Our primary objectives in this investigation are to ascertain whether dust chimneys are commonplace within quiescent galaxies and how, if at all, they might relate to recent star-formation within the disk. We begin by addressing the first of these issues.
Unfortunately, there are only 5 galaxies, out of the original sample, which are orientated
sufficiently close to edge-on (
)
to carry out an unambiguous search for
extraplanar structures. This subset is too small to result in any unequivocal statements
about the overall occurence of dust chimneys. Of the 5 galaxies depicted in
Figs. 1 to 6, 3 harbour very chaotic dust lanes (NGC 891, NGC 4013, NGC
4302) with numerous curvi-linear structures extending up to 2 kpc from the midplane. Many of
the extinction features extend to a kpc or so above the midplane before arching back towards
the disk. Others show no sign of reconnecting with the main dust layer and appear to
fragment at maximum z-height. More spherically-shaped dust clouds are also recognizable,
usually at
kpc, and appear completely isolated from the disk. The maximum
z-height at which extraplanar dust is discernible is about the same in all 3 galaxies
(z=1.7 kpc). (However, we might expect that diminishing bulge light would preclude a
detection of extinction features at much greater z-heights). Of the 2 remaining galaxies
in Figs. 1 to 6, UGC 4278 appears to contain only small amounts of
extraplanar dust and NGC 4762 none at all.
In the HS99 study, 5 galaxies are labelled as manifesting chimneys (out of a total of 7).
Three of these objects appear in our final sample (NGC 891, NGC 4302, NGC 4013) but the other
two (NGC 4217 and NGC 5907) we have already rejected as not being sufficiently edge-on to
make any unambiguous statements about extraplanar dust. It is interesting to note that NGC 4217 (and possibly NGC 5746 from our original sample) both exhibit some filament-like
features which extend to larger (apparent) z-heights than can probably be accounted for by
projection of disk structure onto the plane of the sky. However, in the strictest sense
(using the
criterion), the HS99 study and the present work indicate
collectively that 5 out of 10 spirals possess dust chimneys. Whilst the current statistics
are small, we concur with HS99 that the "chaotic" dust lane in NGC 891 can no longer be
considered anomalous and, indeed, high-lattitude dust appears to occur in half of all
quiescent spiral galaxies.
The detection of structures both below and above the midplane, argues against warps
being the cause of the chimney phenomenon. However, it is less easy to dismiss the
possibility of flaring in the outer regions of the disk being a contributory factor.
Optical images of spirals more inclined to the line-of-sight, such as NGC 253
(
), do exhibit numerous protuberances from the main dust lane and,
moreover, at various distances from the nucleus (Sofue et al. 1994). In Fig. 7, we
highlight similar features evident in two other slightly-inclined spirals that have recently
come to our attention (NGC 2976 and NGC 4928). Although line-of-sight ambiguities would
inhibit us from labelling these particular features as definitely extraplanar, their
similarity to the vertical structures depicted in Figs. 1 to 6 is
striking. The fact that such structures are not concentrated at the edge of the disk,
appears to confirm that flaring cannot be the mechanism producing dust chimneys. HS97 have
also presented cogent arguments, based on velocity information for the gas in NGC 891 and
its relationship to the dust chimneys, as to why gas-flaring cannot be the reason why
chimneys are observed in this galaxy.
In Table 4, we present the mean optical depths of extraplanar dust features found
in our final galaxy sample. We also include total masses for dust and gas residing outside
the main disk. The gas mass is calculated assuming a gas-to-dust ratio of 150
i.e. appropriate to gas with a solar-type metal abundance (Whittet 1992). The typical
optical depth for the extinction features identified in Figs. 1 to 6 is
estimated as
.
Our poor resolution of the features, combined with the
neglect of scattering effects, means that we could have underestimated the true column
density of dust by at least a factor of 5. Thus an optical depth closer to unity is probably
more likely. The extraplanar gas associated with the chimneys is
1% of the total
HI+H2 mass, assuming a canonical mixture of gas and dust in these structures. We note,
however, that if grains are expelled from the disk by radiation pressure rather than
convective flow (Sect. 6.4), dust and gas might be effectively decoupled from one
another. Under such circumstances the amount of gas in the extraplanar layer may be
considerably different to our estimate.
