A ionized reflecting skin above the accretion disk of GX 349+2

R. Iaria; A. D'Aí; T. Di Salvo; N. R. Robba; A. Riggio; A. Papitto; L. Burderi

doi:10.1051/0004-6361/200911936

Free Access

Issue		A&A Volume 505, Number 3, October III 2009


Page(s)		1143 - 1151
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/200911936
Published online		11 August 2009

A ionized reflecting skin above the accretion disk of GX 349+2

R. Iaria¹ - A. D'Aí¹ - T. Di Salvo¹ - N. R. Robba¹ - A. Riggio² - A. Papitto² - L. Burderi²

1 - Dipartimento di Scienze Fisiche ed Astronomiche, Università di Palermo, via Archirafi 36, 90123 Palermo, Italy
2 - Dipartimento di Fisica, Università degli Studi di Cagliari, SP Monserrato-Sestu, KM 0.7, 09042 Monserrato, Italy

Received 24 February 2009 / Accepted 13 June 2009

Abstract
Context. The broad emission features in the Fe-K $\alpha$ region of X-ray binary spectra represent an invaluable probe to constrain the geometry and the physics of these systems. Several Low Mass X-ray binary systems (LMXBs) containing a neutron star (NS) show broad emission features between 6 and 7 keV and most of them are now interpreted as reflection features from the inner part of an accretion disk, in analogy to those observed in the spectra of X-ray binary systems containing a black bole candidate.
Aims. The NS LMXB GX 349+2 was observed by the XMM-Newton satellite which allows, thanks to its high effective area and good spectral resolution between 6 and 7 keV, a detailed spectroscopic study of the Fe-K $\alpha$ region.
Methods. We study the XMM data in the 0.7-10 keV energy band. The continuum emission is modelled by a blackbody component plus a multicolored disk blackbody. A very intense emission line at 1 keV, three broad emission features at 2.63, 3.32, 3.9 keV and a broader emission feature in the Fe-K $\alpha$ region are present in the residuals. The broad emission features above 2 keV can be equivalently well fitted with Gaussian profiles or relativistic smeared lines (diskline in XSPEC). The Fe-K $\alpha$ feature is better fitted using a diskline component at 6.76 keV or two diskline components at 6.7 and 6.97 keV, respectively
Results. The emission features are interpreted as resonant transitions of S XVI, Ar XVIII, Ca XIX, and highly ionized iron. Modelling the line profiles with relativistic smeared lines, we find that the reflecting plasma is located at less than 40 km from the NS, a value compatible with the inner radius of the accretion disk inferred from the multicolored disk blackbody component ( $24 \pm 7$ km). The inclination angle of GX 349+2 is between 40 $^\circ$ and 47 $^\circ$ , the emissivity index of the primary emission is between -2.4 and -2, and the reflecting plasma extends up to (2-8) $\times 10^8$ cm.
Conclusions. We compare our results with the twin source Sco X-1 and with the other NS LMXBs showing broad relativistic lines in their spectra. We conclude that the blackbody component in the spectrum is the primary emission that hits the inner accretion disk producing the emission lines broadened by relativistic and Doppler effects dominant around the neutron star.

Key words: line: identification - line: formation - stars: individual GX 349+2 - X-rays: binaries - X-rays: general

1 Introduction

Low-mass X-ray binaries (LMXBs) consist of a low-mass star ( $M<1~M_{\odot}$ ) and a neutron star (NS), which generally has a relatively weak magnetic field (B<10¹⁰ G). In these systems, the X-ray source is powered by accretion of mass overflowing the Roche lobe of the companion star and forming an accretion disk around the neutron star. LMXBs containing a neutron star (NS LMXBs) are generally divided into Z and Atoll sources, according to the path they describe in an X-ray color-color diagram (CD) or hardness-intensity diagram (Hasinger & van der Klis 1989) assembled by using the source count rate and colors calculated over a typical (usually 2-20 keV) X-ray energy range. Atoll sources are usually characterized by relatively low luminosities (0.01-0.2 $L_{\rm Edd}$ ) and often show transient behavior, while the Z sources in the Galaxy are among the most luminous LMXBs, persistently accreting close to the Eddington limit ( $L_{\rm Edd}$ ) for a 1.4 $M_{\odot}$ NS. The position of an individual source in the CD, which determines most of the observed spectral and temporal properties of the source, is thought to be an indicator of the instantaneous mass accretion rate (e.g. Hasinger et al. 1990; van der Klis 1995, for a review). It has been suggested that the mass accretion rate (but not necessarily the X-ray luminosity) of individual sources increases along the track from the top left to the bottom right, i.e. from the islands to the banana branch in atoll sources and from the horizontal branch (hereafter HB) to the normal branch (NB) and to the flaring branch (FB) in Z sources.

GX 349+2, also known as Sco X-2, was called a peculiar case among the Z sources (Kuulkers & van der Klis 1998). Similar to the case of Sco X-1, GX 349+2 shows a short and underdeveloped HB (if at all). The source variability in the frequency range below 100 Hz is closely correlated with the source position on the X-ray CD, as in other Z sources. Quasi periodic oscillations at kHz frequencies (kHz QPO) were detected in the NB of its Z-track (Zhang et al. 1998). However, GX 349+2, which sometimes shows broad noise components changing not only with the position in the Z, but also as a function of the position in the hardness-intensity diagram, differs somewhat from the other Z sources and shows similarities to the behavior seen in bright atoll sources, such as GX 13+1 and GX 3+1 (O'Neill et al. 2001,2002; Kuulkers & van der Klis 1998).

