OPTICAL SPECTROSCOPY OF Hα FILAMENTS IN COOL CORE CLUSTERS: KINEMATICS, REDDENING, AND SOURCES OF IONIZATION
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McDonald-2012-OPTICAL SPECTROSCOPY.pdf
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Author(s)
McDonald, Michael A.
Veilleux, Sylvain
Rupke, David S. N.
Date Issued
February 2012
Journal
Astrophysical Journal
Publisher
Institute of Physics/American Astronomical Society
Citation
McDonald, Michael, Sylvain Veilleux, and David S. N. Rupke. “OPTICAL SPECTROSCOPY OF Hα FILAMENTS IN COOL CORE CLUSTERS: KINEMATICS, REDDENING, AND SOURCES OF IONIZATION.” The Astrophysical Journal 746, no. 2 (February 2, 2012): 153. © 2012 American Astronomical Society.
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Final published version
Abstract
We have obtained deep, high spatial and spectral resolution, long-slit spectra of the Hα nebulae in the cool cores of nine galaxy clusters. This sample provides a wealth of information on the ionization state, kinematics, and reddening of the warm gas in the cool cores of galaxy clusters. We find evidence for only small amounts of reddening in the extended, line-emitting filaments, with the majority of filaments having E(B – V) < 0.2. We find, in agreement with previous works, that the optical emission in cool core clusters has elevated low-ionization line ratios. The combination of [O III]/Hβ, [N II]/Hα, [S II]/Hα, and [O I]/Hα allow us to rule out collisional ionization by cosmic rays, thermal conduction, and photoionization by intracluster medium (ICM) X-rays and active galactic nuclei as strong contributors to the ionization in the bulk of the optical line-emitting gas in both the nuclei and filaments. The data are adequately described by a composite model of slow shocks and star formation. This model is further supported by an observed correlation between the line widths and low-ionization line ratios which becomes stronger in systems with more modest star formation activity based on far-ultraviolet observations. We find that the more extended, narrow filaments tend to have shallower velocity gradients and narrower line widths than the compact filamentary complexes. We confirm that the widths of the emission lines decrease with radius, from FWHM ~600 km s[superscript –1] in the nuclei to FWHM ~100 km s[superscript –1] in the most extended filaments. The variation of line width with radius is vastly different than what is measured from stellar absorption lines in a typical giant elliptical galaxy, suggesting that the velocity width of the warm gas may in fact be linked to ICM turbulence and, thus, may provide a glimpse into the amount of turbulence in cool cores. In the central regions (r < 10 kpc) of several systems the warm gas shows kinematic signatures consistent with rotation, consistent with earlier work. We find that the kinematics of the most extended filaments in this sample are broadly consistent with both infall and outflow, and recommend further studies linking the warm gas kinematics to both radio and X-ray maps in order to further understand the observed kinematics.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637x/746/2/153
