w.bian et al- stellar and gaseous velocity dispersions in type ii agns at 0.3 < z < 0.83 from the...

8/3/2019 W.Bian et al- Stellar and gaseous velocity dispersions in type II AGNs at 0.3 < z < 0.83 from the Sloan Digital Sky Survey

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Mon. Not. R. Astron. Soc. 000, 000000 (0000) Printed 23 May 2006 (MN LATEX style file v2.2)

Stellar and gaseous velocity dispersions in type II AGNs at

0.3 < z < 0.83 from the Sloan Digital Sky Survey

W.Bian1,2, Q. Gu3, Y. Zhao3, L. Chao1 and Q. Cui11Department of Physics and Institute of Theoretical Physics, Nanjing Normal University, Nanjing 210097, China2Key Laboratory for Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100039, China3Department of Astronomy, Nanjing University, Nanjing 210093, China

23 May 2006

ABSTRACTWe apply the stellar population synthesis code by Cid Fernandes et al. to model thestellar contribution for a sample of 209 type II AGNs at redshifts 0.3 < z < 0.83from the Sloan Digital Sky Survey. The reliable stellar velocity dispersions () areobtained for 33 type II AGNs with significant stellar absorption features. Accordingto the L[OIII] criterion of 3 10

8 L, 20 of which can be classified as type II quasars.We use the formula of Greene & Ho to obtain the corrected stellar velocity dispersions(c). We also calculate the supermassive black holes masses from

c

in these higher-redshift type II AGNs. The [O III] luminosity is correlated with the black hole mass,and no correlation is found between the [O III] luminosity and the Eddington ratio.Three sets of two-component profiles are used to fit multiple emission transitions ([OIII]4959, 5007 and [O II]3727, 3729) in these 33 stellar-light subtracted spectra.We also measure the gas velocity dispersion (g) from these multiple transitions, and

find that g can trace c

(although with considerable scatter), which confirms thatthe gaseous kinematics of narrow line regions in these type II quasars are primarilydominated by the gravitational potential of the bulge. The distribution of < g/c >is 1.240.76 for the core [O III] line and 1.200.96 for the [O II] line, which suggeststhat g of the core [O III] and [O II] lines can trace c within about 0.1 dex in thelogarithm of c. For the secondary driver, we find that the deviation of g from

c

iscorrelated with the Eddington ratio.

Key words: galaxies:active galaxies:nuclei quasars: emission lines

1 INTRODUCTION

Recent advances on the study of normal galaxies and activegalactic nuclei (AGNs) are that we found more evidence forthe existence of central supermassive black holes (SMBHs)and the relationship between SMBHs and bulge propertiesof host galaxies (Gebhardt et al. 2000; Ferrarese & Mer-ritt 2000; Tremaine et al. 2002; Begelman 2003; Shen et al.2005). We can use the stellar and/or gaseous dynamics toderive the SMBHs masses in nearby inactive galaxies. How-ever, it is much more difficult for the case of AGNs. Withthe broad emission lines from broad-line regions (BLRs)(e.g.H, Mg II, CIV; H), the reverberation mapping methodand the empirical size-luminosity relation can be used toderive the virial SMBHs masses in AGNs (Kaspi et al. 2000;Vestergaard 2002; McLure & Jarvis 2002; Wu et al. 2004;

Greene & Ho 2006a). It has been found that nearby galax-ies and AGNs follow the same strong correlation betweenthe central SMBHs masses (MBH) and stellar bulge velocitydispersion () (the MBH relation) (Nelson et al. 2001;

Tremaine et al. 2002; Greene & Ho 2006a, 2006b), which alsoimplied that the mass from reverberation mapping method

is reliable.

According to the unification model of active galacticnuclei (e.g. Antonucci 1993; Urry & Padovani 1995), AGNscan be classified into two classes depending on whether thecentral engine and BLRs are viewed directly (type I AGNs)or are obscured by circumnuclear medium (type II AGNs).In type I AGNs, by using the broad emission lines from BLRs(the reverberation mapping method or the empirical size-luminosity relation), we can derive virial SMBHs masses. Itis not easy to study their host galaxies because their opticalspectra are dominated by the non-stellar emission. This isespecially true for luminous AGNs, where the continuumradiation from central source outshines the stellar light from

the host galaxy.In type II AGNs, the obscuration of BLRs makes both

the reverberation mapping method and the empirical size-luminosity relation impossible to derive SMBHs masses.

