A&A 365, L248-L253 (2001)
R. S. Warwick1, J.-P. Bernard2, F. Bocchino3, A. Decourchelle4, P. Ferrando4, R. G. Griffiths1, F. Haberl5, N. La Palombara6, D. Lumb3, S. Mereghetti6, A. M. Read5, D. Schaudel5, N. Schurch1, A. Tiengo7, and R. Willingale1
Send offprint request: R. S. Warwick
1 -
Department of Physics and Astronomy,
University of Leicester, Leicester LE1 7RH, UK
2 -
Institute d'Astrophysique Spatiale, Orsay, France
3 -
Space Science Department, ESTEC, 2200 AG Noordwijk, The Netherlands
4 -
Service d'Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France
5 -
Max-Planck-Institut für extraterrestrische Physik, 85740, Garching, Germany
6 -
Istituto di Fisica Cosmica "G. Occhialini'', CNR, 20133 Milano, Italy
7 -
XMM-SOC, Villafranca Satellite Tracking Station, 28080 Madrid, Spain
Received 2 October 200 / Accepted 9 November 2000
Abstract
Recent XMM-Newton observations reveal an extended
(
)
low-surface brightness X-ray halo in the supernova remnant G21.5-0.9.
The near circular symmetry, the lack of any limb brightening and the
non-thermal spectral form, all favour an interpretation of this outer halo
as an extension of the central synchrotron nebula rather than as a shell
formed by the supernova blast wave and ejecta. The X-ray spectrum of
the nebula exhibits a marked spectral softening with radius, with
the power-law spectral index varying from
in the
core to
at the edge of the halo. Similar spectral
trends are seen in other Crab-like remnants and reflect the impact of
the synchrotron radiation losses on very high energy electrons as they
diffuse out from the inner nebula. A preliminary timing analysis provides
no evidence for any pulsed X-ray emission from the core of G21.5-0.9.
Key words: ISM: individual (G21.5-0.9) - supernova remnants - X-rays: ISM
Author for correspondance: rsw@star.le.ac.uk
Of the 225 known supernova remnants (SNRs) in our galaxy no more
than
are classified as Crab-like remnants (Green 2000).
Prominent members of this
class of SNR, also known as plerions, include the Crab Nebula, CTB 87,
and 3C 58. The characteristic centre-filled radio and X-ray morphologies
of the Crab-like SNRs is thought to be due to the presence of
an active pulsar which powers a bright synchrotron nebula. In the case
of the Crab nebula, 33 ms pulsations testify to the presence
of the central spinning neutron star, although in many Crab-like systems
there is no direct evidence for pulsed emission. Typically a Crab-like
SNR exhibits a flat power-law spectrum in the radio regime which eventually
steepens at shorter wavelengths to join smoothly to a similarly featureless
power-law X-ray continuum. This non-thermal form for the radio to X-ray
spectrum is a consequence of the continuous injection by the pulsar
of high energy electrons, which suffer radiation and adiabatic losses
as they diffuse through the nebula; however the details of the process
are undoubtedly complex (e.g. Reynolds & Chanan 1984).
A feature of the Crab-like remnants, which distinguishes them from both
shell-like and composite-type SNRs (the latter typically exhibiting
a filled-centre X-ray morphology within a radio shell), is the
lack of any evidence for an outer shell structure marking the progress of
the blastwave from the original supernova explosion.
G21.5-0.9 is a SNR with many of the characteristics of
a Crab-like remnant (e.g. Becker & Szymkowiak 1981;
Asaoka & Koyama 1990). To date there has been no detection
of pulsed emission in either the radio or X-ray bands
(e.g. Biggs & Lyne 1996; Slane et al. 2000). However,
recent X-ray observations made by Chandra have pinpointed
the probable location of the pulsar, namely a very compact
central core on a scale of 2'' embedded within a more extended
(
30'' radius) synchrotron nebula (Slane et al. 2000).
A faint extended halo was also detected which might correspond to the
outer "shell'' formed from the expanding ejecta and the passage of the
supernova-driven blastwave (Slane et al. 2000). In this
interpretation G21.5-0.9 would be best described as a composite remnant.
