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Quasars Classes and Their Relationships

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Fifty Years of Quasars

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 386))

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Abstract

Most of the questions in this chapter deal with sources that do not show the “classical” broad emission-line spectrum that characterizes the majority of known AGNs at high and low redshift. If that majority represents a “parent population” of AGNs, is the apparent absence of broad lines a result of obscuration, orientation, or different physical conditions? Can all of the subclasses be unified under the AGN umbrella? With the unification scheme set in place and assumed to be fundamentally correct, there are at least four overarching questions: do all type-2 AGNs possess an obscured broad-line region? Or how can we distinguishing type-2 AGNs without a broad-line region if they exist? Where is the low end of quasar activity? The least luminous AGNs are the so-called low-ionization nuclear emission-line regions (LINERs), but it is legitimate to ask if they are all true AGNs.

Contributions by Mauro D’Onofrio, Paola Marziani, Jack W. Sulentic, Deborah Dultzin, Yuri Efimov, Martin Gaskell, Marianne Vestergaard, Damien Hutsemékers, Alberto Franceschini, Ari Laor, Dirk Grupe, Sebastian Lipari, Begõna García Lorenzo, Evencio Mediavilla, Todd Boroson, Mike Eracleous, Isabel Marquez-Perez, Elmar Körding, and Heino Falcke

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Notes

  1. 1.

    Note that in some of the objects where the type-2 identification is based only on the Hβ line, may in fact be type 1.9 Seyferts, that is, Seyferts where a broad component is detected in Hα and not in Hβ. Seyfert 1.9 objects are clearly not “true type-2” AGNs.

  2. 2.

    We use the definition by Kellermann et al. [148] where AGNs are considered to be radio loud which radio to optical ratio R > 10.

  3. 3.

    This is the base of a wind, thought to be emitted by the disks of most quasars and invoked to explain their broad absorption lines.

  4. 4.

    A similar sequence is invoked to explain their generally old stellar populations [23, 261], more evolved central morphologies [144], and richer environments [159] when compared to those of Sy.

  5. 5.

    This is in good agreement with the 72% of LINERs that [7] find in a smaller sample of early-type galaxies with ionized gas.

  6. 6.

    Note, however, that at low accretion rates, it is not clear that the X-ray emission comes from the accretion flow or perhaps rather from the jet itself [192, 194].

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Authors and Affiliations

  1. Dipartimento di Astronomia, Università degli Studi di Padova, Vicolo Osservatorio 3, I35122, Padova, Italy

    Mauro D’Onofrio & Alberto Franceschini

  2. INAF, Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, IT35122, Padova, Italy

    Paola Marziani

  3. Instituto de Astrofísica de Andalucía (CSIC), Granada, Spain

    Jack W. Sulentic & Isabel Marquez-Perez

  4. Instituto de Astronomia, Universidad Nacional Autonoma de Mexico (UNAM), 70-264, Mexico, D.F., Mexico

    Deborah Dultzin

  5. Crimean Astrophysical Observatory, 98409, Nauchny, Crimea, Ukraine

    Yuri Efimov

  6. Departamento de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Av. Gran Bretaña 1111, Valparaíso, Chile

    Martin Gaskell

  7. The Dark Cosmology Centre, The Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100, Copenhagen 0, Denmark

    Marianne Vestergaard

  8. Steward Observatory and Department of Astronomy, University of Arizona, 933 N. Cherry Avenue, Tucson, 85721, Arizona, USA

    Marianne Vestergaard

  9. F.R.S. - FNRS, Institute of Astrophysics and Geophysics, University of Liège, Allée du six août 17 B5c, B-4000, Liège, Belgium

    Damien Hutsemékers

  10. Physics Department, Technion - Israel Institute of Technology, Technion City, Haifa, 32000, Israel

    Ari Laor

  11. The Pennsylvania State University, 525 Davey Lab., University Park, PA, 16082, USA

    Dirk Grupe

  12. Observatorio Astronómico de la Univ. Nac. de Córdoba, Laprida 854, X5000BGR, Córdoba, Argentina, and CONICET, Argentina

    Sebastian Lipari

  13. Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain

    Begoña Garcıa Lorenzo & Evencio Mediavilla

  14. National Optical Astronomy Observatory, Tucson, AZ, USA

    Todd Boroson

  15. Department of Astronomy and Astrophysics and Center for Gravitational Wave Physics, The Pennsylvania State University, 525 Davey Lab., University Park, PA, 16802, USA

    Mike Eracleous

  16. Deparment of Astronomy, Radbound Universiteit Nijmegen, IMAPP, The Netherlands

    Elmar Körding & Heino Falcke

  17. ASTRON, Dwingeloo, The Netherlands

    Heino Falcke

  18. Max-Planck Institut für Radioastronomie, Bonn, Germany

    Heino Falcke

Authors
  1. Mauro D’Onofrio
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  2. Paola Marziani
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  3. Jack W. Sulentic
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  4. Deborah Dultzin
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  5. Yuri Efimov
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  6. Martin Gaskell
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  7. Marianne Vestergaard
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  8. Damien Hutsemékers
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  9. Alberto Franceschini
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  10. Ari Laor
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  11. Dirk Grupe
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  12. Sebastian Lipari
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  13. Begoña Garcıa Lorenzo
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  14. Evencio Mediavilla
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  15. Todd Boroson
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  16. Mike Eracleous
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  17. Isabel Marquez-Perez
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  18. Elmar Körding
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  19. Heino Falcke
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Corresponding author

Correspondence to Jack W. Sulentic .

Editor information

Editors and Affiliations

  1. , Dipartimento di Astronomia, Università di Padova, Vicolo Osservatorio 3, Padova, 35122, Italy

    Mauro D'Onofrio

  2. , Osservatorio Astronomico di Padova, Istituto Nazionale di Astrofisica (INAF), Vicolo dell' Osservatorio 5, Padova, 35122, Italy

    Paola Marziani

  3. , (IAA-CSIC), Instituto de Astrofisica de Andalucia, Camino Bajo del Huetor 50, Granada, 18008, Spain

    Jack W. Sulentic

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© 2012 Springer-Verlag Berlin Heidelberg

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D’Onofrio, M. et al. (2012). Quasars Classes and Their Relationships. In: D'Onofrio, M., Marziani, P., Sulentic, J. (eds) Fifty Years of Quasars. Astrophysics and Space Science Library, vol 386. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-27564-7_4

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  • DOI: https://doi.org/10.1007/978-3-642-27564-7_4

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