A&A 422, L47-L50 (2004)
DOI: 10.1051/0004-6361:20040172
A. W. Strong1 - I. V. Moskalenko2,3 - O. Reimer4 - S. Digel5 - R. Diehl1
1 - Max-Planck-Institut für extraterrestrische Physik,
Postfach 1312, 85741 Garching, Germany
2 -
NASA/Goddard Space Flight Center, Code 661, Greenbelt, MD 20771, USA
3 -
Joint Center for Astrophysics, University of Maryland, Baltimore County,
Baltimore, MD 21250, USA
4 -
Ruhr-Universität Bochum, 44780 Bochum, Germany
5 -
W.W. Hansen Experimental Physics Laboratory, Stanford University,
Stanford, CA 94305, USA
Received 5 April 2004 / Accepted 12 May 2004
Abstract
We present a solution to the apparent discrepancy between the radial
gradient in the diffuse Galactic -rayand the
distribution of supernova remnants, believed to be the sources of
cosmic rays. Recent determinations of the pulsar distribution have
made the discrepancy even more apparent. The problem is shown to be
plausibly solved by a variation in the
-to-N(H2) scaling factor.
If this factor increases by a factor of 5-10 from the inner to the
outer Galaxy, as expected from the Galactic metallicity gradient,
we show that the source distribution
required to match the radial gradient of
-raysbe reconciled with
the distribution of supernova remnants as traced by current studies of
pulsars. The resulting model fits the EGRET
-ray
extremely well in longitude, and reproduces the mid-latitude inner
Galaxy intensities better than previous models.
Key words: gamma rays - galactic structure - interstellar medium - cosmic rays - supernova remnants - pulsars
The puzzle of the Galactic -raygoes back to the time of the COS-B satellite (Strong et al. 1988; Bloemen et al. 1986); using HI and CO surveys to trace the atomic and
molecular gas, the Galactic distribution of emissivity per H atom is a
measure of the cosmic-ray (CR) flux, for the gas-related bremsstrahlung and
pion-decay components. However the gradient determined in this way is much
smaller than expected if supernova remnants (SNR) are the sources of cosmic
rays, as is generally believed. This discrepancy was confirmed with the
much more precise data from EGRET on the COMPTON Gamma Ray Observatory,
even allowing for the fact that inverse-Compton emission (unrelated to
the gas) is more important than originally supposed (Strong et al. 2000).
A possible explanation of the small gradient in terms of CR propagation,
involving radial variations of a Galactic wind, was recently put forward by
Breitschwerdt et al. (2002).
However the derivation of the Galactic distribution of SNR,
commonly based on radio surveys, is subject to large
observational selection effects, so that it can be argued that the
discrepancy is not so serious. But other tracers of the distribution
of SNR are available, in particular pulsars; the new sensitive Parkes
Multibeam survey with 914 pulsars has been used by Lorimer (2004)
to derive the Galactic distribution, and this confirms the
concentration to the inner Galaxy. Figure 1 compares the
pulsar distribution from Lorimer (2004) with a CR source
distribution which fits the EGRET -ray(Strong et al. 2000). If the
pulsar distribution indeed traces the SNR, then there is a serious
discrepancy with
-rays. The distribution of SNR given by
Case & Bhattacharya (1998) is not so peaked, but the number of known SNR is much
less than the number of pulsars and the systematic effects very
difficult to account for (Green 1996). But even this flatter
distribution is hard to reconcile with that required for
-rays.
Another, quite independent, tracer of the SNR distribution is the
1809 keV line of 26Al; whether this originates mainly in type II supernovae or masssive stars is not important in this context, since both trace star-formation/SNR. The COMPTEL 26Al maps
(Knödlseder et al. 1999; Plüschke et al. 2001) show that the emission is very
concentrated to the inner radian of the Galaxy. The density of free
electrons shows a similar distribution (Cordes & Lazio 2003). The
26Al measurements are not subject to the selection effects of
other methods; although they have their own uncertainties, they
support the type of distribution which we adopt in this paper.
