GALAXIES, X-RAY EMISSION
Giuseppina Fabbiano
The study of the x-ray emission of normal galaxies is a very recent
part of astronomy. This work has been made possible by the sensitive
x-ray imaging observations of the Einstein (HEAO 2) satellite,
launched by NASA in
November 1978. Before then, with the exclusion of
the bright x-ray sources associated with Seyfert nuclei, only four
galaxies were known to emit x-rays: the Milky Way, M31 (Andromeda),
and the Magellanic Clouds. The Einstein satellite observed over 200
galaxies during its 2 1/2-yr life span. Some were detected with enough
detail to allow a study of their x-ray morphology, spectra, and
individual sources, and to make comparisons with optical, infrared,
and radio data. These observations have shown that normal galaxies of
all morphological types are spatially extended sources of x-ray
emission with luminosities in the range of
1038-1042 erg s-1. Although
this is only a small fraction of the total energy output of a galaxy,
x-ray observations are uniquely suited to study phenomena that are
otherwise elusive. These include the end products of stellar evolution
(supernova remnants and compact remnants, such as neutron stars, white
dwarfs, and black holes), the hot component of the interstellar
medium, and active nuclear regions.
SPIRAL AND IRREGULAR GALAXIES
Normal stars are responsible for the optical emission of galaxies.
However, their integrated x-ray emission is only a small fraction of
the x-ray emission of a normal galaxy. Observations of the Milky Way
and of the Local Group galaxies suggest that a good fraction of the
x-ray emission of late-type (spiral and irregular) galaxies is due to
a collection of a relatively small number of individual bright
sources, such as close accreting binaries with a compact companion,
and supernova remnants, with luminosities ranging from ~ 1035
erg s-1 up
to a few times 1038 erg s-1.
Only a few very bright individual x-ray sources can be detected in
the Einstein images of more distant galaxies, which typically appear
as extended x-ray emission regions, because at that distance
individual sources could not be resolved with the Einstein
instruments. However, we believe that the x-ray emission of these
galaxies is due to sources akin to those detected in the Local
Group. The x-ray spectra of these galaxies are consistent with the
hard spectra expected from binary x-ray sources, and the x-ray
luminosities are linearly correlated with the emission in the optical
B band, suggesting that the x-ray emission is mostly due to sources
constituting a constant fraction of the stellar population.
In the pre-Einstein era, the x-ray sources of the Milky Way were
classified as young Population I, or spiral arm, sources with massive
early-type star counterparts and Population II, or bulge sources, with
low-mass stellar counterparts. The Einstein imaging observations of
spiral galaxies have led us to modify this classification and to gain
new insight into the evolution of binary x-ray sources. We can now
identify a ``spiral arm,'' a ``bulge,'' and a ``disk'' component of the
x-ray emitting population.
The presence of spiral arm and bulge (and globular cluster) x-ray
sources is immediately demonstrated by the x-ray images of nearby
galaxies. Bright point sources are detected in the spiral arms of
M31
(see Fig. 1) and M33. In particular, one of the
M33 sources has a
variable light curve that is similar to those of some massive Galactic
x-ray binaries. A bulge component of the x-ray emitting population is
also evident in M31, these sources have properties similar to those of
low-mass x-ray binaries in the Galaxy. Statistical analyses of the
sample of spirals observed with Einstein indicate that x-ray bulge
emission is present in all bulge-dominated spirals. Disk x-ray sources
are suggested by the close resemblance of the radial profile of the
x-ray surface brightness of a few face-on spirals (M83, M51, and NGC 6946) with that of the optical light of their
exponential disk. This
implies that a good fraction of low-mass x-ray binaries may originate
from the evolution of binary systems belonging to the disk stellar
population, rather than from dynamical evolution (capture of a
low-mass companion by a compact object in a dense environment and/or
disruption of globular clusters), as has been suggested to explain
galactic low-mass binaries.
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Figure 1. The circles show the positions of
the x-ray sources of M31, superimposed onto an optical
photograph. (Courtesy of L. Van Speybroeck. Reproduced, with
permission, from the Annual Review of Astronomy and Astrophysics,
27 © 1989 by Annual Reviews, Inc.) Notice the
clustering of sources in the bulge.
