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The blueshift of the [O III] emission line in NLS1s

W. Bian [1] , Q. Yuan [1] & Y. Zhao [2] [1] Department of Physics, Nanjing Normal University, Nanjing 210097, China [2] National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China. The blueshift of the [O III] emission line in NLS1s. Outline.

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The blueshift of the [O III] emission line in NLS1s

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  1. W. Bian[1], Q. Yuan[1] & Y. Zhao[2] [1] Department of Physics, Nanjing Normal University, Nanjing 210097, China [2] National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China The blueshift of the [O III] emission line in NLS1s

  2. Extreme starburst: Near and Far, August 15-19, 2005 Outline 1. Introduction: NLS1s, M- σrelation, the blueshift of [O III], the “blue outlier” 2. SDSS sample and analysis 3. Results 4. Summary

  3. Extreme starburst: Near and Far, August 15-19, 2005 1. Introduction 1.1 What are NLS1s ? Observation: • Narrow Hβ line width. FWHM(Hβ) < 2000 km s-1 • Strong optical Fe II multiples • Weak [O III] ([OIII]/Hβ < 3) • Soft X-ray excess • Rapid soft/hard X-ray variability • Theory: • Less massive black hole • Higher Eddington ratio • Early stage of AGN evolution

  4. Extreme starburst: Near and Far, August 15-19, 2005 150 NLS1s from SDSS EDR (Williams R.J., Pogge R.W., Mathur S, 2003, AJ, 124, 3042) 22 NLS1s from HST observation (Constantin & Shields, 2003, PASP, 115, 592)

  5. Extreme starburst: Near and Far, August 15-19, 2005 1.2 M – σrelation in NLS1s (Bian & Zhao, MNRAS, 2004, 347, 607; Grupe & Mathur, 2004, ApJ, 606, L41; Botte, 2005, MNRAS, 356, 789) Dynamics of NLRs in NLS1s would be different than that of other AGN

  6. Extreme starburst: Near and Far, August 15-19, 2005 1.3 The shift of the peak of [O III] relative to Hβ Two largest blueshift of [O III] (Aoki K., et al., 2005, ApJ, 618, 601) 216 low-redshift AGN (Zamanzov R., et al., 2002, ApJ, 576, L9)

  7. Extreme starburst: Near and Far, August 15-19, 2005 The [O III] blueshift versus the FWHM(Hβ), and Fe IIλ4570/ Hβ In the population A region of the Eigenvector 1 parameter domain => strong Fe II lines and narrow Hβline

  8. Extreme starburst: Near and Far, August 15-19, 2005 Ref: Boroson T. A., Oke J. B., 1987, PASP, 99, 809 Grupe D., Thomas H.-C., Leighly K. M., 2001, A&A, 369, 450 Veron-Cetty M.-P., Veron, P., Goncalves A. C., 2001, A&A, 372, 730 Grupe D., Leighly K. M. 2002, in X-Ray Spectroscopy of AGN with Chandra and XMM-Newton, ed. T. Boller (MPE Rep. 279; Garching: MPE), 287 Zamanzov R., et al., 2002, ApJ, 576, L9 Marziani P., et al., 2003, MNRAS, 345, 1133 Aoki K., Kawaguchi T., OhtacK., 2005, ApJ, 618, 601

  9. Extreme starburst: Near and Far, August 15-19, 2005 2. SDSS sample and analysis • 150 NLS1 in SDSS EDR • IRAF-SPECFIT: correct the blue wind of [O III] (1) a power-law continuum (2) Fe II multiples (3) Three two-component sets for H βand [O III] 4959, 5007.

  10. Extreme starburst: Near and Far, August 15-19, 2005 3. Results 3.1 Distributions of the blueshift

  11. Extreme starburst: Near and Far, August 15-19, 2005 Criterion: 3.2 The “blue outliers” For SDSS J0102226.31-003904.6:

  12. Extreme starburst: Near and Far, August 15-19, 2005 For SDSS J024037.89+001118.9:

  13. Extreme starburst: Near and Far, August 15-19, 2005 3.3 Correlations between the blueshift and some parameters

  14. Extreme starburst: Near and Far, August 15-19, 2005 4. Summary • Two-component models to fit the emission lines of [O III] 4959, 5007 and Hβin SDSS NLS1s. • Mean blueshift is -52km s-1. • Seven ``blue outliers“ are found. The largest blueshift of SDSS J0102226-003904 is -931km s-1. • Strong correlations between the [O III] blueshift and the Eddington ratio, and Fe IIλ4570/ Hβ. Clues to the origin of the ``blue outliers“ . • [O III] =>σ

  15. Extreme starburst: Near and Far, August 15-19, 2005 Thank you !

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