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70 Chapter 2. Multiwavelength approach to LS 5039 The mean X-ray intensity in the energy range 3–30 keV shows a slight decreasing trend with 19.7 ± 0.2 count s −1 at the beginning of the observation (upper panel of Fig. 2.15) compared to 16.6 ± 0.1 count s −1 and 16.2 ± 0.2 count s −1 for the middle and bottom panels of Fig. 2.15, respectively. The fractional rms of the 3–30 keV lightcurve corresponding to the entire observation is 9%. The fact that no X-ray pulsations have been found in RX J1826.2−1450 is con- sistent with the proposed idea that radio emission and X-ray pulsations from X-ray binaries seem to be statistically anti-correlated (Fender et al. 1997, Fender & Hendry 2000), i.e., no X-ray pulsar has ever shown significant radio emission. We have not computed the orbital phase of each one of the PCA/RXTE observations according to the ephemeris by McSwain et al. (2001), since the ∼ 1000 d difference between their T value and our observations is too high to obtain reli- able results due to the lack of accuracy for the orbital period (as we have seen in Sect. 2.5.4). Spectrum Since the lightcurve of the entire observation does not show sharp features, i.e., there is no significant spectral change throughout the observation, we obtained one average PCA energy spectrum from the complete observation, that can be seen in Fig. 2.17. Acceptable fits of the X-ray continuum were obtained with an unabsorbed power- law model, giving a reduced χ 2 =1.14 for 56 degrees of freedom (dof). A multicolor disk model, as expected from an optically thick accretion disk (Mitsuda et al. 1984) plus a power-law gave a reduced χ2 ν =1.11 for 53 dof. Bremsstrahlung and two blackbody component models did not fit the data. Although the addition of a blackbody component to the power-law formally produces an acceptable fit, the value of the blackbody normalization was very low, with the error bar close to zero. In fact, an F-test shows that the inclusion of a blackbody component is not significant. The most salient feature that appears in the spectrum of RX J1826.2−1450 is a strong iron line at ∼ 6.6 keV (Fig. 2.17). A Gaussian fit to this feature gives a line centered at 6.62±0.04 keV, with an equivalent width (EW ) of 0.75±0.06 keV and a F W HM of 0.9 ± 0.2 keV. The best-fit results are given in Table 2.9.
2.6. The X-ray counterpart: RX J1826.2−1450 71 Figure 2.17: PCA spectrum of RX J1826.2−1450 / LS 5039. The continuous line represents the best-fit power-law model plus a Gaussian component for the iron line. When this component is omitted the line shows up clearly in the residuals. Table 2.9: Spectral fit results for the power-law model plus a Gaussian component for the iron line in RX J1826.2−1450 / LS 5039. Uncertainties are given at 90% confidence for one parameter of interest. The spectrum was fitted in the energy range 3–30 keV. Parameters Fitted values NH [×10 21 cm −2 ] 2 +1 −2 Γ 1.95 ± 0.02 Eline(Fe) [keV] 6.62 ± 0.04 EWline(Fe) [keV] 0.75 ± 0.06 F W HMline(Fe) [keV] 0.9 ± 0.2 χ 2 r (dof) 1.14 (56)
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UNIVERSITAT DE BARCELONA Departamen
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Per a la meva neboda Blanca, que va
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feina no presentada en aquesta tesi
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desfogar-nos conjuntament, per la s
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From the scientifical point of view
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Gràcies a la meva germana Nàdia,
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ii CONTENTS I Discovery and study o
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iv CONTENTS II A search for new mic
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vi CONTENTS
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viii Resum de la tesi d’Eddington
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x Resum de la tesi imprescindible p
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xii Resum de la tesi dels sistemes
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xiv Resum de la tesi un comportamen
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xvi Resum de la tesi MilliARC SEC 4
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xviii Resum de la tesi per poder de
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xx Resum de la tesi valors força s
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xxii Resum de la tesi 2. D’entre
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xxiv Resum de la tesi pano Alemán
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xxvi Resum de la tesi 3.3 Observaci
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xxviii Resum de la tesi habitual en
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xxx Resum de la tesi Per tant, si l
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xxxii BIBLIOGRAFIA
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2 Chapter 1. Introduction and backg
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10 Chapter 1. Introduction and back
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Page 66 and 67: 20 Chapter 1. Introduction and back
Page 74 and 75: 28 BIBLIOGRAPHY Lewin, W. H. G., va
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Page 79 and 80: Chapter 2 Multiwavelength approach
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Page 135 and 136: Bibliography Blandford, R. D., & K
Page 137 and 138: BIBLIOGRAPHY 91 Merck, M., Bertsch,
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Page 161 and 162: Bibliography Ankay, A., Kaper, L.,
Page 163 and 164: BIBLIOGRAPHY 117 Schaerer, D., de K
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122 Chapter 4. The cross-identifica
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130 BIBLIOGRAPHY
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132 Chapter 5. Radio and optical ob
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DECLINATION (J2000) DECLINATION (J2
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148 BIBLIOGRAPHY
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150 Chapter 6. EVN and MERLIN obser
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166 BIBLIOGRAPHY
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General conclusions 171 Since each
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