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20 Chapter 1. Introduction and background near the Galactic center; and GRS 1915+105, the first superluminal source to be discovered in the Galaxy, and recently found to have the most massive black hole as well as the longest orbital period in the microquasar group. We can see that up to now, four sources have shown superluminal motions, namely GRS 1915+105, GRO J1655−40, XTE J1748−288 and V4641 Sgr, while such phenomenon is also suspected in XTE J1550−564. We show in Fig. 1.6 the distribution in galactic coordinates of the microquasars listed in Table 1.3, together with their respective names. Galactic latitude [deg] 90 60 30 0 −30 −60 XTE J1118+480 LS I +61 303 Microquasars in the Galaxy Cyg X−1 Cyg X−3 GRS 1758−258 GRS 1915+105 SS 433 LS 5039 Sco X−1 V4641 Sgr XTE J1748−288 GRO J1655−40 Cir X−1 GX 339−4 1E1740.7−2942 XTE J1550−564 LMXB LMXB (rel. jets ?) HMXB HMXB (rel. jets ?) −90 180 120 60 0 300 240 180 Galactic longitude [deg] Figure 1.6: Distribution of known microquasars in galactic coordinates. Filled circles represent those sources where relativistic jets have been imaged, while open circles are used for those where hints of relativistic jets have been seen or are clearly suspected.
1.2. Microquasars 21 1.2.4 Accretion disk and jet formation It is currently accepted that the formation of relativistic radio jets requires the presence of a compact object (a potential well) and an accretion disk surrounding it. The mechanism of jet formation and collimation is not yet well understood, but we can gain knowledge and test proposed models after performing observations like the ones of GRS 1915+105 shown in Fig. 1.7. We can see that after a large- amplitude quasi-periodic oscillation, the X-ray flux drops substantially, a behavior interpreted as the emptying of the inner accretion disk. At the same time, the X- ray spectrum becomes significantly hard, until when an X-ray spike is seen. Then the X-ray spectrum softens again and we can see the starting of a flare at infrared wavelengths, which is interpreted in terms of synchrotron emission by an expanding plasma cloud, as shown above the lightcurves, ejected just when the X-ray spike took place. As the plasma cloud expands adiabatically, the maximum of the emitted energy shifts to longer wavelengths, and a subsequent flare is detected in the radio. Luminosity [arbitrary units] 1.0 0.5 0.0 X−RAYS Disk emptying 280.000 INFRARED Ejection RADIO km/s 7.9 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.7 8.8 8.9 UT Time [hours] Figure 1.7: Simultaneous multiwavelength behavior at X-ray, radio and infrared wavelengths of GRS 1915+105 during 1997 September 9 (from Mirabel et al. 1998).
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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,
Page 16 and 17: ii CONTENTS I Discovery and study o
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2.6. The X-ray counterpart: RX J182
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2.6. The X-ray counterpart: RX J182
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2.7. The γ-ray counterpart: 3EG J1
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2.7. The γ-ray counterpart: 3EG J1
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2.8. A proposed scenario to explain
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Figure 2.23: Scenario where the mul
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2.9. Conclusions 87 8. We have carr
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Bibliography Blandford, R. D., & K
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BIBLIOGRAPHY 91 Merck, M., Bertsch,
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Chapter 3 LS 5039 as a runaway micr
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3.1. Positions and proper motions 9
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3.1. Positions and proper motions 9
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3.3. The past trajectory of LS 5039
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3.4. SNR G016.8−01.1 101 DECLINAT
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3.4. SNR G016.8−01.1 103 Normaliz
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3.4. SNR G016.8−01.1 105 Galactic
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3.5. The H i surroundings of LS 503
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3.6. Discussion 109 experienced a h
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3.6. Discussion 111 At this point w
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3.7. Conclusions 113 6. Finally, th
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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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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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