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Figure 1: CR source density as function of Galactocentric radius R. Dotted: as used in Strong et al. (2000), solid line: based on pulsars (Lorimer 2004) as used in this work, vertical bars: SNR data points from Case & Bhattacharya (1998). Distributions are normalized at R = 8.5 kpc. |
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A major uncertainty in the models of diffuse Galactic -ray
is the distribution of molecular hydrogen, as traced by the
integrated intensity of the J = 1-0 transition of 12CO,
.
Gamma-ray analyses have in fact provided one of the
standard values for the scaling factor
=
;
with only the assumption that cosmic rays
penetrate molecular clouds freely, the
-rayare free of the
uncertainties of other methods (e.g. those based on the assumption of
molecular cloud
virialization). However previous analyses, e.g.
Strong & Mattox (1996), Hunter et al. (1997), Strong et al. (2000), have usually assumed that
is independent of Galactocentric radius R, since otherwise the
model has too many free parameters. But there is now good reason to
believe that
increases with R, both from COBE/DIRBE studies
(Sodroski et al. 1997,1995) and from the measurement of a Galactic
metallicity gradient combined with the strong inverse dependence of
on metallicity in external galaxies (Israel 1997,2000).
A rather rapid radial variation of
is expected, based on a
gradient in [O/H] of 0.04-0.07 dex/kpc
(Andrievsky et al. 2002; Hou et al. 2000; Deharveng et al. 2000; Smartt 2001; Rolleston et al. 2000) and the
dependence of
on metallicity in external galaxies:
-2.5 [O/H] (Israel 1997,2000), giving
,
amounting to a factor 1.3-1.5 per kpc, or an order of magnitude between the inner and outer Galaxy
. A less rapid
dependence,
-1.0 [O/H], was found by
Boselli et al. (2002), which however still implies a significant
(R)
variation. Boissier et al. (2003) also combine the metallicity gradient
with
(Z) within individual galaxies, to obtain radial profiles
of H2, and give arguments for the validity of this procedure.
Digel et al. (1990) found that molecular clouds in the outer Galaxy
(R
12 kpc) are underluminous in CO, with
a factor 4
2 times the inner Galaxy value. Sodroski et al. (1997,1995) derived a similar variation (
/10
20 = 0.12R - 0.34) when modelling
dust emission for COBE data. Pak et al. (1998) predicted the physical origin for a variation of
with Z. Papadopoulos et al. (2002)
and Papadopoulos (2004) discuss the physical state of this metal-poor gas phase
in the outer parts of spiral galaxies (relatively warm and diffuse). Observations of H2 line emission from NGC 891
with ISO (Valentijn & van der Werf 1999) indicate a massive cool molecular
component in the outer regions of this galaxy, supporting the trend
found in our Galaxy.
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Figure 2:
![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 2 illustrates some of the possible
variations
implied by these studies. For the cases where metallicity is used to
estimate
,
the values are normalized approximately to the
values used in the present
-ray, since we are only
interested in comparing the variations of
.
From the viewpoint of
-rays, the effect of a steeper CR source distribution is
compensated by the increase of
.
Thus we might expect to resolve
the apparent discrepancy in the source distribution, and improve our
understanding of the Galactic
-ray. In this paper we
investigate quantitatively this possibility. Note that the
-rays include major contributions from interactions with atomic hydrogen
and from inverse Compton scattering, both of which are independent of
;
this means that the
variation has to be quite large to
have a significant effect.
The EGRET and COMPTEL data are the same as described in
Strong et al. (2000,2004a). The EGRET data consist of the standard product
counts and exposure for 30 MeV-10 GeV, augmented with data for 10-120 GeV. The -raysources in the 3EG catalogue have been removed as described in Strong et al. (2000). The HI and CO data are as
described in Moskalenko et al. (2002) and Strong et al. (2004a); they consist of combined
surveys divided into 8 Galactocentric rings on the basis of kinematic
information. Full details of the procedures for comparing models with
data are given in Strong et al. (2004a) to which the reader is referred.
![]() |
Figure 3:
Longitude profile of ![]() ![]() ![]() |
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We use the GALPROP program (Strong et al. 2000,2004a) to compute the models.