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Some of the sources detected in spiral galaxies have x-ray
luminosities well above the Eddington limit for accretion onto a
one-solar-mass compact object, which is ~ 1.3 x 1038 erg
s-1. One of these
sources is the supernova SN 1980k detected in NGC 6946 approximately
35 days after maximum light. The variability reported for some bright
sources in M101 suggests point-like objects, possibly bright accretion
binaries. If these sources are truly single objects, they could
indicate the presence of massive black holes in these galaxies. It is,
however, possible that the distances of some galaxies might have been
overestimated, making these sources appear more luminous that they are
in reality.
Another source of x-ray emission that has been searched for in
spiral galaxies is diffuse thermal emission from a hot phase of the
interstellar medium. Supernovae release ~ 1042 erg
s-1 in a galaxy,
and it has been suggested that hot gaseous coronae, or galactic
fountains, could be produced and should be visible in soft x-rays in
the Einstein range. There is evidence of soft thermal diffuse emission
both in the galactic plane and in the Large Magellanic Cloud (LMC),
and perhaps in M33. However, this type of emission has not been
detected in more distant galaxies. The lack of intense diffuse soft
x-ray emission could imply that most of the supernova energy is
radiated in the unobservable far ultraviolet. The only reported
instance of this type of soft x-ray emission in a spiral galaxy is in
the edge-on galaxy NGC 4631, where this component could have an x-ray
luminosity of 5 x 1039 erg s-1, which represents
~ 13% of the total emission in the Einstein band.
STARBURST GALAXIES AND NUCLEAR OUTFLOWS
Bluer starburst, often interacting, galaxies tend to have enhanced
x-ray emission when compared with galaxies with redder, more normal,
colors. The bulk of the x-ray emission of these galaxies can be
understood in terms of a number of young supernova remnants and
massive x-ray binaries, with X-ray luminosity possibly enhanced by the
low metallicity of the accreting gas, similar to those observed in the
Magellanic Clouds.
There are galaxies in which the starburst activity is confined to
the nuclear regions. Starburst nuclei studied in x-rays include the
Milky Way galactic center region, and the nuclei of M82, NGC 253, M83,
NGC 6946, IC 342, and NGC 3628. A common characteristic of the
emission spectrum of these nuclei is their intense far-infrared
emission, indicative of dusty nuclear regions heated by newly formed
early-type stars. The x-ray emitting regions are extended (whenever
they are observed with high enough spatial resolution) and in M82
there is evidence of a population of bright individual sources. To
explain this emission requires, in different cases, different amounts
of evolved sources (supernova remnants and x-ray binaries)
superimposed on the integrated stellar emission from a young stellar
population.
An unexpected result of the Einstein observations of these nuclei has
been the discovery of extended emission components, suggestive of
gaseous bipolar outflows from the nuclear regions, in the edge-on
galaxies M82 and NGC 253. These outflows, if generally
associated with
violent star formation activity, could be responsible for the formation
and enrichment of a large part of the gaseous intracluster medium.
ELLIPTICAL AND SO GALAXIES
A hot gaseous component dominates the x-ray emission of x-ray-luminous
early-type galaxies. These galaxies can be ~ 100 times brighter in
x-rays than spiral galaxies of similar optical magnitude, where the
x-ray emission instead is due to evolved stellar sources. These x-ray
bright galaxies also tend to have x-ray spectra different from those
of binary sources, and sometimes show distortions of their x-ray
surface brightness, relative to the optical images
(Fig. 2). The
latter suggest that the x-ray emission is not due to the stellar
population and is consistent with the interaction of the hot galactic
halo with a surrounding cluster gas.
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Figure 2. The x-ray map of NGC 4472, an
elliptical galaxy in the Virgo cluster, obtained with the imaging
proportional counter of the Einstein observatory. Notice the
asymmetrical halo. (Reproduced, with permission, from the Annual
Review of Astronomy and Astrophysics, 27 © 1989 by
Annual Reviews, Inc.)
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X-ray observations have revealed the presence of a long-sought
interstellar medium in early-type galaxies, whose apparent absence had
been explained by invoking galactic winds to remove the gaseous
by-products of stellar evolution. The amount of hot gas present in
these galaxies can be as high as 1010 solar masses,
significantly more
than the amount of cold interstellar medium seen in neutral hydrogen
and in the infrared, which is well below the amount of interstellar
medium seen in spiral galaxies. Not all E and SO galaxies, however,
may be able to retain their hot interstellar medium. The Einstein
survey has shown that there is a wide spread of x-ray luminosities in
early-type galaxies of similar optical luminosity. The lowest x-ray
luminosities can be explained easily by the integrated emission of
bulge-type x-ray sources in these galaxies and do not require any
additional gaseous component. The ability (or lesser ability) to
retain a hot gaseous halo might be the result of several factors,
including large amounts of dark matter in the galaxy, the amount of
supernovae present, and the interaction with a surrounding hot cluster
medium.
