Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://uranus.sai.msu.ru/~seif/ST10_apj_722_586.pdf Äàòà èçìåíåíèÿ: Thu Sep 23 10:37:44 2010 Äàòà èíäåêñèðîâàíèÿ: Mon Oct 1 19:54:23 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: optical telescope

The Astrophysical Journal, 722:586­604, 2010 October 10
C

doi:10.1088/0004-637X/722/1/586

2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A.

ON THE NATURE OF THE COMPACT OBJECT IN SS 433: OBSERVATIONAL EVIDENCE OF X-RAY PHOTON INDEX SATURATION
Elena Seifina1 and Lev Titarchuk2
1

,3 ,4

Moscow State University/Sternberg Astronomical Institute, Universitetsky Prospect 13, Moscow 119992, Russia; seif@sai.msu.ru 2 Dipartimento di Fisica, Universita di Ferrara, Via Saragat 1, I-44100 Ferrara, Italy; titarchuk@fe.infn.it ` 3 George Mason University, Fairfax, VA 22030, USA 4 NASA/Goddard Space Flight Center, Code 663, Greenbelt, MD 20771, USA; lev@milkyway.gsfc.nasa.gov Received 2010 April 1; accepted 2010 August 17; published 2010 September 22

ABSTRACT We present an analysis of the X-ray spectral properties observed from the black hole candidate (BHC) binary SS 433. We have analyzed Rossi X-ray Timing Explorer data from this source, coordinated with Green Bank Interferometer/ RATAN-600. We show that SS 433 undergoes an X-ray spectral transition from the low hard state to the intermediate state (IS). We show that the X-ray broadband energy spectra during all spectral states are well fitted by a sum of the socalled bulk motion Comptonization (BMC) component and by two (broad and narrow) Gaussians for the continuum and line emissions, respectively. In addition to these spectral model components, we also find a strong feature that we identify as a "blackbody-like (BB)" component in which the color temperature is in the range of 4­5 keV in 24 IS spectra during the radio outburst decay in SS 433. Our observational results on the "high-temperature BB" bump lead us to suggest the presence of gravitationally redshifted annihilation line emission in this source. In fact, this spectral feature has been recently reproduced in Monte Carlo simulations by Laurent & Titarchuk. We have also established the photon index saturation at about 2.3 in index versus mass accretion correlation. This index­mass accretion correlation allows us to evaluate the low limit of the black hole (BH) mass of the compact object in SS 433, Mbh 2 solar masses, using the scaling method using BHC GX 339-4 as a reference source. Our estimate of the BH mass in SS 433 is consistent with the recent BH mass measurement using the radial velocity measurements of the binary system by Hillwig & Gies, who find that Mx = (4.3 ± 0.8) solar masses. This is the smallest BH mass found up to now among all BH sources. Moreover, the index saturation effect versus mass accretion rate revealed in SS 433, as in a number of other BH candidates, is strong observational evidence for the presence of a BH in SS 433. Key words: accretion, accretion disks ­ black hole physics ­ stars: individual (SS 433) Online-only material: color figures

1. INTRODUCTION The famous object SS 433 (V 1343 Aql) holds a special place in late twentieth-century astronomy as the first microquasar discovered in our Galaxy (see reviews by Margon 1984 and Fabrika 2004). Observations of SS 433 have been carried out in all energy ranges for more than 30 years. Its key observational feature is the 162.5 day precession period of the jets that is revealed by the line features. The radial velocity curves of these lines are well described by a kinematical model which reveals key parameters of the jets: v = 0.26c and i = 79 (Margon 1984). Moreover, Romney et al. (1987) used and combined these results with the radio observations of the associated supernova remnant W50 which allowed them to estimate a distance of 5 kpc to SS 433. SS 433 is an X-ray/optical binary with Algol-type orbital eclipses. This source is characterized by two distinct spectral states: the quiescent hard state in which the persistent jet flow takes place and the soft state when massive jet blobs are ejected (Fielder et al. 1987). While the quiescent state has been well studied by numerous X-ray missions, only a few massive jet ejection events simultaneous with the X-ray soft state have so far been seen (Safi-Harb & Kotani 2003; Band et al. 1989). Because the ejection of a massive jet blob is a rare (on average two times per year) and short (approximately 10 days) event, we only have observations for part of this jet ejection. SS 433 shows many kinds of variability related to regular (orbital and precessional) and irregular (flaring) activities. Although precession, binary orbital, and nutation periods 586