GALPROP was extended to allow a variable
(R) to be input. The
distribution of CR sources is assumed to follow that of
pulsars in the form given by Lorimer (2004), as shown in
Fig. 1. The other parameters, in particular the CR nucleon and electron injection spectral shape and propagation parameters, are taken from the "optimized model'' of
Strong et al. (2004a). As before the halo height is taken as zh = 4 kpc,
and the maximum radius R = 20 kpc. The isotropic background is as
derived in Strong et al. (2004b). Since in this work we simply wish to
demonstrate the possibility to obtain a plausible solution, we adopt a
heuristic approach, adjusting
(R) to obtain a satisfactory
solution as shown in Fig. 2. The electron flux has been
scaled down by a factor 0.7 relative to Strong et al. (2004a) to obtain an
optimal fit.
Figures 3 and 4 show the longitude and latitude
distributions for 1-2 GeV, compared to EGRET data. A rather rapid
variation of
is required to compensate the CR source gradient,
but it is fully compatible with the expected variation based on
metallicity gradients and the COBE result, as described in the
Introduction. The longitude and latitude fits are good except in the
outer Galaxy where the prediction is rather low. One possible reason
for this is that the CR source density does not fall off so fast
beyond the Solar circle as given by the adopted pulsar distribution,
which has an exponential decay. Another possibility could be even
larger amounts of H2 in the outer Galaxy than we have assumed (see
discussion in Introduction). We have chosen the range 1-2 GeV for
the profiles since this is where the gas contribution and hence the
effect of
is maximal. An exhaustive comparison of profiles in
all energy ranges is beyond the scope of this Letter, but in fact the
agreement is good at all energies. The larger CR gradient in this
model has another consequence: the predicted inverse-Compton emission
in the inner Galaxy is more intense at intermediate latitudes where
the interstellar radiation field is still high; this is precisely the
region where previous models (Strong et al. 2000,2004a; Hunter et al. 1997) have had
problems to reproduce the EGRET data. Figure 5 shows the model
spectrum of the inner Galaxy compared with EGRET data; the fit is
similar to that of models (Strong et al. 2004a) with ad hoc source
gradient and constant
.
The prediction is rather high above 20 GeV, however the EGRET data are least certain in this range (Strong et al. 2004a).
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Figure 4:
Latitude profile of ![]() ![]() |
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![]() |
Figure 5:
Spectrum of inner Galaxy,
![]() ![]() |
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We have shown that a good fit to the EGRET data is obtained with the
particular combination of parameters chosen. We can however ask
whether the pulsar source distribution combined with a constant
could also give a good fit if we reduce the CR electron intensity, to
supress the inner Galaxy peak from inverse Compton emission. This can
indeed reproduce the longitude profile in the inner Galaxy, but fails
badly to account for the latitude distribution, since it has a large
deficit at intermediate latitudes. Some variation of
is
therefore required. The suggested variation of
would have
significant impact on the Galactic H2 mass and distribution.
Warm molecular hydrogen in the outer parts of spiral galaxies that is
not traced by CO emission may be detectable by the Spitzer observatory in 28
m vibrational emission. These issues will be addressed in future work.
Two a priori motivated developments allow us to obtain a more
physically plausible model for Galactic -rays, simultaneously
allowing a CR source distribution similar to SNR as traced by pulsars
and an expected variation in the
-to-N(H2) conversion
factor. Obviously the uncertainty in both the source distribution and
are large so our solution is far from unique, but it
demonstrates the possibility to obtain a physically-motivated model
without resorting to an ad hoc source distribution. This result
supports the SNR origin of CR. The resulting model also gives
improved predictions for
-raysthe inner Galaxy at mid-latitudes.
We have therefore achieved a step towards a better understanding of
the diffuse Galactic
-ray. This result is important input
to the development of models for the upcoming GLAST mission. This
Letter is intended only to point out the potential importance of the
effect. The next step will be a more quantitative analysis to derive
(R) from the
-raythemselves.
Acknowledgements
We thank F. Israel and D. Lorimer and the referee for useful discussions. I.V.M. acknowledges partial support from a NASA Astrophysics Theory Program grant, O.R. acknowledges support from the BMBF through DLR grant QV0002.