Here we report further recent X-ray observations of G21.5-0.9 made
by XMM-Newton which help to clarify the nature of the extended
X-ray halo in this object.
![]() |
Figure 1:
Left panel: the raw XMM-Newton EPIC PN image of
G21.5-0.9. The pixel size is 4'' and the image is 8' on a side.
A logarithmic intensity scaling has been applied. The vertical and horizontal
white bands correspond to the gaps between adjacent CCD chips of the PN
camera. Right panel: EPIC MOS image of G21.5-0.9. The pixel size
is 1'' and the image is 8' on a side. The image has been spatial
filtered with a Gaussian smoothing mask with width
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G21.5-0.9 was observed as a calibration target during orbits 60-62 and
64-65 of the XMM-Newton mission. Here we focus on measurements from
orbit 60 (date: 2000/04/07; start time: 12.35 UT; end time 22.57 UT) in
which the SNR was observed on-axis by the EPIC MOS and PN cameras
(Turner et al. 2001; Strüder et al. 2001)
giving a total accumulated exposure time of 30 ks. For these
observations all three EPIC cameras were operated in the standard full-frame
mode with the medium filter selected. Attitude information files
are not yet available but all the indications are that a stable pointing was
maintained for the duration of the observation
.
The recorded events were screened with the XMM Science Analysis Software (SAS) to remove known hot
pixels and other bad data and pre-processed using the latest CCD gain values.
X-ray events corresponding to patterns 0-12 for the two MOS cameras (similar
to grades 0-4 in ASCA) were used, whereas for the PN only pattern 0
events (single pixel events) were accepted. Investigation of the full-field
count-rate revealed a number of flaring events in the non-cosmic component
of the background during the observation. As a final step in the data
screening we identified a period when the background was essentially
"quiescent'', with full-field background rates in the MOS and PN cameras
of 2.5 and
6 count/s. Selecting events only in this
low-background period lead to effective exposure times of 13800 s and
11800 s for the MOS and PN cameras respectively.
![]() |
Figure 2: The radial profile of the X-ray surface brightness of G21.5-0.9 (dotted curve). The counts in the broad-band MOS image were accumulated in annuli of 10'' width out to a maximum radius of 200''. The mean background level in the annular region from r = 200'' to 240'' was then subtracted. Note that within a radius of 150'' the statistical errors are smaller than the plotted points. The presence of the south-western point source has a marginal impact at r = 115''. By way of comparison, the point spread function of mirror module 3 (MOS 1) at 1.5 keV is also shown (dashed-dotted line) (Aschenbach et al. 2000) |
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Figure 3: The softness ratio image of G21.5-0.9 derived from the MOS 1 + MOS 2 datasets. Softness ratio is defined here as SR = (S-H)/(S+H), where S and H represent the 1-3 keV and 3-10 keV band images respectively. The S and H band images were initially heavily smoothed with a tophat filter of width 30 pixels (1 pixel = 1''). Red to blue colours reflected a decreasing softness ratio. The black contours are based on the combined S+H smoothed image |
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Given the observed soft X-ray cut-off in the spectrum of G21.5-0.9 (see Sect. 4),
we utilize the 1-10 keV energy band in the spatial analysis. The raw image of
G21.5-0.9 from the PN dataset binned into 4'' pixels is shown in Fig.
1 (left panel). The bright synchrotron nebula at the
centre of this SNR is the most prominent feature of the image, although
the central core is clearly surrounded by a more extended low
surface-brightness emission region. In addition a point source is evident
2' to the south-west of the centre of the remnant.
To avoid the complications due to the chip boundaries in the PN data we have
based our spatial analysis on the data from the MOS cameras (since the
field of view of the central chip in the MOS
cameras comfortably encompasses the full extent of the SNR). Broad band
images were constructed for both MOS 1 and 2 cameras
utilizing 1'' pixels. The MOS 1 and 2 images were then aligned (by eye)
using the nebula core and the south-western point source as fiducial marks
and co-added. Figure 1 (right panel) shows the resultant image
after applying a Gaussian smoothing filter with a width
= 2 pixels
(FWHM of 4.7'').
