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X-Ray Analysis of Starburst and AGN Components

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X-Ray Analysis of Starburst and AGN Components Technische Universit¨at Munc¨ hen International Max-Planck Research School on Astrophysics Max-Planck-Institut fur¨ Extraterrestrische Physik X-Ray Analysis of Starburst and AGN Components Yi Fan Vollst¨andiger Abdruck der von der Fakult¨at fur¨ Physik der Technischen Universit¨at Munc¨ hen zur Erlangung des akademischen Grades eines Doktors der Naturwissenschaften genehmigten Dissertation. Vorsitzender: Univ.-Prof. Dr. M. Ratz Prufer¨ der Dissertation: 1. Hon.-Prof. Dr. G. Hasinger 2. Univ.-Prof. Dr. R. Kruc¨ ken Die Dissertation wurde am 19.04.2007 bei der Technischen Universit¨at Munc¨ hen ein- gereicht und durch die Fakult¨at fur¨ Physik am 14.05.2007 angenommen. SUMMARY The X-ray properties of Starburst and Active Galactic Nuclei (AGN) components of three galaxies (NGC 6240, NGC 2782, and NGC 1386) in the local universe are analysed in this dissertation. These galaxies are well suited to study the physics of Starburst and AGN components. They serve as the nearby laboratories for the corresponding objects at high redshifts. The X-ray observations of these galaxies were performed with the ACIS-S detector of Chandra X-ray observatory. The Chandra ACIS-S imaging spec- troscopy allows us to do both imaging analysis and spectral analysis of the data in great detail. It is possible for us to spatially resolve the different contributing components of the complex sources, do the spectral analysis of these components separately, and derive their physical properties systematically. The Chandra ACIS-S observation of the Ultraluminous Infrared galaxy NGC 6240 which contains a binary AGN, demostrates that starburst and AGN components con- tribute to its X-ray emission. The bright extended emission, both near the AGNs and extending over spatial scales of 10 kpc, probably originates from hot thermal plasma and high-mass X-ray binaries. This emission is attributed to starburst activity. The 2-10 keV luminosity of the bright extended emission correlated with the infrared lu- minosity is a good indicator of the current global star formation rate in the galaxy. Surrounding the bright extended emission, a weak halo component appears to be ex- tended on a scale of ∼40 kpc, with evidence for thermal emission (with a constant temperature kT ∼ 0.6 keV). The northern and southern AGNs located in the center of the galaxy are heavily obscured and the reflection components dominate in the Chan- dra bandpass. Strong neutral Fe Kα lines at 6.4 keV are detected from the two nuclei. The southern nucleus is also found to show ionized iron lines at energies higher than 6.4 keV, indicating the existence of a warm scattering medium. A \jet-like" structure close to the southern nucleus seems to be scattered emission. For the starburst galaxy NGC 2782, the Chandra data allow us to disentangle the X-ray emission from this galaxy, for the first time, into three contributing components. A weak large-scale halo emission extends northward and southward, respectively. The bright extended emission including a southern shell-like emission is correlated with the optical (Hα) and radio bubble structures. The correlation of X-ray and optical/radio emission as well as the thermal-plasma spectrum of the bright extended emission indi- cates starburst-driven superwinds as the origin. In the center of the galaxy, a compact core source dominates in the high energy X-ray band (above 2 keV). We found indica- tions for an Fe Kα line with large equivalent width. Therefore, the emission from this compact core source is most likely the reflected/scattered component of an obscured AGN. However, we can not rule out the possibility of an Ultraluminous X-ray source (ULX) in the center of this galaxy, even though we consider it unlikely. In the Seyfert 2 galaxy NGC 1386, the soft X-ray extended emission is spatially resolved and coincident with the optical [OIII] emission from the narrow line region (NLR). The spectrum of the extended emission can be fitted by a black-body or a bremsstrahlung model. A soft X-ray structure north of the nucleus is correlated with an optical blob in the [OIII] images. This structure is in the outer part of the NLR. The large equivalent width of the Fe Kα line in combination with the ratio of the [OIII] and X-ray luminosity suggests that the AGN in NGC 1386 is also heavily obscured. iii iv ZUSAMMENFASSUNG In der vorliegenden Dissertation werden die R¨ontgeneigenschaften von Starburst - und aktiven galaktischen Kern (AGN) - Komponenten dreier Galaxien (NGC 6240, NGC 2782, NGC 1386) im lokalen Universum analysiert. Diese Galaxien eignen sich gut dazu, die Physik von Starburst und AGN Komponenten zu untersuchen. Sie dienen als nahe Laboratorien fur¨ die entsprechenden Objekte bei h¨oheren Rotverschiebun- gen. Die Beobachtungen dieser drei Galaxien wurden mit dem ACIS-S Detektor des R¨ontgensatelliten Chandra durchgefuhrt.