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Galaxy Morphology

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Galaxy Morphology Galaxy Morphology1 Ronald J. Buta Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 Received ; accepted arXiv:1102.0550v1 [astro-ph.CO] 2 Feb 2011 1To be published in Planets, Stars, and Stellar Systems, Vol. 6, Series Editor T. D. Oswalt, Volume editor W. C. Keel, Springer Reference, 2011 –2– ABSTRACT Galaxy morphology is a product of how galaxies formed, how they inter- acted with their environment, how they were influenced by internal perturba- tions, AGN, and dark matter, and of their varied star formation histories. This article reviews the phenomenology of galaxy morphology and classification with a view to delineating as many types as possible and how they relate to physical interpretations. The old classification systems are refined, and new types intro- duced, as the explosion in available morphological data has modified our views on the structure and evolution of galaxies. Subject headings: galaxies: spiral; galaxies: elliptical; galaxies: S0s; galaxies: structure; galaxies: high redshift; galaxies: classification; galaxies: peculiar; galaxies: dwarfs; galaxies: clusters; galaxies: active; galaxies: isolated; galaxies: Galaxy Zoo project Index terms: Hubble-Sandage-de Vaucouleurs classification; spiral galaxies; elliptical galaxies; S0 galaxies; irregular galaxies; resonance ring galaxies; outer rings; inner rings; nuclear rings; secondary bars; nuclear bars; pseudorings; grand design spirals; flocculent spirals; merger morphologies; tidal tails; collisional ring galaxies; polar ring galaxies; barred galaxies; lens galaxies; spiral arm classes; counter-winding spiral galaxies; anemic spiral galaxies; spiral arm multiplicity; dust lanes; pseudobulges; classical bulges; dust-lane elliptical galaxies; shell/ripple galaxies; ultra-luminous infrared galaxies; bar ansae; brightest cluster members; low surface brightness galaxies; dwarf galaxies; dwarf spiral galaxies; dwarf spheroidal galaxies; Galaxy Zoo project; isolated galaxies; blue compact dwarf galaxies; star-forming galaxy morphologies; warped disks; stellar mass morphology; luminosity classes; boxy ellipticals; disky ellipticals; late-type galaxies; early-type galaxies; –3– Magellanic barred galaxies; color galaxy morphology; atomic and molecular gas galaxy morphology Contents 1 Introduction 6 2 Overview 8 3 Galaxy Classification 12 4 A Continuum of Galactic Forms 15 5 Galaxy Types: Stage, Family, and Variety 17 5.1 Elliptical and Spheroidal Galaxies . 17 5.2 S0andSpiralGalaxies .............................. 21 5.3 IrregularGalaxies................................. 27 6 Other Dimensions to Galaxy Morphology 28 6.1 OuterRingsandPseudorings .......................... 28 6.2 InnerandOuterLenses.............................. 30 6.3 NuclearRingsandBars ............................. 31 6.4 SpiralArmMorphologies............................. 33 6.5 LuminosityEffects ................................ 37 –4– 7 The Morphology of Galactic Bars and Ovals 38 8 Dust Morphologies 41 9 The Morphologies of Galactic Bulges 43 10 Effects of Interactions and Mergers 46 10.1 NormalversusCatastrophicRings. ... 46 10.2 Environmental Effects on Star-FormingDisks . .... 51 10.3 Interacting and Peculiar Galaxies . 54 10.3.1 Tidal Tails, Arms, and Bridges . 54 10.3.2 Dust-Lane Ellipticals . 55 10.3.3 Shell/Ripple Galaxies . 56 10.3.4 Ultra-Luminous Infrared Galaxies . 57 10.4Warps ....................................... 58 10.5 The Morphology of Active Galaxies . 59 10.6 The Morphology of Brightest Cluster Members . .... 61 11 Star Formation Morphologies 62 11.1 Hα Imaging .................................... 62 11.2 Ultraviolet Imaging . 64 11.3 Atomic and Molecular Gas Morphology . 65 –5– 12 Infrared Observations: Galactic Stellar Mass Morphology 69 13 Intermediate and High Redshift Galaxy Morphology 74 14 Giant Low Surface Brightness Galaxies 81 15 Galaxy Morphology in Color 83 15.1NormalGalaxies ................................. 83 15.2DwarfGalaxies .................................. 85 15.2.1 dE,dS0,BCD,andcEGalaxies . 85 15.2.2 Local Group Dwarf Spheroidals and Irregulars . .. 87 15.2.3 DwarfSpirals ............................... 88 15.3GalaxyZooProject................................ 89 15.4IsolatedGalaxies ................................. 91 15.5DeepFieldColorImaging ............................ 