Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21536403m&link_type=abstract
American Astronomical Society, AAS Meeting #215, #364.03; Bulletin of the American Astronomical Society, Vol. 42, p.552
Astronomy and Astrophysics
Astronomy
Scientific paper
We present early results from a survey of 21 cooling flow clusters covering 1-2 orders of magnitude in mass, temperature and mass deposition rate, aimed at explaining the presence and morphology of warm, ionized gas in the cores of cooling flow clusters. Using the Maryland-Magellan tunable filter on the Baade 6.5-m telescope at Magellan we have taken a census of these mysterious Hα filaments with unprecedented depth and resolution. These data have been supplemented with archival X-Ray (Chandra), UV (HST, GALEX, XMM-OM), near-IR (2MASS) and radio (VLA) observations. Armed with the most detailed picture of the warm, ionized gas in cooling flow clusters to date, we investigate the possible mechanisms for producing the observed morphologies (magnetic fields, runaway cooling, interaction with satellites, etc) as well as possible ionization mechanisms (young stars, heat conduction from the ICM, collisional heating from cosmic rays, etc). In a recently published pilot study, we present results for the famous cluster Abell 1795. With the improved spatial resolution (DIQ ˜ 0.5"), we resolve the famous 50kpc filament into two, intertwined strands with individual widths unresolved (< 1 kpc). These strands are roughly coincident with strands of point sources detected in the far-UV, likely the sites of star formation. While the ratio of the UV flux to the Hα flux are consistent with photoionization from young stars, the high [N II]/Hα ratio and slight spatial offsets between the UV and Hα centroids suggest additional heating mechanisms must play a minor role.
McDonald Michael
Veilleux Sylvain
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