Di Salvo et al. (2001), using BeppoSAX data, showed that the source energy spectrum below 30 keV could be well fit by a blackbody (with a temperature of 0.5-0.6 keV) and a Comptonized component (with seed-photon temperature of 1 keV and electron temperature of 2.7 keV). Three discrete features were observed in the spectrum: an emission line at 1.2 keV, probably associated with L-shell Fe XXIV or Ly- $\alpha$ Ne X, an emission line at 6.7 keV (Fe XXV) and an absorption edge at 8.5 keV, both corresponding to emission from the K-shell of highly-ionized iron (Fe XXV). Iaria et al. (2004), analysing a long BeppoSAX observation, found similar parameters of the the continuum components below 30 keV, detected the presence of emission lines associated with Fe XXIV and Fe XXV, and detected an emission line at 2.65 keV associated with S XVI. The long BeppoSAX observation allowed us to study changes of the parameters of the Fe XXV emission line along the position of the source in the CD from the NB/FB apex to the FB, inferring that the equivalent width of the line decreases from 77 eV to 18 eV going from the NB/FB apex to the FB. The width of the Fe XXV emission line, modelled by a Gaussian line, was between 250 and 300 eV.

Cackett et al. (2008), analysing two Suzaku observations of GX 349+2, modelled the Fe XXV emission line with a relativistic smeared line (diskline in XSPEC). The authors constrained the energy of the line to be between 6.4 and 6.97 keV, finding that the line energy was 6.97_-0.02 keV, associated with Fe XXVI and not compatible with a Fe XXV iron line as previously obtained by Iaria et al. (2004) and Di Salvo et al. (2001). The emissivity index, $\beta$ , was $-4.1 \pm 0.3$ , the inner radius in gravitational radii, $R_{\rm g}$ , was $8.0 \pm 0.4$ , the inclination angle of the source was $23 \pm 1$ degrees, the equivalent width of the line was $76 \pm 6$ eV.

In this paper, we analyse an XMM-Newton observation of GX 349+2, finding that the prominent relativistic line is well constrained around 6.7 keV and identified as the resonant transition of Fe XXV. In the following, we discuss our results and compare them with the recent literature.

2 Observation

The XMM-Newton Observatory (Jansen et al. 2001) includes three 1500 cm²X-ray telescopes each with an European Photon Imaging Camera (EPIC, 0.1-15 keV) at the focus. Two of the EPIC imaging spectrometers use MOS CCDs (Turner et al. 2001) and one uses pn CCDs (Strüder et al. 2001). Reflection grating spectrometers (RGS, 0.35-2.5 keV, den Herder et al. 2001) are located behind two of the telescopes. The region of sky containing GX 349+2 was observed by XMM-Newton between 2008 March 19 16:42:41 UT to March 19 22:58:55 UT (OBSid 0506110101) for a duration of 22.5 ks. Since GX 349+2 is one of the brightest X-ray sources, in order to minimize the effects of telemetry saturation and pile-up, the MOS1 and MOS2 instruments were switched off and the EPIC-pn camera was operated in Timing mode with medium filter during the observation. In this mode, only one central CCD is read out with a time resolution of 0.03 ms. This provides a one dimensional (4 $.\mkern-4mu^\prime$ 4 wide) image of the source with the second spatial dimension being replaced by timing information. The faster CCD readout results in a much higher count rate capability of 1500 cts/s before charge pile-up becomes a serious problem for point-like sources. The EPIC-pn telemetry limit is approximatively 450 c/s for the timing mode. If the rate is higher, then the counting mode is triggered and part of the science data are lost. This is the case for the observation presented in this work; saturation occurs for 55% of the observing time, giving an exposure time of 22.5 ks for RGS1 and RGS2, respectively, and 10 ks for EPIC-pn.

$\begin{figure} \includegraphics[width=9cm,clip]{11936fg1.ps} \end{figure}$	Figure 1: Epic-pn lightcurve of GX 349+2 in the energy band 1-10 keV. The bin time is 30 s.
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$\begin{figure} \includegraphics[width=9cm,clip]{11936fg2.ps} \end{figure}$	Figure 2: Color-intensity diagram of GX 349+2. The [4-10 keV]/[1-4 keV] hardness ratio increases for a count rate lower than 1580 c/s. The bin time is 100 s.
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We plot the Epic-pn lightcurve in the 1-10 keV energy range in Fig. 1 which clearly shows that the count rate is largely variable. To understand whether the variability of the source intensity is energy dependent, we extract the lightcurves in the 1-4 keV and 4-10 keV energy range, respectively, and plot the hardness ratio [4-10 keV]/[1-4 keV] versus the count rate in the 1-10 keV energy range in Fig. 2. We find that the spectrum becomes harder for a count rate below 1580 c/s corresponding to the time interval between 10⁴ and $1.5 \times 10^4$ s from the start of the observation.

$\begin{figure} \includegraphics[width=9cm,clip]{11936fg3.ps} \end{figure}$	Figure 3: Upper panel: 1-4 keV Epic-pn lightcurve. Middle panel: 4-10 keV Epic-pn lightcurve. Bottom panel: [4-10 keV]/[1-4 keV] hardness ratio. The bin time is 30 s for each lightcurve. The red dot-dashed vertical lines indicate the three selected time intervals.
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Plotting the 1-4 keV, 4-10 keV lightcurve and the [4-10 keV]/[1-4 keV] hardness ratio versus time (see Fig. 3), it seems that there is no correlation between the 1-4 keV and 4-10 keV count rate. The 1-4 keV count rate is quite constant at 1200 c/s between 0 and $9 \times 10^3$ s and between $1.5 \times 10^4$ and $2.2 \times 10^4$ s from the start, and it decreases between $9 \times 10^3$ and $1.5 \times 10^4$ s, showing some flaring activity. The 4-10 keV count rate is quite constant at 530-550 c/s between 0 and $6 \times 10^3$ s and between $1.9 \times 10^4$ and $2.25 \times 10^4$ s, while it increases to 600 c/s between $6 \times 10^3$ and $1.9 \times 10^4$ s.