At a qualitative level there is clearly excellent
agreement between the images from the PN and MOS cameras. The bright centre
of the synchrotron nebula (i.e. the region within
of
the centre) shows deviations from circular symmetry, in particular there is
an indentation in the north-west quadrant. At a slightly lower level of
surface brightness a curious "spur'' is evident which appears
initially to track northwards away from the core region but then at
sweeps round in an arc into the north-eastern quadrant of
the remnant. These spatial features match rather well to similar structure
seen in the higher spatial resolution images from Chandra (Slane et al.
2000). One of the strengths of the EPIC cameras on XMM-Newton
is, of course, the sensitivity afforded to extended, relatively low-surface
X-ray emission. This is evident in the images of Fig. 1 in which
a low surface brightness "halo'' is well delineated out to
.
This halo exhibits a near perfect circular symmetry apart
from the hint of a "linear termination'' along its northern rim (note
that out-of-time events, namely events recorded during the period
when charge is transferred to the readout node, partly mask this feature
in the PN image).
In order to investigate more quantitatively the spatial extent of the low surface brightness halo, we have calculated the azimuthally-averaged radial profile of the X-ray emission (Fig. 2).
The surface brightness
away from the centre of the synchrotron nebula drops rapidly out to
.
A plateau region is then reached corresponding to the low
surface brightness halo. A sharp further decline in the surface brightness
then sets in at
,
with the signal eventually falling
below the detection threshold at
.
In this paper
we define the remnant's outer radius to be 150'' at which
point the surface brightness is roughly one-fifth of the plateau value.
We first examined the spectral properties of G21.5-0.9 by plotting the softness ratio image shown in Fig. 3, which shows that the core of the nebula is significantly harder than the low-surface brightness halo.
We have investigated the spectral characteristics of the core of
G21.5-0.9 using data from both the PN and MOS cameras. The X-ray spectrum of
the core of the nebula was obtained using a circular extraction region
of radius 48'' centred on the position of peak surface brightness.
Background spectra were extracted from representative regions
greater than 200'' away from the SNR. The source spectra were
binned to a minimum of 20 counts per spectral channel, in order to apply
minimisation techniques. The source and corresponding background
spectra were then analysed using the XSPEC V11.01 and the most
recent response matrices available from the EPIC team. The spectral
modelling assumed a power-law continuum (photon spectral index,
,
and normalisation, A) subject to soft X-ray absorption
in cool gas along the line of sight (with an equivalent hydrogen
column density,
).
Figure 4 shows the observed count rate spectra for the
PN, MOS 1 and MOS 2 detectors together with the corresponding
best-fitting model spectra.
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Figure 4: Upper panel: the observed PN (blue), MOS 1 (red) and MOS 2 (green) count rate spectra for the core region of G21.5-0.9. In each case the corresponding best fitting spectral model is represented by the solid histogram. Lower panel: the ratio of the predicted to the observed count rate spectra |
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Camera | ![]() |
![]() |
Ac | ![]() |
PN | 2.33+0.05-0.05 | 1.86+0.03-0.03 | 1.56+0.08-0.07 | 1278/1203 |
MOS 1 | 2.28+0.06-0.06 | 1.86+0.04-0.04 | 1.55+0.09-0.09 | 384/425 |
MOS 2 | 2.21+0.06-0.06 | 1.86+0.04-0.04 | 1.61+0.09-0.09 | 448/423 |
a Column density in units of
![]() |
b Photon spectral index. |
c Normalisation in units of
![]() |
The spectral variations revealed in Fig. 3 were investigated
by extracting spectra from the PN dataset from a set of annular regions
centred on the point of peak surface brightness. The resulting spectra were then fitted as before with a simple
absorbed power-law model. Initially we allowed
to
vary as a free parameter between the different spectral datasets
but, in the event, excellent fits were obtained with
fixed
at the value obtained for the core region (Table 1).