(162 days, 13.08 days, and 6.28 days, respectively) are well known, a noticeable variability associated with shorter scales is poorly investigated. It is worth noting that the fast variability on a timescale of a few minutes was investigated by Zwitter et al. (1991) and Goranskij et al. (1987) in the optical V band. More recently, X-ray fast variability of a 50 s timescale during the flaring stage was found using Rossi X-ray Timing Explorer (RXTE) observations by Kotani et al. (2002). The power spectrum of SS 433 is well represented and approximated by power law (P - ) in the range of 10-7 to 10-2 Hz according to the X-ray timing data analysis performed by Revnivtsev et al. (2006). They also demonstrated that at frequencies lower than 10-5 Hz the same variability pattern takes place in the optical, radio, and X-ray spectral bands (see their Figure 1). Many questions regarding the complex behavior of SS 433 during outburst states as well as the nature of this compact object and its mass are still not answered. However, there is no shortage of models which are based on radio, optical, and X-ray variations of radiation detected from SS 433 (see, e.g., Marshall et al. 2002; Fabrika 2004; Safi-Harb & Kotani 2003). The variation in mass estimates of the compact (Mx ) and optical (Mv ) objects and the mass ratio (q = Mx /Mv ) are quite broad. Kawai et al. (1989) and later Antokhina at el. (1992), using Ginga observations of SS 433, estimated q 0.15 and q = 0.15­0.25, respectively. On the other hand, Kotani et al. (1996) using ASCA observations found q 0.06­0.31 in the frame of the precessing jet model by taking into account thermal adiabatic cooling of the jets (Brinkmann et al. 1991). Later highresolution observations by Gies et al. (2002) found the presence


No. 1, 2010

ON THE NATURE OF THE COMPACT OBJECT IN SS 433
Table 1 List of Sets (Groups) of RXTE Observation of SS 433

587

Number of Set R1 R2 R3 R4 R5 R6 R7

Dates, MJD 50191­50194 50868­50907 52222­52238 52544.46­52544.74, 52913­52914 53076­53092 53239­53610 54085­54096

RXTE Proposal ID 10127 20102, 30273 60058 70416, 80429 90401 90401, 91103, 91092 92424

UT Dates 1996 Apr 18­21 1998 Feb 24­Apr 4 2001 Nov 9­11 2002 Apr 18­21 2004 Mar 12­28 2005 Jul 28­Aug 28 2006 Dec 17­27

Type of Light Curve Outburst Outburst Outburst Outburst decay Outburst decay

Ref. 1 1,2 1 1 1, 2 This work This work

References. (1) Filippova et al. 2006; (2) Nandi et al. 2005.

of absorption lines in the spectrum of the optical A (A7Ib) supergiant companion. These orbital Doppler-shifted absorption lines and stationary He ii emission from the companion allowed an estimate of the mass ratio of q = 0.35, implying the binary masses Mx = 4.3 ± 0.8 M and Mv = 12.3 ± 3.3 M in SS 433 (see Hillwig & Gies 2008 for details). Thus, the average mass ratio inferred from this X-ray data analysis q 0.25 is smaller than that inferred from optical observations q 0.35. One comes to the conclusion that in the literature there is a large variation in the mass estimates of the compact object (Mx ), secondary star (Mv ), and their mass ratio (q = Mx /Mv ) in SS 433. The nature of the compact object was inferred using the mass estimate or its upper limit. No other strong arguments were used to determine the nature of the compact object in SS 433 which is an eclipsing X-ray binary system, with the primary most likely a black hole (BH), or possibly a neutron star (see, e.g., Cherepashchuk 2002). In this work, we apply a substantially new approach for diagnosing the nature of the compact object in SS 433. In Section 2.1, we present details of radio and X-ray observations of SS 433. The analysis of X-ray spectra is shown in Section 2.2. We discuss the X-ray spectral evolution of SS 433 in Section 3. X-ray spectral properties as a function of orbital phase are investigated in Section 4. The results of timing and power spectrum analysis are presented in Section 5. We consider an interpretation of observational results and show our arguments for BH presence in SS 433 in Section 6. We present a discussion and concluding remarks in Section 7. 2. OBSERVATIONS AND DATA REDUCTION 2.1. Listing of X-ray Observations Used for Data Analysis We analyzed the archival data collected by PCA/RXTE (Bradt et al. 1993) which were obtained in the time period from 1996 April to 2006 December. These data allow us to investigate SS 433 in the broad X-ray energy band (3­150 keV) during the quiescent and outburst states. The RXTE data for SS 433 are available through the HEASARC public archive (http://heasarc.gsfc.nasa.gov) at the NASA Goddard Space Flight Center (GSFC). As we have already mentioned, SS 433 shows continuous (associated with a quiet state) and sporadic (associated with an active state) variability. For investigation of the outburst state and to compare it with the quiescent state, we only selected observations during uneclipsed intervals of the binary orbital period. In fact, X-ray eclipse occurs around optical primary minima at phases | | 0.1. As a result, we only used observations taken at interval | | > 0.1 to exclude the eclipse orbital modulation. In total, these type of observations include 90 episodes of phases that are outside of eclipses. Moreover, 27 observations during eclipses taken at different precessional and