Galaxy |
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![]() ![]() |
(105 ![]() |
(107 ![]() |
(109 ![]() |
(![]() |
||
NGC 891 | 0.16 | 2.1 | 3.1 | 9.8 | 0.3 |
NGC 4013 | 0.11 | 0.93 | 1.4 | 4.8 | 0.3 |
NGC 4302 | 0.19 | 2.6 | 3.9 | 4.0 | 1.0 |
UGC 4278 | 0.071 | 0.047 | 0.071 | 2.8 | 0.025 |
NGC 4762 | 0.00 | 0.0 | 0.0 | 0.17 | 0.0 |
HS99 do not appear to list total masses for the extraplanar structures identified in their
larger edge-on galaxy survey (although they give masses for individual, selected features).
For NGC 891 (HS97), an estimate of
2% of the neutral ISM is cited, which is
significantly higher than the value of 0.3% we give in Table 4. The HS97 estimate
relies on 12 well-studied features epitomizing all 120 structure identified in their
investigation. Thus some of the discrepancy may arise from an extrapolation of 12 to 120
objects. However, it is also likely that the current work is less sensitive than the HS97
study - our larger PSF means that we ultimately overlook both smaller and less
optically-thick high-z clouds. We view the extraplanar masses listed in Table 4
very much as lower limits. In 5.1 we analyse the thermal emission from NGC 891 in
the submm regime in order to obtain an upper limit on the amount of dust and gas
situated outside the disk.
We derived the potential energy of the extraplanar structures, identified in the previous
section, using a numerical simulation based on an exponential disk of stars and a spherical
dark matter halo. In the first instance we concentrate on NGC 891 for which the vertical
features are best resolved. Using the dust free photometry from the Xilouris radiation
transfer model, we infer a central luminosity density (
kpc-3), a radial scale-length (3.9 kpc) and an exponential scale-height
(0.35 kpc) for the stars. The stellar luminosity density is converted to a mass density
assuming a mass-to-light ratio of unity. Although the rotation curve of NGC 891 has been
investigated quite closely (Bahcall 1983), the dark matter halo can be described by a variety
of models and is not well constrained in this case. Thus we refer to a fit by van Albada
et al. (1985) to the rotation curve of NGC 3198 - a galaxy similar in type, size and total
magnitude to NGC 891. Following their inference of how dark matter scales with luminous
matter, the dark matter radial mass density was prescribed as follows:
where r is the galactic-centric radius, in kpc, and
constitutes the
mass density in
kpc-3.
A catalogue was created of the 60 or so extraplanar dust features in NGC 891, containing the
relevant optical depth, mass, height above the plane and radial distance. We allow, as we
did previously, for the likelihood that features seen towards the nucleus are situated on
the nearside of the disk. Thus, we set
for features viewed towards the
centre, r=R25 for structures identified at the maximum distance along the major axis
and interpolated values of r for the features between these extremes. The catalogue
records are fed into the numerical simulation which calculates, stepwise, the amount of
energy that is required to lift any particular feature above the relevant part of the plane.
In Table 5, we show entries from the catalogue, including the derived potential
energies, for the 4 extraplanar features highlighted in Fig. 1.
Feature |
Mean z-height | Radius | Mass | P.E. |
(kpc) | (kpc) |
![]() |
(1051ergs) | |
A | 0.85 | 9.6 | 8.2 | 87 |
B | 0.73 | 9.9 | 4.8 | 39 |
C | 1.5 | 10.5 | 1.6 | 31 |
D | 0.92 | 9.9 | 1.1 | 13 |
![]() |
Figure 8: Unsharp-mask images of the galaxies shown in Fig. 7 |
We derive a total potential energy of
ergs for all the extraplanar
structures in NGC 891 with a mean value of
ergs per structure. The
energies are similar to the values found by HS97 but this is coincidental because these
authors use a plane-parallel model with a much lower mass density in the midplane (0.185
109
kpc-3) but a considerably larger stellar scale-height (0.7
kpc). Given that one of our key objectives will be to relate star-formation in the disk with
the occurence of dust chimneys, we compare briefly now the derived potential energy with the
anticipated injection of energy from both supernovae and the HII radiation field. As we show
in Sect. 6.4, the timescale for the formation of dust chimneys is at least
yr. Thus, for a supernova rate of 0.01 yr-1 and an injected energy of
1051 ergs per supernova (Leitherer et al. 1992), only 8% at most of the supernova
energy needs to do work in lifting the chimneys out of the plane. We estimate the power in
the HII radiation field from the FIR luminosity,
,
which we assume to be
reprocessed optical and ultraviolet energy. Devereux & Young (1993) have shown that
correlates spatially with H
emission and sites of massive star
formation in nearby disks (although perhaps 50% may arise from the diffuse interstellar
medium in some spiral types; Walterbos & Greenawalt 1996). Thus, using
to gauge the radiation energy impinging on grains situated in HII
regions, we estimate that only 0.1% of this energy must be transferred into lifting dust
out of the plane. We have assumed here that the photolevitated grains can successfully
transfer their upward momentum to the gas during collisions - a situation which is reached
relatively quickly in numerical simulations of radiation pressure (Davies et al. 1998). We
can conclude, therefore, that both supernovae and radiation pressure provide viable means
for the creation of dust chimneys above spiral disks. As pointed out by the referee,
however, supernova explosions provide a more natural explanation for dust chimneys because
their energy is focussed directly into the base of the chimney structure.
