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  Far Ultraviolet Morphology of Star Forming Filaments in Cool Core Brightest Cluster Galaxies

Tremblay, G. R., O'Dea, C. P., Baum, S. A., Mittal, R., McDonald, M., Combes, F., et al. (2015). Far Ultraviolet Morphology of Star Forming Filaments in Cool Core Brightest Cluster Galaxies. Monthly Notices of the Royal Astronomical Society, 451 (4), 3768-3800. doi:10.1093/mnras/stv1151.

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Item Permalink: https://hdl.handle.net/11858/00-001M-0000-0028-9F31-C Version Permalink: https://hdl.handle.net/11858/00-001M-0000-0028-9F3E-1
Genre: Journal Article

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 Creators:
Tremblay, Grant R., Author
O'Dea, Christopher P., Author
Baum, Stefi A., Author
Mittal, Rupal1, Author
McDonald, Michael, Author
Combes, Françoise, Author
Li, Yuan, Author
McNamara, Brian, Author
Bremer, Malcolm N., Author
Clarke, Tracy E., Author
Donahue, Megan, Author
Edge, Alastair C., Author
Fabian, Andrew C., Author
Hamer, Stephen L., Author
Hogan, Michael T., Author
Oonk, Raymond, Author
Quillen, Alice C., Author
Sanders, Jeremy S., Author
Salomé, Philippe, Author
Voit, G. Mark, Author
Affiliations:
1AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, Hannover, DE, ou_24009              

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Free keywords: Astrophysics, Galaxy Astrophysics, astro-ph.GA
 Abstract: We present a multiwavelength morphological analysis of star forming clouds and filaments in the central ($< 50$ kpc) regions of 16 low redshift ($z<0.3$) cool core brightest cluster galaxies (BCGs). New Hubble Space Telescope (HST) imaging of far ultraviolet continuum emission from young ($\sim 10$ Myr), massive ($> 5$ \Msol) stars reveals filamentary and clumpy morphologies, which we quantify by means of structural indices. The FUV data are compared with X-ray, Ly$\alpha$, narrowband H$\alpha$, broadband optical/IR, and radio maps, providing a high spatial resolution atlas of star formation locales relative to the ambient hot ($\sim10^{7-8}$ K) and warm ionised ($\sim 10^4$ K) gas phases, as well as the old stellar population and radio-bright AGN outflows. Nearly half of the sample possesses kpc-scale filaments that, in projection, extend toward and around radio lobes and/or X-ray cavities. These filaments may have been uplifted by the propagating jet or buoyant X-ray bubble, or may have formed {\it in situ} by cloud collapse at the interface of a radio lobe or rapid cooling in a cavity's compressed shell. The morphological diversity of nearly the entire FUV sample is reproduced by recent hydrodynamical simulations in which the AGN powers a self-regulating rain of thermally unstable star forming clouds that precipitate from the hot atmosphere. In this model, precipitation triggers where the cooling-to- freefall time ratio is $t_{\mathrm{cool}}/t_{\mathrm{ff}}\sim 10$. This condition is roughly met at the maxmial projected FUV radius for more than half of our sample, and clustering about this ratio is stronger for sources with higher star formation rates.

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 Dates: 2015-05-132015
 Publication Status: Issued
 Pages: 36 pages, 30 figures, accepted for publication in MNRAS
 Publishing info: -
 Table of Contents: -
 Rev. Type: -
 Identifiers: arXiv: 1505.03533
DOI: 10.1093/mnras/stv1151
 Degree: -

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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 451 (4) Sequence Number: - Start / End Page: 3768 - 3800 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150