orbital phases were used for the spectral and timing analysis of orbital modulation effects. Precessional ephemerids were taken from Fabrika (2004). The moment of maximal separation between emission lines (T3 ) was taken to be T3 = 2443507.47 JD, the precessional period Pprec = 162.375 days, the orbital period Porb = 13.08211 days, and the moment of primary optical eclipse T0 = 2450023.62 JD (Goranskij et al. 1998). Standard tasks of the HEASOFT/FTOOLS 5.3 software package were utilized for data processing. We used methods recommended by the RXTE Guest Observer Facility according to the RXTE Cookbook (see http://heasarc.gsfc.nasa.gov/ docs/xte/recipes/cook_book.html). For spectral analysis, we used PCA Standard 2 mode data collected in the 3­20 keV energy range. The standard dead time correction procedure has been applied to the data. To construct broadband spectra, HEXTE data have also been used. We subtracted background corrected in off-source observations. To exclude the channels with the largest uncertainties, only data in the 20­150 keV energy range were used for the spectral analysis. In Table 1, we list the groups of RXTE observations covering the source evolution from quiescent to outburst states. We also used public data from the All-Sky Monitor (ASM) on board RXTE. The ASM light curves (2­12 keV energy range) were retrieved from the public RXTE/ASM archive at HEASARC.5 In this paper, we have analyzed X-ray spectra during the quiescent and outburst states with reference to simultaneous radio and optical observations. The monitoring RATAN-600 Radio Telescope (2­8 GHz) data in the 1996­2006 period were provided by S. Trushkin (http://www.sao.ru/cats/satr/XB/). We also used radio observations by the Green Bank Interferometer, NRAO6 obtained from 1996 to 1998 at 2.25 and 8.3 GHz and simultaneous V-band photoelectric photometric observations. Details of optical telescopes, reduction techniques, and compilation methods are given by Goranskij et al. (1998). Additionally, we analyzed the INTEGRAL/IBIS/ISGRI spectra in the flaring state (2004) of SS 433 that were coordinated with the RXTE observations. We have used version 8.0 of the Offline Science Analysis (OSA) software distributed by the INTEGRAL Science Data Center (ISDC, http://isdc.unige.ch; Corvoisier et al. 2003). We also present a comparison of the SS 433 data with that for GRS 1915+105 obtained during BeppoSAX observations. We used two BeppoSAX detectors, the Medium-Energy Concentrator Spectrometer (MECS) and a Phoswich Detection System (PDS), for this analysis. The SAXDAS data package was utilized for performing data analysis. We process the spectral analysis in the good response energy range taking into account
5 6

http://xte.mit.edu/ASM_lc.html http://www.gb.nrao.edu/fgdocs/gbi/arcgbi


588

SEIFINA & TITARCHUK
Table 2 List of GRS 1915+105 Observations Used in Analysis

Vol. 722

Satellite BeppoSAX

ObsID 209850011

Start Time (UT) 2000 Apr 21 08:55:30

End Time (UT) 2000 Apr 21 15:16:47

satisfactory statistics of the source: 1.8­10 keV for MECS and 15­150 keV for PDS. 2.2. Spectral Analysis SS 433 has long been of great interest in X-ray astrophysics, and was observed early on with many satellites such as HEAO-1 (Marshall et al. 1979), EXOSAT (Watson et al. 1986), Tenma (Matsuoka et al. 1986), and Ginga (Kawai et al. 1989). Using HEAO-1, Marshall et al. were the first to demonstrate that SS 433 is an X-ray source. The HEAO-1 continuum was sufficiently modeled as a thermal bremsstrahlung with kT = 14.3 keV, and emission due to Fe­K was detected near 7 keV. The ASCA satellite, which carried X-ray CCD cameras for the first time, detected many pairs of Doppler-shifted emission lines from ionized metals, such as Si, S, Ar, Ca, Fe, and Ni, originating from the twin jets (Kotani et al. 1994). The emission lines were also resolved with the Chandra HETGS, which were found to have Doppler widths of 1000­5000 km s-1 (Marshall et al. 2002; Namiki et al. 2003; Lopez et al. 2006). The broadband continuum (up to 100 keV) is approximated by a thermal bremsstrahlung spectrum with a temperature of 10­30 keV, depending on whether SS 433 is in or out of eclipse (Kawai et al. 1989; Cherepashchuk et al. 2005). Additional complex features were detected from the XMM spectra, however, which could be Compton-scattered emission from the jet base (Brinkmann et al. 2005) or an iron­K absorption edge due to partial covering (Kubota et al. 2007). From the width of an eclipse in the 25­50 keV band with INTEGRAL, Cherepashchuk et al. (2007) and Krivosheyev et al. (2009) propose that a hot extended corona around the accretion disk is responsible for the hard X-ray emission via thermal Comptonization with a temperature of 20 keV. High-quality X-ray spectra covering the broadband are critical in establishing an interpretation of the high-energy spectra of SS 433. In our study, we model the broadband source spectra in XSPEC using an additive model consisting of the sum of the so-called bulk motion Comptonization (BMC) model and two Gaussian line components. The BMC model is a generic Comptonization model which can be applied to upscattering of soft photons injected in a hot cloud. This model consists of two parts: the first part is a direct blackbody (BB) component and the second one is a convolution of the fraction of the BB component with a broken power law, the upscattering Green function. The spectral index of the blue wing is much smaller than that of the red wing + 3. The shape of the Green function (broken power law) is generic and independent of the type of Comptonization, thermal or nonthermal. The name of the model (BMC) has only been used since 1997 (see Titarchuk et al. 1997) when the model was first applied to the case of bulk motion Comptonization. However, this model can be applied to any type of Comptonization, thermal or nonthermal, but it should be, in principle, combined with an exponential cutoff which is related to average plasma energy, for example, plasma temperature for the thermal Comptonization kTe or kinetic energy of the matter in the case of the converging (bulk inflow) Comptonization. In this paper, we consider a scenario related to our model (see Figure 1) where the Compton cloud (CC) along with converging

