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78 Chapter 2. Multiwavelength approach to LS 5039 The importance of the association between LS 5039 and 3EG J1824−1514 is not only because of the discovery of high-energy γ-ray emission in a microquasar, but mainly because of the large number of still unidentified EGRET sources. The Third EGRET catalog contains a total of 271 sources, of which 103 are identified objects: 66 high-confidence AGN, 27 low-confidence AGN, 7 pulsars, 1 detection from the Large Magellanic Cloud, 1 solar flare and the radiogalaxy Centaurus A. Among the remaining 168 unidentified sources (62%), 72 of them have |b| < 10 ◦ . Therefore, this association opens the possibility that some of the high-energy unidentified γ-ray sources at low galactic latitudes could be silent microquasars to be discovered in the near future. +180 Active Galactic Nuclei Unidentified EGRET Sources 3EG J1824-1514 / LS 5039 Third EGRET Catalog E > 100 MeV +90 -90 Pulsars LMC Solar FLare Figure 2.21: The Third EGRET source Catalog shown in galactic coordinates. The size of the symbol represents the highest intensity seen for this source by EGRET. The white cross inside a black circle (l = 16.88 ◦ and b = −1.29 ◦ ) indicates the γ-ray source 3EG J1824−1514, to be associated with LS 5039. Adapted from Hartman et al. (1999). -180
2.8. A proposed scenario to explain the multiwavelength behavior 79 2.8 A proposed scenario to explain the multiwavelength behavior 2.8.1 Spectral energy distribution In Fig. 2.22 we show the observed spectral energy distribution of LS 5039 ranging from radio wavelengths to γ-rays. We have quoted the domains within the electro- magnetic spectrum and the different names of LS 5039 according to each wavelength range. log (ν F ν [erg s −1 cm −2 ]) −7 −9 −11 −13 −15 −17 NVSS J182614−145054 LS 5039 RADIO NIR/OPTIC RX J1826.2−1450 3EG J1824−1514 X−RAY GAMMA−RAY 10 15 20 25 log (ν [Hz]) Figure 2.22: Observed spectral energy distribution of LS 5039. The radio data corre- spond to the fit in Eq. 2.1, the near infrared (NIR) and optical data are those quoted in Table 2.5, the X-ray data comes from the fit to the PCA/RXTE data shown in Fig. 2.17, and the γ-ray data comes from the fit to the spectrum shown in Fig. 2.20.
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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 74 and 75: 28 BIBLIOGRAPHY Lewin, W. H. G., va
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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
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128 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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