¨ Die abbildende Spektroskopie mit Chandra's ACIS-S erlaubt es uns, eine sehr genaue Analyse sowohl von direkten Abbildungen, als auch von Spektren durchzufuhren.¨ So ist es damit m¨oglich, die unterschiedlichen beitragenden Komponenten der komplexen Quellen r¨aumlich aufzul¨osen, ihre Spektren zu analysieren und ihre physikalischen Eigenschaften systematisch herzuleiten. Die Beobachtung der extrem leutchkr¨aftigen Infrarotgalaxie NGC 6240, die einen Doppel-AGN-Kern enth¨alt, mit dem ACIS-S Detektor demonstriert, dass Starburst und AGN Komponenten zu ihrer R¨ontgenemission beitragen. Die helle ausgedehnte Emission, nahe der AGNs ist ub¨ er einen r¨aumlichen Bereich von 10 kpc ausgedehnt, und wird wahrscheinlich von heissem thermischem Plasma und von massereichen R¨ontgen- doppelsternen erzeugt. Diese Emission ist der Starburst-Aktivit¨at zuzuordnen. Die 2-10 keV Helligkeit der hellen ausgedehnten Emission, die mit der Infrarothelligkeit ko- rreliert ist, ist ein guter Indikator fur¨ die derzeitige Sternentstehungsrate der Galaxie. Diese helle ausgedehnte Emission ist von einer schwachen Halokomponente umgeben, die sich bis auf ∼ 40 kpc ausdehnt, in der es Anzeichen fur¨ thermische Emission gibt (mit einer konstanten Temperatur von kT ∼ 0.6 keV). Die n¨ordlichen und sudlic¨ hen AGNs im Zentrum der Galaxie sind stark verdunkelt, so daß ihre reflektierenden Kom- ponenten im Chandra Energieband dominieren. Stark ausgepr¨agte neutrale Fe Kα Lin- ien wurden in beiden Kernen nachgewiesen. Im Spektrum des sudlic¨ hen Kerns findet man außerdem Linien von ionisiertem Eisen bei Energien h¨oher als 6.4 keV, was auf die Existenz eines warmen Streumediums schliessen l¨asst. Eine Jet-¨ahnliche Struktur nahe des sudlic¨ hen Kerns scheint durch gestreute Strahlung zustandezukommen. Fur¨ die Starburstgalaxie NGC 2782 erlauben die Chandra-Daten es uns zum er- sten mal, die R¨ontgenemission in drei beitragende Komponenten aufzuspalten. Eine schwache Halostrahlung breitet sich jeweils nach Norden und Suden¨ aus. Die helle ausgedehnte Strahlung, die auch eine schalenartige Struktur im Suden¨ beinhaltet, ist mit einer blasenartigen optischen (Hα) und Radio Struktur korreliert. Die Korrelation der optischen/Radio Emission, so wie das thermische Spektrum der hellen ausgedehn- ten Strahlung legen einen durch Starburst getriebenen Superwind als Ursache nahe. Im Zentrum der Galaxie dominiert eine kompakte Quelle die harte R¨ontgenstrahlung (oberhalb von 2 keV). Wir finden Anzeichen fur¨ eine Eisenlinie mit hoher Aquiv¨ alent- breite, deshalb ist die Emission dieser kompakten Kernquelle h¨ochstwahrscheinlich auf die reflektierte/gestreute Komponente eines verdeckten AGN zuruc¨ kzufuhren,¨ wobei eine ultraleuchtkr¨aftige Quelle im Zentrum dieser Galaxie nicht ausgeschlossen werden kann, auch wenn das eher unwahrscheinlich ist. Die weiche R¨ontgenstrahlung in der Seyfert-2 Galaxie NGC 1386 wurde r¨aumlich aufgel¨ost und f¨allt mit der optischen [O III] Emission der schmalen Emissionslinien- region (NLR) zusammen. Das Spektrum der ausgedehnten Strahlung kann durch ein v vi Schwarzk¨orperstrahlungs - oder ein Bremsstrahlungs-Modell angen¨ahert werden. Eine klumpenartige Struktur im weichen R¨ontgenband n¨ordlich des Kerns ist mit einem Emissionsgebiet im optischen [O III] verbunden. Diese Struktur ist im ausseren¨ Teil der NLR. Die große Aquiv¨ alentbreite der Fe Kα Linie in Verbindung mit dem Verh¨altnis von [O III] und der R¨ontgenhelligkeit legen nahe, dass der AGN in NGC 1386 ebenso stark obskuriert ist. TABLE OF CONTENTS SUMMARY iii ZUSAMMENFASSUNG v LIST OF FIGURES x LIST OF TABLES xi 1 INTRODUCTION 1 1.1 Obscured Active Galactic Nuclei . 1 1.2 Starbursts . 3 1.2.1 Starburst-driven Superwinds . 3 1.2.2 X-ray spectral components of Starburst galaxies . 4 1.3 Ultraluminous Infrared Galaxies . 4 1.4 The Chandra Mission . 6 1.4.1 Overview . 6 1.4.2 On-orbit performance . 7 1.4.3 Scientific performance . 8 1.5 The aims and the selected objects . 8 1.6 Outline of this dissertation . 10 2 NGC 6240 11 2.1 Introduction . 11 2.1.1 Previous observations . 12 2.1.2 Chandra observations and data reduction . 12 2.2 Imaging analysis . 13 2.2.1 Morphology and different contributing components . 13 2.2.2 Specification of individual regions . 17 2.2.3 Metallicity map . 22 2.2.4 X-ray/optical counterparts and the absolute astrometric accuracy 22 2.3 Spectral analysis . 23 2.3.1 Spectral fitting descriptions . 23 2.3.2 Halo emission . 26 2.3.3 Three loops: Region 1, 2 and 3 . 29 2.3.4 The Extended Region . 37 2.3.5 The binary AGN emission . 41 2.3.6 The jet-like structure . 49 2.4 Discussion . 51 2.4.1 Large scale halo emission . 51 2.4.2 Bright X-ray emission from the Extended Region . 52 2.4.3 Estimate of an upper limit for the luminosity of off-nuclear X-ray sources . 53 2.4.4 The nuclear emission . 55 2.5 Summary . 56 vii viii 3 NGC 2782 58 3.1 Introduction . 58 3.2 Observations and data reduction . 59 3.3 Imaging analysis .
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