flow are located in the innermost part of the source and a Keplerian disk extends from the CC to the optical companion. As we point out, ASCA and Chandra detected many lines of various elements in the soft X-ray band of the spectrum of SS 433. Particularly, iron lines Fe xxv­Fe xxvi dominate at energies 6.5 keV < E < 7 keV and show a double structure due to jet Doppler shifts. In addition to iron line emission, one can see the line emission related to hydrogen--and helium-like ions of Mg, Si, S, Ar, Ca, and Ni which display a double structure also. These line signatures indicate that the lines are formed in the relativistic jet configuration. Along with these lines, there is an appreciable emission feature at 6.4 keV which is visible in the X-ray spectrum of SS 433 (Kotani et al. 1996; Seifina 2000). This line is not subjected to Doppler shifting. Thus, we want to emphasize that by using the forms of these lines we can see features of "moving" and "stationary" structures of material surrounding SS 433. However, the identification and precise theoretical reproduction of the line composition with RXTE is problematic because of its low-energy resolution. As a test trial, we added one Gaussian component to fit the spectrum varying the width and normalization of the line and found that the width of this Gaussian feature ranges roughly from 0.3 to 1 keV. In quite a few cases, the spectral fits using one Gaussian component provide very wide residuals extended from 6 to 9 keV. However, after adding a second narrow Gaussian component (in the 6­9 keV range), the fit quality has been significantly improved. The energies of the first and second Gaussian components, Eline1 and Eline2 , are presented in Table 3. For the first Gaussian Eline1 changes from 6.5 to 6.9 keV, while the range of the second Gaussian varies from 7.1 to 9 keV. In some cases, we see a wide residual taking place around 20 keV which can be a signature of a "high-temperature bbody-like" spectral component of temperature in the range of 4­5 keV. Thus, we use our XSPEC model as wabs*(bmc+Gaussian+Gaussian+bbody) for fitting of SS 433 spectra. In particular, we use a value of hydrogen column NH = 1.2 â 1023 cm2 which was found by Filippova et al. (2006) in calculations of the XSPEC model wabs. The best-fit parameters of the source spectrum are presented in Tables 3­6. For the BMC model, the parameters are the spectral index (photon index = + 1), color temperature of the BB-like injected photons kT , log(A) related to the Comptonized fraction f (f = A/(1 + A)), and normalization of the BB-like component Nbmc . We find that the color temperature kT is about 1 keV for all available RXTE data and thus we fix a value of kT at 1 keV. When the parameter log(A) 1 we fix log(A) = 2 (see Tables 3 and 5), because the Comptonized fraction f = A/(1 + A) 1. The variations of A do not improve fit quality any more. A systematic error of 1% has been applied to the analyzed X-ray spectra. We applied this systematic error to the analyzed RXTE spectra in accordance to the current version of RXTE Cookbook (see http://heasarc.gsfc.nasa.gov/ docs/xte/recipes/cook_book.html) following recommended methods by RXTE Guest Observer Facility. In Figure 1, we present a suggested geometry of the X-ray source in SS 433 (see further explanation of the geometry below). Similar to the ordinary bbody XSPEC model, the normalization Nbmc is a ratio of the source (disk) luminosity to the square of the distance D: Nbmc = L 1039 erg s 10 kpc D
2

-1

.

(1)


