Weimin YuanYunnan Observatory/NAOC, CAS, Kunming, China

Systematic study of a large sample of Systematic study of a large sample of NLS1 galaxies from SDSS NLS1 galaxies from SDSS

—— first results first results

H. Zhou, T.-G. Wang, H. Lu, X. Dong J. Wang, Y. LuUniversity of Science & Technology of China

Hefei

H. Zhou, T.-G. Wang, W. Yuan, et al. 2006, ApJS, 166, 128

Narrow Line Seyfert 1 galaxiesNarrow Line Seyfert 1 galaxies

narrow Balmer lines FWHM(Hβ)<2000km/s [OIII]/ Hβ small (<3)

strong FeII soft X-ray: steep spectrum, rapid variability outflows ([OIII] and CIV)…)

extreme region in the eigenvector 1 space small BH mass and high L/LEdd useful to constrain AGN models

Controversial and unexplored issues~ 400 NLS1s known before our sample (incl. e.g., the SDSS

EDR NLS1 sample of ~150, Williams et al. 2002)

broad band SED black hole mass determination, MBH - sigma relation NLS1s with flat soft X-ray spectra [OIII] strength, NLR, outflows host galaxies type 2 counterparts optical variability radio-loud NLS1, radio-emission, jets? accretion models evolution

A larger and homogeneous NLS1 sample is needed

Analysis of SDSS spectra Analysis of SDSS spectra

Search from SDSS spectroscopic targets as galaxies and QSO

Spectral decomposition of host galaxy starlight and nuclear (continuum + emission lines), using our EL-ICA algorithm (Ensemble Learning – Independent Component Analysis)

Using 6 IC synthesized galaxy templates built up from the SSP spectral library of Bruzual & Charlot 2003 Lu et al. 2006, AJ, 131, 790

stellar V dispersion also obtained

Spectral line fitting

broad and narrow line de-blending

HαregionHβregion

NLS1 sample from the SDSS DR3NLS1 sample from the SDSS DR3

The sample was drawn from ~387,483 galaxies and QSO in the SDSS DR3 (z<0.8)

Selection criteria: Hα or Hβ detected at >10 σ significance level FWHM < 2200 km/s

The sample: 2011 NLS1

1885 NLS1 (FWHM<2000 km/s)

<7% have radio detection (c.f. 10% for BL AGN)

NLS1 fraction: 15% in radio-quiet & radio-intermediate AGN (R<1)

10% in moderate radio-loud AGN (1<R<2)

<5% in very radio-loud AGN (R>2)

The FeII emission in NLS1s is ~twice stronger than normal BL AGN

notenote

The conventional NLS1 definition mayThe conventional NLS1 definition may

include some AGNs with IMBH mass include some AGNs with IMBH mass

Objects with MObjects with MBHBH <~ 10 <~ 1066 M⊙ M⊙

See poster # 268 for our IMBH See poster # 268 for our IMBH ((<~ 10<~ 1066 M⊙ M⊙ )) AGN sample AGN sample

Line EW – luminosity relation --- (inverse) Baldwin effect

Hβluminosity λL λ luminosity at 5100Ǻ

EW

Hβ

EW

FeII

Soft X-ray Slope vs. FWHM (Balmer)

Turnover line-width ~ 1000km/s

FWHM Hβ(km/s) FWHM Hα(km/s)

RO

SA

T p

hoto

n

ind

ex

RO

SA

T p

hoto

n

ind

ex

Narrow line region

No difference between NLS1 and normal BL AGN

Black hole mass – Black hole mass – stellar velocity dispersion relationstellar velocity dispersion relation

MBH: estimated from line-width and luminosity (e.g. kaspi et al. 2000, Mclure & Jarvis 2002, Dietrich & Hamann)

σσ: : measured from fitting the nuclear starlight spectra of host galaxies by the galaxy-nuclear spectral decomposition algorithm stellar velocity dispersion (km/s)(km/s)

Bla

ck h

ole

mas

s (M

⊙)

Trai

mai

ne e

tal.

