Rose, Tom and Edge, A. C. and Combes, F. and Gaspari, M. and Hamer, S. and Nesvadba, N. and Peck, A. B. and Sarazin, C. and Tremblay, G. R. and Baum, S. A. and Bremer, M. N. and McNamara, B. R. and O’Dea, C. and Oonk, J. B. R. and Russell, H. and Salomé, P. and Donahue, M. and Fabian, A. C. and Ferland, G. and Mittal, R. and Vantyghem, A. (2019) 'Constraining cold accretion onto supermassive black holes : molecular gas in the cores of eight brightest cluster galaxies revealed by joint CO and CN absorption.', Monthly notices of the Royal Astronomical Society., 489 (1). pp. 349-365.
To advance our understanding of the fuelling and feedback processes which power the Universe’s most massive black holes, we require a significant increase in our knowledge of the molecular gas which exists in their immediate surroundings. However, the behaviour of this gas is poorly understood due to the difficulties associated with observing it directly. We report on a survey of 18 brightest cluster galaxies lying in cool cores, from which we detect molecular gas in the core regions of eight via carbon monoxide (CO), cyanide (CN) and silicon monoxide (SiO) absorption lines. These absorption lines are produced by cold molecular gas clouds which lie along the line of sight to the bright continuum sources at the galaxy centres. As such, they can be used to determine many properties of the molecular gas which may go on to fuel supermassive black hole accretion and AGN feedback mechanisms. The absorption regions detected have velocities ranging from -45 to 283 km s−1 relative to the systemic velocity of the galaxy, and have a bias for motion towards the host supermassive black hole. We find that the CN N = 0 - 1 absorption lines are typically 10 times stronger than those of CO J = 0 - 1. This is due to the higher electric dipole moment of the CN molecule, which enhances its absorption strength. In terms of molecular number density CO remains the more prevalent molecule with a ratio of CO/CN ∼10, similar to that of nearby galaxies. Comparison of CO, CN and H I observations for these systems shows many different combinations of these absorption lines being detected.
|Full text:||(AM) Accepted Manuscript|
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|Publisher Web site:||https://doi.org/10.1093/mnras/stz2138|
|Publisher statement:||This article has been accepted for publication in the Monthly notices of the Royal Astronomical Society ©: 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||30 July 2019|
|Date deposited:||07 August 2019|
|Date of first online publication:||02 August 2019|
|Date first made open access:||No date available|
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