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100 Chapter 3. LS 5039 as a runaway microquasar the two OB associations found in the path of LS 5039 are too close to us to be related to it. Since we have not been able to fix a limit on the integration time in the past thanks to a possible relationship with an OB association, we will use the vertical distribution of early-type stars in the Galaxy for this purpose. O-type stars are typically located at distances within 45 ± 20 pc from the galactic midplane (Reed 2000), i.e., from Z −65 to Z +65 pc. According to the galactic latitude of LS 5039 and using a distance of 2.9 ± 0.3 kpc, its actual height is Z = −65 ± 7 pc. Since it is escaping from the galactic plane, we can compute the trajectory backward in time up to when it had a height of Z = +65 pc, which was ∼ 1.1 Myr ago. Hence, the SN explosion probably took place in the last ∼ 1.1 Myr. Thus, for a possible association of LS 5039 with a SNR, we will focus our attention on the galactic trajectory of the binary system for the last ∼ 1 Myr. In addition, the likelihood of detecting a SNR decreases with time, so it is not expected that the radio emission of the SNR can be observed much beyond the time interval considered above (e.g., Shklovskii 1968). A search in a catalog of galactic supernova remnants (Green 2000) reveals the presence of several SNRs near the path of LS 5039 on the plane of the sky, though the center of none of them is crossed by its trajectory. Only three of them, namely SNR G016.7+00.1, SNR G016.8−01.1, and SNR G018.8+00.3, are within 1 ◦ of the LS 5039 path. The distance to SNR G016.7+00.1 was estimated to be at ∼ 14 kpc by Reynoso & Mangum (2000), making impossible an association with LS 5039. Dubner et al. (1999) concluded that SNR G018.8+00.3 is located at 1.9 ± 0.5 kpc, and has an age of ∼ 16 000 yr. Although the distance is not very different from the one to LS 5039, the age of this SNR is by far too short to be associated with the microquasar. Hence, the only remaining candidate is SNR G016.8−01.1, which deserves a detailed study. 3.4 SNR G016.8−01.1 A wide field radio map of the surrounding of LS 5039 is shown in Fig. 3.2, with the microquasar (contours) and the nearby SNR G016.8−01.1 (grey scale), together with the position of the H ii-region RCW 164 (which is the stronger source in the
3.4. SNR G016.8−01.1 101 DECLINATION (J2000) -14 30 35 40 45 50 55 -15 00 LS 5039 SNR G016.8-01.1 o b = -0.8 RCW 164 18 26 30 15 00 25 45 30 15 00 24 45 30 RIGHT ASCENSION (J2000) Figure 3.2: Wide field radio map of LS 5039, its nearby shell-like SNR G016.8−01.1 and the H ii-region RCW 164 (which is the stronger source in the field). The grey scale emission is taken from the Parkes-MIT-NRAO tropical survey at the 6 cm wavelength (Tasker et al. 1994). The overlaid contours correspond to the NVSS map of the region at the 20 cm wavelength (Condon et al. 1998). The arrow marks the proper motion sense (see text). The dashed line is the computed trajectory for the last 10 5 yr, with the corresponding error boxes in position at that epoch and 5 × 10 4 yr ago. The dotted line represents positions with a galactic latitude of −0.8 ◦ for reference purposes.
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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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28 BIBLIOGRAPHY Lewin, W. H. G., va
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30 BIBLIOGRAPHY
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Chapter 2 Multiwavelength approach
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2.3. An interesting target in the s
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2.4. The radio counterpart: NVSS J1
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Page 95 and 96: 2.4. The radio counterpart: NVSS J1
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Page 111 and 112: 2.6. The X-ray counterpart: RX J182
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Page 127 and 128: Figure 2.23: Scenario where the mul
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Page 135 and 136: Bibliography Blandford, R. D., & K
Page 137 and 138: BIBLIOGRAPHY 91 Merck, M., Bertsch,
Page 139 and 140: Chapter 3 LS 5039 as a runaway micr
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Page 159 and 160: 3.7. Conclusions 113 6. Finally, th
Page 161 and 162: Bibliography Ankay, A., Kaper, L.,
Page 163 and 164: BIBLIOGRAPHY 117 Schaerer, D., de K
Page 165: Part II A search for new microquasa
Page 168 and 169: 122 Chapter 4. The cross-identifica
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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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