No. 1, 2010

Table 3 Best-fit Parameters of the Spectral Analysis of PCA and HEXTE Observation of SS 433 in 3­150 keV Energy Rangea Observational ID 10127-01-01-00 10127-01-02-00 10127-01-03-00 10127-01-04-00 10127-01-05-00 10127-01-06-00 10127-01-07-00 20102-01-01-00 20102-01-02-00 20102-01-03-00 20102-01-04-00 20102-01-05-00 20102-01-06-00 20102-02-01-02 20102-02-01-03 20102-02-01-04 20102-02-01-05 20102-02-01-01 20102-02-01-06 20102-02-01-07 20102-02-01-000 20102-02-01-00 20102-02-01-11 20102-02-01-08 20102-02-01-09 20102-02-01-10 20102-01-07-00 20102-02-02-01 20102-02-02-00 30273-01-01-00 30273-01-01-01 30273-01-02-00 30273-01-02-010 30273-01-02-01 30273-01-03-000 30273-01-03-00 30273-01-03-010 30273-01-03-01 30273-01-03-02 30273-01-05-01 30273-01-05-03 30273-01-05-00 30273-01-05-02 60058-01-01-00 MJD (day) 50191.10 50192.10 50192.71 50193.06 50193.27 50193.77 50194.91 50868.77 50870.24 50871.91 50873.18 50874.92 50876.72 50876.79 50877.58 50877.64 50877.71 50877.79 50878.00 50878.58 50878.64 50878.97 50879.16 50879.37 50879.51 50879.57 50889.73 50897.85 50898.78 50899.72 50900.73 50901.74 50902.74 50903.06 50903.73 50903.99 50904.72 50904.99 50905.20 50906.00 50906.13 50906.79 50907.13 52222.29 0.852 0.931 0.973 0.005 0.020 0.087 0.149 0.642 0.754 0.895 0.991 0.111 0.250 0.255 0.315 0.320 0.325 0.331 0.347 0.391 0.396 0.421 0.436 0.452 0.463 0.467 0.244 0.865 0.953 0.007 0.083 0.162 0.239 0.263 0.314 0.334 0.390 0.410 0.427 0.487 0.498 0.548 0.574 0.105 0.1820 0.1882 0.1911 0.1941 0.1950 0.1980 0.2051 0.3609 0.3700 0.3810 0.3850 0.3988 0.4099 0.4104 0.4152 0.4156 0.4160 0.4165 0.4178 0.4214 0.4218 0.4238 0.4249 0.4263 0.4271 0.4275 0.4902 0.5402 0.546 0.551 0.558 0.5642 0.5704 0.5724 0.5765 0.5781 0.5826 0.5843 0.5856 0.5905 0.5913 0.5953 0.5975 0.7082 = -1 1.03(2) 1.11(1) 1.43(3) 1.36(2) 1.38(3) 1.40(2) 1.13(1) 0.97(2) 1.00(1) 1.15(2) 1.36(3) 1.19(4) 1.19(4) 1.20(5) 1.11(4) 1.36(2) 1.18(3) 1.14(1) 1.09(1) 1.18(4) 1.14(2) 1.12(1) 1.09(3) 0.99(4) 1.13(4) 1.22(2) 0.86(7) 1.10(2) 1.33(1) 1.39(1) 1.13(1) 0.99(1) 1.07(1) 0.98(4) 1.17(1) 1.15(3) 1.17(1) 1.21(3) 1.25(6) 1.06(2) 1.09(4) 1.23(1) 1.20(5) 1.07(7) log(A)b 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 0.36(9) 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 Nbmc c 2 (L39 /d10 ) 3.20(3) 2.23(3) 2.01(9) 1.87(2) 1.95(5) 2.03(2) 2.83(9) 1.64(2) 1.84(2) 2.14(5) 1.67(7) 1.68(6) 1.67(6) 1.81(6) 1.74(6) 1.67(2) 1.84(4) 1.96(2) 2.03(1) 2.09(6) 2.0(1) 1.9(1) 1.73(5) 1.71(9) 1.60(6) 1.72(3) 0.72(3) 1.72(3) 1.85(2) 1.58(1) 1.72(3) 1.74(3) 1.93(2) 1.98(9) 2.01(2) 1.98(5) 1.90(2) 1.90(4) 2.01(6) 1.86(4) 1.93(6) 2.00(2) 1.98(6) 1.97(7) Eline1 , (keV) 6.90(9) 6.87(1) 6.89(1) 6.88(1) 6.86(2) 6.89(1) 6.88(7) 6.59(1) 6.54(1) 6.56(1) 6.58(1) 6.57(2) 6.57(2) 6.58(3) 6.59(2) 6.58(1) 6.61(2) 6.63(1) 6.637(6) 6.68(2) 6.64(8) 6.67(8) 6.62(1) 6.60(2) 6.66(1) 6.66(1) 6.70(3) 6.16(1) 6.60(1) 6.58(1) 6.56(1) 6.60(1) 6.643(8) 6.67(2) 6.616(8) 6.63(1) 6.565(8) 6.59(2) 6.58(3) 6.55(1) 6.54(2) 6.533(8) 6.54(2) 6.67(4) line1 (keV) 0.66(1) 0.73(2) 0.64(2) 0.69(2) 0.67(5) 0.63(2) 0.61(1) 0.34(2) 0.29(2) 0.26(3) 0.36(2) 0.33(5) 0.33(5) 0.36(6) 0.43(4) 0.36(2) 0.39(4) 0.42(1) 0.42(1) 0.46(4) 0.44(1) 0.46(1) 0.45(3) 0.50(5) 0.60(3) 0.46(2) 0.59(6) 0.45(3) 0.35(2) 0.35(1) 0.34(2) 0.41(2) 0.47(1) 0.55(5) 0.40(1) 0.42(3) 0.33(7) 0.34(4) 0.35(7) 0.35(3) 0.38(5) 0.28(1) 0.34(5) 0.42(7) Nline1 3.74(6) 3.1(1) 2.2(1) 2.3(1) 2.2(2) 2.3(1) 3.06(8) 1.68(7) 1.80(8) 1.9(1) 1.82(8) 2.1(2) 2.1(2) 2.2(2) 2.4(2) 1.82(8) 2.23(7) 2.37(8) 2.53(6) 2.5(2) 2.41(7) 2.44(7) 2.24(4) 2.6(2) 2.8(2) 2.4(1) 0.44(7) 1.9(1) 1.90(8) 1.81(4) 1.82(8) 2.02(8) 2.32(7) 2.6(2) 2.32(7) 2.4(1) 2.09(7) 2.1(1) 2.01(6) 2.2(1) 2.2(2) 2.04(7) 2.2(2) 1.8(2) Eline2 , (keV) 8.70(4) 8.83(5) 8.64(7) 8.75(6) 8.6(1) 8.65(6) 8.63(4) 7.95(6) 7.71(3) 7.70(4) 7.95(3) 7.9(1) 7.9(1) 7.8(3) 8.01(9) 7.95(3) 7.96(8) 8.01(4) 8.06(3) 8.1(3) 8.6(1) 8.20(4) 8.02(6) 8.1(1) 8.9(1) 8.22(7) 8.6(1) 8.05(5) 7.92(3) 7.92(3) 7.83(3) 7.92(3) 8.12(3) 8.3(1) 7.98(3) 8.13(8) 7.80(2) 7.88(7) 7.8(1) 7.94(6) 7.8(1) 7.7(2) 7.9(1) 7.9(1) Nline2
c



