|
The major components of the COMPTEL instrumental line background can
be attributed to eight individual isotopes, namely 2D, 22Na,
24Na, 28Al, 40K, 52Mn, 57Ni, and 208Tl
(Weidenspointner 1999). Identification of these
isotopes was achieved in an iterative process, starting from the most
prominent lines. The
and E2 spectra (see
Fig. 6) are particularly useful for the
identification of isotopes that give rise to single photon (type A) or multiple photon (type C) events, respectively. The
diagnostic power of E1 spectra is limited since they do
not exhibit line features at the energy of the incident photons, but
only rather broad features at the corresponding Compton edges. Due to
the correlated signatures in
E1-E2 space,
individual spectral features can be accentuated by applying suitable
event selections. Viable isotope identifications are required to
account self-consistently for spectral features in selected regions of
the
E1-E2 dataspace (see the detailed
explanations in Appendix B), as well as for
their variation with time and/or incident cosmic-ray intensity
(discussed in Sect. 5). The telescope response to
individual isotopes was modelled through Monte Carlo simulations.
The isotopes, their half-lifes, most important decay channels, and
main production channels are summarized in
Table 1. Below, a review of the isotope
identifications is given (a more detailed account on the COMPTEL
instrumental line background can be found in, e.g., Weidenspointner
1999).
Thermal-neutron capture on hydrogen results in the production of a
stable 2D nucleus and the emission of a single 2.22 MeV
photon, as seen in
(see top panel in
Fig. 6). The liquid scintillator NE 213A in the D1
detector modules consists of 9.2% H and 90.8% C by mass, making it
an efficient moderator for neutrons. The instrumental 2.22 MeV
photons are isotropically emitted from the D1 scintillators and
constitute single photon (type A) background events. The average
moderation and absorption times in the D1 scintillator for an incident
neutron are a few
s and about 3 10-4 s, respectively,
hence the instrumental 2.22 MeV line is a quasi-prompt background
component that follows the local, instantaneous cosmic-ray intensity
(Weidenspointner et al. 1996). This quasi-prompt
nature of the production/emission of the 2.22 MeV line is the reason
for treating, in the following, the stable isotope 2D as if it
were unstable, and for referring to it as "short-lived''. In
principle, the initial scatterings of the incident neutrons could be
identified by their PSD values. However, the time-scale for the
moderation and absorption of an incident high-energy neutron is too
long to associate the initial scatterings with the delayed neutron
capture producing the
-ray. The instrumental 2.22 MeV events
therefore cannot be rejected by a selection on PSD.
The bulk of the neutrons producing 2D are expected to be of atmospheric origin, with secondary neutrons produced in the spacecraft being of minor importance. This follows from measurements of the fast-neutron flux in the D1 detector and Monte Carlo simulations of the production of secondary neutrons in cosmic-ray interactions (Morris et al. 1995a), as well as from an estimate for the neutron absorption efficiency of the D1 detector.
The main production channels for 24Na are neutron-capture
reactions such as 27Al(n, )24Na and proton
reactions such as 27Al(p, 3pn)24Na. The Al structure of
the D1 detector system is the primary source of 24Na
activation.
As described in Sect. 3, spectral features of
the 24Na background in both the
and
E2 spectra can be understood by considering its cascade
nature (type C events). In particular, the two photons with
energies of 1.37 MeV and 2.75 MeV produce line features at about
1.3 MeV and 2.7 MeV in E2 (see bottom panel in
Fig. 6).
In addition, the time-variation of the 24Na event rate is
consistent with expectations for an isotope with a half-life of 15 h
that is produced during SAA passages (see
Sect. 5.1). Also, ToF distributions summed using data
selections that favour 24Na events have the characteristics of
type C background events, i.e. they peak slightly below a ToF
value of 5 ns (see Fig. 7), corresponding to an
average distance of the location of the photon emission from the D1
module of about 20-30 cm.
