{
  "id": "1504.03330",
  "version": "v1",
  "published": "2015-04-13T20:00:54.000Z",
  "updated": "2015-04-13T20:00:54.000Z",
  "title": "Elliptical Galaxies and Bulges of Disk Galaxies: Summary of Progress and Outstanding Issues",
  "authors": [
    "John Kormendy"
  ],
  "comment": "46 pages, 10 postscript figures, accepted for publication in Galactic Bulges, ed. E. Laurikainen, R. F. Peletier, & D. A. Gadotti (New York: Springer), in press (2015)",
  "categories": [
    "astro-ph.GA",
    "astro-ph.CO"
  ],
  "abstract": "This is the summary chapter of a review book on galaxy bulges. Bulge properties and formation histories are more varied than those of ellipticals. I emphasize two advances: 1 - \"Classical bulges\" are observationally indistinguishable from ellipticals, and like them, are thought to form by major galaxy mergers. \"Disky pseudobulges\" are diskier and more actively star-forming (except in S0s) than are ellipticals. Theys are products of the slow (\"secular\") evolution of galaxy disks: bars and other nonaxisymmetries move disk gas toward the center, where it starbursts and builds relatively flat, rapidly rotating components. This secular evolution is a new area of galaxy evolution work that complements hierarchical clustering. 2 - Disks of high-redshift galaxies are unstable to the formation of mass clumps that sink to the center and merge - an alternative channel for the formation of classical bulges. I review successes and unsolved problems in the formation of bulges+ellipticals and their coevolution (or not) with supermassive black holes. I present an observer's perspective on simulations of dark matter galaxy formation including baryons. I review how our picture of the quenching of star formation is becoming general and secure at redshifts z < 1. The biggest challenge is to produce realistic bulges+ellipticals and disks that overlap over a factor of 10**3 in mass but that differ from each other as observed over that whole range. Second, how does hierarchical clustering make so many giant, bulgeless galaxies in field but not cluster environments? I argue that we rely too much on AGN and star-formation feedback to solve these challenges.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-04-13T20:00:54.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "disk galaxies",
      "elliptical galaxies",
      "outstanding issues",
      "nonaxisymmetries move disk gas",
      "dark matter galaxy formation"
    ],
    "publication": {
      "doi": "10.1007/978-3-319-19378-6_16",
      "journal": "Galactic Bulges",
      "year": 2016,
      "volume": 418,
      "pages": 431
    },
    "note": {
      "typesetting": "TeX",
      "pages": 46,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "adsabs": "2016ASSL..418..431K",
      "inspire": 1359416
    }
  }
}