Extreme starburst: Near and Far, August 15-19, 2005Extreme starburst: Near and Far, August 15-19, 2005

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

W. BianW. Bian[1][1], Q. Yuan, Q. Yuan[1][1] & Y. Zhao & Y. Zhao[2][2]

[1] Department of Physics, Nanjing Normal University, Nanjing[1] Department of Physics, Nanjing Normal University, Nanjing210097, China210097, China

[2] National Astronomical Observatories, Chinese Academy of [2] National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, ChinaSciences, Beijing 100012, China

Extreme starburst: Near and Far, August 15-19, 2005Extreme starburst: Near and Far, August 15-19, 2005

Outline

1. Introduction: NLS1s, M- 1. Introduction: NLS1s, M- σσrelation, relation, the bluthe blueshift of [O III], the “blue outlier” eshift of [O III], the “blue outlier”

2. SDSS sample and analysis2. SDSS sample and analysis3. Results3. Results4. Summary4. Summary

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1.1 What are 1.1 What are NLS1s ?NLS1s ?

Observation:Observation: • Narrow Narrow Hβ line widthHβ line width. . FWHM(Hβ) < 2000 km sFWHM(Hβ) < 2000 km s-1-1

• Strong optical Fe II multiplesStrong optical Fe II multiples• Weak [O III] ([OIII]/Hβ < 3)Weak [O III] ([OIII]/Hβ < 3)• Soft X-ray excessSoft X-ray excess• Rapid soft/hard X-ray variabilityRapid soft/hard X-ray variability

Theory:• Less massive black hole• Higher Eddington ratio • Early stage of AGN evolution

1. Introduction

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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)

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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

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216 low-redshift AGN(Zamanzov R., et al., 2002, ApJ, 576, L9)

Two largest blueshift of [O III] (Aoki K., et al., 2005, ApJ, 618, 601)

1.3 The shift of the peak of [O III] relative to Hβ

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The [O III] blueshift versus the FWHM(Hβ), and Fe IIλ4570/ HβIn the population A region of the Eigenvector 1 parameter domain

=> strong Fe II lines and narrow Hβ line

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

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2. SDSS sample and analysis

• 150 NLS1 in SDSS EDR150 NLS1 in SDSS EDR• IRAF-SPECFIT: correct the blue wind of [O III]IRAF-SPECFIT: correct the blue wind of [O III] (1) a power-law continuum(1) a power-law continuum (2) Fe II multiples(2) Fe II multiples (3) Three two-component sets for H (3) Three two-component sets for H ββ and and [O III] 4959, 5007.[O III] 4959, 5007.

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3. Results3. Results

3.1 Distributions of the blueshift3.1 Distributions of the blueshift

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3.2 The “blue outliers”3.2 The “blue outliers”

For SDSS J0102226.31-003904.6:

Criterion:

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For SDSS J024037.89+001118.9:

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3.3 Correlations between the blueshift 3.3 Correlations between the blueshift andand

some parameterssome parameters

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4. Summary

• Two-component models to fit the emission lines oTwo-component models to fit the emission lines of [O III] 4959, 5007 and Hf [O III] 4959, 5007 and Hββin SDSS NLS1s.in SDSS NLS1s.

• Mean blueshift is Mean blueshift is -52km s-52km s-1-1..• Seven ``blue outliers“ are found. The largest bluSeven ``blue outliers“ are found. The largest blu

eshift of SDSS eshift of SDSS J0102226-003904 is -931km s is -931km s-1-1..• Strong correlations between the [O III] blueshift aStrong correlations between the [O III] blueshift a

nd the Eddington ratio, and Fe IInd the Eddington ratio, and Fe IIλλ4570/ H4570/ Hββ. Clues . Clues to the origin of the to the origin of the ``blue outliers“ .``blue outliers“ .

• [O III] =>[O III] =>σσ

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Thank you !Thank you !