Since the count rate of the source is variable, we divide the lightcurve into three time intervals as indicated in Fig. 3 by the red dot-dashed lines. We base our choice on the 4-10 keV count rate that is 550 c/s in the first and third time interval and around 600 c/s in the second time interval. Our choice allows us to highlight possible changes in the Fe-K $\alpha$ region of the spectrum. In Table 1 we report the exposure times of the selected time intervals for RGS1, RGS2 and EPIC-pn instruments.

Table 1: Time intervals selected in the EPIC-pn lightcurve.

2.1 Spectral analysis of the averaged spectrum

We extract the X-ray data products of the RGS and EPIC-pn cameras using the Science Analysis Software (SAS) version 8.0.0, extracting only single and double events (patterns 0 to 4) from EPIC-pn data. Initially we extracted source EPIC-pn events from a $69.7\hbox{$^{\prime\prime}$ }$ wide column (RAWX between 29 and 45) centered on the source position (RAWX =37). Background events were obtained from a box of the same width with RAWX between 2 and 18.

Table 2: Percentage of photon pile-up at different energies.

The 0.5-12 keV Epic-pn count rate extracted from the source region is almost 1800 c/s; since the maximum Epic-pn count rate should be 800 c/s to avoid a deteriorated response due to photon pile-up, we expect the presence of pile-up. We checked the pile-up fraction at different energies using the epatplot tool in SAS, finding a photon pile-up percentage of 1.3%, 2%, 3.2%, 5.1%, 7.4%, and 9.8% at 5, 6, 7, 8, 9, and 10 keV, respectively. The values with the associated errors are reported in Table 2. Since our aim is the study of the Fe-K $\alpha$ region of the spectrum, we investigated how to minimize the photon pile-up effects in the energy range 5-8 keV. Initially we extracted the source EPIC-pn spectrum, excluding the brightest column (RAWX =37) in the CCD. The photon pile-up fraction did not change significantly; we obtained a photon pile-up percentage of 1.1%, 1.7%, 3.1%, 4.7%, 6.7%, and 9.2% at 5, 6, 7, 8, 9, and 10 keV. Finally, excluding the two brightest columns at RAWX =37 and RAWX =38, we found a photon pile-up fraction of 0.2%, 0.6%, 1.6%, 1.9%, 4.8%, and 6.5% at 5, 6, 7, 8, 9, and 10 keV. In this case, the 0.5-12 keV Epic-pn count rate is 920 c/s. The photon pile-up percentage values with the associated errors are reported in Table 2 and the plot of the fraction patterns of single and double events are shown in Fig. 4. After this investigation, we chose to extract the Epic-pn spectrum excluding the two brightest columns at RAWX =37 and RAWX =38 from the source region to avoid any doubt on the validity of our analysis.

Since the high available statistics, the EPIC-pn spectrum shows evident calibration issues between 2 and 2.5 keV due to the Au edge near 2.3 keV, we excluded the EPIC-pn data between 2.1 and 2.5 keV from our analysis. The EPIC-pn spectrum has been rebinned so as not to oversample the energy resolution by more than a factor of 4 and to have 20 counts per energy channel. The adopted Epic-pn energy range is 0.7-2.1 keV and 2.5-10 keV. The spectrum is fitted using XSPEC version 12.3.1

The extracted RGS1 spectrum does not show instrumental issues and we select data in the 0.6-2 keV energy band for our analysis. The extracted RGS2 spectrum shows calibration problems for CCD 9 and we will not use data from this instrument for our analysis. Since we are interested in the study of the Fe-K $\alpha$ region, in the following we concentrate our spectral analysis on the Epic-pn data, after having checked that the RGS1 spectrum is consistent with the Epic-pn data and does not show more features.

$\begin{figure} \par\includegraphics[width=9cm,clip]{11936fg4.ps} \end{figure}$	Figure 4: Patterns of single (blue color) and double (red color) events extracted from the source region excluding RAWX 37 and 38. The patterns are plotted versus the 60-2000 ADU channel range, corresponding to 0.3-10 keV.
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$\begin{figure} \includegraphics[width=9cm,clip]{11936fg5.ps} \end{figure}$	Figure 5: Residuals (in units of $\sigma$ ) in the 0.7-10 keV energy range. The adopted continuum is composed of blackbody plus a multicolored disk blackbody, both absorbed by neutral matter. In the residuals, clear emission features are evident at 1, 2.7, 3.35, 3.9 and in the Fe-K $\alpha$ region of the spectrum.
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Table 3: Averaged continuum and identified broad Gaussian lines below 6 keV.

The continuum emission was fitted adopting the model by Cackett et al. (2008) for the Suzaku spectrum of GX 349+2: i.e. a blackbody component plus a multicolored disk blackbody (DISKBB in XSPEC) both absorbed by neutral neutral matter (WABS in XSPEC); because of the narrower energy range of our Epic-pn data (0.7-10 keV) with respect to the Suzaku data we did not add to the model a power-law component necessary to fit the Suzaku data above 10 keV. We obtained a reduced $\chi^2_{\rm red}= 7.73$ with 282 degree of freedom (d.o.f.). The residuals, plotted in Fig. 5, suggest the presence of broad emission lines at 1, 2.7, 3.35, 3.9 keV and, finally a broader emission line between 6 and 7 keV. Initially, we added five Gaussian components to fit these emission features. Since the line around 2.7 keV is near the hole in the Epic-pn data, we fixed the energy of the line at 2.62 keV, imposing that it is associated with the Ly- $\alpha$ S XVI transition; furthermore we fixed its width at 140 eV. We obtain a $\chi^2_{\rm red}({\rm d.o.f.})= 1.51(269)$ and a $\chi^2$ improvement of $\Delta \chi^2 = 1775$ . The significance in units of $\sigma$ of the lines at 1, 2.62, 3.32, 3.9, and 6.7 keV is 14, 7, 15, 9, and 13, respectively. The best-fit values are reported in Tables 3 (Col. 2) and 4 (Col. 2). We identify the broad emission lines centered at 1.051^+0.006_-0.015 keV, 3.33^+0.03_-0.04 keV, and 3.93^+0.03_-0.02 keV as Fe XXII transition, Ly- $\alpha$ Ar XVIII transition, and resonance transition of Ca XIX, respectively. The centroid of the broader line between 6 and 7 keV is not identifiable because we find a line centered at $6.80 \pm 0.02$ keV. We also note that, while the FWHMs of the broad lines below 6 keV are between 0.2 and 0.4 keV, the broader line in the Fe-K $\alpha$ region has a FWHM of 0.6-0.7 keV (the line profile is visible in the residuals shown in Fig. 6).

