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University of Groningen Host Galaxies and Environments of Compact Extragalactic Radio Sources Labiano Ortega, Alvaro

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University of Groningen Host Galaxies and Environments of Compact Extragalactic Radio Sources Labiano Ortega, Alvaro University of Groningen Host galaxies and environments of compact extragalactic radio sources Labiano Ortega, Alvaro IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2006 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Labiano Ortega, A. (2006). Host galaxies and environments of compact extragalactic radio sources. s.n. Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 05-10-2021 RIJKSUNIVERSITEIT GRONINGEN Host galaxies and environments of compact extragalactic radio sources PROEFSCHRIFT ter verkrijging van het doctoraat in de Wiskunde en Natuurwetenschappen aan de Rijksuniversiteit Groningen op gezag van de Rector Magnificus, dr. F. Zwarts, in het openbaar te verdedigen op vrijdag 24 februari 2006 om 10:30 uur door Alv´ aro Labiano Ortega geboren op 14 januari 1977 te Madrid, Spanje Promotor: Prof. Dr. P. D. Barthel Co-promotores: Dr. C. P. O’Dea Dr. R. C. Vermeulen Beoordelingscommissie: Prof. Dr. A. G. de Bruyn Prof. Dr. J. M. van der Hulst Prof. Dr. R. F. Peletier ISBN-nummer: To my parents Cover Image: Artistic representation of the center of an AGN. Credit: Sonoma State University, NASA E/PO, Aurore Simonnet. http://epo.sonoma.edu Back-cover Image: God laughing at a general physics book. Credit: c Joaqun Salvador Lavado (QUINO), Humano se Nace. Editorial Lumen, 1991. Cover design: Abril Gonzalez´ Aragon.´ Contents 1 Introduction 1 1.1 What are the AGN? ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 2 1.2 Radio galaxies ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 5 1.3 What are the GPS and CSS sources? ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 6 1.3.1 Recurrent or smothered sources ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 7 1.3.2 Transient sources ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 7 1.3.3 Frustrated scenario ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 7 1.3.4 Young scenario ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 7 1.4 Current model of the GPS and CSS sources ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 8 1.5 The spectral shape. Synchrotron self-absorption ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 9 1.6 GPS quasars ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 10 1.7 Thesis project ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 13 1.8 Thesis outline ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 14 2 Compact and extended radio sources in the southern sky 15 2.1 Introduction ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 16 2.2 The Molonglo Southern 4 Jy Sample ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 16 2.3 VLA observations of MS4 compact sources £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 17 2.4 Data reduction and mapping ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 17 2.5 Notes on individual sources ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 17 2.6 Results ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 21 2.7 Summary ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 22 3 Optical imaging and spectroscopy of candidate GPS radio sources 33 3.1 Introduction ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 34 3.2 Observations and data reduction ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 34 3.3 Results ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 35 3.3.1 Identifications ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 35 3.3.2 Magnitudes ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 35 3.3.3 Spectra and redshifts ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 36 3.3.4 Stellar synthesis models ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 36 3.4 Notes on individual sources ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 38 3.5 Summary ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 43 vi CONTENTS 4 HST/STIS low dispersion spectroscopy of three CSS sources: Evidence for jet-cloud interaction 53 4.1 Introduction ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 54 4.2 Observations ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 55 4.3 Data reduction ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 55 4.4 Results ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 60 4.4.1 Ionization diagnostics ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 60 4.4.2 Can the central AGN power the emission line luminosity in the ex- tended nebulae? ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ 61 4.4.3 Diagnostic ratios vs. kinematics and distance ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 64 4.4.4 Cloud properties ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 68 4.5 Summary ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 68 5 H I absorption in 3C 49 and 3C 268.3 71 5.1 Introduction ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 72 5.2 Observations and data reduction ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 73 5.2.1 Spectrum analysis ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¡ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 73 5.3 Results ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 75 5.3.1 The Milliarcsecond Scale Continuum Structure ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 76 5.3.2 The H I Absorption ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 79 5.4 Discussion ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 80 5.5 Summary ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 81 6 H I in the one-sided “compact double” radio galaxy B2050+364 83 6.1 Introduction ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 84 6.2 Observations and data processing ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 85 6.2.1 Observations ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 85 6.2.2 Initial calibration and data averaging ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 86 6.2.3 Self-calibration; continuum imaging and modeling ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 87 6.2.4 Spatially resolved spectroscopy ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 88 6.3 Results ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 91 6.3.1 VLBI continuum structure of B2050+364 at 1 GHz ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 91 6.3.2 H I absorption distribution £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 92 6.4 Multi-frequency Radio Continuum Structure ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 93 6.5 Discussion ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 95 6.5.1 B2050+364: a one-sided core-jet structure ? ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 95 6.5.2 The optical redshifts and H I: infall or outflow ? ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 97 6.5.3 The locations of the H I absorbers relative to the radio source ¢ ¡ ¢ 98 6.6 Summary ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 100 7 Star formation in hosts of compact radio galaxies 103 7.1 Introduction ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 104 7.2 Observations and data reduction ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ 104 7.3 Nuclear and emission line contamination ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 106 7.4 UV morphology ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ 107 7.4.1 Notes on individual sources ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 107 vii 7.5 UV and radio properties ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 110 7.6 Stellar synthesis models ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 112 7.7 Summary ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 113 8 Concluding remarks 129 8.1 Developments in the field ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ 129 8.2 Detailed contributions by this thesis ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ £ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 133 8.3 The bottom line: Strong interaction between radio source and host ¢ ¢ ¡ ¢ 134 8.4 Ongoing and future work ¢ ¢ ¡ ¢ £ ¢ ¡ ¢ ¢ ¡ ¢ ¡ ¢ ¡ ¢ ¢ £ ¢ ¡ ¢ ¡ ¢ ¢ ¡ ¢ 135 Nederlandse samenvatting 139 English Summary 141 Bibliography 153 List of Publications 155 Acknowledgements 157 viii Though this be madness, yet there is method in 't. William Shakespeare Hamlet, II, 2. 1 Introduction N 1908, Edward Arthur Fath took an optical spectrum of a galaxy, NGC 1068, and Ifound that the ”spectrum is composite, showing both bright and absorption lines” (Fath 1909). In 1917, higher resolution spectra showed that these emission lines were similar to those observed in planetary nebulae (Slipher 1917). During the next decades, astronomers observed nuclear emission lines in several spiral nebula (see Fig 1.1). Thirty five years after Fath’s observations, Carl Keenan Seyfert realized that several of these galaxies formed a ¡ different group (Seyfert
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