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24 Chapter 1. Introduction and background 1.3 Motivation of the thesis As we have seen, the current number of microquasars is ∼ 16. This number could increase dramatically if, as it has been proposed by Fender & Hendry (2000), radio emission from X-ray binaries always arises from relativistic jets. This would imply that all REXBs, ∼ 40 systems, are microquasars. However, the situation is not so clear yet and REXBs appear as a rather heterogeneous group including both high-mass (e.g., Cyg X-3, LS I +61 303) and low-mass companions (e.g., Aql X-1, GX 339−4). Moreover, in the latter group, radio emission has been detected in all six Z sources and only in a few Atoll sources. In addition, the detection of radio emission does not seem to be limited to a particular type of compact object, since there are REXBs harboring black holes (e.g., GRO J1655−40, Cyg X-1) and neutron stars (e.g., Aql X-1, Sco X-1). Moreover, when one begins to further divide the group of REXBs according to their optical or compact companion or whether radio jets are present or not, the number of systems is no longer enough to perform a meaningful statistical study. The situation is even worse when we focus on microquasars. There is an important question to be answered: what is the matter content of the jets? Up to now, atomic emission lines have only been observed in the jets of SS 433, indicating that the jets are baryonic. However, some of the proposed models can only account for leptonic (e + e − ) jets. Therefore, it is crucial to unveil the matter content if we want to correctly model the accretion/ejection processes that take place near compact objects. Another interesting issue is the possibility of microquasars being sources of high energy γ-rays. Before this work, the 26.5 d periodic REXB LS I +61 303 was the only X-ray binary that could be associated with a high-energy γ-ray source (E > 100 MeV) of the third EGRET catalog (Hartman et al. 1999), namely 3EG J0241+6103 (Kniffen et al. 1997). The search for new REXBs could allow new findings. Indeed, the current most promising candidate is LS 5039 (see Part I), which appears to be associated with the source 3EG J1824−1514 (Paredes et al. 2000). Although these associations will only be confirmed, or discarded, by future missions such as GLAST, clearly a sample of two sources is a very poor one, and any attempt to discover new REXBs/microquasars, and look for possible high energy γ-ray emission, is warranted. Hence, two reasons gave us a strong motivation to start a long-term project
1.3. Motivation of the thesis 25 focused on the search for new microquasars in the Galaxy: 1. Every new microquasar has allowed new interesting phenomenological findings, which have to be taken into account in the proposed models to explain the accretion/ejection processes taking place near compact objects. 2. To enhance the reduced sample and allow meaningful statistical studies in the future. In Part I of this thesis we present the discovery and subsequent study of the microquasar LS 5039. This was the first source to be discovered within the most global approach presented in Part II. There we explain how we have used the best available X-ray and radio catalogs to search for new REXB/microquasar candidates. We state our general conclusions in Part III.
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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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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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