2002

Black hole mass – Black hole mass – stellar velocity dispersion relationstellar velocity dispersion relation

stellar velocity dispersion (km/s)(km/s)

Bla

ck h

ole

mas

s (M

⊙)

Possible contamination of σσ by the rotation galactic disk?

Use only nearby galaxies with face-on disks or their SDSS fiber aperture 3” dominated by galactic bulges

NLS1 are underage AGN in which the growth of the SMBH lags the formation of the bulge

Trai

mai

ne e

tal.

2002

e.g. Mathur et al. 2001, Grupe & Mathur 2004, Biao & Zhao 2004, , Botte et al. 2004,

Wang & Lu, Wandel 2002, 2004, ……)

summarysummary

Providing to the AGN community with the largest NLS1 sample

The frequency of finding NLS1s depends strongly on optical luminosity and radio-loudness

Turnover of the trend of soft X-ray Slope vs. FWHM (Balmer) Inverse Baldwin effect seen in Hbeta and FeII NLR in NLS1s is not different from that of BLS1s

finding NLS2 is challenging NLS1s are underage AGN in which the growth of the SMBH

lags the formation of the bulge

Current workCurrent work

• Search for optical variability ~150 covered in the SDSS SN survey

(preliminary results see poster #280 Y. Ai et al.) optical monitoring

• X-ray data analysis (XMM, ROSAT, etc.)

a sample of ~40 objects with XMM data

XMM-Newton XMM-Newton spectral fitsspectral fits

one power law: 10/22

PL + soft x-ray excess: 12/22

No significant Fe K line

Other models, e.g.

p-free model

(S. Mineshige’s talk)

one power law

Broken power law

Example of spectral fits to XMM dataExample of spectral fits to XMM dataL. Fan, et al. in prep..

Results of spectral fits for the XMM sub-sample with Results of spectral fits for the XMM sub-sample with enough photon counts (~30 objects)enough photon counts (~30 objects)

L. Fan, et al. in prep..

distribution of the photon index of the distribution of the photon index of the underlying power-lawunderlying power-law

Current work and future planCurrent work and future plan• much detailed statistical analysis

Fraction of NLS1 w.r.t. luminosity, z, etc. ……

• broad band properties and SED UV (Galex)

• Host galaxy morphology and stellar contents• new radio/X-ray observations• photometric/spectroscopic monitor, variability study • possible black hole mass measurement by

reverberation mapping• Cosmic evolution: NLS1 sample at higher redshifts

using the MgII line

A NLS1-blazar composite J0324+3410

SDSS spectrum: typical of NLS1

HST residual image

one-armed spiral

A NLS1-blazar composite SDSS J0324+3410

Non-thermal continuum SED resembles Mrk 421

TeV γ-ray detected (3 σ) by Whipple (Falcone 0’4)

Intra-night large amplitude variability

X-ray fast variability seen by Swift

myth ?

NLS1: high accretion rate

HPB: low accretion rate

HPB blazarZhou, Wang, Yuan et al. 2006 ApJL submitted

AGN with IMBH in the dwarf galaxy J1605+1748AGN with IMBH in the dwarf galaxy J1605+1748

MMBHBH~ 6 x10~ 6 x104 4 MM ⊙ ⊙ (Kaspi et al. 2005) (Kaspi et al. 2005)

2.5 x102.5 x105 5 MM ⊙ ⊙ (Bentz et al.2006) (Bentz et al.2006)

Dong, Wang, Yuan, et al., ApJ submitted, astro-ph/0610145

poster # 268poster # 268

host galaxy Mhost galaxy MRR~ -17.8~ -17.8

IMBH in the dwarf galaxy J1605+1748IMBH in the dwarf galaxy J1605+1748

NLS1s from SDSSNLS1s from SDSS(3) Frequency of finding NLS1s: (3) Frequency of finding NLS1s:

strongly dependent on optical luminositystrongly dependent on optical luminosity

The Fe II emission strength

The FeII emission in NLS1s is ~twice stronger than normal BL AGN

R4570 = Fe II (λ4434-4684) / Hβ

Radio-loudnessRadio-loudness