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150 Chapter 6. EVN and MERLIN observations Table 6.1: Observing scheme for target sources and calibrators (EVN and MERLIN). 1XRS name Phase-reference calibrators Cycling scheme (a) Obs. Time [s] [s] J001442.2+580201 J0007+5706 (b) 300/150 7200 J013106.4+612035 J0147+5840 2×(300/150)/300/120 8000 4C 61.02 (c) J042201.0+485610 (c) TXS 0422+496 300/150/300/120/300/150 7500 NRAO 150 J062148.1+174736 J0630+1738 (b) 300/150 6200 J072259.5−073131 1RXS J072418.3−071508 2×(270/180)/240/180 6100 J072418.3−071508 1RXS J072259.5−073131 2×(180/270)/180/240 4700 (a) target/calibrator/2nd calibrator. (b) Used in the VLBI fringe fitting process to guide the target source fringe detection (see text). (c) No fringes found to the radio source. 6.2.1 MERLIN MERLIN is a connected radio interferometer across England, with baselines reaching up to 217 km length. This array observed with 2-bit sampling at dual polarization with two blocks of 16 channels, each channel of 1 MHz bandwidth. We analyzed the left hand circular polarization data excluding one channel at both edges of the band, yielding a final bandwidth of 14 MHz. The correlator integration time was of 4 s. Some antennas did not observe during short periods due to strong winds. Since some of the target radio sources were faint, we scheduled the observations introducing phase-reference calibrators with cycle times of around 7 min (compatible with the expected coherence times). The observing scheme is described in Table 6.1, where we quote the total on-source time for the target sources in the last column. We also observed the fringe-finder DA 193 and the MERLIN flux density calibrator 3C 286. The MERLIN data reduction was carried out at Jodrell Bank Observatory, using standard procedures within the aips software package. We did not detect 1RXS J042201.0+485610. All other sources were detected, and accurate positions for the target radio sources were obtained via phase-referencing. These positions, presented in Table 6.2, were used later as a priori information for the VLBI cor-
6.2. Observations and data reduction 151 Table 6.2: MERLIN positions for the five detected target sources, obtained via phase- referencing. The uncertainties quoted for the target sources were provided by the jmfit task in aips (measuring in the phase-referenced image) and do not include systematic errors. The positions of all phase-reference calibrators except 1RXS J072418.3−071508 have an accuracy better than 1 mas. Target sources Phase-reference calibrators 1RXS name α (J2000.0) δ (J2000.0) Source name α (J2000.0) δ (J2000.0) J001442.2+580201 00 h 14 m 42. s 12822 +58 ◦ 02 ′ 01. ′′ 2460 J0007+5706 (a) 00 h 07 m 48. s 47110 +57 ◦ 06 ′ 10. ′′ 4540 ±0. s 00013 ±0. ′′ 0022 J013106.4+612035 01 h 31 m 07. s 23210 +61 ◦ 20 ′ 33. ′′ 3752 J0147+5840 (a) 01 h 47 m 46. s 54380 +58 ◦ 40 ′ 44. ′′ 9750 ±0. s 00014 ±0. ′′ 0016 J062148.1+174736 06 h 21 m 47. s 75264 +17 ◦ 47 ′ 35. ′′ 0818 J0630+1738 (b) 06 h 30 m 07. s 25870 +17 ◦ 38 ′ 12. ′′ 9300 ±0. s 00006 ±0. ′′ 0017 J072259.5−073131 07 h 22 m 59. s 68188 −07 ◦ 31 ′ 34. ′′ 8009 1RXS J072418.3 (c) 07 h 24 m 17. s 2912 −07 ◦ 15 ′ 20. ′′ 339 ±0. s 00011 ±0. ′′ 0022 −071508 J072418.3−071508 (d) 07 h 24 m 17. s 2912 −07 ◦ 15 ′ 20. ′′ 339 J0730−116 07 h 30 m 19. s 1125 −11 ◦ 41 ′ 12. ′′ 601 ±0. s 0007 ±0. ′′ 010 (a) Position from Patnaik et al. (1992). (b) Position from Browne et al. (1998). (c) This position was obtained from VLA observations (listed in the line below). (d) The entries in this line correspond to VLA observations reported in Chapt. 5 (Table 5.1). relation. The position given in Table 6.2 for the quasar 1RXS J072418.3−071508 was obtained from the VLA observations presented in Sect. 5.2. The position of 1RXS J072259.5−073131 is deduced from the phase-reference offset relative to the source 1RXS J072418.3−071508 provided by MERLIN. To image the sources, we averaged the data in frequency and exported them to be processed into the difference mapping software difmap (Shepherd et al. 1994), where we time-averaged the data in 32 s bins after careful editing. 6.2.2 EVN The EVN observations were performed with the array described in Table 6.3, record- ing in MkIV mode with 2-bit sampling at 256 Mbps with left hand circular polarization. A bandwidth of 64 MHz was used, divided into 8 intermediate frequency (IF) bands (v6cm-256-8-2-L mode). Some antennas did not observe during short periods due to strong winds or snow.
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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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2.5. The optical/IR star: LS 5039 5
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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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