We have also investigated the possibility that the Fe-K $\alpha$ feature is a blending of lines. We fitted the broad Fe-K $\alpha$ emission feature as a blending of Fe XXV (6.7 keV) and Fe XXVI (6.97 keV) emission lines adopting two Gaussian profiles and fixing their energies at the expected rest-frame values; the values of the fit are reported in Tables 3 (Col. 3) and 4 (Col. 3). Even in this case the Fe XXV and Fe XXVI emission lines appear to be broad, having widths of 200 eV (FWHM=0.5 keV).

$\begin{figure} \par\includegraphics[width=9cm,clip]{11936fg6.ps} \end{figure}$	Figure 6: Residuals in the 5.5-7.7 keV energy range. These can be fitted adopting a Gaussian profile or, equivalently, a relativistic smeared line (diskline in XSPEC)
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Table 4: Broad Gaussian lines between 6 and 7 keV.

Under the hypothesis that the broadening of the lines is produced by the relativistic motion of the emitting plasma in the accretion disk close to the neutron star, we fit the line profiles at 2.62, 3.32, 3.90, and 6.80 keV with relativistic disk line components (DISKLINE in XSPEC). Assuming that the emission features are produced in the same region, we impose that the inner radius, the outer radius, the emissivity index, and the inclination angle of the system are the same for all these components. Adding these components to the continuum emission we find a slightly better fit, $\chi^2_{\rm red}({\rm d.o.f.})= 1.47(268)$ .

Table 5: Best-fit values of the parameters obtained fitting the emission features with relativistic smeared lines (diskline in XSPEC). The Fe-K $\alpha$ feature is modelled with one diskline component.

$\begin{figure} \par\includegraphics[width=9cm,clip]{11936fg7.ps} \end{figure}$	Figure 7: Data, model, and residuals (in units of $\sigma$ ) in the 0.7-10 keV energy range after adding the disk line components discussed in the text.
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$\begin{figure} \includegraphics[width=9cm,clip]{11936fg8.ps} \end{figure}$	Figure 8: Unfolded spectrum in the energy range 5.5-7.7 keV; the Fe XXV relativistic line profile is shown.
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Table 6: Best-fit values of the parameters obtained fitting the emission features with relativistic smeared lines (diskline in XSPEC). The Fe-K $\alpha$ feature is modelled with two diskline components.

We find that the emissivity index of the accretion disk is -2.1, the inner radius is less than 25 gravitational radii (GM/c², hereafter $R_{\rm g}$ ), corresponding to 52 km for a NS mass of 1.4 $M_{\odot}$ , and the inclination angle of the system is 41 $^\circ$ . The best-fit values of the parameters are reported in Table 5 (Col. 2); we plot data and residuals in the 0.7-10 keV energy band and the corresponding unfolded spectrum in the Fe-K $\alpha$ region in Figs. 7 and 8, respectively.

The Fe-K $\alpha$ line has an energy of $6.76 \pm 0.02$ keV and it is not compatible (at a 90% confidence level) with the rest-frame value of the Fe XXV transition (6.7 keV). We therefore tried to fit the Fe-K $\alpha$ broad feature adopting two diskline components associated with Fe XXV and Fe XXVI transitions. We fixed the energy values at 6.7 and 6.97 keV, respectively. The best-fit parameters are reported in Table 6 (Col. 2); in this case we obtain $\chi^2_{\rm red}({\rm d.o.f.})= 1.48(268)$ and similar parameters of the emissivity index and inclination angle of the source. We find an emissivity index of $-2.2 \pm 0.2$ , an inner radius less than 26 $R_{\rm g}$ , corresponding to 52 km for a NS mass of 1.4 $M_{\odot}$ , and an inclination angle of the system of $43^{\rm +4}_{-3}$ deg.

The extrapolated absorbed and unabsorbed flux in the 0.1-100 keV energy range was $1.2~\times~10^{-8}$ and $1.4~\times~10^{-8}$ erg cm^-2 s^-1, respectively. We obtain an equivalent hydrogen column density of $0.74~\times~10^{22}$ cm^-2; the same value was obtained by Christian & Swank (1997) using the Einstein solid-state spectrometer (SSS; 0.5-4.5 keV), estimating a distance to the source of $5~\pm~1.5$ kpc (hereafter we will use this distance). Adopting this value as the distance to the source, the extrapolated unabsorbed luminosity in the 0.1-100 keV energy range was $4.3~\times~10^{37}$ erg s^-1.