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2 W. Bian, Q. Gu, Y. Zhao, L. Chao, Q. Cui

However, we can use the well-known MBH relation to de-rive SMBHs masses if we can accurately measure the stellarbulge velocity dispersion (). There are mainly two meth-ods to measure , one is in Fourier space (e.g. Tonry &

Davis 1979), the other is in pixel space (e.g. Greene & Ho2006b and reference therein). These years it is popular to usethe combination of galaxy template spectra broadened by aGaussian kernel (e.g. Kauffmann et al. 2003; Cid Fernandeset al. 2004a; Greene & Ho 2006b). Though it is still not aneasy task to measure , it has been shown successfully toderive through fitting stellar absorption features: such asCa II 8498, 8542, 8662 triplet, Mg Ib 5167, 5173, 5184triplet, and Ca H+K 3969, 3934, etc.

On the other hand, Nelson & Whittle (1996) find thatthe gaseous velocity dispersion (g) of [O III]5007 from thenarrow-line regions (NLRs) is nearly the same as for asample of 66 Seyfert galaxies, and suggest that the gaseous

kinematics of NLRs be primarily governed by the bulge grav-itational potential. Nelson (2000) find a tight relation be-tween MBH and [OIII] (the [O III]5007 velocity dispersion)for AGNs, very similar to the relation of MBH, althoughwith more scatter, which strongly suggests that g can beused as a proxy for . For lower-redshift type II AGNswith 0.02 < z < 0.3, Kauffmann et al. (2003) have investi-gated the properties of their hosts from the Sloan Digital SkySurvey (SDSS) Data Release One (DR1), measured andestimated the SBMHs masses from (Brinchmann et al.2004). By using this sample, Greene & Ho (2005) measuredthe gaseous velocity dispersion (g) from multiple transi-tions ([O II] 3727, [O III] 5007, and [S II] 6716, 6731)and compared and g. They found that g from these

multiple transitions trace very well, although for someemission features showing considerable scatter.

Type II quasars are the luminous analogs of low-luminosity type II (Seyfert 2) galaxies. The obscuration ofBLRs makes quasars appear to be type II quasars (obscuredquasars). Some methods have been used to discover type IIquasars, but only a handful have been found. Recently, Za-kamsa et al. (2003) present a sample of 291 type II AGNs atredshifts 0.3 < Z < 0.83 from the SDSS spectroscopic data.About half are type II quasars if we use the [O III] 5007line luminosity to represent the strength of the nuclear ac-tivity. How about the g relation for type II quasars?And how about their SMBHs masses and the Eddington ra-

tios Lbol/LEdd (i.e. the bolometric luminosity as a fractionof the Eddington luminosity)?Here we used the sample of Zakamsa et al. (2003) to

study these questions in type II quasars. In section 2, weintroduce the data and the analysis. Our results and discus-sion are given in Sec. 3. All of the cosmological calculationsin this paper assume H0 = 70 km s

1 Mpc1, M = 0.3, = 0.7.

2 DATA AND ANALYSIS

With SDSS, Zakamsa et al. (2003) present a sample of 291type II AGNs at redshifts 0.3 < z < 0.83. We download

these spectra from SDSS Data Release Four (DR4) and thespectra for 202 type II AGNs at redshifts 0.3 < z < 0.83are obtained. SDSS spectra cover 3800-9200 A, with resolu-tion (/) of 1800 < R < 2100 and sampling of 2.4 pixels

per resolution element. The fibers in the SDSS spectroscopicsurvey have a diameter of 3 on the sky, for our Type IIAGNs sample at redshifts 0.3 < z < 0.83, the projected fi-bre aperture diameter typically contains about 90% of the

total host galaxy light (Kauffmann & Heckman 2005), andthus makes it feasible to observe significant stellar absorp-tion features, which is the key point to accurately measurethe stellar velocity dispersion () in this paper.

