Active galactic nuclei in the sloan digital sky survey. II. Emission-line luminosity function

Lei Hao, A. Strauss, Xiaohui Fan, Christy A. Tremonti, David J. Schlegel, Timothy M. Heckman, Guinevere Kauffmann, Michael R. Blanton, James E. Gunn, Patrick B. Hall, Željko Ivezić, Gillian R. Knapp, Julian H. Krolik, Robert H. Lupton, Gordon T. Richards, Donald P. Schneider, Iskra V. Strateva, Nadia L. Zakamska, J. Brinkmann, Gyula P. Szokoly

Research output: Contribution to journalArticle

150 Citations (Scopus)

Abstract

The emission-line luminosity function of active galactic nuclei (AGNs) is measured from about 3000 AGNs included in the main galaxy sample of the Sloan Digital Sky Survey within a redshift range of 0 < z < 0.15. The Hα and [O III] λ5007 luminosity functions for Seyfert galaxies cover a luminosity range of 10 5-10 9 L in Hα, and the shapes are well fitted by broken power laws, without a turnover at fainter nuclear luminosities. Assuming a universal conversion from emission-line strength to continuum luminosity, the inferred 5-band magnitude luminosity function is comparable to both the AGN luminosity function of previous studies and the low-redshift quasar luminosity function derived from the Two-Degree Field redshift survey. The inferred AGN number density is approximately one-fifth of all galaxies, and about 6 × 10 -3 of the total light of galaxies in the r band comes from nuclear activity. The numbers of Seyfert 1 and Seyfert 2 galaxies are comparable at low luminosity, while at high luminosity, Seyfert 1 galaxies outnumber Seyfert 2 galaxies by a factor of 2-4. In making the luminosity function measurements, we assume that the nuclear luminosity is independent of the host galaxy luminosity, an assumption we test a posteriori and show to be consistent with the data. Given the relationship between black hole mass and host galaxy bulge luminosity, the lack of correlation between nuclear and host luminosity suggests that the main variable that determines the AGN luminosity is the Eddington ratio, not the black hole mass. This appears to be different from luminous quasars, which are most likely to be shining near the Eddington limit.

Original languageEnglish (US)
Pages (from-to)1795-1808
Number of pages14
JournalAstronomical Journal
Volume129
Issue number4
DOIs
StatePublished - Apr 2005

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active galactic nuclei
luminosity
galaxies
Seyfert galaxies
quasars
field survey
turnover
power law

Keywords

  • Galaxies: active
  • Galaxies: Seyfert
  • Galaxies: starburst
  • Quasars: emission lines
  • Surveys

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Hao, L., Strauss, A., Fan, X., Tremonti, C. A., Schlegel, D. J., Heckman, T. M., ... Szokoly, G. P. (2005). Active galactic nuclei in the sloan digital sky survey. II. Emission-line luminosity function. Astronomical Journal, 129(4), 1795-1808. https://doi.org/10.1086/428486

Active galactic nuclei in the sloan digital sky survey. II. Emission-line luminosity function. / Hao, Lei; Strauss, A.; Fan, Xiaohui; Tremonti, Christy A.; Schlegel, David J.; Heckman, Timothy M.; Kauffmann, Guinevere; Blanton, Michael R.; Gunn, James E.; Hall, Patrick B.; Ivezić, Željko; Knapp, Gillian R.; Krolik, Julian H.; Lupton, Robert H.; Richards, Gordon T.; Schneider, Donald P.; Strateva, Iskra V.; Zakamska, Nadia L.; Brinkmann, J.; Szokoly, Gyula P.

In: Astronomical Journal, Vol. 129, No. 4, 04.2005, p. 1795-1808.

Research output: Contribution to journalArticle

Hao, L, Strauss, A, Fan, X, Tremonti, CA, Schlegel, DJ, Heckman, TM, Kauffmann, G, Blanton, MR, Gunn, JE, Hall, PB, Ivezić, Ž, Knapp, GR, Krolik, JH, Lupton, RH, Richards, GT, Schneider, DP, Strateva, IV, Zakamska, NL, Brinkmann, J & Szokoly, GP 2005, 'Active galactic nuclei in the sloan digital sky survey. II. Emission-line luminosity function', Astronomical Journal, vol. 129, no. 4, pp. 1795-1808. https://doi.org/10.1086/428486
Hao, Lei ; Strauss, A. ; Fan, Xiaohui ; Tremonti, Christy A. ; Schlegel, David J. ; Heckman, Timothy M. ; Kauffmann, Guinevere ; Blanton, Michael R. ; Gunn, James E. ; Hall, Patrick B. ; Ivezić, Željko ; Knapp, Gillian R. ; Krolik, Julian H. ; Lupton, Robert H. ; Richards, Gordon T. ; Schneider, Donald P. ; Strateva, Iskra V. ; Zakamska, Nadia L. ; Brinkmann, J. ; Szokoly, Gyula P. / Active galactic nuclei in the sloan digital sky survey. II. Emission-line luminosity function. In: Astronomical Journal. 2005 ; Vol. 129, No. 4. pp. 1795-1808.
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abstract = "The emission-line luminosity function of active galactic nuclei (AGNs) is measured from about 3000 AGNs included in the main galaxy sample of the Sloan Digital Sky Survey within a redshift range of 0 < z < 0.15. The Hα and [O III] λ5007 luminosity functions for Seyfert galaxies cover a luminosity range of 10 5-10 9 L ⊙ in Hα, and the shapes are well fitted by broken power laws, without a turnover at fainter nuclear luminosities. Assuming a universal conversion from emission-line strength to continuum luminosity, the inferred 5-band magnitude luminosity function is comparable to both the AGN luminosity function of previous studies and the low-redshift quasar luminosity function derived from the Two-Degree Field redshift survey. The inferred AGN number density is approximately one-fifth of all galaxies, and about 6 × 10 -3 of the total light of galaxies in the r band comes from nuclear activity. The numbers of Seyfert 1 and Seyfert 2 galaxies are comparable at low luminosity, while at high luminosity, Seyfert 1 galaxies outnumber Seyfert 2 galaxies by a factor of 2-4. In making the luminosity function measurements, we assume that the nuclear luminosity is independent of the host galaxy luminosity, an assumption we test a posteriori and show to be consistent with the data. Given the relationship between black hole mass and host galaxy bulge luminosity, the lack of correlation between nuclear and host luminosity suggests that the main variable that determines the AGN luminosity is the Eddington ratio, not the black hole mass. This appears to be different from luminous quasars, which are most likely to be shining near the Eddington limit.",
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