We analyze the spatially resolved kinematics of gas and stars for a sample of ten hidden type 1 AGNs in order to investigate the nature of their central sources and the scaling relation with host galaxy stellar velocity dispersion. We select our sample from a large number of hidden type 1 AGNs, which are identified based on the presence of a broad (full width at half maximum ≳1000 kms-1) component in the Hα line profile and which are frequently mis-classified as type 2 AGNs because AGN continuum and broad emission lines are weak or obscured in the optical spectral range. We used the Blue Channel Spectrograph at the 6.5-m Multiple Mirror Telescope to obtain long-slit data with a spatial scale of 0.3 arcsec pixel-1. We detected broad Hβ lines for only two targets; however, the presence of strong broad Hα lines indicates that the AGNs we selected are all low-luminosity type 1 AGNs. We measured the velocity, velocity dispersion, and ux of stellar continuum and gas emission lines (i.e., Hβ and [OIII]) as a function of distance from the center. The spatially resolved gas kinematics traced by Hβ or [OIII] are generally similar to the stellar kinematics except for the inner center, where signatures of gas out ows are detected. We compare the luminosity-weighted effective stellar velocity dispersions with the black hole masses and find that our hidden type 1 AGNs, which have relatively low back hole masses, follow the same scaling relation as reverberation-mapped type 1 AGN and more massive inactive galaxies.

Abstract
1. Introduction
2. Observations
    2.1. Sample Selection
    2.2. Observations and Data Reduction
3. Analysis
    3.1. Stellar Pseudo-continuum Fitting
    3.2. Emission Line Fitting
4. Results
    4.1. Type 1 AGN Features
    4.2. Gas and Stellar Kinematics
    4.3. Effect of Rotational Broadening in SVD 
    4.4. MBH–bold0mu mumu * Relation 
Summary and Conclusions 
Acknowledgments
References

• Donghoon Son(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea/Department of Astronomy and Center for Galaxy Evolution Research, Yonsei University, Seoul 03722, Republic of Korea)
• Jong-Hak Woo(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea/Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea)
• Da-In Eun(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea)
• Hojin Cho(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea)
• Marios Karouzos(Nature Astronomy, Springer Nature, 4 Crinan Street, N1 9XW, London, UK)
• Songyeon Park(Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea)