Issue |
A&A
Volume 508, Number 1, December II 2009
|
|
---|---|---|
Page(s) | 395 - 400 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361/200912815 | |
Published online | 15 October 2009 |
A&A 508, 395-400 (2009)
The first cyclotron harmonic of 4U 1538-52
J. J. Rodes-Roca1,2 - J. M. Torrejón1 - I. Kreykenbohm3,4 - S. Martínez Núñez1 - A. Camero-Arranz5 - G. Bernabéu1
1 - Department of Physics, Systems Engineering and Sign Theory,
University of Alicante, 03080 Alicante, Spain
2 - Department of Physics and Astronomy, University of Leicester,
Leicester LE1 7RH, UK
3 - Dr. Karl Remeis-Sternwarte, Sternwartstr. 7, 96049 Bamberg, Germany
4 - Erlangen Centre for Astroparticle Physics (ECAP),
Erwin-Rommel-Str. 1, 91058 Erlangen, Germany
5 - National Space Science and Technology Center, 320 Sparkman Drive,
Huntsville, AL 35805, USA
Received 2 July 2009 / Accepted 2 October 2009
Abstract
Context. Cyclotron resonant scattering features are
an essential tool for studying the magnetic field of neutron stars. The
fundamental line provides a measure of the field strength, while the
harmonic lines provide information about the structure and
configuration of the magnetic field. Until now only a handful of
sources are known to display more than one cyclotron line and only two
of them have shown a series of harmonics.
Aims. The aim of this work is to see the first
harmonic cyclotron line, confirming the fundamental line at 22 keV,
thus increasing the number of sources with detected harmonic cyclotron
lines.
Methods. To investigate the presence of absorption
or emission lines in the spectra, we have combined RXTE
and INTEGRAL spectra. We modeled the
3-100 keV continuum emission with a power law with an
exponential cut off and look for the second absorption feature.
Results. We show evidence of an unknown cyclotron
line at 47 keV
(the first harmonic) in the phase-averaged X-ray spectra of
4U 1538-52. This line is detected by several telescopes at
different epochs, even though the S/N of each individual spectrum is
low.
Conclusions. We conclude that the line-like
absorption is a real feature, and the most straightforward
interpretation is that it is the first harmonic, thus making 4U 1538-52
the fifth X-ray pulsar with more than one cyclotron line.
Key words: X-rays: binaries - pulsars: individual: 4U 1538-52
1 Introduction
Cyclotron resonant scattering features (CRSFs), usually referred to as
``cyclotron lines'', have proved to be powerful tools for directly
studying
the magnetic field in neutron stars. CRSFs are present in the hard
X-ray spectra of several X-ray pulsars and originate in the ``cyclotron
process'' under extreme conditions. Through
keV
(the ``12-B-12 law'', where z is the gravitational
redshift), an energy of the fundamental feature in the hard
X-rays indicates that the magnetic fields are rather strong (
G). Under such
conditions, the interaction of the electrons and
radiation must be treated quantum-mechanically. The behaviour of an
electron in a strong magnetic field
implies that the electron energy must be quantized in so-called Landau
levels. These absorption features stem from the
resonant scattering of photons by electrons, also referred to as
cyclotron lines.
While the fundamental energy of the cyclotron line provides valuable information about the magnitude of the field, it is only through the detection and the analysis of the harmonic lines that we can get direct information about the geometrical configuration of the B field (Harding & Daugherty 1991; Araya-Góchez & Harding 2000; Schönherr et al. 2007). However, to date, only in a handful of systems have harmonic lines been discovered, and only two systems have shown more than two (Santangelo et al. 1999; Coburn et al. 2005). It is therefore paramount to add as many systems to this selected group as we can.
In this work, we present a spectral analysis of the high mass
X-ray
binary pulsar 4U 1538-52. It is an eclipsing system consisting of
the B0 I supergiant star QV Nor and a neutron star with an orbital
period of 3.728
days (Clark 2000).
The orbital
eccentricity is
0.08
(Corbet et al. 1993),
although more
recently a higher value of
0.17
was deduced by Clark
(2000). The
X-ray eclipse lasts
0.6
days (Becker et al.
1977). The
system is fairly bright in X-rays.
The estimated flux is
in
the 3-100 keV range (Rodes 2007). Thus,
assuming a
distance of the source of
kpc
(Becker
et al. 1977;
Parkes et al. 1978)
and an isotropic
emission, the luminosity follows
erg/s.
The magnetized neutron star has a spin
period of
529
s (Davison 1977;
Becker et al. 1977).
