A transition mass for black holes to show broad emission lines
  Although the super-massive (AGN) and stellar mass (XRBs) black holes have
many properties in common, the broad emission lines (BELs) are exclusively
signatures of the AGN. Based on the detection of these lines from SDSS data
bases, there seems to be no AGN with mass M_BH \lesssim 10^5 M_sun. In this
paper we investigate if such low mass black holes are really non-existent or
they are undetected because the BELs in them are not produced efficiently.
Using the ionizing spectral energy distribution for a wide range of black hole
mass, 10 - 10^9 M_sun, spanning XRBs to AGN, we calculate the equivalent widths
(EWs) of ultraviolet and optical lines Ly\alpha 1216 \AA, H\beta 4861 \AA, CIV
1549 \AA and MgII 2798 \AA. The LOC (locally optimally emitting cloud) model
has been used to describe the broad emission line region (BELR) for the
calculations. We find that the hardening of the SED shape with decreasing mass
do not decrease the BEL EWs. However, finite size of the BELR, as measured by
the line widths, which is controlled by the mass of the black hole, regulates
the production of these emission lines. There seems to be a peak in the EWs of
the emission lines for typical AGN black holes of ~ 10^8 M_sun, below which the
lines become intrinsically fainter with a sharp fall-off below ~ 10^6 M_sun.
This may be the cause of the absence of low mass AGN in SDSS.