2.2 Spectral analysis of the selected time intervals

To study possible changes of the broad emission line in the Fe-K $\alpha$ region of the XMM spectrum of GX 349+2, we extracted the EPIC-pn spectrum from interval 2 (Spectrum 2) and from intervals 1 and 3 together (Spectrum 1+3). Since the 4-10 keV lightcurve (Fig. 3, middle panel) indicates a higher count rate in time interval 2 than in intervals 1 and 3, we expect a harder spectrum corresponding to interval 2. The lower statistics in the time-selected spectra, due to the lower exposure times, requires that we fix some parameters of the diskline components. We fixed the outer radius and the inclination angle of the system to the values obtained fitting the spectrum corresponding to the whole observation. Initially we adopted only a diskline component to fit the Fe-K $\alpha$ broad feature, obtaining an energy value of $6.74 \pm 0.04$ and $6.78 \pm 0.03$ keV corresponding to Spectrum 1+3 and 2, respectively. We note that while the line energy is compatible with Fe XXV transition for Spectrum 1+3, it is not compatible for Spectrum 2, which is when the count rate in the 4-10 keV energy band increases. The best-fit values are reported in Table 5 (Cols. 3 and 4).

As a consequence of this result, we fitted the Fe-K $\alpha$ broad feature in Spectra 2 and 1+3 adopting two diskline components with energies fixed at 6.7 and 6.97 keV. Also in this case we fixed the outer radius and the inclination angle of the system to the values obtained fitting the average spectrum. The best-fit values are reported in Table 6 (Cols. 3 and 4). We find that the main differences between Spectrum 1+3 and Spectrum 2 is the value of the blackbody normalization that is larger in Spectrum 2. Also we note that the flux of the line at 1 keV, the S XVI line, the Ar XVIII line, the Ca XIX line, and Fe XXV line is lower in Spectrum 2 than Spectrum 1+3 while the flux of the Fe XXVI line is larger in Spectrum 2 than Spectrum 1+3. In the following section we discuss these results.

3 Discussion

We performed a spectral analysis of a 22.5 ks XMM observation of GX 349+2 in the 0.7-10 keV energy range. The large flux from the source caused a telemetry overflow in the EPIC-pn data collection, resulting in an effective exposure time of 10 ks. We fit the continuum emission, adopting a blackbody plus a multicolored disk blackbody and both these components are absorbed by neutral matter. Five emission features were clearly visible in the spectrum.

Initially we fitted these features using Gaussian profiles and finding their energies at 1.05, 2.62 (fixed), 3.32, 3.9, and 6.8 keV. The corresponding widths and equivalent width were 90, 140 (fixed), 190, 100, and 280 eV, respectively, and 22, 6, 12, 9 and 49 eV, respectively. We associated the first four lines with L-shell Fe XXII-XXIII transition, Ly- $\alpha$ S XVI, Ly- $\alpha$ Ar XVIII, and Ca XIX resonance transition, respectively. The broader emission feature in the Fe-K $\alpha$ region was not identifiable, hence we supposed that it is a blending of Fe XXV and Fe XXVI emission lines. Fitting the broad feature adopting two Gaussian profiles centered at 6.7 and 6.97 keV we obtained that their corresponding widths were 220 and 280 eV. We conclude that if the Fe-k $\alpha$ feature is a blend of Fe XXV and Fe XXVI emission lines, these lines are intrinsically broad.

BeppoSAX observed three emission lines in the spectrum of GX 349+2 (Di Salvo et al. 2001; Iaria et al. 2004): the first one centered at $1.18 \pm 0.03$ keV, interpreted as the L-shell Fe XXIV transition, the second at $2.60 \pm 0.06$ keV, interpreted as the Ly- $\alpha$ S XVI transition and, finally, the third at $6.75 \pm 0.01$ keV, interpreted as the Fe XXV transition. In this observation, we find that the centroid of the broad emission line at 1 keV is at a lower energy, suggesting an L-shell transition of less ionized iron (Fe XXII-XXIII) although we cannot exclude a more complex blending of Fe XXI-XXIV. The widths and equivalent widths of these three lines are very similar comparing our observation and the two BeppoSAX observations of GX 349+2 (Di Salvo et al. 2001; Iaria et al. 2004) in the non-flaring state. Iaria et al. (2004) found, during interval 2 in the non-flaring state, widths of <80, <120 and $210 \pm 80$ eV, and equivalent widths of $23 \pm 8$ , $7^{\rm +4}_{-1}$ , and $52 \pm 11$ eV corresponding to the Fe XXIV, S XVI, and Fe XXV emission lines. Furthermore, Di Salvo et al. (2001) obtained equivalent widths for the Fe-K $\alpha$ line of 71 eV and 34 eV, in the non-flaring and flaring state of the source, respectively. From these rough comparisons it seems that the source is in a non-flaring state during the observation discussed in this work, although we cannot assert this conclusion without an accurate analysis of the time variabilities.

These emission features can be fitted slightly better adopting smeared relativistic lines. The large widths of the lines suggest that these are produced by reflection of the primary spectral component by the accretion disk. Similar broad emission features, discussed as smeared lines, were observed in several systems containing a neutron star, such as Ser X-1 (Bhattacharyya & Strohmayer 2007), SAX J1808.4-3658 (Cackett et al. 2009a; Papitto et al. 2009), 4U 1705-44 (Di Salvo et al. 2009,2005), GX 340+0 (D'Aì et al. 2009), 4U 1636-536 (Pandel et al. 2008), X 1624-490 (Iaria et al. 2007), and 4U 1820-30 and GX 349+2 (Cackett et al. 2008), and the authors of these papers agree in interpreting the broadening as due to relativistic and Doppler effects. In the following, we show the self-consistency of the disk reflection scenario, discussing the parameters reported in Table 6.

We infer the inner radius of the accretion disk, $R_{\rm disk}$ , using the normalization value of the multicolored disk blackbody and the inclination angle of the source, $i=43^{\rm +4}_{-3}$ deg, obtained by the relativistic smeared line, finding that $R_{\rm disk}$ is $8~\pm~3$ and $8~\pm~2$ km for Spectrum 1+3 and 2, respectively. The blackbody radius, $R_{\rm BB}$ , inferred by the best-fit values of the blackbody normalization, is $4.2~\pm~1.4$ and $4.5~\pm~1.4$ km for Spectrum 1+3 and 2, respectively, too small to be associated with the X-ray emission from the NS surface.

