| THE CENSUS
OF PLANETARY NEBULAE IN THE LOCAL GROUP
Planetary Nebulae (PNe), the fate of the vast
majority of stars with a mass similar to the Sun or a few times higher, represent
a short but well characterised stage of stellar evolution. It is the time
at which stars experiment their last thermonuclear burning on the surface
of a core that has been left naked by strong mass loss during the previous
red giant phase. The combination of a hot luminous star (up to 500,000 K
and to more than 10,000 solar luminosities) and a low density expanding wind,
allows the formation of extremely luminous nebulae that reprocess the energetic
continuum radiation from the stellar nucleus into specific emission-line
spectra from atomic ionised gas. This makes PNe easily observable in our
own Galaxy, but equally well detectable in external galaxies even with relatively
The technique used for searching PNe in external galaxies is almost invariably
that of obtaining a narrow-band, continuum-subtracted image in a filter
isolating the forbidden emission at 5007Å from double-ionised atomic
oxygen [OIII]. A large fraction of the total luminosity of the star is in
fact concentrated in this line, and this is the unique property that makes
individual stars in the planetary nebula phase visible to very large distances:
up to several hundred solar luminosities can be emitted in a single and
very narrow spectral line. Observation of the hydrogen Hα line, also very
bright, is sometimes added to discriminate against the detection of highly
redshifted galaxies (e.g. [OII] emitting galaxies at redshift z=0.34, which
shifts the O+ emission to the rest wavelength of [OIII]5007, or Lyman-a
emitters at redshift 3.1), or to estimate the ionisation class and discuss
possible contamination by compact HII regions. Another basic criterium to
select candidate extragalactic PNe is that they are not spatially resolved
by ground based imaging, their sizes being usually a fraction of a parsec
which translates into a couple of hundredth of an arcsec at a distance of
1 Mpc, approximately the outer edge of the Local Group.
PNe in external galaxies provide a tool to investigate some important
astrophysical problems. First of all, their number reflects the total mass
of the underlying stellar population from which they derive. Extragalactic
PNe also provide important information on the chemical evolution of the host
galaxies, as the nebular abundances of elements like oxygen, neon, sulphur,
or argon, do not vary significantly during the evolution of low-mass stars.
Therefore the abundances of these elements probe the initial metallicity of
their environment at the time when their progenitors were born. This covers
a range in ages that can be hardly covered using other classes of stars.
Moreover, nowadays PNe are used as reliable extragalactic distance indicators,
through the invariance of their luminosity function with galaxian type and
metallicity. And finally, as they are also detected in stellar systems of
low surface brightness, they are extremely valuable test particles to map
the dynamics of stars in galaxies up to very large galactocentric distances.
For the reasons above, an intense search for PNe in nearby galaxies, as
one of the main objectives of the Local Group Census (LGC), was started.
The LGC is a narrow-band survey of the galaxies of the Local Group observable
from La Palma, that was awarded observing time within the INT Wide Field
Imaging Survey programme. The aim of the survey is to find, catalogue and
study old and young emission-line populations (e.g. HII regions, PNe, SN remnants,
LBVs, WR stars, symbiotic binaries, etc.) to unprecedented levels. The value
of narrowband [OIII], Hα, [SII], and HeII images is enhanced with complementary
broad band data (g, r, i). This enables, in principle, the linkages between
stellar populations to be probed.
The first part of the analysis of the survey data
has been focused on the search for PNe in dwarf irregular galaxies of the
Local Group. This is of particular interest as dwarf galaxies are the most
numerous galaxies in the nearby Universe. According to the hierarchical
scenarios of galaxies formation, dwarf galaxies are the first structures
to form and from them merging larger galaxies are built. The Local Group,
which appears to the rest of the Universe as an ordinary collection of dwarf
galaxies (90% of its 40 known members) dominated by two main spiral galaxies,
is an ideal laboratory as the low-luminosity dwarf galaxies can be studied
Before this census, only a small number of PNe were known in the dwarf
irregular galaxies of the Local Group. With the present survey, so far 16
PNe in IC 10, 5 in Sextans B and 3 in IC 1613 were newly discovered, while
the existence of one candidate planetary nebula in Leo A, one in Sextans
A, and about 25 in NGC 6822 were confirmed. No PNe are instead found in
GR8, as expected because of the small luminosity of this galaxy.
|The data are illustrated in these colour
figures; in each image green is the
[OIII] emission, red the Hα one, while blue corresponds to the broad band
Sloan-g images, mainly dominated by continuum stellar emission. In these
images, planetary nebulae stand out as green or yellow dots (a striking example
is the green luminous object on the upper-left side of the image of Leo A).
[ JPEG | TIFF
The LGC detections provide a more complete view of the population of PNe
in the Local Group. With these new data, it appears to be consistent with
the predictions of the stellar evolution theories, as the number of observed
PNe in each galaxy scales reasonably well with the luminosity of the galaxy.
In spite of this agreement, there are also some interesting peculiarities.
For instance, Sextans A and Sextans B have very similar V-band luminosities
and mass, but while five PNe were discovered in Sextans B, only one candidate
is detected in Sextans A. Statistically, this difference is only marginally
significant, but may suggest some differences in their star formation history,
as evidenced by the stronger main-sequence population of Sextans A compared
to Sextans B.
The behaviour of the numbers of planetary nebulae
with galaxy metallicity was also investigated, and found a possible lack
of PN when [Fe/H]<<–1.0, which might indicate that below this point
the formation rate of PNe is much lower than for stellar populations of near
solar abundances. This might in turn be related to the mass loss mechanism
in evolved red-giants, that is governed by radiation pressure on dust grains,
and is therefore sensitive to a significant deficiency of heavy elements
in the stellar atmosphere.
Another result of the survey is the discovery of candidate planetary nebulae
at large galactocentric distances, like in the case of IC10 where they cover
an area of 3.6×2.7kpc, much more extended than the 25 mag×arcsec–2
diameter (1.1×1.3 kpc).
The new detections of the LGC are clearly a starting point for future spectroscopical
studies of individual objects, aimed at confirming their nature as PNe and,
more important, at determining their physical and chemical properties and
of their host galaxies.
R., et al., 2003, "The Census of Planetary Nebulae in the Local Group",
ING Newsl., 7, 11.
L., et al., 2002, "The Local Group Census: Planetary nebulae in Sextans
B", A&A, 386, 869.
L., et al., 2003, "The Local Group Census: Planetary nebulae in IC 10, Leo
A and Sextans A", A&A, 407, 51.