The pulse-phase averaged X-ray spectrum of 4U 1538-52 has
usually
been described either by an absorbed power law modified by a high
energy cutoff, a power law modified by a Fermi-Dirac cutoff, or by two
power laws with indices of opposite sign multiplied by an exponential
cutoff (the NPEX model, Mihara 1995; Rodes
et al. 2006).
In addition to these continuum models, an iron
fluorescence line at 6.4 keV
and a cyclotron resonant scattering
feature at
20 keV
discovered by Ginga (Clark et al.
1990) are
needed to describe the data. The variability of
this CRSF was studied by Rodes-Roca et al. (2008).
Rossi X-ray Timing Explorer (RXTE) (Coburn 2001) and
BeppoSAX data (Robba et al. 2001) did not show
evidence of the first harmonic at
40 keV. Robba et
al. (2001)
presented some evidence of an absorption feature
around 50 keV; however, because of the lack of a
signal-to-noise ratio of the
spectrum at these energies, the feature could not be confirmed.
In this paper, we report on the 3-100 keV analysis based on the observations of 4U 1538-52 performed by the RXTE and INTEGRAL satellites. In Sect. 2 we describe the observations and data analysis. In Sect. 3 spectral analysis are presented, and summarized in Sect. 4.
2 Observations
2.1 RXTE data
To study the presence of spectral features, we have used all archival data from RXTE on this source: three observations have been carried out in 1996, 1997, and 2001. The first one, is a monthly observation between 1996 November 24 and 1997 December 13. The second and third ones cover a complete orbital period. In our analysis we used data from both RXTE pointing instruments, the Proportional Counter Array (PCA) and the High Energy X-ray Timing Experiment (HEXTE).
To extract the spectra, we used the standard
RXTE analysis software FTOOLS.
This package takes care of the modeling of PCA
background, the dead
time corrections of HEXTE data and generates the
appropriate response matrices
for the spectral analysis.
The PCA consists of five co-aligned Xenon
proportional counter
units with a total effective area of 6000 cm2
and a nominal
energy range from 2 keV to over 60 keV (Jahoda
et al. 1996).
However, because of response problems above
20
keV and the Xenon-K edge around 30 keV, we restricted the use
of the
PCA to the energy range from 3 keV to
20 keV (see also Kreykenbohm et al. 2002).
Systematic uncertainties
are taken into account by the standard spectral analysis.
The HEXTE consists of two clusters of four NaI(Tl)/CsI(Na) Phoswich scintillation detectors with a total net detector area of 1600 cm2. These detectors are sensitive from 15 keV to 250 keV (Rotschild et al. 1998), however, response matrix, instrument background and source count rate, limit the energy range from 17 to 100 keV. Background subtraction in HEXTE is done by source-background swapping of the two clusters every 32 s throughout the observation. For the HEXTE, the response matrices were generated with HXTRSP, version 3.1. We used HXTDEAD version 2.0.0 to correct for the dead time. In order to improve the statistical significance of the data, we added the data of both HEXTE clusters and created an appropriate response matrix by using a 1:0.75 weighting to account for the loss of a detector in the second cluster. We also binned several channels together of the HEXTE data at higher energies and chose the binning as a compromise between increased statistical significance while retaining a reasonable energy resolution.
Table 1: Details of observations.
2.2 INTEGRAL data
INTEGRAL (Winkler
et al. 2003) has a unique broad band capability
thanks to its four science instruments (imager IBIS,
spectrometer SPI, X-ray monitor JEM-X,
and optical
monitor OMC) which allow us to study a source from
3 keV up to
10 MeV and in the optical simultaneously. The imager IBIS
has
a very large field of view of
which allows us to
observe many sources at the same time. Together with a large
collecting area of
and decent energy resolution of 9% at
100 keV makes IBIS the prime instrument
for our analysis.
Since its launch on October 17, 2002, INTEGRAL observatory has been constantly collecting a wealth of data. INTEGRAL data are organized in revolutions (i.e. 72 h long satellite orbits around the Earth) and then science windows which are typically 1800 s to 3600 s long.
The source was observed by the hard X-ray imager (IBIS) camera on board INTEGRAL during the regular scans of the Galactic plane and the Norma survey. Figure 2 shows an IBIS/ISGRI mosaic image of the Norma Arm region in the energy range 20-100 keV. The source 4U 1538-52 (labelled as H 1538-522) is clearly detected and its position is well determined, allowing us to extract its spectrum without contamination of other sources in the field of view of the instrument.
![]() |
Figure 1:
Combined spectrum and model of data obtained with PCA
(3-20 keV) and HEXTE
(17-100 keV). Both data sets belong to the run carried out in
2001 and their orbital phases are 0.53 and 0.66, respectively.
Bottom panels show the residuals in units of |
Open with DEXTER |
To extract INTEGRAL data, we used the Offline
Science
Analysis Software (OSA) version 7.0, as distributed by the Integral
Science Data Centre (ISDC) following the respective
cookbook
instructions. For IBIS, we selected all public data
up to
revolution 400 with the source in the fully coded field of
view of the
instrument, resulting in
400
Science Windows (ScWs). In a first
step we created a mosaic of the full data set to obtain a catalog of
the detected sources in the field of view. Since 4U 1538-522
is
relatively close to the galactic centre, the catalog contains other 15
sources, among them several bright sources such as
4U 1700-377. We
then used this catalog to extract the spectrum of 4U 1538-522
using
all 400 ScWs in order to obtain a high signal-to-noise ratio.
Since all
other sources in the field are several degrees away, source confusion
is not a problem. For JEM-X we used all data
of monitor number one (JEM-X 1) within 2
to ensure a
reliable spectrum resulting in approximately 55 ScWs. And
for SPI, the selection of all available data within
a 8
radius (the
fully coded field of view of the instrument) allowed us to obtain
969 ScWs. The selected spectra then have an effective exposure
time of 720 ksec for IBIS,
1907 ksec for SPI, and
360 ksec for JEM-X.
See Table 1 for the details of all observations which have been used in this work.
Table 2: Fitted parameters for the RXTE spectra in Fig. 1.
3 Spectral analysis
For spectral analysis we used the XSPEC (Arnaud 1996) fitting package, released as a part of XANADU in the HEASoft tools.
3.1 RXTE analysis
Figure 1
shows PCA and HEXTE
phase-averaged spectrum at
orbital phases 0.53 (left panel) and 0.66 (right panel). The raw data
together the best-fit model and the residuals of the fit as the
difference
between observed flux and model flux divided by the uncertainty of the
observed flux, i.e. in units of ,
are included in this plot. The dip
of the second cyclotron line at
47 keV is apparent in
the raw data.
The RXTE continuum is properly described by an
absorbed powerlaw modified
by an exponential cutoff at
keV
( CUTOFFPL in XSPEC, Arnaud 1996), see
Table 2.
Analytically, CUTOFFPL is given by the
equation,
![]() |
(1) |
where



![[*]](/icons/foot_motif.png)
A significant absorption feature is present in the residuals around
47 keV.
When other models are used to describe the underlying
continuum, i.e. an absorbed powerlaw with a Fermi-Dirac cutoff
(Tanaka 1986)
or the
NPEX model (Mihara 1995),
the overall residuals were higher,
but none of them was
able to account for the absorption feature at
47 keV.
![]() |
Figure 2: IBIS/ISGRI mosaic image of the Norma Arm region where the source is located and clearly detected. |
Open with DEXTER |
![]() |
Figure 3:
Combined spectrum and model obtained with JEM-X (left),
ISGRI (upper right), and SPI
(lower right). The continuum is modeled by the CUTOFFPL
model without any cyclotron lines applied. The bottom panel
shows the residuals in units of |
Open with DEXTER |
3.2 INTEGRAL analysis
In Fig. 3,
we present the combined JEM-X,
ISGRI and SPI spectrum using all
data. The spectra of
all three instruments were fitted simultaneously with a
CUTOFFPL model, using the latest response
matrices
provided by the OSA software (see Sect. 2.2 for more
details).
A factor term was included in the model to
allow for the adjustment of efficiencies between different instruments.
No
photoelectric absorption has been used since the INTEGRAL
spectra start only at 4 keV and none was required by the data.
An
absorption column below
is expected to have no
noticeable effect below 5 keV. Nevertheless JEM-X
data are needed to constrain the X-ray continuum
model.
Likewise, neither the very broad
Gaussian at 12 keV, nor the iron fluorescence line at
6.4 keV are
required by the JEM-X data and were therefore not
added to the
model. As can clearly be seen in Fig. 3, significant
absorption line structures are present at
20 keV (the well
known CRSF) and
keV
after fitting the continuum with a cutoffpl model (best-fit parameters
of continuum are given in Table 3). Data from
JEM-X, ISGRI and SPI
have been fitted simultaneously.
Table 3: Fitted parameters for the INTEGRAL spectrum in Fig. 3.
3.3 Combined RXTE and INTEGRAL analysis
To further explore this second feature and in order to achieve the
highest significance at high energies, we jointly fitted the data of
the high energy instruments of the two satellites, HEXTE,
ISGRI, and SPI. We fixed the
continuum parameters
,
the power law photon index and
,
the cutoff energy
of the exponential cutoff, to the values given
in Table 3.
In Table 4 we show the best fit parameters for each spectrum we used in Fig. 4. Data from SPI, ISGRI and HEXTE have been fitted individually. As the continuum parameters are frozen, we have not included them in this table. The results of the spectral fits from three different instruments show that the values describing the shape of the cyclotron lines are consistent with one to another within uncertainties.
![]() |
Figure 4:
Spectra and continuum model (cutoffpl) obtained with ISGRI,
SPI (lower), and HEXTE.
The bottom panel shows the residuals in units of |
Open with DEXTER |
Table 4: Fitted parameters for the fundamental and the first harmonic CRSF.
As evident from Fig. 4, the two
cyclotron
absorption features are clearly seen in the raw data of the three
instruments. Although
SPI has a very high energy resolution, the compared
to
ISGRI rather low signal-to-noise ratio required the
use of
rather broad energy bins. Therefore we will use ISGRI
as the
prime instrument in our study together with HEXTE
while
SPI data will be used for comparison. In summary, to
get the
best fit parameters of the absorption features, we have combined
ISGRI and HEXTE data including a
factor for free
normalization between the two instruments (see Fig. 5 top panel).
The two absorption features at 22 keV and
47 keV
are modeled using the CYCLABS model from
XSPEC (Arnaud 1996).
We started by modeling the fundamental cyclotron line that was
discovered by the Ginga satellite observatory
(Clark et al. 1990
see Fig. 5
second panel). After the
inclusion of the fundamental cyclotron line at
keV,
the
improves from 5.5 for
47 degrees of freedom (d.o.f.) to
3.4, for 44 dof (F-test:
).
Although residuals improve significantly
(see Fig. 5
third panel),
another absorption feature can be seen at
47 keV.
Including a second
cyclotron line at
keV
improves the fit further resulting in a
of 1.4 for 41 d.o.f. (F-test:
see
Fig. 5
bottom panel).
ISGRI data (filled grey circles in Fig. 5)
has a far better resolution than HEXTE at these
energies. However,
the overall shape is virtually identical, ruling out any instrumental
or
circumstantial effects.
The final fit parameters are given in Table 5.
Data from HEXTE and ISGRI have
been fitted simultaneously.
![]() |
Figure 5:
Cyclotron line modeling of the phase-averaged spectra HEXTE/ISGRI
of 4U 1538-52. Top panel: spectra and best fit
model (cutoffpl and two cyclotron lines) obtained with HEXTE
and ISGRI. Bottom panels show the residuals in
units of |
Open with DEXTER |
The F-test is known to be problematic when used to test the significance of an additional spectral feature (see Protassov & van Dik 2002), even if systematic uncertainties are not an issue. However, the low false alarm probabilities may make the detection of the line stable against even crude mistakes in the computation of the significance (Kreykenbohm 2004). Therefore, taking into account these caveats, we can conclude that the the first harmonic CRSF is detected with high significance in the spectrum of this source.
Table 5: Best fit parameters for the fundamental and the first harmonic CRSF.
Although the uncertainties of the determined values are rather
large,
these values are consistent with one another within uncertainties.
This makes it extremely unlikely that the 47 keV
feature results from a calibration problem.
Nevertheless, the line
parameters depend slightly on the shape of the continuum (for example,
using the NPEX component (Mihara 1995) and two
cyclotron absorption lines,
we obtained the line centre energies at
22 keV and
44 keV,
for the fundamental and first harmonic respectively).
In short, this feature has been found to be present under the following circumstances:
- three different telescopes and instruments: Narrow Field Instruments (NFIs) on board BeppoSAX (Robba et al. 2001), HEXTE on board RXTE, and IBIS/ISGRI on board INTEGRAL (this work);
- different epochs within the same telescope (i.e. 1996, 1997, 2001 using RXTE);
- different orbital phases within a given epoch and instrument (Fig. 1).
4 Summary and discussion
We presented the spectral analysis of 4U 1538-52 using data
from
RXTE and INTEGRAL. We present
evidence for a previously
unknown absorption line like feature in the phase-averaged spectrum of
the source. As we have shown in Sect. 3, we have been
able to achieve a good fit to the phase-averaged spectra by including
a Lorentzian absorption line at 47 keV into the model
(see
Fig. 5).