In an x-ray-luminous galaxy with a large hot gaseous halo, the gas
is so dense that it will cool in a time shorter than the galaxy's
lifetime and then accrete to the galaxy's core, giving rise to
``cooling flows.'' These cooling flows would have interesting
consequences: One could be the formation of new stars from matter
detaching from the flows; another could be the accretion of gas into
the nucleus and the consequent fueling of nuclear sources. There is
some evidence of the latter, in that powerful radio sources, connected
with nuclear activity, tend to be found in x-ray-bright, gas-rich
galaxies. The presence of a hot gaseous halo is also determinant in
the formation of extended radio lobes. In the range of radio core
power (i.e., of the intensity of the nuclear source) of the radio
galaxy Centaurus A, powerful radio lobes more extended than the
optical size of the parent galaxy are only found in relatively
gas-poor (i.e., x-ray-dim) galaxies.
One of the potentially very important results of x-ray observations
of early-type galaxies is the possibility of measuring their
masses. The method generally used employs the equation of hydrostatic
equilibrium, in which the gas pressure and the gravitational pull
balance. Combining this with the ideal gas law, one obtains
M (< rgas) = -[(rgas
kTgas) / (GµmH)]
[(d log gas) / (d log r) +
(d log Tgas) / (d log r)]
Four quantities must therefore be measured to determine the mass
within a certain radius rgas: the radius itself, the
temperature TgasT
at that radius, and the temperature and gas-density (gas) gradients at
that radius. The uncertainty in the mass measurement will reflect the
uncertainties in the determination of these quantities. Applied to
M87, the dominant galaxy at the center of the Virgo cluster, this
method reveals a large amount of dark matter. However, when this
method is applied to more normal early-type galaxies, which are more
than 100 times less x-ray-luminous that M87, the uncertainties are
very large and the presence of large dark halos cannot be demonstrated
firmly, although it is suggested in some cases. X-ray measurements
with the German satellite ROSAT (launched June 1,1990) and with the
future satellites AXAF and XMM will allow accurate mass determinations
in the x-ray-bright early-type galaxies. In the case of less
x-ray-luminous galaxies it will have to be established first that the
x-ray emission is due to a gaseous halo and not to a collection of
binary x-ray sources. It will also be important to consider the effect
of supernovae on the energy balance of the halo.
GALAXIES AND THE X-RAY BACKGROUND
The extragalactic x-ray background was discovered by Riccardo
Giacconi, Herbert Gursky, Frank Paolini, and Bruno Rossi in 1962 in
data from the same rocket flight that led to the discovery of the
first extrasolar source of x-rays, Sco X-1. Since then a great deal of
effort has been spent to determine if this radiation is due to the
integrated contributions of different classes of discrete sources or
if diffuse processes are responsible for it. The integrated emission
of normal galaxies could explain ~ 13% of the 2-keV extragalactic x-ray
background. If one includes in this estimate the contribution of
low-activity nuclei present in a fraction of these galaxies, the
effect of starburst activity, and even more the possibility that these
types of activities were more pronounced in the past, this
contribution could be significantly larger.
Additional Reading
Fabbiano, G. (1986). The x-ray properties of normal galaxies.
Pub. Astron. Soc. Pacific 98 525.
Fabbiano, G. (1989). X-rays from normal galaxies.
Ann. Rev. Astron. Ap. 27 87.
Fabian, A.C., ed. (1988). Cooling Flows in Clusters and Galaxies.
Kluwer, Dordrecht.
Helfand, D.J. (1984). Endpoints of stellar evolution: X-ray surveys
of the Local Group. Pub. Astron. Soc. Pacific 96 913.
Long, K.S. and Van Speybroeck, L.P. (1983). X-ray emission from
normal galaxies. In Accretion Driven X-Ray Sources, W. Lewin
and E.P.J. van den Heuvel, eds. Cambridge University Press,
New York, p. 117.
See also Background Radiation, X-Ray; Clusters of Galaxies,
X-Ray Observations; Galaxies, Starburst; X-Ray Sources, Galactic
Distribution.