produced by cloud-cloud collisions in the ILR region of the NGC 1068 nuclear bar can explain the distorted kinematics and enhanced SiO abundances in the CND. The hypothesis of a jet-ISM interaction, driving the large-scale expansion of the molecular ring, can also explain shocks. Independent evidence of shocks is provided by the detection of CH3OH and HNCO. Line ratios involving these tracers and SiO in the CND are similar to those measured in prototypical shocked regions in our Galaxy. Yet the strength and abundance of CN in NGC 1068 can be explained neither by shocks nor by PDR chemistry. Alternatively, the high global abundances measured for CN and SiO, which agree with the theoretical predictions of XDR models, and the conspicuous correlation of CN/CO and SiO/CO ratios with the irradiation of hard X-rays, suggest that the CND of NGC 1068 has become a giant X-ray-dominated region.
We acknowledge the IRAM staff from the Plateau de Bure and from Grenoble for carrying out the observations and help provided during the data reduction. We heartily thank Andrew Baker for making available his PhD thesis work and for the helpful discussions and comments on our paper. S.G.B. and A.F. acknowledge support from MICIN within program CONSOLIDER INGENIO 2010, under grant ``Molecular Astrophysics: The Herschel and ALMA Era - ASTROMOL'' (Ref. CSD2009-00038).
References
- Amo-Baladrón, M. A., Martín-Pintado, J., Morris, M. R., Muno, M. P., & Rodríguez-Fernández, N. J. 2009, ApJ, 694, 943 [NASA ADS] [CrossRef] [Google Scholar]
- Athanassoula, E. 1992, MNRAS, 259, 345 [NASA ADS] [CrossRef] [Google Scholar]
- Bachiller, R., & Pérez-Gutiérrez, M. 1997, ApJ, 487, L93 [NASA ADS] [CrossRef] [Google Scholar]
- Baker, A. J. 2000, Ph.D. Thesis [Google Scholar]
- Bergin, E. A., Neufeld, D. A., & Melnick, G. J. 1998, ApJ, 499, 777 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
- Bland-Hawthorn, J., Gallimore, J. F., Tacconi, L. J., et al. 1997, Ap&SS, 248, 9 [NASA ADS] [CrossRef] [Google Scholar]
- Blietz, M., Cameron, M., Drapatz, S., et al. 1994, ApJ, 421, 92 [NASA ADS] [CrossRef] [Google Scholar]
- Boger, G. I., & Sternberg, A. 2005, ApJ, 632, 302 [NASA ADS] [CrossRef] [Google Scholar]
- Brinks, E., Skillman, E. D., Terlevich, R. J., & Terlevich, E. 1997, Ap&SS, 248, 23 [NASA ADS] [CrossRef] [Google Scholar]
- Buta, R., & Combes, F. 1996, Fund. Cosmic Phys., 17, 95 [Google Scholar]
- Caselli, P., Hartquist, T. W., & Havnes, O. 1997, A&A, 322, 296 [NASA ADS] [Google Scholar]
- Charnley, S. B., Kress, M. E., Tielens, A. G. G. M., & Millar, T. J. 1995, ApJ, 448, 232 [NASA ADS] [CrossRef] [Google Scholar]
- Colbert, E. J. M., Weaver, K. A., Krolik, J. H., Mulchaey, J. S., & Mushotzky, R. F. 2002, ApJ, 581, 182 [NASA ADS] [CrossRef] [Google Scholar]
- Davies, R., Genzel, R., Tacconi, L., Sánchez, F. M., & Sternberg, A. 2008, Mapping the Galaxy and Nearby Galaxies, 144 [CrossRef] [Google Scholar]
- Davies, R. I., Hicks, E., Schartmann, M., et al. 2010, IAU Symp., 267, 283 [NASA ADS] [Google Scholar]
- Dehnen, W., Bland-Hawthorn, J., Quirrenbach, A., & Cecil, G. N. 1997, Ap&SS, 248, 33 [NASA ADS] [CrossRef] [Google Scholar]
- de Vaucouleurs, G., de Vaucouleurs, A., Corwin, H. G., Jr., et al. 1991, Third Reference Catalogue of Bright Galaxies [Google Scholar]
- Emsellem, E., Fathi, K., Wozniak, H., et al. 2006, MNRAS, 365, 367 [NASA ADS] [CrossRef] [Google Scholar]
- Fuente, A., Martin-Pintado, J., Cernicharo, J., & Bachiller, R. 1993, A&A, 276, 473 [NASA ADS] [Google Scholar]