The derived photon spectral index shows a steady increase with
radius from a value of
at the centre to
at the outer edge of the low surface brightness halo (Fig. 5).
![]() |
Figure 5: The observed variation in the photon spectral index versus radius as measured in the PN data |
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Figure 6:
Upper panel: the observed count rate spectra and best-fitting
absorbed power-law model for the core (
![]() ![]() ![]() |
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We next investigated whether there is any evidence for thermal emission
from the halo component, focussing on the PN spectrum extracted from an
outer (
r = 96'' - 144'') annular region. As a first step we fitted
a two component model, comprising a power-law and a (solar abundance, MEKAL)
thermal component. The result was a modest improvement in the
with
respect to the power-law model (see Table 2)
which the F-test shows to be marginally significant for two additional
parameters.
Model | ![]() |
![]() |
kTc |
![]() |
![]() |
PL | 2.33e | 2.45+0.06-0.06 | - | - | 258/231 |
2-Comp | 2.33e | 2.39+0.12-0.12 | ![]() |
- | 253/229 |
NEI | 2.33e | - | 3.1+0.2-0.2 | 7+3-3 | 356/230 |
NEI | 1.69+0.11-0.11 | - | 4.4+0.5-0.5 | 3+2-3 | 277/229 |
a Column density in units of
![]() |
b Photon spectral index. |
c Temperature in keV. |
d Ionization timescale in units of
![]() |
e Fixed parameter. |
We also examined the spectrum of the brightest part of the spur feature (located directly to the north of the core) but unfortunately the signal-to-noise ratio was too low to distinguish between thermal and power-law spectral forms.
The total integrated X-ray flux of G21.5-0.9 within a radius of 144'',
corrected for the line-of-sight absorption, is
erg cm-2 s-1 in the 2-10 keV band.
Assuming a distance of 5 kpc based on HI absorption measurements
(Davelaar et al. 1986), this implies an
X-ray luminosity of
.
Finally we have briefly considered the spectral properties of the
south-west point source. We obtained an on-source spectrum from
the PN dataset using an extraction cell of 16'' radius. A
complementary background spectrum was taken (on the same CCD)
using a cell of the same dimension sited equidistant from the centre
of G21.5-0.9.
Spectral fitting indicated a relatively hard spectrum (
or
keV) and a column density of
.
As the latter is
about a factor two lower than the derived
of G21.5-0.9, we can conclude
that this point source is a foreground object with respect to the SNR.
If we estimated its distance as
3 kpc (i.e. roughly half the
distance to the SNR in line with the ratio of
for the two sources)
then the inferred 2-10 keV luminosity is
.
This point source is positionally
coincident with the emission-line star SS397.
We have carried out a preliminary search for pulsed X-ray emission
using EPIC data from the full observation (i.e. including
periods of relatively high background rate). The photon events in the
1-10 keV band from a region of 8'' radius centred on the core
of G21.5-0.9 were extracted for all three cameras. Next the event times were
barycentric corrected using the standard SAS task "Barycen'' and the
latest available "Reconstructed Orbit'' file. Power spectra were then
calculated for the combined data from all three cameras and the PN dataset
alone. No evidence was found for a significant periodic signal. In terms of
the amplitude of an underlying sinusoidal signal, the detection threshold
was
ct/s in the frequency range
- 0.17 Hz for the PN + MOS combination
(the upper frequency limit being set by the frame time of the MOS CCDs).
Corresponding values for the PN-only data were
ct/s in the frequency range
- 2 Hz.
In terms of the pulsed fraction (of the core emission)
the limits are roughly
and
respectively.
In a recent paper reporting Chandra observations, Slane et al.
(2000) consider the possibility that the low-surface brightness
halo surrounding the central synchrotron nebula in G21.5-0.9 might
be the shell formed from the ejecta and blastwave of
the original supernova explosion. The present XMM-Newton observations
help delineate the spatial extent and morphology of this component.
Crucially the new spectral information demonstrates that the extended halo
has a spectral form devoid of any significant line features. If the halo
emission is thermal then the lack of line emission implies that the plasma
is far from ionization equilibrium. Our NEI modelling confirms
a low ionization state with
.
