A transition mass for black holes to show broad emission lines
Abstract
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 MBH 105 Msun. 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 - 109 Msun, spanning XRBs to AGN, we calculate the equivalent widths (EWs) of ultraviolet and optical lines Lyα 1216 , Hβ 4861 , CIV 1549 and MgII 2798 . 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 ~ 108 Msun, below which the lines become intrinsically fainter with a sharp fall-off below ~ 106 Msun. This may be the cause of the absence of low mass AGN in SDSS.
Turn this paper into a lesson
ArcXiv compiles a structured reading guide from this paper's metadata: plain-English importance, contributions, prerequisite concepts, which sections to read first, flashcards, and a quiz. Grounded in the abstract, never invented.