Taking into account possible modifications of the multicolored disk blackbody component due to electron scattering (White et al. 1988; Shakura & Syunyaev 1973), the measured color temperature, $T_{\rm col}$ , is related to the effective temperature of the inner disk, $T_{\rm col}= f T_{\rm eff}$ , where f is the spectral hardening factor, and $R_{\rm eff} = f^2 R_{\rm measured}$ . Adopting f=1.7 as estimated by Shimura & Takahara (1995) for a luminosity around 10% of the Eddington limit, close to the 25% of the Eddington limit estimated for GX 349+2 in our analysis, the corrected value of $R_{\rm disk}$ is $24 \pm 7$ km. The radius of the accretion disk is compatible with the value of the inner radius obtained by the relativistic smeared lines, that is, assuming a neutron star mass of 1.4 $M_{\odot}$ , <41 km and $19^{\rm +41}_{-6}$ km, for Spectrum 1+3 and 2, respectively. In the same way, correcting the radius of the blackbody component for the electron scattering, we infer that $R_{\rm BB} = 13 \pm 4$ km. This radius is compatible with the NS radius and suggests that the blackbody component is produced very close the NS surface. In this scenario, we directly observe the emission from inside the inner radius of the accretion disk, that is close the NS surface, and the blackbody component is interpreted as the direct emission from a compact corona and/or a boundary layer (BL) located between the neutron star and the inner radius of the disk. We should expect a Comptonized emission from the compact corona and/or BL, but if it is optically thick the Comptonized component results saturated and mimics a blackbody emission in the adopted energy range.

We observe, for the first time, reflection from the inner accretion disk that involves not only the K-transitions of iron but also ions of lighter elements such as sulfur, argon and calcium which all correspond to a similar ionization parameter. We observe emission lines associated with S XVI, Ar XVIII, Ca XIX, and Fe XXV, which correspond to an ionization parameter Log $(\xi) \simeq 3$ . A similar detection was reported by Di Salvo et al. (2009) analysing XMM data of 4U 1705-44.

Using the relation $\xi = L_{\rm x}/(n_{\rm e} r^2)$ , where $L_{\rm x}$ is the unabsorbed luminosity in the 0.1-100 keV, $n_{\rm e}$ the electron density of the plasma, and r the distance from the source of the emitting plasma we can roughly estimate the electron density $n_{\rm e}$ adopting as distance from the source the inner and outer accretion disk radius, $R_{\rm in}$ and $R_{\rm out}$ , obtained from the diskline components. We obtain that the electron density $n_{\rm e}$ decreases from 10²² to 10¹⁷ cm^-3 going from the inner to the outer radius. These values of electron densities are in agreement with the values reported by Vrtilek et al. (1993), who estimated the electron density of an extended cloud to be 10²² cm^-3 near the equatorial plane at a distance from the neutron star surface of less than 10⁸ cm (see Fig. 2 in Vrtilek et al. 1993).

From the analysis of the two selected spectra, we find that the extrapolated (not absorbed) flux in the 0.1-100 keV band of the multicolored disk blackbody is approximately constant: $(0.61~\pm~0.12)~\times~10^{-8}$ and $(0.49 \pm 0.05)\times 10^{-8}$ erg cm^-2 s^-1 for Spectrum 1+3 and 2, respectively. The blackbody component has a larger flux in Spectrum 2 ( $0.94 \pm 0.03 \times 10^{-8}$ erg cm^-2 s^-1) than in Spectrum 1+3 ( $0.77~\pm~0.02~\times~10^{-8}$ erg cm^-2 s^-1). This suggests that the intensity change during the observation is driven by the blackbody component. In our scenario the blackbody component is associated with the emission from a BL around the compact object and this emission illuminates the surface of the inner accretion disk producing the reflection lines observed in the spectra. We note that the line fluxes are higher in Spectrum 1+3 than in Spectrum 2 except for the flux associated with the Fe XXVI line which shows an anticorrelated behaviour.

Our scenario may easily explain these results: in fact, if the emission from the BL increases, the flux illuminating the accretion disk increases, then the ionization parameter of the reflecting matter also increases under the hypothesis that the density of the matter does not change. This implies that transitions of heavier ions are more probable, since lighter ions such as S XVI, Ar XVIII, Ca XIX, and Fe XXV decrease in number while heavier ions such as Fe XXVI increase in number, giving a larger flux of the Fe XXVI line and a lower flux of the other lines.

GX 349+2 is a NS LMXBs belonging to the Z-class sources and its behaviour is very similar to the prototype of its class, Sco X-1. Steeghs & Casares (2002) analysed the optical spectrum of Sco X-1 and obtained a firm mass ratio limit of $q \la 0.61$ from the phase-resolved spectroscopy, where q is the ratio of the companion star mass to the neutron star mass. If we assume that the optical periodicity of $21.9~\pm~0.4$ h, observed in GX 349+2 by Wachter & Margon (1996), is the orbital period of the system, the mass function of GX 349+2 is $f(M)= 0.032~M_{\odot}$ (see Wachter & Margon 1996). We find that the inclination angle of the system is $43^{\rm +4}_{-3}$ deg. Assuming a neutron star mass of 1.4 $M_{\odot}$ we find $q \sim 0.56$ , a value very similar to the upper limit estimated for Sco X-1, giving a mass of the companion star of $M_{\rm c} = 0.78^{\rm +0.07}_{-0.06}~M_{\odot}$ , typical for a NS LMXB of the Z class ( $q \le 0.61$ for Sco X-1, Steeghs & Casares 2002; $q = 0.34 \pm 0.04$ for Cyg X-2, Casares et al. 1997).