2 red

(dof)

F1 /F2

d

Rem (a) ecl ecl ecl ecl ecl

0.28(4) 0.21(3) 0.19(4) 0.19(4) 0.22(9) 0.21(4) 0.2(2) 0.23(4) 0.39(5) 0.47(7) 0.36(4) 0.3(1) 0.3(1) 0.03(1) 0.4(1) 0.36(4) 0.4(1) 0.30(5) 0.34(3) 0.2(1) 0.04(2) 0.2(3) 0.30(7) 0.3(1) 0.19(6) 0.26(5) 0.04(2) 0.32(5) 0.38(4) 0.39(4) 0.29(4) 0.29(4) 0.31(4) 0.3(1) 0.36(4) 0.33(8) 0.47(4) 0.45(1) 0.4(1) 0.36(7) 0.38(5) 0.47(4) 0.4(1) 0.27(7)

1.17(78) 1.27(78) 0.77(78) 1.14(78) 0.99(78) 1.21(78) 1.16(78) 1.01(77) 1.57(77) 1.28(78) 1.02(78) 0.85(77) 0.85(77) 0.93(77) 0.98(77) 1.01(77) 0.70(77) 0.94(77) 1.42(77) 0.84(77) 0.63(77) 0.84(77) 1.34(77) 0.68(77) 0.89(77) 0.79(77) 1.03(76) 0.79(77) 1.44(77) 1.38(77) 1.40(77) 1.32(77) 1.20(77) 0.80(77) 1.02(77) 0.98(77) 0.98(77) 0.76(77) 1.29(77) 1.01(77) 1.09(77) 0.95(77) 0.81(77) 0.79(77)

6.06/4.61 4.40/3.13 3.07/1.46 2.99/1.51 3.25/1.87 3.18/1.58 5.15/3.64 3.30/2.73 3.42/2.97 3.79/2.64 3.79/2.64 2.74/1.84 2.73/1.80 2.90/1.94 3.01/2.21 2.60/1.32 3.01/2.10 3.34/2.45 3.51/2.75 3.41/2.42 2.84/1.89 3.52/2.42 3.02/2.32 3.33/2.81 3.04/1.92 2.85/1.82 1.22/1.25 3.04/2.24 3.00/1.40 2.49/1.21 3.16/2.17 3.32/2.85 3.52/2.73 3.81/3.21 3.35/2.34 3.32/2.31 3.31/2.30 3.12/2.04 3.21/2.01 3.32/2.61 3.42/2.64 3.24/2.12 3.21/2.21 3.47/2.84