We first model the stellar contribution in the SDSSspectra of type II AGNs through the modified version ofthe stellar population synthesis code, STARLIGHT (ver-sion 2.0, Cid Fernandes et al. 2001; Cid Fernandes et al.2004a; Cid Fernandes et al. 2004b; Garcia-Rissman et al.2005), which adopted the new stellar library from Bruzual& Charlot (2003). The code does a search for the linearcombination of Simple Stellar Populations (SSP) to matcha given observed spectrum O. The model spectrum M is:

M(x, M0 , AV, v, ) = M0

Nj=1

xjbj,r

G(v, )(1)

where bj, LSSP (tj , Zj)/L

SSP0 (tj , Zj) is the spectrum of

the jth SSP normalized at 0, r 100.4(AA0 ) is the

reddening term, x is the population vector, M0 is the syn-thetic flux at the normalization wavelength, G(v, ) isthe line-of-sight stellar velocity distribution, modeled as aGaussian centered at velocity v and broadened by . Thematch between model and observed spectra is calculated by2(x, M0 , AV, v, ) =

N=1

[(O M) w]2, where the

weight spectrum w is defined as the inverse of the noisein O. For more detail, please refer to Cid Fernandes et al.

(2005).Prior to the synthesis, the Galactic extinction is cor-

rected by using the extinction law of Cardelli, Clayton &Mathis (1989) and the AV value from Schlegel, Finkbeiner& Davis (1998) as listed in the NASA/IPAC ExtragalacticDatabase (NED). The spectra are transformed into the restframe defined by the redshift given in their FITS header. Thespectrum is normalized at 4020A and the signal-to-noise ra-tio is measured in the S/N window between 4730 and 4780A. Masks of 20 30 A around obvious emission lines areconstructed for each object individually. Because the red-shift coverage of this type II AGNs sample, we focus on thestrongest stellar absorption features of Ca II K and the G-

band, which are less affected by nearby emission lines. Anf 1.5 power-law component is used to account for the

contribution from the AGN continuum emission (Watanabeet al. 2003). Finally we check visually our spectral fittingresults one by one.

For our sample, the S/N in the S/N window varies be-tween 0.3 and 21.5. The fitting results for high S/N objectsare usually better than those for low S/N ones. After in-specting the fitting results, we find that the fitting goodnessdepends not only on the S/N (> 5), but also on the ab-sorption lines equivalent widths (EWs > 1.5A). At last weselect 33 type II AGNs, which are shown significant stel-lar absorption features and are well fitted to derive reliablemeasurement of stellar velocity dispersion .

The [O III]5007 luminosity (L[OIII]) is subject to ex-tinction by interstellar dust in the host galaxy and in ourGalaxy, which is usually corrected by using the Balmerdecrement. However, for most objects in the sample of Za-

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3

kamsa et al. (2003), H cannot be showed in SDSS spectra.Therefore the extinction is not corrected. In order to checkthat these sub-sample is representative of total sample ofZakamsa et al. (2003) respect to [O III]5007 luminosity

(L[OIII]), we plotted the histograms of the L[OIII] distribu-tion for sub-sample and total-sample (see figure 1). And thenwe used the T-test and found that at the 0.95 level, the dif-ference of these two population is not significantly different.L[OIII] is directly adopted from table 1 in Zakamsa et al.(2003). Using the L[OIII] criterion of 310

8 L(the logarithmis 8.477), which corresponds to the intrinsic absolute mag-nitudes MB < 23 (Zakamsa et al. 2003), 20 objects can beclassified as type II quasars. Fig. 1 shows a sample fittingfor SDSS J150117.96+545518.2 with S/N=20.5. The finalresults are presented in table 1. All the fittings for 33 typeII AGNs are appended in the appendix.

After subtracting the synthetic stellar components and

the AGNs continuum, we obtain the clean pure emission-line spectra as shown in the top panel of figure 2, wherewe can analysis the pure emission-line profiles in detail byusing the multi-component spectral fitting task SPECFIT(Kriss 1994) in the IRAF-STSDAS package 1. Because ofthe asymmetry of profiles of [O III]4959, 5007 lines, twosets of two-gaussian profiles are used in order to removeproperly the asymmetric blue/red wings of [O III] line. Wetake the same linewidth for each component, and fix the fluxratio of [O III]4959 to [O III]5007 to be 1:3. For threeobjects, we cant fit the [O III] lines for their irregular [OIII] lines (See table 1). For the [O II] 3727, 3729 lines, weuse two-gaussian profiles and fix their wavelength separationto the laboratory value, the ratio of the line intensities is

allowed to vary during the fitting. The decomposition for [OII] lines is more difficult because of relatively low S/N andthat the expected line widths are comparable to the pairseparation (2.4A). We do not fit [S II] 6716, 6731 for ourlarger redshifts of our sample. For more details, please referto Bian, Yuan & Zhao (2005, 2006). Our sample fitting forSDSS J150117.96+545518.2 is showed in figure 3.