93 16 Large-Scale Automated Galaxy Classification 93 17 The Status and Future of Morphological Studies 94 –6– 1. Introduction In the nearly 100 years since galaxy morphology became a topic of research, much has been learned about galactic structure and dynamics. Known only as “nebulae” at that time, galaxies were found to have a wide range of largely inexplicable forms whose relations to one another were a mystery. As data accumulated, it became clear that galaxies are fundamental units of matter in space, and an understanding of how they formed and evolved became one of the major goals of extragalactic studies. Even in the era of space observations, galaxy morphology continues to be the backbone of extragalactic research as modern instruments provide information on galactic structure across a wide range of distances and lookback times. In spite of the advances in instrumentation and the explosion of data, classical galaxy morphology (i. e., the visual morphological classification in the style of Hubble and others) has not lost its relevance. The reasons for this are as follows: 1. Morphology is still a logical starting point for understanding galaxies. Sorting galaxies into their morphological categories is similar to sorting stars into spectral types, and can lead to important astrophysical insights. Any theory of galaxy formation and evolution will have to, at some point, account for the bewildering array of galactic forms. 2. Galaxy morphology is strongly correlated with galactic star formation history. Galaxies where star formation ceased gigayears ago tend to look very different from those where star formation continues at the present time. Classical morphology recognizes these differences in an ordered way. 3. Information on galaxy morphology, in the form of new types of galaxies, multi-wavelength views of previously known galaxy types, and higher resolution views of all or part of some galaxies, has exploded as modern instrumentation has superceded the old photographic –7– plates that were once used exclusively for galaxy classification. 4. Galaxy classification has gone beyond the realm of a few thousand galaxies to that of a million galaxies through the Galaxy Zoo project. Not only this, but GalaxyZoo has taken morphology from the exclusive practice of a few experts to the public at large, thus facilitating citizen science at its best. Galaxy Zoo images are also in color, thus allowing the recognition of special galaxy types and features based on stellar populations or gaseous emission. 5. Finally, deep surveys with the Hubble Space Telescope have extended morphological studies well beyond the realm of the nearby galaxies that dominated early catalogues, allowing detailed morphology to be distinguished at unprecedented redshifts. Now, more than ever, galaxy morphology is a vibrant subject that continues to provide surprises as more galaxies are studied for their morphological characteristics across the electromagnetic spectrum. It is clear that a variety of effects are behind observed morphologies, including environmental density and merger/interaction history, internal perturbations, gas accretions, nuclear activity, secular evolution, as well as the diversity in star formation histories, and that a global perspective based on large numbers of galaxies will improve theoretical models and give a more reliable picture of galactic evolution. The goal of this article is to present the phenomenology of galaxy morphology in an organized way, and highlight recent advances in understanding what factors influence morphology and how various galaxy types are interpreted. The article is a natural follow-up to the excellent review of galaxy morphology and classification by Sandage (1975) in Volume IX of the classic Stars and Stellar Systems series. It also complements the recently published de Vaucouleurs Atlas of Galaxies (Buta, Corwin, & Odewahn 2007, hereafter the dVA), which provided a detailed review of the state and technique of galaxy classification up to about the year 2005. Illustrations are very important in a review of this nature, –8– and the article draws on a large number of sources of images. For this purpose, the Sloan Digital Sky Survey (SDSS), the NASA/IPAC Extragalactic Database (NED), and the dVA have been most useful. 2. Overview As extended objects rather than point sources, galaxies show a wide variety of forms, some due to intrinsic structures, others due to the way the galaxy is oriented to the line of sight. The random orientations, and the wide spread of distances, are the principal factors that can complicate interpretations of galaxy morphology. If we could view every galaxy along its principal axis of rotation, and from the same distance, then fairer comparisons would be possible. Nevertheless, morphologies seen in face-on galaxies can also often be recognized in more inclined galaxies (Figure 1). It is only for the highest inclinations that morphology switches from face-on radial structure to vertical structure. In general we either know the planar structure in a galaxy, or we know its vertical structure, but we usually cannot know both well from analysis of images alone. Galaxy morphology began to get interesting when the “Leviathan
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