- Fuente, A., Rizzo, J. R., Caselli, P., Bachiller, R., & Henkel, C. 2005, A&A, 433, 535 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Fuente, A., García-Burillo, S., Usero, A., et al. 2008, A&A, 492, 675 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Galliano, E., & Alloin, D. 2002, A&A, 393, 43 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Gallimore, J. F., Baum, S. A., O'Dea, C. P., & Pedlar, A. 1996, ApJ, 458, 136 [NASA ADS] [CrossRef] [Google Scholar]
- García-Burillo, S., & Guélin, M. 1995, A&A, 299, 657 [NASA ADS] [Google Scholar]
- García-Burillo, S., & Martín-Pintado, J. 2001, The Promise of the Herschel Space Observatory, 460, 163 [NASA ADS] [Google Scholar]
- García-Burillo, S., Guélin, M., & Cernicharo, J. 1993, A&A, 274, 123 [NASA ADS] [Google Scholar]
- García-Burillo, S., Martín-Pintado, J., Fuente, A., & Neri, R. 2000, A&A, 355, 499 [NASA ADS] [Google Scholar]
- García-Burillo, S., Martín-Pintado, J., Fuente, A., & Neri, R. 2001, ApJ, 563, L27 [NASA ADS] [CrossRef] [Google Scholar]
- García-Burillo, S., Graciá-Carpio, J., Guélin, M., et al. 2006, ApJ, 645, L17 [NASA ADS] [CrossRef] [Google Scholar]
- García-Burillo, S., Combes, F., Usero, A., & Graciá-Carpio, J. 2008, J. Phys. Conf. Ser., 131, 012031 [NASA ADS] [CrossRef] [Google Scholar]
- Gerssen, J., Allington-Smith, J., Miller, B. W., Turner, J. E. H., & Walker, A. 2006, MNRAS, 365, 29 [NASA ADS] [CrossRef] [Google Scholar]
- Graciá-Carpio, J., García-Burillo, S., Planesas, P., & Colina, L. 2006, ApJ, 640, L135 [NASA ADS] [CrossRef] [Google Scholar]
- Graciá-Carpio, J., García-Burillo, S., Planesas, P., Fuente, A., & Usero, A. 2008, A&A, 479, 703 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Guilloteau, S., & Lucas, R. 2000, in Imaging at Radio through Submillimeter Wavelengths, ed. J. G. Mangum, & S. J. E. Radford, ASP Conf. Ser., 299 [Google Scholar]
- Guilloteau, S., Delannoy, J., Downes, D., et al. 1992, A&A, 262, 624 [NASA ADS] [Google Scholar]
- Helfer, T. T., & Blitz, L. 1995, ApJ, 450, 90 [NASA ADS] [CrossRef] [Google Scholar]
- Huchra, J. P., Vogeley, M. S., & Geller, M. J. 1999, ApJS, 121, 287 [NASA ADS] [CrossRef] [Google Scholar]
- Hüttemeister, S., Mauersberger, R., & Henkel, C. 1997, A&A, 326, 59 [NASA ADS] [Google Scholar]
- Hüttemeister, S., Dahmen, G., Mauersberger, R., et al. 1998, A&A, 334, 646 [NASA ADS] [Google Scholar]
- Iwasawa, K., Fabian, A. C., & Matt, G. 1997, MNRAS, 289, 443 [NASA ADS] [CrossRef] [Google Scholar]
- Jansen, D. J., van Dishoeck, E. F., Black, J. H., Spaans, M., & Sosin, C. 1995, A&A, 302, 223 [NASA ADS] [Google Scholar]
- Kohno, K., Matsushita, S., Vila-Vilaró, B., et al. 2001, The Central Kiloparsec of Starbursts and AGN: The La Palma Connection, 249, 672 [NASA ADS] [Google Scholar]
- Krips, M., Eckart, A., Neri, R., et al. 2006, A&A, 446, 113 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Krips, M., Neri, R., García-Burillo, S., et al. 2008, ApJ, 677, 262 [NASA ADS] [CrossRef] [Google Scholar]
- Kuijken, K., & Merrifield, M. R. 1995, ApJ, 443, L13 [NASA ADS] [CrossRef] [Google Scholar]
- Lepp, S., & Dalgarno, A. 1996, A&A, 306, L21 [NASA ADS] [Google Scholar]
- Lintott, C., & Viti, S. 2006, ApJ, 646, L37 [NASA ADS] [CrossRef] [Google Scholar]
- Loenen, A. F., Spaans, M., Baan, W. A., & Meijerink, R. 2008, A&A, 488, L5 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Maloney, P. R. 1997, Ap&SS, 248, 105 [Google Scholar]
- Maloney, P. R., Hollenbach, D. J., & Tielens, A. G. G. M. 1996, ApJ, 466, 561 [NASA ADS] [CrossRef] [Google Scholar]
- Martín, S., Requena-Torres, M. A., Martín-Pintado, J., & Mauersberger, R. 2008, ApJ, 678, 245 [NASA ADS] [CrossRef] [Google Scholar]
- Martín, S., Martín-Pintado, J., & Mauersberger, R. 2009, ApJ, 694, 610 [NASA ADS] [CrossRef] [Google Scholar]