Within several nearby, starburst galaxies, such as M 82, an association has been observed
between kpc-scale dust outflows and concentrations of recent star-formation in the central
disk. Hot gas, pushed out along the minor axis by massive stars and supernova explosions,
generates a diffuse nebula of H
shells and streamers as it collides with ambient
gas in the halo. At the same time, dust and neutral gas from the disk are entrained at the
working surface of the expansion so that a network of optically-thick filaments becomes
established around the H
superbubble (Ichikawa et al. 1994; Phillips 1993). In
this section, we search for an analogous effect in quiescent disks. We examine the
distribution of H
emission from our sample and attempt to relate it to the
occurence of dust chimneys. R96 has already presented a detailed description of the
H
emission from our edge-on galaxies. In addition to bright emission from HII
regions, a layer of diffuse ionized gas (DIG) is found in several of the objects. When
present, the DIG often extends to several kpc above the disk and possesses an emission
measure, perpendicular to the disk, which is comparable to the Reynolds layer in the Galaxy
(Reynolds 1992; Kulkarni & Heiles 1988). Brightest DIG emission tends to occur above
regions undergoing enhanced star-formation but, as we discuss later, the mechanism by which
the emission-line nebula becomes established above quiescent disks may differ in some ways
from the starburst superwind phenomenon.
To compare the distribution of extraplanar dust with H
emission from both the disk
and the DIG layer, we employ two methods. Firstly, we superimpose the unsharp-mask images in
Figs. 1 to 6 onto the relevant H
image so that a simple visual
inspection can be made. Secondly, we produce a profile by integrating, in z-height, both
the extraplanar dust mass and the H
emission at each position along the major
axis. An overlay of the unsharp-mask image over the emission-line frame reveals no obvious
correspondance between either (i) the distribution of extraplanar dust and HII regions in
the disk, or (ii) the presence of extraplanar dust and an increased DIG brightness.
Figures 9 and 10 illustrate the case for NGC 891 and NGC 4302. We find that
H
emission from the extraplanar layer exhibits a far more diffuse distribution
than that of the dust chimneys. Overall, the extraplanar ionized gas is far less likely to
form discrete structures which might be matched to individual extinction features.
Certainly, no parallel can be found with starburst galaxies where dust appears to collect at
the working surface of hot gas expelled from the disk.
Our more quantitative approach, of profiling along the major axis, employs a rectangular
mask to separate H
radiation from the disk with that emitted by the DIG layer. The
width of the mask is fixed at
where:
Here, i,
and
are the inclination, stellar scale-length and
stellar scale-height, respectively. These are taken from the radiation transfer parameters
given in Table 3 (cf. Eq. (1) used to define the extraplanar layer for the
dust). The H
flux is integrated, in z-height, up to the box boundary for
emission from the disk and beyond the box boundary for radiation from the DIG. In
Fig. 11, we plot the amount of extraplanar dust at each point along the major axis
against the corresponding H
emission from HII regions in the disk. In
Fig. 12, the extraplanar dust is compared with the corresponding DIG emission. A
sampling interval, along the major axis, of 1 kpc has been used for all the galaxies
depicted. Of the 4 galaxies plotted (NGC 4762 shows no evidence of either extraplanar dust
or ionized gas and is therefore not included) only NGC 4013 appears to show any correlation
between the distribution of extraplanar dust and the brightness of H
emission. We
checked for stronger correlations over smaller and larger scale-sizes but found that the
behaviour of the plotted data remained more or less unaltered for different sampling
intervals.
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