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64 Chapter 2. Multiwavelength approach to LS 5039 Radial velocity [km/s] 30 20 10 0 −10 −20 −30 0.0 0.5 1.0 Orbital phase Figure 2.13: Radial velocity measurements obtained with the INT on 2002 July 23–31, folded using the ephemeris of McSwain et al. (2001). We show in Fig. 2.13 our obtained data with the INT folded with the ephemeris of McSwain et al. (2001), and plotted using the same X, Y intervals as in Fig. 2.11. While with those ephemeris the minimum takes place at phase 0.96 (see Fig. 2.11), here it occurs at phase ∼0.1–0.2. This indicates that the period used is not accurate enough, which is compatible with the error quoted in the McSwain et al. (2001) ephemeris (possible improvement of ephemeris is discussed in Casares et al. 2002). In order to obtain the rotational broadening, we have followed the technique applied to A0620-00 by Marsh et al. (1994) and described in their paper. Essentially, we subtract different broadened versions of a O7V((f)) template (HD 168075) from the Doppler corrected sum of our LS 5039 spectra and perform a χ 2 test on the residuals. The O7V spectrum was broadened by convolution with the rotational profile of Gray (1976) which assumes a linearized limb darkening coefficient ɛ. We have taken ɛ=0.20 which is appropriate for the stellar parameters of our star (Teff 35000 K, log g = 4) in the B-band. We performed the analysis independently for the two groups of spectra at different resolutions, 83 and 30 km s −1 , and we find
2.6. The X-ray counterpart: RX J1826.2−1450 65 that the minimum χ 2 is achieved for the spectrum broadened by σbroad = 105 ± 1 and 126±12 km s −1 , respectively. Since the template has a rotational broadening of σHD 168075 = 79 ± 3 km s −1 (Penny 1996), we need to sum this quadratically to σbroad in order to get the true rotational broadening of LS 5039. Therefore, we obtain 131 ± 3 and 149 ± 12 km s −1 for the two resolutions. These numbers are in excellent agreement with the value V sin i = 131 ± 6 km s −1 obtained McSwain et al. (2001). 2.6 The X-ray counterpart: RX J1826.2−1450 The X-ray binary name that appears in the Liu et al. (2000) catalog of HMXBs, which always comes from X-ray satellites, is RX J1826.2−1450, after the ROSAT All Sky Suvey (RASS). However, in the definitive version of the ROSAT Bright Source Catalog (RBSC) it is listed as 1RXS J182615.1−145034. In this section we present the long-term X-ray lightcurve obtained by ASM/RXTE, pointed observations by PCA/RXTE and pointed observations by BeppoSAX. 2.6.1 The ASM/RXTE data As we have mentioned in Sect. 2.4.3, LS 5039 was included at our request in the catalog of the All Sky Monitor (ASM), onboard the Rossi X-ray Timing Explorer (RXTE), in order to follow its behavior in the X-ray domain. An analysis of the first ∼ 33 months of ASM/RXTE data was presented in Ribó et al. (1999). Here we report ASM/RXTE 19 observations spanning almost six and a half years (MJD 50136.78–52501.41), from 1996 February to 2002 August. The dataset contains more than 1800 daily flux measurements in the energy range 1.5–12 keV. Each data point represents the one-day average of the fitted source fluxes from a number (typically 5– 10) of individual ASM dwells, of ∼90 s each (see Levine et al. 1996 for more details). The one-day average light curve is shown in Fig. 2.14. The big gap between Modified Julian Date ∼ 50400 and ∼ 50500 corresponds to the passage of the Sun close to the source during the first year of observations. This gap repeats the following years (near MJD 50800, 51150, 51900 and 52250). That is the reason why we have a dataset of only 1800 one-day average points spanning nearly ∼ 2400 days. 19 Quick-look results provided by the ASM/RXTE team.
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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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12 Chapter 1. Introduction and back
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Bibliography Ankay, A., Kaper, L.,
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BIBLIOGRAPHY 117 Schaerer, D., de K
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Part II A search for new microquasa
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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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150 Chapter 6. EVN and MERLIN obser
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General conclusions 171 Since each
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