- Martín-Pintado, J., de Vicente, P., Fuente, A., & Planesas, P. 1997, ApJ, 482, L45 [NASA ADS] [CrossRef] [Google Scholar]
- Martín-Pintado, J., de Vicente, P., Rodríguez-Fernández, N. J., et al. 2000, A&A, 356, L5 [NASA ADS] [Google Scholar]
- Martín-Pintado, J., Rizzo, J. R., de Vicente, P., Rodríguez-Fernández, N. J., & Fuente, A. 2001, ApJ, 548, L65 [NASA ADS] [CrossRef] [Google Scholar]
- Meier, D. S., & Turner, J. L. 2005, ApJ, 618, 259 [NASA ADS] [CrossRef] [Google Scholar]
- Meijerink, R., & Spaans, M. 2005, A&A, 436, 397 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Meijerink, R., Spaans, M., & Israel, F. P. 2007, A&A, 461, 793 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Millar, T. J., Herbst, E., & Charnley, S. B. 1991, ApJ, 369, 147 [NASA ADS] [CrossRef] [Google Scholar]
- Mitchell, G. F. 1984, ApJS, 54, 81 [NASA ADS] [CrossRef] [Google Scholar]
- Müller-Sánchez, F., Davies, R. I., Genzel, R., et al. 2009, ApJ, 691, 749 [NASA ADS] [CrossRef] [Google Scholar]
- Nisini, B., Codella, C., Giannini, T., et al. 2007, A&A, 462, 163 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Ogle, P. M., Brookings, T., Canizares, C. R., Lee, J. C., & Marshall, H. L. 2003, A&A, 402, 849 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Pérez-Beaupuits, J. P., Aalto, S., & Gerebro, H. 2007, A&A, 476, 177 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Pérez-Beaupuits, J. P., Spaans, M., van der Tak, F. F. S., et al. 2009, A&A, 503, 459 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Pérez-Gutiérrez, M. J. P. 1999, Ph.D. Thesis, Universidad Complutense de Madrid (UCM) [Google Scholar]
- Planesas, P., Scoville, N., & Myers, S. T. 1991, ApJ, 369, 364 [NASA ADS] [CrossRef] [Google Scholar]
- Rodríguez-Fernández, N. J., Combes, F., Martín-Pintado, J., Wilson, T. L., & Apponi, A. 2006, A&A, 455, 963 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Rodríguez-Fernández, N., Tafalla, M., Gueth, F., & Bachiller, R. 2010, A&A, 516, A98 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Rotaciuc, V., Krabbe, A., Cameron, M., et al. 1991, ApJ, 370, L23 [NASA ADS] [CrossRef] [Google Scholar]
- Schilke, P., Walmsley, C. M., Pineau des Forets, G., & Flower, D. R. 1997, A&A, 321, 293 [NASA ADS] [Google Scholar]
- Schinnerer, E., Eckart, A., Tacconi, L. J., Genzel, R., & Downes, D. 2000, ApJ, 533, 850 [NASA ADS] [CrossRef] [Google Scholar]
- Sternberg, A., & Dalgarno, A. 1995, ApJS, 99, 565 [NASA ADS] [CrossRef] [Google Scholar]
- Sternberg, A., Genzel, R., & Tacconi, L. 1994, ApJ, 436, L131 [NASA ADS] [CrossRef] [Google Scholar]
- Strong, A. W., Bloemen, J. B. G. M., Dame, T. M., et al. 1988, A&A, 207, 1 [NASA ADS] [Google Scholar]
- Tacconi, L. J., Genzel, R., Blietz, M., et al. 1994, ApJ, 426, L77 [NASA ADS] [CrossRef] [Google Scholar]
- Usero, A., García-Burillo, S., Fuente, A., Martín-Pintado, J., & Rodríguez-Fernández, N. J. 2004, A&A, 419, 897 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Usero, A., García-Burillo, S., Martín-Pintado, J., Fuente, A., & Neri, R. 2006, A&A, 448, 457 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Voit, G. M. 1991, ApJ, 379, 122 [NASA ADS] [CrossRef] [Google Scholar]
- Wannier, P. G. 1980, ARA&A, 18, 399 [NASA ADS] [CrossRef] [Google Scholar]
- Young, A. J., Wilson, A. S., & Shopbell, P. L. 2001, ApJ, 556, 6 [NASA ADS] [CrossRef] [Google Scholar]
- Zinchenko, I., Henkel, C., & Mao, R. Q. 2000, A&A, 361, 1079 [NASA ADS] [Google Scholar]
- Ziurys, L. M., Friberg, P., & Irvine, W. M. 1989, ApJ, 343, 201 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
Footnotes
- ... XDR?
- Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
- ... non-coplanar
- In this context a combination of elongated and non-coplanar orbits cannot be excluded.
- ... values
- As for
, we adopt for
the average values measured in the SB and the CND.
- ... data
- A high-resolution
map would be required to quantitatively probe SiO density changes inside the CND.
- ... smoothing
- Using version 4.1 of CIAO package.
All Tables
Table 1: Observational parameters of the SiO and CN PdBI data.
Table 2: Line ratios measured in prototypical regions.
All Figures
![]() |
Figure 1:
Continuum maps obtained with the PdBI towards the nucleus of
NGC 1068 at 3 mm (grey scale contours: 3%, 5%, 10%,
15%, 25% to 85% in steps of 15% of the maximum =
39.8 mJy beam-1) and
1 mm (white contours: 20% to 95% in steps of 15% of the
maximum = 14.2 mJy beam-1).
The lowest contours correspond to |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
a) (Upper panel) SiO
integrated intensity map (contour levels are 3 |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
CN integrated intensity map. Contour levels are 3 |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
a) (Upper panel)
SiO isovelocities contoured over false-color velocity maps. Velocities
span the range [1050 km s-1,
1225 km s-1] in steps of
25 km s-1. The velocity scale
is HEL. The AGN position is marked with a star. The position of the
kinematic major axis derived from SiO at
|
Open with DEXTER | |
In the text |
![]() |
Figure 5:
a) (Upper panel)
Position-velocity diagram of CO(1-0) (contours; data from S00 degraded
to the resolution of SiO) and SiO(2-1) (color scale; this work) along
|
Open with DEXTER | |
In the text |
![]() |
Figure 6:
Same as Fig. 4
showing in a) (Upper panel)
CN isovelocities, derived from the high frequency (HF) 2-1 transition
of CN, contoured over false-color velocity maps. Velocities span the
range [1025 km s-1,
1200 km s-1] in steps of
25 km s-1. Similarly, we show
in b) (Lower panel)
the p-v diagram of CN along the
major axis at |
Open with DEXTER | |
In the text |
![]() |
Figure 7:
LVG results for SiO, assuming a kinetic temperature of
|
Open with DEXTER | |
In the text |
![]() |
Figure 8:
SiO abundances estimated from the LVG model as a function of the SiO
column density per velocity width (
|
Open with DEXTER | |
In the text |
![]() |
Figure 9:
a) ( Upper left panel) SiO(2-1)/CO(1-0)
velocity-integrated intensity ratio (
|
Open with DEXTER | |
In the text |
![]() |
Figure 10: a) ( Upper panel) SiO abundance as a function of gas density in the high velocity gas at the position of the AGN (solid line) and in the low velocity at the edge of the CND (dashed line). The abundances are derived from the mean SiO and CO brightness temperatures within the respective velocity windows as defined in text. The SiO abundance in the two regions can be the same only within the grey area. b) ( Lower panel) Same as a) but particularized for the density and abundance ranges for CN. |
Open with DEXTER | |
In the text |
![]() |
Figure 11:
Spectra obtained with the IRAM 30 m telescope in selected
molecular line tracers of shock chemistry. We show in a) (
Upper panel) the spectra of the 2-1 line of CH3OH.
Intensity scale is in |
Open with DEXTER | |
In the text |
![]() |
Figure 12: a) ( Left panel) Chandra X-ray image of NGC 1068 (contours: 15, 30, 50, 100, 200, 400, 600, 1000, 2000 and 3000 counts) obtained in the 0.25-7.5 keV band by Young et al. (2001) is overlaid on the PdBI SiO map (color scale in units of Jy km s-1 beam-1). b) ( Middle panel) The X-ray image obtained in the 6-8 keV band by Ogle et al. (2003) (contours: 0.2, 0.5, 1, 2, 4, 8, 15, 25, 40, 80 and 100 counts) is overlaid on the SiO(2-1)/CO(1-0) brightness temperature ratio (color scale) at the SiO spatial resolution. c) ( Right panel) Same as b) but with the X-ray image obtained in the 6-8 keV band overlaid on the CN(2-1)/CO(1-0) ratio (color scale) at the CO spatial resolution. Ellipses show beams of SiO and CO as in Fig. 9. |
Open with DEXTER | |
In the text |
![]() |
Figure 13: a) ( Left panel) The SiO(2-1)/CO(1-0) brightness temperature ratio versus the X-ray flux in the 6-8 keV band. The straight line represents the best fit to the points taking into account uncertainties visualized by the errorbars. The coefficient of determination of the regression is r2=0.6. b) ( Right panel) Same as a) but showing the CN(2-1)/CO(1-0) ratio. The coefficient of determination of the regression is r2=0.7. |
Open with DEXTER | |
In the text |
Copyright ESO 2010
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.