Timing the starburst-AGN connection

Vivienne Wild, Timothy Heckman, Stephane Charlot

Research output: Contribution to journalArticlepeer-review

184 Citations (Scopus)

Abstract

The mass of supermassive black holes at the centre of galaxies is tightly correlated with the mass of the galaxy bulges which host them. This observed correlation implies a mechanism of joint growth, but the precise physical processes responsible are a matter of some debate. Here, we report on the growth of black holes in 400 local galactic bulges which have experienced a strong burst of star formation in the past 600 Myr. The black holes in our sample have typical masses of 106.5-107.5 M-circle dot and the active nuclei have bolometric luminosities of the order of 1042-1044 erg s-1. We combine stellar continuum indices with H alpha luminosities to measure a decay time-scale of similar to 300 Myr for the decline in star formation after a starburst. During the first 600 Myr after a starburst, the black holes in our sample increase their mass by on-average 5 per cent and the total mass of stars formed is about 103 times the total mass accreted on to the black hole. This ratio is similar to the ratio of stellar to black hole mass observed in present-day bulges. We find that the average rate of accretion of matter on to the black hole rises steeply roughly 250 Myr after the onset of the starburst. We show that our results are consistent with a simple model in which 0.5 per cent of the mass lost by intermediate-mass stars in the bulge is accreted by the black hole, but with a suppression in the efficiency of black hole growth at early times plausibly caused by supernova feedback, which is stronger at earlier times. We suggest this picture may be more generally applicable to black hole growth, and could help explain the strong correlation between bulge and black hole mass.

Original languageEnglish
Pages (from-to)933-947
Number of pages15
JournalMonthly Notices of the Royal Astronomical Society
Volume405
Issue number2
DOIs
Publication statusPublished - 21 Jun 2010

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