40K is one of the contributors to the spectral line feature at
about 1.4 MeV in
(see top panel of
Fig. 6). A prominent line at this energy was
present before launch in some of the calibration data, and at
that time was tentatively identified with primordial 40K
radioactivity, contained e.g. in the concrete of the buildings.
The 1.4 MeV line was still present after launch, however, and did
not vary with any orbital parameter, indicating an instrumental
origin as well.
A viable explanation for the instrumental 1.4 MeV line was the
potassium in the glass of the D1 PMTs (van Dijk 1996).
Electron capture by 40K results in the emission of a single
1.46 MeV photon (type A event). This origin is supported by the
fact that a disproportionate fraction of the photons at 1.46 MeV
interact in the outer sections of the D1 scintillator, indicating that
the photons enter the D1 detectors from the sides, consistent with the
location of the D1 PMTs. Also, the observed
distribution at 1.46 MeV peaks at high
values, again
indicating that the photons enter from the sides. These
characteristics were reproduced in Monte Carlo
simulations. Furthermore, the potassium content in the D1 PMTs derived
from the observed 1.4 MeV line rate is consistent with the
manufacturer's specifications, as was confirmed by radiological
measurements of a PMT in the laboratory. The mass of the PMT front
window (made of Corning France 801.51) is about 24.9 g, with a
potassium mass fraction of 6%; the mass of the PMT side and back
glass (both made of Schott 8245) is about 40.7 g and 9.1 g,
respectively, both with a potassium mass fraction of 0.14%. The front
window contains more than 95% of the potassium in the PMTs and is
closest to the detectors. The 40K background therefore is
dominated by the front window. The 40K activity of the front
window, normalized to its mass, is about 0.2 decays s-1 g-1.
Routine data processing and the investigation of galactic 1.8 MeV line
emission from radioactive 26Al indicated the build-up of a broad
background component at about 1.5 MeV in
(see top
panel of Fig. 6). Investigations of the energy
distribution of this background feature, as well as of its ToF
dependence, led to its identification with the
-decay of
22Na produced in the D1 detector material (Oberlack
1997). This background component is produced by a two
photon cascade (type C event) with energies of
500 keV and
1.3 MeV, consistent with the absorption of the
1.275 MeV photon in D2, and the scattering of an annihilation 511 keV
photon in D1 (the reverse process, involving absorption of the 511 keV
photon in D2, is suppressed because 511 keV is below the D2
threshold). The ToF distribution of the 1.275 MeV 22Na line in
E2 is consistent with the ToF signature of the 24Na
cascade. The build-up of the feature is consistent with an isotope of
half-life of 2.6 y (see Sect. 5.1).
The most important process for the production of 22Na in the D1 detector are proton interactions in the aluminium structure, the main channel being 27Al(p, 3p3n)22Na. Based on the production cross-sections, some 22Na should also be produced in proton interactions with silicon, found in the glass of the D1 PMTs, such as Si(p, 4pxn). It is expected that most of the 22Na production occurs during SAA passages (see Sect. 5.1).
The isotope 28Al is produced by thermal-neutron capture on
aluminium, the most abundant element in the D1 detector. The existence
of the strong 2D line due to thermal-neutron capture on
hydrogen indicates the presence of a thermal-neutron flux in the D1
scintillators. The cross-section for thermal-neutron capture on
aluminium has a value of 0.28 mb (cf. 0.33 mb for hydrogen). Upon
its -decay, 28Al can generate a type C
background event: the 1.78 MeV photon is absorbed in D2, with a
bremsstrahlung photon (from the
)
scattering in D1. A
small fraction of the 28Al decays result in type A
background events from the double scattering of the 1.78 MeV
photon.
From the beginning of the mission a weak, albeit significant, line feature at about 1.8 MeV has consistently been present in the E2 distribution (see bottom panel of Fig. 6). The position of this feature is independent of E1, as expected for a type C event. Additional support for the identification of 28Al comes from the fact that, as expected, the 1.8 MeV feature is short-lived (see Sect. 5.2).
