We search for misclassified type 1 AGNs among type 2 AGNs identified with emission line flux ratios, and investigate the properties of the sample. Using 4 113 local type 2 AGNs at 0.02 < z < 0.05 selected from Sloan Digital Sky Survey Data Release 7, we detected a broad component of the Hα line with a Full-Width at Half-Maximum (FWHM) ranging from 1 700 to 19 090 km s−1 for 142 objects, based on the spectral decomposition and visual inspection. The fraction of the misclassified type 1 AGNs among type 2 AGN sample is 3.5%, implying that a large number of missing type 1 AGN population may exist. The misclassified type 1 AGNs have relatively low luminosity with a mean broad Hα luminosity, log LHα = 40.50 ± 0.35 erg s−1, while black hole mass of the sample is comparable to that of the local black hole population, with a mean black hole mass, log MBH = 6.94 ± 0.51 M⊙. The mean Eddington ratio of the sample is log Lbol/LEdd = −2.00±0.40, indicating that black hole activity is relatively weak, hence, AGN continuum is too weak to change the host galaxy color. We find that the Oiii lines show significant velocity offsets, presumably due to outflows in the narrow-line region, while the velocity offset of the narrow component of the Hα line is not prominent, consistent with the ionized gas kinematics of general type 1 AGN population.

Abstract
1. INTRODUCTION
2. SAMPLE SELECTION
3. ANALYSIS
    3.1. Spectral Decomposition
    3.2. Emission Line Fitting
    3.3. Black HoleMass and Eddington ratio
4. RESULTS
    4.1. Sample Properties
    4.2. Comparison with MPA-JHU
    4.3. Velocity offset of the emission lines
    4.4. Kinematics of the ionized gas
5. DISCUSSION AND CONCLUSIONS
REFERENCES

• HONG-JIN KWON(R&E Program, Gyeonggi Science High School for the Gifted)
• SANG CHUL KIM(Korea Astronomy and Space Science Institute)
• SEUNG-EON LEE(R&E Program, Gyeonggi Science High School for the Gifted)
• JAE-HYUK KIM(R&E Program, Gyeonggi Science High School for the Gifted)
• HYUN-JIN BAE(Department of Astronomy and Center for Galaxy Evolution Research, Yonsei University)
• DAESEONG PARK(Department of Physics and Astronomy, University of California Irvine)
• JI-GANG KIM(Astronomy Program, Department of Physics and Astronomy, Seoul National University, R&E Program, Gyeonggi Science High School for the Gifted)
• JONG-HAK WOO(Astronomy Program, Department of Physics and Astronomy, Seoul National University) CORRESPONDING AUTHOR