Furthermore Sco X-1 shows twin compact radio lobes forming an angle, with respect the line of sight, of $44~\pm~6$ deg (error at 1 $\sigma$ , see Fomalont et al. 2001). If the jet from the source producing the radio lobes is almost perpendicular to the equatorial plane of the system then the angle of $44~\pm~6$ deg corresponds to the inclination angle of the system, similar to the inclination angle of $43^{\rm +4}_{-3}$ deg obtained for GX 349+2 in this work. Our results indicate that Sco X-1 and GX 349+2 are very similar sources, as already suggested by other authors (see e.g. Kuulkers & van der Klis 1998).

Although our scenario looks reasonable, our values of the diskline parameters are not compatible with the recent ones reported by Cackett et al. (2008). Cackett et al., analysing Suzaku data of GX 349+2, fitted the broad emission feature in the Fe-K $\alpha$ region adopting a smeared relativistic line with the outer radius fixed at 1000 $R_{\rm g}$ . They found a line energy associated with Fe XXVI, an inner radius of $16.5 \pm 0.8$ km, an emissivity index of $-4.1 \pm 0.3$ and an inclination angle of the system of $23^{\circ} \pm 1^{\circ}$ . The differences in line energy, emissivity index, and inner radius of the reflecting skin could be explained supposing that GX 349+2 was observed in a different spectral state. We find that the Fe-K $\alpha$ broad emission feature is associated with the Fe XXV line or a blending of Fe XXV and Fe XXVI in which the Fe XXV line is more intense. Our measurement is similar to the previous BeppoSAX observations of GX 349+2 (Di Salvo et al. 2001; Iaria et al. 2004) and to the two recent Chandra observations of this source (Cackett et al. 2009b). In all these observations GX 349+2 was in NB/FB and/or in the bottom part of the FB. The only exception is the Suzaku observation of GX 349+2 (Cackett et al. 2008) where the broad emission line seems associated with Fe XXVI, suggesting that the source was in a different state; in fact, as discussed by Cackett et al., it is possible that GX 349+2 was in NB during that observation.

However, the different inclination angles of the system obtained in this work and by Cackett et al. (2008) cannot be easily explained since the inclination angle of the system should not depend on the state of the source and should not change. Using the inclination angle obtained by Cackett et al. we obtain a mass ratio $q \sim 1.25$ and a companion star mass of $1.74^{\rm +0.12}_{-0.11}~M_{\odot}$ for a neutron star mass of 1.4 $M_{\odot}$ , that is quite unusual for NS LMXBs.

Higher statistics spectroscopic studies are needed to put tighter constraints on the system parameters of this source, since these can give important information on the whole binary system and on the physics of the accretion flow close to the compact object.

4 Conclusions

We analysed a XMM observation of GX 349+2, finding the presence of prominent emission features associated with S XVI, Ar XVIII, Ca XIX, Fe XXV and, possibly, Fe XXVI. The emission features can be fitted with relativistic smeared lines ( diskline). The continuum emission was fitted adopting a multicolored disk blackbody plus a blackbody component. We investigated the scenario in which the broad emission lines are formed by reflection from an ionized skin in the inner region of the accretion disk illuminated by the emission of a compact corona (or a boundary layer) surrounding the neutron star that we fitted with a blackbody component with a temperature of 1.8 keV. We find a self-consistent explanation of our results. The inner radius of the disk blackbody is $24 \pm 7$ km while the broad lines give an inner disk radius of less than 40 km from the neutron star center. We discuss that the electron density of the reflecting plasma is between 10¹⁷ and 10²² cm^-3 and that the inclination angle of the source is around 43 $^\circ$ . Finally, we infer that, for an inclination angle of 43 $^\circ$ , the mass of the companion star is 0.78 $M_{\odot}$ .

Acknowledgements

We are very grateful to the referee for his/her suggestions and comments.