3 RESULTS AND DISCUSSION

3.1 The uncertainties of stellar velocity dispersion() and gaseous velocity dispersion (g)

The derived stellar velocity dispersion was corrected by theinstrumental resolutions of both the SDSS spectra and theSTELIB library. Cid Fernandes et al. (2004a) have used theirstellar population synthesis method to study a sample of 79nearby galaxies observable from the southern hemisphere, ofwhich 65 are Seyfert 2 galaxies. The S/N in the S/N win-dow varies between 10 and 67. They compared their withvalues from the literature and found the agreement is good.And they estimated that the uncertainty in is typicallyabout 20 km s1. Recently, Cid Fernandes et al. (2005) ap-ply their synthesis method to a larger sample of 50362 galax-ies from the SDSS Data Release 2 (DR2). Their derived

1 IRAF is distributed by the National Optical Astronomy Obser-vatories, which are operated by the Association of Universities forResearch in Astronomy, Inc., under cooperative agreement withthe National Science Foundation.

is consistent very well with that of the MPA/JHU group(Kauffmann et al. 2003). The median of the difference be-tween the two estimates is just 9 km s1. We have carefullychecked our synthesis fitting result one by one and picked

out 33 type II AGNs that are well fitted and the stellar ve-locity dispersion () are reliably derived. The spectral S/Nfor these objects are in the range of 5 to 21.5, most of whichare larger than 10, thus the typical uncertainty in shouldbe around 20 km s1.

Recent, Greene & Ho (2006a, 2006b) used the direct-fitting method (Barth et al. 2002) to study the the sys-tematic biases of form different regions around Ca IItriplet, Mg Ib triplet, and Ca H+K stellar absorption fea-tures, which are introduced by both template mismatch andcontamination from AGNs. They argue that the Ca II tripletprovides the most reliable measurements of and thereis a systematic offset between CaK and derived from

other spectral regions. For our higher-redhsift sample andthe SDSS wavelength coverage 3800-9200A, it is impossi-ble to measure from Ca II triplet. Therefore, for higher-redhsift type II AGNs, new observation around Ca II tripletis necessary in the future. Here we used the following for-mula to obtain the corrected velocity dispersion c(Greene& Ho 2006b),

c = (1.40 0.04) (71 5). (2)

For three objects, is near the instrumental resolution andthe corrected c is unliable. These objects are omitted in ournext analysis, which are denoted as in table 1.

The gaseous velocity dispersion (g) is obtainedfrom full width half maximum (FWHM) of emis-sion lines by assuming the Gaussian profile: g[OII] =

FWHM[OII]/2.35 and g[OIII] = FWHM[OIII]/2.35. Consid-ering the SDSS spectrum resolution, the intrinsic g derivedfrom FWHM([OIII]) may be instrumentally broadened. Theintrinsic g value can be approximated by g = (

2obs

(inst/(1 + z))2)1/2, where z is the redshift. For the spectra

from SDSS, the mean values of inst are 74 km s1(the loga-

rithm is 1.87 dex) for [O II], and 60 km s1(the logarithm is1.78 dex) for [O III] (Greene & Ho 2005), respectively. Theresults ofg are listed in table 1 (Columns 7 and Columns 8).After removing the effect of instrumental broadening, someobjects become unresolved (see table 1). Measurements ofgbelow the resolution limit (74 and 60 km s1for [O II] and

[O III], respectively) are not reliable. The error of g is de-rived from the error of the linewidth. For the linewidth, thetypical error is about 10 per cent. However, the systematiceffects are neglected, e.g. the uncertainties of the continuumsubtraction, and component decomposition (Bian, Yuan &Zhao 2005).

3.2 The SMBHs masses and Eddington ratios intype II quasars

Using the reverberation mapping method or the empiri-cal size-luminosity relation, it is impossible to estimate theSMBHs masses in type II quasars for the lack of emission

line from BLRs. Here we use the formulae to derive theSMBHs masses in type II quasars from stellar velocity dis-persion (Tremaine et al. 2002), which is MBH( M) =108.13(c/(200 kms

1))4.02.

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4 W. Bian, Q. Gu, Y. Zhao, L. Chao, Q. Cui

We also calculate the Eddington ratio, Lbol/LEdd . Weuse [O III] luminosity as a surrogate for the AGN lumi-nosity (Heckman et al., 2004; Greene & Ho 2005), Lbol =3500L[OIII], to calculate the bolometric luminosity Lbol, and

LEdd = 1.261038MBH/ M ergs s1. The results of SMBHsmasses and Eddington ratios in type II AGNs are also pre-sented in table 1 (Columns 12 and 13). We also calculatedthe SMBHs masses and Eddington ratios for the lower-redshifts type II AGNs at 0.02 < z < 0.3 presented byKauffmann et al. (2003). For the typical uncertainties of20km s1for = 200 km s

1, the errors of log wouldbe about 0.05 dex, corresponding 0.17 dex for logMBH ,and almost the same for Lbol/LEdd (Bian, Yuan, & Zhao2005). Here we didnt consider the cosmology evolution ofMBH relation (e.g. Woo et al. 2006), which is a questionopen to debate.

In figure 4, we compared the distribution of SMBHs

masses and Eddington ratios in the lower-redshifts sampleand the higher-redshifts sample. It is found that the typeII AGNs at higher-redshifts have higher SMBHs masses andhigher Eddington ratios.

It is well known that the Eddington ratio is an impor-tant parameter to describe the accretion process in AGNs.The [O III] luminosity is usually used as a surrogate forthe AGN luminosity (Heckman et al. 2004 and the refer-ence therein). In figure 5, we plot the [O III] luminosityversus the SMBHs masses. Using a least-squares regression,we derive the correlation between MBH and L[OIII] to be:log(L[OIII]/L) = (6.830.65)+(0.220.08)log(MBH/M).The correlation coefficient R is 0.45, with a probability ofP = 0.012 for rejecting the null hypothesis of no correla-

tion. However, no correlation is found between the [O III]luminosity and the accretion ratio. From the peptonizationmodel, the strength of [O III] is controlled by the NLRscovering factor, its density, and ionization parameter (e.g.Baskin & Laro 2005). The relation between the [O III] lumi-nosity and the AGN bolometric luminosity is still a questionto debate.

3.3 The g relation

The existence of a good correlation between stellar velocitydispersion () and ionized gas velocity dispersion (g) (e.g.Nelson & Whittle 1996) suggests that the gaseous kinemat-

ics of NLRs in Seyfert galaxies be primarily dominated bythe bulge gravitational potential, which is further confirmedby Nelson & Whittle (1996). Most recently, Greene & Ho(2005) have investigated a large and homogeneous sampleof lower-redshift (0.02 < z < 0.3) Type II AGNs from theSDSS, and found that g traces . Though the gas kine-matics of NLRs are governed by the gravitational potentialof the bulges, they also find that the accretion rate plays animportant secondary role.

Following Greene & Ho (2005), we study the g c

relation for 33 Type II AGNs at redshifts 0.3 < z < 0.83after measuring the gas velocity dispersion (g) from thenarrow emission lines from NLRs, and the stellar velocitydispersion (c) from the Ca H+K, G-band absorption fea-

ture, which is shown in figure 2. It is obvious that, the linewidths of the core component of [O III] and [O II] can ap-proximately trace the stellar velocity dispersion, althoughwith a considerable scatter (see figure 6). We confirm that

the higher-redshift narrow-line AGNs follow the same trendas the lower-redshift ones, where the gas kinematics in NLRsis dominated by gravitational potential of the bulge andthe velocity dispersion in the gas and stars are compara-

ble. In order to qualify the comparison between g andc, we calculate the distribution of < g/

c >. The value

is 1.24 0.76 for the the core component of [O III] line,1.20 0.96 for the [O II] line, which suggest that g of thethe core component of [O III] and [O II] lines can trace cwithin 0.09 and 0.08 dex in the logarithm of c, respectively,and that the high-ionization [O III] line traces c as well asthe low-ionization [O II] line. If we use the line width of[O III] core component to estimate the SMBHs masses fromM[OIII] = 10