The above mentioned isotopes were not sufficient to account entirely
for the pronounced and broad 1.4 MeV feature in
E2 that built up over the mission. After subtracting the
effects of the other isotopes, there was clear evidence for a build-up
of the 1.4 MeV residual, whose half-life was estimated to be between
that of 24Na and that of 22Na (assuming that it is due to a
single isotope). The E1 dependence of the 1.4 MeV residual
in E2 suggested that the line is due to a
-decay
and therefore arises from type C background events.
After detailed modelling of the E2 and
spectra, taking into account the material composition of the D1
detector, it was concluded that the 1.4 MeV residual is due to a blend
of two different isotopes, namely 52Mn (1.43 MeV) and 57Ni
(1.38 MeV).
The isotope 52Mn is produced in SAA-proton interactions
with the Fe, Cr, and Ni in the D1
detector, found mainly
in the electronics. Matters are complicated by the
fact that 52Mn can be produced in either its ground state or
an isomeric state. These two states have different half-lifes and
decay schemes. The time variation
of the 52Mn event rate suggests that this isotope is
more likely produced in the ground state (
T1/2 = 5.6 d) than in
the isomeric state (
T1/2 = 21.1 min), as described in
Sect. 5.1. In this case, most 52Mn events are
due to the absorption of a 1.43 MeV photon in D2, accompanied by the
scattering of another photon, from the radioactive decay or positron
annihilation, in D1.
The isotope 57Ni is expected to be mostly produced by proton
interactions with Ni and Cu in the D1 detector during SAA
passages. The 57Ni background is mainly produced by the
absorption of the 1.38 MeV photon in D2, with one of the 511 keV
annihilation photons scattering in D1 (type C event). Similar to
52Mn, the identification of 57Ni, which has a
half-life of about 36 h, is supported
by modelling the observed long-term variation of its
background contribution (see Sect. 5.1).
Similar to the 1.4 MeV feature, the 2.7 MeV feature in E2represents a blend of lines from more than a single isotope. In addition to 24Na, at least one component with a very long half-life (exceeding that of 22Na) is present. The position of the residual is about 2.6 MeV. 208Tl, which is part of the natural 232Th decay chain, is the most viable candidate.
The isotope 208Tl undergoes -decay through several
channels, all of which involve the emission of at least two photons,
implying that the 208Tl multiple photon (type C) events are
efficient in triggering the telescope. The half-life of 208Tl is
only 3.1 min. If the isotope is part of a natural decay chain,
however, then its effective half-life is equal to the longest
half-life of any of its parent isotopes, which in this case is the
isotope 232Th with a half-life of
1.4 1010 y. The
main channel for the production of background events by 208Tl is
the absorption of the 2.61 MeV photon in D2, with another photon
scattering in D1.
It was assumed that 208Tl is distributed like 40K and is
only present in the front glass of the D1 PMTs. This was tested by
recording -ray spectra of a spare D1 PMT using a Ge
spectrometer. Taking the COMPTEL results for the 40K and
208Tl lines at face value, and assuming that both isotopes are
equally distributed in the D1 PMTs, one expects that the 208Tl
activity is about 10-2 decays s-1 g-1 in the front
window or about 6% of that of 40K, based on the simulated
efficiencies, corresponding to a 232Th mass fraction of a few
10-8. Unfortunately, the laboratory measurement of 208Tl
was inconclusive. The 1.46 MeV 40K line is detected at the
12
level above the general background (
counts). The strongest 208Tl lines at 2.61 MeV and 0.58 MeV,
however, with intensities of 100% and 85.5%, were only detected at
the 0.9
(
counts) and 1.4
(
counts) level, respectively. Although consistent with
expectations, these numbers are insufficient to test the
assumptions. Much longer integration times are needed.
Copyright ESO 2001