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No evidence for a central IMBH in M15

F. Kirsten ; Wouter Vlemmings (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik)
Astronomy and Astrophysics (0004-6361). Vol. 542 (2012),
[Artikel, refereegranskad vetenskaplig]

Intermediate mass black holes (IMBHs) with expected masses M. approximate to 10(4) M-circle dot are thought to bridge the gap between stellar mass black holes ( M. approximate to 3-100 M-circle dot) and supermassive black holes found at the centre of galaxies ( M. > 10(6) M-circle dot). Until today, no IMBH has been confirmed observationally. The most promising objects to host an IMBH as their central mass are globular clusters. Here, we present high sensitivity multi-epoch 1.6 GHz very long baseline interferometry observations of the globular cluster M15 that has been suggested to host an IMBH. Assuming the IMBH to be accreting matter from its surrounding we expect to detect it as a point source moving with the global motion of the cluster. However, we do not detect any such object within a radius of 6000 AU of the cluster centre in any of the five observations spread over more than one year. This rules out any variability of the putative IMBH on the time scale of one to two months. To get the most stringent upper limit for the flux density of the putative IMBH we concatenate the data of all five epochs. In this data we measure a 3 sigma upper flux limit of 10 mu Jy for a central source. We employ the fundamental plane of black hole activity to estimate the mass of the central IMBH candidate. Based on previous X-ray observations of M15 our measurements indicate a 3 sigma upper mass limit of approximate to 500 M-circle dot.

Nyckelord: globular clusters: individual: M15 (NGC 7078), black hole physics, techniques: interferometric, radio, mass black-holes, globular-cluster m15, x-ray sources, advection-dominated accretion, fundamental plane, radio-emission, dynamical models, galaxy, nuclei, binary



Denna post skapades 2012-09-04. Senast ändrad 2015-07-10.
CPL Pubid: 162879

 

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Projekt

Denna publikation är ett resultat av följande projekt:


Advanced radio astronomy in Europe (RADIONET-FP7) (EC/FP7/227290)