References

Bhattacharyya, S., & Strohmayer, T. E. 2007, ApJ, 664, L103 [NASA ADS] [CrossRef] (In the text)
Cackett, E. M., Miller, J. M., Bhattacharyya, S., et al. 2008, ApJ, 674, 415 [NASA ADS] [CrossRef] (In the text)
Cackett, E. M., Altamirano, D., Patruno, A., et al. 2009a, ApJ, 694, L21 [NASA ADS] [CrossRef]
Cackett, E. M., Miller, J. M., Homan, J., et al. 2009b, ApJ, 690, 1847 [NASA ADS] [CrossRef] (In the text)
Casares, J., Charles, P., & Kuuklers, E. 1997, NASA STI/Recon Technical Report N, 98, 99651 [NASA ADS] (In the text)
Christian, D. J., & Swank, J. H. 1997, ApJS, 109, 177 [NASA ADS] [CrossRef] (In the text)
D'Aì, A., Iaria, R., Di Salvo, T., Matt, G., & Robba, N. R. 2009, ApJ, 693, L1 [NASA ADS] [CrossRef] (In the text)
den Herder, J. W., Brinkman, A. C., Kahn, S. M., et al. 2001, A&A, 365, L7 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
Di Salvo, T., D'Ai', A., Iaria, R., et al. 2009, ArXiv e-prints
Di Salvo, T., Iaria, R., Méndez, M., et al. 2005, ApJ, 623, L121 [NASA ADS] [CrossRef]
Di Salvo, T., Robba, N. R., Iaria, R., et al. 2001, ApJ, 554, 49 [NASA ADS] [CrossRef] (In the text)
Fomalont, E. B., Geldzahler, B. J., & Bradshaw, C. F. 2001, ApJ, 558, 283 [NASA ADS] [CrossRef] (In the text)
Hasinger, G., & van der Klis, M. 1989, A&A, 225, 79 [NASA ADS] (In the text)
Hasinger, G., van der Klis, M., Ebisawa, K., Dotani, T., & Mitsuda, K. 1990, A&A, 235, 131 [NASA ADS]
Iaria, R., Di Salvo, T., Robba, N. R., et al. 2004, ApJ, 600, 358 [NASA ADS] [CrossRef] (In the text)
Iaria, R., Lavagetto, G., D'Aí, A., di Salvo, T., & Robba, N. R. 2007, A&A, 463, 289 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
Jansen, F., Lumb, D., Altieri, B., et al. 2001, A&A, 365, L1 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
Kuulkers, E., & van der Klis, M. 1998, A&A, 332, 845 [NASA ADS] (In the text)
O'Neill, P. M., Kuulkers, E., Sood, R. K., & Dotani, T. 2001, A&A, 370, 479 [NASA ADS] [CrossRef] [EDP Sciences]
O'Neill, P. M., Kuulkers, E., Sood, R. K., & van der Klis, M. 2002, MNRAS, 336, 217 [NASA ADS] [CrossRef]
Pandel, D., Kaaret, P., & Corbel, S. 2008, ApJ, 688, 1288 [NASA ADS] [CrossRef] (In the text)
Papitto, A., di Salvo, T., D'Ai, A., et al. 2009, A&A, 493, L39 [NASA ADS] [CrossRef] [EDP Sciences]
Shakura, N. I., & Syunyaev, R. A. 1973, A&A, 24, 337 [NASA ADS]
Shimura, T., & Takahara, F. 1995, ApJ, 445, 780 [NASA ADS] [CrossRef] (In the text)
Steeghs, D., & Casares, J. 2002, ApJ, 568, 273 [NASA ADS] [CrossRef] (In the text)
Strüder, L., Briel, U., Dennerl, K., et al. 2001, A&A, 365, L18 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
Turner, M. J. L., Abbey, A., Arnaud, M., et al. 2001, A&A, 365, L27 [NASA ADS] [CrossRef] [EDP Sciences] (In the text)
van der Klis, M. 1995, in Flares and Flashes, Lecture Notes in Physics (Berlin: Springer Verlag), ed. J. Greiner, H. W. Duerbeck, & R. E. Gershberg Lecture Notes in Physics, 454, IAU Colloq., 151, 321
Vrtilek, S. D., Soker, N., & Raymond, J. C. 1993, ApJ, 404, 696 [NASA ADS] [CrossRef] (In the text)
Wachter, S., & Margon, B. 1996, AJ, 112, 2684 [NASA ADS] [CrossRef] (In the text)
White, N. E., Stella, L., & Parmar, A. N. 1988, ApJ, 324, 363 [NASA ADS] [CrossRef]
Zhang, W., Strohmayer, T. E., & Swank, J. H. 1998, ApJ, 500, L167 [NASA ADS] [CrossRef] (In the text)

Footnotes

... mode: See Table 3 in the XMM-Newton Users Handbook published on 15 July 2008.
... pile-up: See Table 3 in the XMM-Newton Users Handbook published on 15 July 2008

All Tables

Table 1: Time intervals selected in the EPIC-pn lightcurve.

Table 2: Percentage of photon pile-up at different energies.

Table 3: Averaged continuum and identified broad Gaussian lines below 6 keV.

Table 4: Broad Gaussian lines between 6 and 7 keV.

All Figures

$\begin{figure} \includegraphics[width=9cm,clip]{11936fg1.ps} \end{figure}$	Figure 1: Epic-pn lightcurve of GX 349+2 in the energy band 1-10 keV. The bin time is 30 s.
Open with DEXTER
In the text

$\begin{figure} \includegraphics[width=9cm,clip]{11936fg2.ps} \end{figure}$	Figure 2: Color-intensity diagram of GX 349+2. The [4-10 keV]/[1-4 keV] hardness ratio increases for a count rate lower than 1580 c/s. The bin time is 100 s.
Open with DEXTER
In the text

$\begin{figure} \includegraphics[width=9cm,clip]{11936fg3.ps} \end{figure}$	Figure 3: Upper panel: 1-4 keV Epic-pn lightcurve. Middle panel: 4-10 keV Epic-pn lightcurve. Bottom panel: [4-10 keV]/[1-4 keV] hardness ratio. The bin time is 30 s for each lightcurve. The red dot-dashed vertical lines indicate the three selected time intervals.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{11936fg4.ps} \end{figure}$	Figure 4: Patterns of single (blue color) and double (red color) events extracted from the source region excluding RAWX 37 and 38. The patterns are plotted versus the 60-2000 ADU channel range, corresponding to 0.3-10 keV.
Open with DEXTER
In the text

$\begin{figure} \includegraphics[width=9cm,clip]{11936fg5.ps} \end{figure}$	Figure 5: Residuals (in units of $\sigma$ ) in the 0.7-10 keV energy range. The adopted continuum is composed of blackbody plus a multicolored disk blackbody, both absorbed by neutral matter. In the residuals, clear emission features are evident at 1, 2.7, 3.35, 3.9 and in the Fe-K $\alpha$ region of the spectrum.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{11936fg6.ps} \end{figure}$	Figure 6: Residuals in the 5.5-7.7 keV energy range. These can be fitted adopting a Gaussian profile or, equivalently, a relativistic smeared line (diskline in XSPEC)
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{11936fg7.ps} \end{figure}$	Figure 7: Data, model, and residuals (in units of $\sigma$ ) in the 0.7-10 keV energy range after adding the disk line components discussed in the text.
Open with DEXTER
In the text

$\begin{figure} \includegraphics[width=9cm,clip]{11936fg8.ps} \end{figure}$	Figure 8: Unfolded spectrum in the energy range 5.5-7.7 keV; the Fe XXV relativistic line profile is shown.
Open with DEXTER
In the text

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