8.13([OIII]/(200kms1))4.02 M, we would over-

estimate SMBHs masses by 0.38 dex.For comparison, Greene & Ho (2005) derived the dis-

tribution of < g/ > of lower-redshift type II AGNs with

0.02 < z < 0.3, which are 1.34 0.66 for the [O III] line,1.000.35 for the [O III] core line, and 1.130.38 for the [OII] line. We also calculate the the distribution of < g/

c >

for the sample of Seyfert galaxies (Nelson & Whittle 1996),the value is 1.150.68, suggesting that g of the [O III] linecan trace c within 0.06 dex in the logarithm of

c . Our

results are thus consistent with theirs.To first order, the line widths of the core component

of [O III] and [O II] for both low-redshift and high-redshiftType II AGNs is primarily controlled by the gravitationalpotential of the bulges of host galaxies, and can proximatelytrace the stellar velocity dispersion. As we know, the errorsin virial SMBHs masses derived from galaxy dynamics orsize-luminosity relation is about 0.5 dex (e.g. Magorrian et

al. 1998; Kaspi et al. 2000; Bian & Zhao 2004a, 2004b). Wealso can use the line-width of the core component of [O III]or [O II] to estimate the black hole mass.

In order to find the secondary effect of the line broad-ening in gas lines from NLRs for our higher-redshift narrow-line AGNs, we study the relation between the deviation ofg from

c ( = logg log

c) and the Eddington ratio

(Lbol/LEdd) (Greene & Ho 2005). Using the least-squares re-gression, we find a median strong correlation between thesetwo dimensionless parameters. For the [O III] line, the re-lation is: = (0.09 0.04) + (0.27 0.04)log(Lbol/LEdd).The Spearman rank correlation coefficient R is 0.77, witha probability of P < 104 for rejecting the null hypoth-

esis of no correlation. For the [O II] line, the relation is = (0.11 0.04) + (0.22 0.05)log(Lbol/LEdd), R=0.68,Pnull = 0.00181 (see figure 7). We also find the comparablecorrelation between and Mbh. These results confirm thatthe nuclei accretion process and/or nuclei SMBHs would ef-fect the line width of gas lines from NLRs, although the pri-mary driver is from the gravitational potential of the bulge.

4 CONCLUSION

The stellar population synthesis code is used to model thestellar contribution for a sample of 209 type II AGNs at red-

shifts 0.3 < z < 0.83 from SDSS. According to the L[OIII]criterion of 3 108 L, 20 of which can be classified as typeII quasars. The main conclusions can be summarized as fol-lows.

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The reliable are measured for 33 type II AGNs withsignificant stellar absorption features. We used the formulaof Greene & Ho to obtain the corrected stellar velocity dis-persions (c). And SMBHs masses are calculated from the

MBHc relation. A median strong relation between the [OIII] luminosity and the SMBH mass is found, no correlationbetween the [O III] luminosity and the Eddington ratio. The gas velocity dispersion (g) in NLRs is measured

using three sets of two-gaussian profiles to fit [O III]4959,5007 and [O II]3727, 3729) in these 33 stellar-light sub-tracted spectra. We find that g can trace

c with consider-

able scatter, which confirms that the gaseous kinematics ofNLRs in these type II quasars are primarily dominated bythe gravitational potential of the bulge. The distribution of < g/

c > is 1.24 0.76 for the

core [O III] line and 1.20 0.96 for the [O II] line, whichsuggests that g can trace

c within about 0.1 dex in the

logarithm of c

. The deviation of g from c

is correlatedwith the Eddington ratio.

ACKNOWLEDGMENTS

This work has been supported by the NSFC (No. 10403005;No. 10473005; No. 10273007) and NSF from Jiangsu Provin-cial Education Department (No. 03KJB160060). QGUwould like to acknowledge the financial supports from ChinaScholarship Council (CSC) and the National Natural ScienceFoundation of China under grants 10103001 and 10221001.Funding for the creation and distribution of the SDSSArchive has been provided by the Alfred P. Sloan Foun-

dation, the Participating Institutions, NASA, the NationalScience Foundation, the US Department of Energy, theJapanese Monbukagakusho, and the Max Planck Society.The SDSS Web site is http:// www.sdss.org/. This researchhas made use of the NASA/IPAC Extragalactic Database,which is operated by the Jet Propulsion Laboratory at Cal-tech, under contract with NASA.

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