This absorption line is clearly
visible whenever the signal-to-noise ratio in the spectrum is good
enough to allow an analysis of the data. The most straightforward
interpretation for this feature is that it is the first harmonic of
the
22 keV
fundamental CRSF.
According to the theory, cyclotron lines are due to the
resonant
scattering of photons by electrons whose energies are quantized into
Landau levels by the magnetic field (Mészáros
1992). The
quantized energy levels of the electrons are
harmonically spaced in the first order, such that the first harmonic
line should be placed at twice the energy of the fundamental line,
i.e. keV.
In reality, however, the
coupling factor between the fundamental and first harmonic is with
slightly higher than 2.0. This
anharmonic spacing,
however, has been observed already in several systems where more than
one line is present. As explained by Schönherr et al. (2007), the
relativistic photon-electron scattering already produces some
anharmonicity, because photons with energies close to the Landau
levels may not escape the plasma if their energies are not changed by
inelastic scattering. This, however, can not be the only reason
because some systems show an anharmonic spacing larger than that
predicted by this effect. A possibility to explain this difference is
to take into account that the optical depths of the fundamental and
the first harmonic could be different if they are formed at different
heights above the neutron star. With increasing height, the strength
of the magnetic field decreases resulting in a different CRSF
energy. Another possibility is to consider a displacement of the
magnetic dipole which would also explain the difference of energy of
the two lines if the lines originate from the different poles of the
neutron star. Therefore a significant phase dependence of the strength
of the both lines is expected, however, the low signal-to-noise ratio
at
higher energies prevents us to test this hypothesis with the current
data sets.
We are grateful to the anonymous referee for useful and detailed comments. Part of this work was supported by the Spanish Ministry of Education and Science Primera ciencia con el GTC: La astronomía española en vanguardia de la astronomía europea CSD200670 and Multiplicidad y evolución de estrellas masivas project number AYA200806166C0303. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center and through the INTEGRAL Science Data Center (ISDC), Versoix, Switzerland. S.M.N. is a researcher of the Programme Juan de la Cierva, funded by the MICINN. J.M.T. acknowledges the support by the Spanish Ministerio de Educación y Ciencia (MEC) under grant PR2007-0176. A.C.A. thanks for the support of this project to the Spanish Ministerio de Ciencia e Innovación through the 2008 postdoctoral program MICINN/Fulbright under grant 2008-0116. J.J.R.R. acknowledges the support by the Spanish Ministerio de Educación y Ciencia (MEC) under grant PR2009-0455.
References
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Footnotes
- ... USA
- Fundación Española de Ciencia y Tecnología, C/ Rosario Pino, 14-16, 28020 Madrid, Spain.
- ... FTOOLS
- Available at http://heasarc.gsfc.nasa.gov
- ...
cookbook
- Available at http://isdc.unige.ch
- ... limit
- Also in Tables 3, 4 and 5.
All Tables
Table 1: Details of observations.
Table 2: Fitted parameters for the RXTE spectra in Fig. 1.
Table 3: Fitted parameters for the INTEGRAL spectrum in Fig. 3.
Table 4: Fitted parameters for the fundamental and the first harmonic CRSF.
Table 5: Best fit parameters for the fundamental and the first harmonic CRSF.
All Figures
![]() |
Figure 1:
Combined spectrum and model of data obtained with PCA
(3-20 keV) and HEXTE
(17-100 keV). Both data sets belong to the run carried out in
2001 and their orbital phases are 0.53 and 0.66, respectively.
Bottom panels show the residuals in units of |
Open with DEXTER | |
In the text |
![]() |
Figure 2: IBIS/ISGRI mosaic image of the Norma Arm region where the source is located and clearly detected. |
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Combined spectrum and model obtained with JEM-X (left),
ISGRI (upper right), and SPI
(lower right). The continuum is modeled by the CUTOFFPL
model without any cyclotron lines applied. The bottom panel
shows the residuals in units of |
Open with DEXTER | |
In the text |
![]() |
Figure 4:
Spectra and continuum model (cutoffpl) obtained with ISGRI,
SPI (lower), and HEXTE.
The bottom panel shows the residuals in units of |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Cyclotron line modeling of the phase-averaged spectra HEXTE/ISGRI
of 4U 1538-52. Top panel: spectra and best fit
model (cutoffpl and two cyclotron lines) obtained with HEXTE
and ISGRI. Bottom panels show the residuals in
units of |
Open with DEXTER | |
In the text |
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