We present medium-resolution spectra ( R \sim 2000 –4000 ) at 0.4–1.0 \mu m and 0.7–2.5 \mu m of 16 active galactic nuclei ( AGNs ) selected with red color in the near-infrared ( NIR ) of J - K > 2.0 mag at z \sim 0.3 .
We fit the H \beta , H \alpha , P \beta , and P \alpha lines from these spectra to obtain their luminosities and line widths .
We derive the E ( B - V ) color excess values of the NIR-red AGNs using two methods , one based on the line-luminosity ratios and another based on the continuum slopes .
The two E ( B - V ) values agree with each other at rms dispersion \sim 0.249 .
About half of the NIR-red AGNs have g ^ { \prime } - K < 5 magnitude , and we find that these NIR red , but blue in optical-NIR AGNs , have E ( B - V ) \sim 0 , suggesting that a significant fraction of the NIR color-selected red AGNs are unobscured or only mildly obscured .
After correcting for the dust extinction , we estimate the black hole ( BH ) masses and the bolometric luminosities of the NIR-red AGNs using the Paschen lines to calculate their Eddington ratios ( \lambda _ { Edd } ) .
The median Eddington ratios of nine NIR-red AGNs ( \log ( \lambda _ { Edd } ) \simeq - 0.654 \pm 0.176 ) are only mildly higher than those of unobscured type 1 AGNs ( \log ( \lambda _ { Edd } ) \simeq - 0.961 \pm 0.008 ) .
Moreover , we find that the M _ { BH } – \sigma _ { \ast } relation for three NIR-red AGNs is consistent with that of unobscured type 1 AGNs at similar redshift .
These results suggest that the NIR red color selection alone is not effective at picking up dusty , intermediate-stage AGNs .