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Understanding the Formation and Evolution of Disc Break Features in Galaxies

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Understanding the Formation and Evolution of Disc Break Features in Galaxies UNDERSTANDING THE FORMATION AND EVOLUTION OF DISC BREAK FEATURES IN GALAXIES JARKKO LAINE Astronomy Research Unit University of Oulu Finland Academic Dissertation to be presented with the assent of the Faculty of Sci- ence, University of Oulu, for public discussion in the Auditorium GO101, on September 16th, 2016, at 12 o'clock. REPORT SERIES IN PHYSICAL SCIENCES Report No. 101 OULU 2016 • UNIVERSITY OF OULU Opponent Prof. John Beckman, Instituto de Astrof´ısicade Canarias, La Laguna, Spain Reviewers Prof. Jari Kotilainen, Finnish Centre for Astronomy with ESO, University of Turku, Finland Dr. Ruym´anAzzollini, Mullard Space Science Laboratory, United Kingdom Custos Docent Eija Laurikainen, Astronomy Research Unit, University of Oulu, Finland ISBN 978-952-62-1303-3 ISBN 978-952-62-1304-0 (PDF) ISSN 1239-4327 Juvenes Print Oulu 2016 i Laine, Jarkko Johannes: Understanding the formation and evolu- tion of disc break features in galaxies Astronomy Research Unit P.O. Box 3000 FIN-90014 University of Oulu FINLAND Abstract The discs in galaxies are radially extended, rotationally supported, flattened systems. In the cosmological Lambda Cold Dark Matter model the formation of the discs is intimately connected with galaxy formation. Generally it is as- sumed that the discs have exponentially decreasing stellar surface brightness profiles, but completely satisfactory theoretical explanation for this has not been presented. Large number of studies in the past decade have challenged this view, and have found a change in the slope of the surface brightness profile in the outer regions of many galaxies discs: the surface brightness can decrease more, or less, steeply than in the inner regions. The transition be- tween the two slopes is often called a disc break. Consequently, the discs are divided in three major categories: single exponential Type I, down-bending break Type II, and up-bending break Type III. Formation of these break fea- tures has been linked to the initial formation of the discs, internal evolution, and also with the interactions between galaxies. By studying the detailed properties of the disc break features, the evolutionary history of discs, and galaxies in general, can be better understood. The thesis work focuses on the structural analysis of the galaxies in the Spitzer Survey of Stellar Structure in Galaxies (S4G), which consists of 2352 galaxies observed in the 3.6 and 4.5 µm mid-infrared wavelengths with the Spitzer space telescope. Work has been carried out as a part of the data- analysis pipelines of the S4G survey, utilizing surface photometry. In addi- tion, special emphasis has been put on the study of the disc and disc break properties in a wide range of galaxy morphological types and stellar masses. The thesis work attempts to at least partially understand how galaxy stellar mass and observed wavelength affect the properties of the discs and breaks, and how galaxy structural components are connected with the breaks. The data comprises mainly of the 3.6 µm infrared data, providing a view to the stellar mass distribution of galaxies. We find that the Type II breaks are the most common disc profile type, found in 45 ± 2% of the sample galaxies, consisting of 759 galaxies in the stellar mass range 8:5 . log10(M∗=M ) . 11. Type I discs are found in 31 ± 2%, and the Type III breaks in 23 ± 2% of the sample. The fraction of the profile types also depends of the galaxy stellar mass: fractions of the Types II and III ii increase, while Type I fraction decreases, with increasing stellar mass. We attribute these changes with stellar mass to the increased frequency of bar resonance structures in higher mass galaxies, which are commonly associated with a Type II break, and to the increased fraction of Type III profiles in generally more massive early-type disc galaxies. In addition to the Type II breaks associated with bar resonance structures, we find that nearly half of these breaks relate to the visual spiral outer edge, confirming previous results of the Type II break connection with galaxy structure, and thus the internal evolution rather than initial formation of discs. Complementary data in optical wavelengths from the Sloan Digital Sky Survey shows a strong change in the properties of the discs inside the Type II breaks, indicating that the inner discs are evolving via star formation. In late- type spiral galaxies (T & 4) with a Type II break, possible evidence of radial stellar migration is found in the outer disc: the slope of the surface brightness profile is shallower in the infrared compared to optical wavelengths, indicating that older stellar populations are more evenly spread throughout the disc. Formation of the Type I and III profiles remain poorly understood. However, indication that some of the Type III profiles are formed by environmentally driven processes is found, with a correlation between the properties of the local environment and the disc profile parameters. Furthermore, indication of star formation possibly causing the up-bends in spiral galaxies is found through a presence of young stellar population in the outer disc section. Key words: Galaxies, galaxy formation, galaxy evolution, galaxy environ- ment, photometry, infrared, optical Acknowledgments The work presented in this PhD thesis has been performed at the Astronomy Research Unit in the University of Oulu. First of all I would like to thank the supervisors of the thesis work, Docent Eija Laurikainen and Professor Heikki Salo, for your support and guidance throughout these past years. Without your tremendous help this work would not have been possible. I thank you also for introducing me to the S4G and other collaborations, which have provided unique opportunities. Special thanks goes to the past and present fellow PhD students of the galaxy group: Sim´onD´ıaz-Garc´ıa,Mart´ınHerrera-Endoqui, Marius Lehmann, Aku Venhola, and Joachim Janz, for your company, support, and help dur- ing these years. I am also grateful for all the other members of the astron- omy unit: Pertti Rautiainen, S´ebastienComer´on,J¨urgenSchmidt, Xiaodong Liu, Vitaly Neustroev, Soile Kukkonen, and Tuulia Pennanen, for creating a pleasant and supportive atmosphere to work in. I would also like to thank Prof. Jari Kotilainen and Dr. Ruym´anAzzollini for the pre-examination of this thesis. Many others are also deserving of my gratitude, however they are too numerous to be listed here. Financial support from the Vilho, Yrj¨o,and Kalle V¨ais¨al¨afoundation of the Finnish Academy of Science and Letters, Finnish Academy, Physics Department of University of Oulu, and University of Oulu Graduate School is also acknowledged. Finally, I thank my friends near and far for all your time and company, which has always reminded me of what is truly important in life. I am deeply grateful for my parents and family. You have always allowed me to find my own way, and have supported me in whichever path I choose. Oulu, August 2016 Jarkko Laine iii iv LIST OF ORIGINAL PAPERS The present thesis contains an introductory part and the following papers, referred in the text by their Roman numerals: I. Laine J., Laurikainen E., Salo H., Comer´onS., Buta R. J., Zaritsky D., Athanassoula E., Bosma A., Mu~noz-Mateos J.-C., Gadotti D. A., Hinz J. L., Erroz-Ferrer S., Gil de Paz A., Kim T., Men´endez-Delmestre K., Mizusawa T., Regan M. W., Seibert M., Sheth K. Monthly Notices of the Royal Astronomical Society, 2014, 441, 3: Morphology and environment of galaxies with disc breaks in the S4G and NIRS0S II. Mu~noz-MateosJ.-C., Sheth K., Regan M., Kim T., Laine J., Erroz- Ferrer S., Gil de Paz A., Comeron S., Hinz J. L., Laurikainen E., Salo H., Athanassoula E., Bosma A., Bouquin A. Y. K., Schinnerer E., Ho L., Zaritsky D., Gadotti D. A., Madore B., Holwerda B., Men´endez- Delmestre K., Knapen J. H., Meidt S., Querejeta M., Mizusawa T., Seibert M., Laine S., Courtois H. The Astrophysical Journal Supplement Series, 2015, 219, 1: The Spitzer Survey of Stellar Structure in Galaxies (S4G): Stellar Masses, Sizes, and Radial Profiles for 2352 Nearby Galaxies III. Salo H., Laurikainen E., Laine J., Comer´onS., Gadotti D. A., Buta R. J., Sheth K., Zaritsky D., Ho L., Knapen J., Athanassoula E.; Bosma A., Laine S., Cisternas M., Kim T., Mu~noz-MateosJ.-C., Regan M. W., Hinz J. L., Gil de Paz A., Men´endez-Delmestre K., Mizusawa T., Erroz-Ferrer S., Meidt S. E.. Querejeta M. The Astrophysical Journal Supplement Series, 2015, 219, 1: The Spitzer Survey of Stellar Structure in Galaxies (S4G): Multi-component Decomposition Strategies and Data Release IV. Laine J., Laurikainen E., Salo H. Astronomy & Astrophysics, submitted: Influence of galaxy stellar mass and observation wavelength on disc breaks v Author contributions All the papers included in this thesis are results of teamwork. In papers I and IV the author performed the data-analysis and was the primary writer. In paper II the author has participated in large part of the data-analysis and writing of chapter 4, and has contributed to the data-analysis described in the other chapters. In paper III the author has a strong contribution to the data-analysis (> 20%) and has participated in the planning of the methods used in the study. In addition, the author has participated in the work of following papers which are not included in this thesis: 1. Zaritsky, D., McCabe, K., Aravena, M., Athanassoula, E., Bosma, A. et al. The Astrophysical Journal, 2016, 818, 1: Globular Cluster Populations: Results Including S4G Late-type Galaxies 2. Querejeta, M., Meidt, S. E., Schinnerer, E., Cisternas, M., Mu~noz-Mateos, J. C. et al. The Astrophysical Journal Supplement Series, 2015, 219, 1: The Spitzer Survey of Stellar Structure in Galaxies (S4G): Precise Stellar Mass Distributions from Automated Dust Correction at 3.6 µm 3.
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