The temperature derived for the continuum (bremsstrahlung) emission is
4-5 keV which is rather hot, even for a very young SNR. Assuming the
distance to
G21.5-0.9 is 5 kpc (Davelaar et al. 1986) and taking
a maximum shell expansion velocity of
,
we can estimate the (minimum) elapse time since the shock heating of the
bulk of the X-ray emitting gas in the outer halo to be
100 yrs.
Applying the above constraint on
then gives
.
However, the observed X-ray luminosity of
the outer halo, if interpreted as bremsstrallung radiation, sets a
requirement for a significantly higher electron density,
.
There would appear therefore to be
considerable difficulties in interpreting the extended X-ray halo in
G21.5-0.9 as a thermal shell.
There are known examples of SNR shells which exhibit non-thermal X-ray spectra due to local particle acceleration (e.g. SN 1006, Koyama et al. 1995; G347.3-0.5, Slane et al. 1999). However, in the case of G21.5-0.9 the lack of any limb brightening, the smooth transition in spectral index throughout the remnant and the remarkable circular symmetry, all suggest an interpretation of the outer halo as an extension of the central synchrotron nebula. We conclude therefore, on the basis of the present observations, that G21.5-0.9 is a true Crab-like system rather than a composite (centre-filled plus thermal shell) object.
The observed spectral softening with radius in G21.5-0.9 most
likely reflects the impact of synchrotron radiation losses on very high
energy electrons as they flow from the region of the termination shock
around the pulsar to the edges of the nebula. For example, if the nebula
magnetic field is 0.4 mG (Slane et al. 2000 ), then the
synchrotron lifetime of the
20 TeV electrons producing 5 keV X-rays
is only
2 yrs. Similar spectral trends due to "synchrotron burn-off''
are seen in other Crab-like SNR, such as 3C 58 (Torii et al. 2000).
In fact the variation in photon spectral index from a value of 1.63 at the
centre of the G21.5-0.9 to 2.45 at the edge of its halo is amazingly
similar to the index range seen in the Crab nebula (Willingale et al.
2001). In the case of the Crab nebula the spatial and spectral
distribution of the optical to hard X-ray continuum has been explained in
terms a magnetohydrodynamic flow of plasma and magnetic flux in a particle
dominated wind (e.g. Kennel & Coroniti 1984). For G21.5-0.9,
the origin of halo which represents a "plateau'' in the surface
brightness extending from
-130'' remains unclear,
but could possibly be the result of an unusual magnetic field geometry
(see below).
One interesting contrast is that the radio extent of the Crab nebula
is roughly a factor four greater than that observed in X-rays, whereas for
G21.5-0.9 the dimensions of the X-ray halo exceeds that of the radio
synchrotron nebula (which has a major axis of 90'';
Fürst et al. 1988) by a similar factor. Slane et al.
(2000) note that no radio "shell'' is detectable to a (1
)
threshold of
at 1 GHz.
If we make the assumption that the ratio of the core to halo flux is the
same in the X-ray and radio regimes, then we predict the average
surface brightness of an underlying radio halo (between r = 60''-130 '')
to be roughly 5 times this gethreshold. The inference is that very deep
radio observations may well reveal the presence of an extended radio halo
in G21.5-0.9.
The differences in the spatial morphology of the Crab and G21.5-0.9 could be due to the viewing orientation. Specifically the near circular symmetry of G21.5-0.9 might be explained if our line of sight is reasonably aligned with the spin axis of the resident pulsar, so as to give a near face-on view of a putative inner torus. This hypothesis might also explain the non-detection of pulsed X-ray emission from the core of G21.5-0.9, but is hard to reconcile with the axisymmetric structure seen in high frequency radio maps and the near radial distribution of the magnetic field lines (Fürst et al. 1988). In this setting the spur-like feature which emanates northwards from the core could a "plerionic'' wisp associated with a complex inner magnetic field and/or jet structure.
Acknowledgements
The results presented in this paper are based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). We thank the whole XMM-Newton team for the hard work and dedication which underlies the success of the mission.