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Multi-Wavelength Study of Narrow-Line Seyfert 1 Galaxies

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Multi-Wavelength Study of Narrow-Line Seyfert 1 Galaxies Multi-Wavelength Study of Narrow-Line Seyfert 1 Galaxies DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Patrizia Romano ***** The Ohio State University 2002 Dissertation Committee: Approved by Professor Bradley M. Peterson, Adviser Professor Richard W. Pogge Advisor Astronomy Graduate Program Dr. Smita Mathur Dr.T.JaneTurner UMI Number: 3076737 ________________________________________________________ UMI Microform 3076737 Copyright 2003 by ProQuest Information and Learning Company. All rights reserved. This microform edition is protected against unauthorized copying under Title 17, United States Code. ____________________________________________________________ ProQuest Information and Learning Company 300 North Zeeb Road PO Box 1346 Ann Arbor, MI 48106-1346 ABSTRACT We study the multiwavelength properties of Ark 564 and Ton S180, two NLS1s that have been the object of extensive multiwavelength spectroscopic campaigns undertaken during the last four years to test the current hypothesis that Narrow-Line Seyfert 1 galaxies (NLS1s) have relatively lower black hole masses and higher accretion rates than normal broad-line Seyfert 1 galaxies (BLS1s) of the same luminosity. We present an analysis of the X-ray variability properties of Ark 564 and Ton S180, based on 35- and 12-day continuous observations with ASCA, respectively. The mean spectra are characterized by a very steep power-law continuum (Γ = 2.54 and 2.44, respectively), a strong soft excess at energies < 2keV,andanFeKα line that has a large equivalent width and originates in ionized material. Their spectral energy distributions peak at significantly higher energies in these objects than in BLS1s (15–100 eV for Ton S180 and ∼ 50 eV in Ark 564). We also find that, based on available UV, FUV and X-ray data on absorption lines, the UV and X-ray absorbers in Ark 564 are physically related, and possibly identical. ii The multiwavelength properties of these two NLS1s are consistent with the predictions of the prevailing model for the structure of NLS1s, i.e. of AGNs with high accretion rate (M˙ ≈ 0.1–0.9) onto a relatively low-mass black hole 6−7 (M ≈ 10 M). iii To my parents and No’, who taught me to follow my dreams, and to Stefano, who helped me realize them. iv ACKNOWLEDGMENTS I wish to thank my advisors, B.M. Peterson, R.W. Pogge, S. Mathur and T.J. Turner, for teaching me and supporting me–each in their unique way–and Anil Pradhan and Don Terndrup, for their encouragement along the years. Their help took different forms that ranged from sound scientific advice to reality check, from proof-reading a manuscript 10 times to fighting software, from a comforting pat on the back to a figurative smack on the side of the head, from supplying sugars to limiting caffeine intake. Cheers go to my Tae Kwon Do gals. Lisa, my sah bum nim, who taught me about power; Deb, my comrade in arms, fellow dissertation struggler who made the time and who taught me about strength and persistence; Kath, tower of strength and true personal inspiration, who brings the grace of a dancer in martial arts; Melanie, my screaming buddy (and possibly the most energetic and ethusiastic woman to walk on this planet), who taught me to “just breathe”; Glenna, strength in motion, who taught me about momentum–and the value of a well-placed kick. And all the others who were there for me through thick and thin. They kept me sane, gave me appropriate targets to hit, quiet places to be, and provided a friendly environment where I could let my hair down. Or up. v They fasted with me, ate with me–they even made sure I was awake in time for my defense. Special tuna-scented thanks go to Oscar and Felix, rotisserie and head-butt furry friends. Last but not least, I wish to thank my parents and my grandmother for supporting me through these long years away from home, and for encouraging me to follow my dreams–even when they involved sciatica and broken bones. Federica and Francesca, my oldtime friends and supporters, out of sight, but not far from my heart. And Stefano, whom I cherish as a brother, a friend, and a lifemate, for his waking me up in the morning and helping me fall asleep at night, and for being there, parted from me and never parted. vi VITA August 21, 1967 . ........ Born– Venice,Italy 1993 . .......................... LaureainAstronomy,UniversityofPadova 1994 . .......................... SummerReaearchProgram,Netherlands Foundation for Research in Astronomy 1994 – 1995 . ................. VisitingScholar,PhysicsDepartment, University of Ljubljana, Slovenia 1995 – 1996 . ................. VisitingScholar,Department of Physics and Astronomy, University of Alabama 1996 – 1997 . ................. GraduateFellow,TheOhioStateUniversity 1997 – 2002 . ................. GraduateTeachingandResearch Associate, The Ohio State University 1999 . .......................... M.S.inAstronomy,TheOhioStateUniversity PUBLICATIONS Research Publications 1. P. Romano, T. Zwitter, M. Calvani, and J. Sulentic, “On the wings of broad H-alpha emission in active galactic nuclei”, Monthly Notices of the Royal Astronomical Society, 279, 165, (1996). 2. P. Romano, P. Marziani, and D. Dultzin-Hacyan, “Balmer Line Variations in vii the Radio-Loud AGN PG 1512+370”, The Astrophysical Journal, 495, 222, (1998). 3. M. Bautista, M., P. Romano, and A.K. Pradhan, “Resonance Averaged Photoionization Cross Sections for Astrophysical Models”, The Astrophysical Journal Supplements, 118, 259, (1998). 4. B.M. Peterson, et al., “X-Ray and Optical Variability in NGC 4051 and the Nature of Narrow-Line Seyfert 1 Galaxies”, The Astrophysical Journal, 542, 161, (2001). 5. T.J. Turner, P. Romano, I.M. George, R. Edelson, S.J. Collier, S. Mathur, and B.M. Peterson, “Multiwavelength Monitoring of the Narrow-Line Seyfert 1 Galaxy Ark 564. I. ASCA Observations and the Variability of the X-Ray Spectral Components”, The Astrophysical Journal, 561, 131, (2001). 6. S. Collier, et al., “Multiwavelength Monitoring of the Narrow-Line Seyfert 1 Galaxy Ark 564. II. Ultraviolet Continuum and Emission-line Variabil- ity”, The Astrophysical Journal, 561, 146, (2001). 7. O. Shemmer, P. Romano, et al., “Multiwavelength Monitoring of the Narrow-Line Seyfert 1 Galaxy Ark 564. III. Optical Observations and the UV–Optical–X-Ray Connection”, The Astrophysical Journal, 561, 162, (2001). 8. P. Romano, T.J. Turner, S. Mathur, and I.M. George, “A 12-day ASCA Observation of the Narrow-Line Seyfert 1 Galaxy Ton S180: Time-Selected Spectroscopy”, The Astrophysical Journal, 564 , 162, (2002). 9. D.M. Crenshaw, et al., “Reddening, Emission-Line, and Intrinsic Ab- sorption Properties in the Narrow-Line Seyfert 1 Galaxy Ark 564”, The Astrophysical Journal, 566, 187, (2002). 10. T.J. Turner, P. Romano, et al., “The Spectral Energy Distribution of the Seyfert Galaxy Ton S180”, The Astrophysical Journal, 568, 120, (2002). viii 11. P. Romano, S. Mathur, R.W. Pogge, B.M. Peterson, and J. Kuraszkiewicz, “FUSE Observations of the Narrow-Line Seyfert 1 Galaxy Arakelian 564”, The Astrophysical Journal, in press, (2002). FIELDS OF STUDY Major Field: Astronomy ix Table of Contents Abstract.................................... ii Dedication................................... iv Acknowledgments............................... v Vita...................................... vii ListofTables................................. xvi ListofFigures.................................xviii ListofAbbreviations.............................xxiii 1 Introduction 1 1.1 Narrow-Line Seyfert 1 Galaxies, a Test Case for AGN Models . 4 1.2TheX-ray/UVWarmAbsorber.................... 8 x 1.3SpectralEnergyDistributionofNLS1s................ 9 1.4TheFocusofThisStudy........................ 11 1.5PublishedWork............................. 14 2 Multiwavelength Monitoring of the Narrow-Line Seyfert 1 Galaxy Ark 564. ASCA Observations and the Variability of the X-ray Spectral Components 16 2.1Introduction............................... 16 2.2ObservationsandDataReduction .................. 18 2.3 The Time Variability . 20 2.3.1 Fractional Variability Amplitude . 22 2.4TheMeanSpectrum.......................... 24 2.4.1 TheSoftComponent...................... 26 2.4.2 The Fe Kα Regime....................... 27 2.4.3 X-rayandUVAbsorption................... 31 2.5 Spectral Variability . 31 2.5.1 MethodandSelectionDetails................. 31 xi 2.5.2 Variability of the Continuum . 33 2.5.3 Variability of the Soft X-ray Hump . 34 2.5.4 Variability of the Fe Emission Line . 37 2.6RMSSpectra.............................. 40 2.7Cross-correlationResults ....................... 41 2.8SummaryofObservationalResults.................. 44 2.9DiscussionandConclusions...................... 46 3 A 12–day ASCA Observation of the Narrow-Line Seyfert 1 Galaxy Ton S180: Time-Selected Spectroscopy 67 3.1Introduction............................... 67 3.2ObservationsandDataReduction .................. 68 3.3 The Time Variability . 70 3.3.1 Fractional Variability Amplitude . 73 3.4TheMeanSpectrum.......................... 74 3.4.1 TheSoftComponent...................... 76 xii 3.4.2 The Fe Kα Regime....................... 78 3.5 Spectral Variability . 80 3.5.1 MethodandSelectionDetails................. 80 3.5.2 Variability of the Continuum . 81 3.5.3 Variability of the Soft X-ray Hump . 82 3.5.4 Variability of the Fe Emission Line . 84 3.5.5 RMSSpectra.......................... 87 3.6SummaryofObservationalResults.................. 88 3.7ComparisonwithArk564......................
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