ON THE NATURE OF THE COMPACT OBJECT IN SS 433

ecl ecl

ecl ecl ecl

589


590

Table 3 (Continued) Observational ID 60058-01-02-00 60058-01-03-00 60058-01-04-00e 60058-01-05-00e 60058-01-06-00e 60058-01-07-00e 60058-01-08-00e 60058-01-09-00e 60058-01-10-00e 60058-01-11-00e 60058-01-12-00 60058-01-13-00 60058-01-15-00e 60058-01-17-00 70416-01-01-00 70416-01-01-01 70416-01-01-02 80429-01-01-00 80429-01-01-01 90401-01-01-01e 90401-01-01-03e 90401-01-01-00e 90401-01-01-02e 90401-01-02-01e 90401-01-02-00e 90401-01-03-01e 90401-01-03-02e 90401-01-03-00e 90401-01-04-01 90401-01-05-01 90401-01-06-00 90401-01-06-01 91103-01-01-00 91103-01-09-00 91103-01-02-01 91103-01-02-00e 91103-01-03-00 91103-01-04-01 91103-01-04-00 91103-01-05-00e 91103-01-05-01e 91103-01-07-00e 91103-01-06-00e 91103-01-06-01e MJD (day) 52223.22 52224.28 52225.27 52226.19 52227.25 52228.24 52229.30 52230.30 52232.15 52233.27 52234.33 52235.33 52236.18 52238.23 52544.46 52544.66 52544.74 52913.69 52914.22 53076.78 53076.85 53077.77 53078.75 53089.07 53089.28 53091.04 53091.82 53092.09 53239.49 53361.71 53363.75 53366.13 53579.63 53580.55 53580.83 53580.90 53581.53 53581.73 53581.89 53582.87 53582.94 53583.56 53583.78 53584.68 0.176 0.257 0.333 0.403 0.484 0.560 0.641 0.717 0.859 0.952 0.028 0.105 0.167 0.324 0.732 0.747 0.753 0.963 0.007 0.423 0.428 0.498 0.573 0.362 0.378 0.512 0.572 0.593 0.860 0.202 0.359 0.540 0.861 0.931 0.952 0.958 0.006 0.021 0.033 0.108 0.113 0.161 0.178 0.246 0.7139 0.7205 0.7266 0.7323 0.7388 0.7449 0.7515 0.7576 0.7690 0.7758 0.7819 0.7881 0.7939 0.8065 0.6951 0.6963 0.6968 0.9711 0.9761 0.9780 0.9784 0.9841 0.9901 0.0538 0.0550 0.0659 0.0707 0.0724 0.9814 0.7352 0.7478 0.7624 0.0791 0.0848 0.0865 0.0870 0.0908 0.0920 0.0930 0.0991 0.0995 0.1034 0.1047 0.1102 = -1 1.19(8) 1.22(8) 1.07(8) 1.06(8) 1.07(5) 1.30(6) 1.31(8) 1.30(5) 1.2(1) 1.20(8) 1.20(9) 1.21(8) 1.19(5) 1.26(5) 1.13(5) 1.00(6) 0.97(6) 1.21(8) 1.22(5) 1.30(2) 1.30(2) 1.32(2) 1.30(1) 1.31(2) 1.30(2) 1.29(2) 1.29(2) 1.31(2) 1.2(1) 1.00(6) 1.09(2) 0.95(7) 1.18(3) 1.19(4) 1.18(3) 1.18(3) 0.94(6) 0.92(2) 0.90(6) 1.2(1) 1.20(6) 1.2(1) 1.19(2) 1.2(1) log(A)b 2.00 2.00 -0.5(4) -0.5(4) -0.1(1) 2.00 0.7(3) 0.5(2) 2.00 2.00 2.00 2.00 2.00 2.00 2.00 0.4(1) 0.7(2) 2.0 2.0 0.4(2) 0.3(1) 0.3(1) 2.00 0.9(6) 1.8(1) 0.16(2) 0.4(1) 2.00 2.00 2.00 2.00 2.00 2.00 2.00 2.00 0.2(2) 0.58(5) 0.6(1) 0.6(1) 0.01(4) 0.9(1) 2.00 2.00 2.00 Nbmc c 2 (L39 /d10 ) 2.04(6) 2.21(7) 1.5(3) 1.9(3) 1.8(3) 2.46(4) 2.5(1) 2.1(1) 2.27(3) 2.06(1) 1.8(1) 2.60(8) 2.58(2) 3.57(7) 1.60(7) 1.7(1) 1.5(1) 1.8(1) 1.84(8) 3.4(1) 3.4(1) 3.03(6) 3.5(1) 3.4(1) 3.6(1) 3.2(1) 3.3(1) 2.8(1) 3.42(8) 1.24(9) 1.46(9) 1.71(6) 2.72(9) 2.4(4) 1.88(5) 2.21(2) 1.6(1) 1.95(1) 1.5(1) 2.5(3) 3.1(4) 3.3(2) 3.2(3) 3.2(3) Eline1 , (keV) 6.95(4) 6.94(1) 7.01(1) 7.03(2) 7.05(1) 6.90(1) 6.95(3) 6.92(4) 6.96(3) 6.97(4) 7.03(5) 6.95(3) 6.99(2) 7.06(3) 6.64(4) 6.57(6) 6.61(6) 7.30(9) 7.42(5) 7.23(3) 7.15(2) 7.06(1) 7.02(3) 7.07(2) 7.12(2) 7.02(3) 7.04(2) 7.10(2) 7.33(3) 6.58(2) 6.60(3) 6.62(3) 7.09(2) 7.22(4) 7.1(1) 6.70(2) 6.96(3) 7.5(1) 6.8(1) 7.08(6) 7.02(6) 7.03(3) 7.08(5) 7.06(3) line1 (keV) 0.43(7) 0.6(1) 0.72(4) 0.63(3) 0.74(5) 0.52(3) 0.55(5) 0.73(6) 0.86(4) 0.63(7) 0.68(9) 0.55(5) 0.67(4) 0.69(4) 0.2(1) 0.2(1) 0.3(1) 1.2(1) 1.8(2) 0.96(8) 0.80(4) 0.75(2) 0.87(4) 0.97(4) 0.80(3) 0.70(7) 0.73(4) 0.90(4) 0.71(4) 0.42(4) 0.31(4) 0.33(7) 0.91(2) 0.87(6) 0.78(2) 0.27(3) 0.99(3) 0.9(1) 1.29(1) 0.75(8) 0.75(9) 0.75(6) 0.90(9) 0.75(5) Nline1 1.3(2) 1.3(3) 2.7(3) 2.5(1) 2.6(3) 2.1(1) 2.2(2) 2.18(3) 3.2(3) 1.9(2) 1.7(3) 2.6(8) 2.6(2) 2.5(2) 1.6(2) 1.2(2) 1.61(6) 2.3(5) 1.06(7) 4.7(6) 4.4(8) 4.3(2) 4.1(4) 5.3(3) 4.3(1) 3.7(4) 3.8(3) 4.2(3) 2.4(1) 1.8(1) 1.8(1) 2.4(2) 3.9(3) 2.1(2) 1.7(5) 0.6(3) 1.61(6) 1.1(4) 3.0(5) 2.8(6) 3.0(6) 2.8(3) 3.0(4) 3.5(3) Eline2 , (keV) 7.9(1) 6.6(1) 9.4(1) 9.4(1) 9.4(1) 8.9(1) 8.80(4) 8.69(4) ... 8.7(2) 8.7(2) 9.0(4) ... ... 7.9(1) 7.7(1) 7.8(1) ... ... 9.2(3) 9.3(2) 9.08(5) 8.9(2) ... 9.2(1) 8.8(1) 9.1(4) ... ... ... 8.3(1) 8.3(1) ... ... 8.7(1) 8.0(2) 9.3(1) 6.9(1) ... ... ... 7.1(4) 7.0(1) 7.01(8) Nline2
c



