A transition mass for black holes to show broad emission lines

Дата и время публикации : 2012-11-14T05:40:03Z

Авторы публикации и институты :
Susmita Chakravorty
Martin Elvis
Gary Ferland

Ссылка на журнал-издание: Ссылка на журнал-издание не найдена
Коментарии к cтатье: 7 pages, 5 figures. Submitted to MNRAS
Первичная категория: astro-ph.CO

Все категории : astro-ph.CO

Краткий обзор статьи: 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 Lyalpha 1216 AA, Hbeta 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.

Category: Physics