2 red

(dof)

F1 /F2

d

Rem (a)

0.3(1) 0.5(3) 0.17(9) 0.02(9) 0.10(9) 0.15(8) 0.25(8) 0.25(8) ... 0.2(1) 0.1(1) 0.2(1) ... ... 0.3(1) 0.4(1) 0.4(2) ... ... 0.1(1) 0.26(8) 0.30(5) 0.1(1) ... 0.80(3) 0.4(1) 0.21(9) ... ... ... 0.27(9) 0.4(1) ... ... 0.2(2) 0.4(1) 0.10(8) 0.4(2) ... ... ... 0.9(2) 0.05(3) 0.6(3)

1.15(77) 1.37(77) 1.09(69) 1.30(69) 1.01(69) 1.08(69) 1.20(69) 0.79(69) 1.2(69) 1.2(69) 1.04(77) 1.17(77) 1.09(69) 1.59(71) 0.93(72) 0.81(71) 0.87(72) 1.13(72) 1.03(72) 1.01(69) 1.03(69) 1.24(69) 1.35(69) 1.17(69) 1.34(69) 1.14(69) 1.08(69) 1.19(69) 1.50(73) 1.15(73) 1.19(73) 1.15(71) 1.17(71) 0.97(74) 1.18(73) 0.97(69) 1.02(73) 1.04(71) 0.85(73) 0.97(69) 1.07(69) 1.04(69) 1.25(69) 1.03(69)

3.22/2.53 3.42/2.61 3.33/1.73 3.91/1.95 3.74/2.13 4.15/2.69 4.12/2.78 3.46/2.17 4.15/2.74 3.57/2.37 3.16/2.07 4.27/3.08 4.85/3.42 5.71/3.94 2.99/2.04 2.76/1.98 2.92/2.23 3.36/2.03 3.22/1.983 8.59/6.54 7.91/4.85 7.72/4.75 7.01/4.63 5.25/3.01 8.01/5.47 5.64/3.58 5.95/3.51 5.93/3.62 5.62/3.98 2.89/2.12 2.87/1.91 3.45/2.96 2.78/1.63 4.20/2.57 3.38/2.13 2.97/1.74 2.79/2.30 2.91/1.90 3.22/2.52 3.90/2.13 5.41/3.34 6.30/3.88 5.56/3.44 6.79/4.01

ecl ecl ecl

SEIFINA & TITARCHUK

ecl ecl

ecl ecl ecl ecl, "A" ecl ecl

"B"

Vol. 722


No. 1, 2010

Table 3 (Continued) Observational ID 91103-01-08-00e 91103-01-09-01e 91092-01-01-00e 91092-01-02-00e 91092-02-01-02 91092-02-01-04 91092-02-01-00 91092-02-01-01 91092-02-07-01 91092-02-01-03 91092-02-02-00 91092-02-03-00 91092-02-04-00Ge 91092-02-05-00e 91092-02-06-01e 91092-02-06-02e 91092-02-06-00e 91092-02-07-00 91092-02-08-00e 91103-01-10-00 92424-01-02-05 92424-01-01-00 92424-01-0