Deep CO observations of dominant cluster galaxies with reported cooling flows

Details Deep CO observations of dominant cluster galaxies with reported cooling flows Deep CO observations of dominant cluster galaxies with reported cooling flows

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283..407b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 283, no. 2, p. 407-416

Statistics

Computation

42

Carbon Monoxide, Computational Astrophysics, Cooling Flows (Astrophysics), Elliptical Galaxies, Galactic Clusters, Intergalactic Media, Interstellar Gas, Spiral Galaxies, X Ray Astronomy, X Ray Spectra, Astronomical Models, Deposition, Gravitational Effects, Ionized Gases, Molecular Clouds, Star Formation

Scientific paper

X-ray observations of galaxy clusters have been interpreted as revealing massive cooling flows in many of them. Whatever the final sink (stars, planets, etc.), the cooling gas is bound to pass through a molecular phase. We have used the IRAM 30m millimeter-wave telescope to observe eight cluster dominant galaxies with high reported gas inflow rates in the (12)CO(1-0) and (12)CO(2-1) lines. Despite low noise levels, none of the galaxies were detected in either line with 1 sigma limits to M(H2) ranging between 4 107 and 1.3 109 solar mass. These values are two orders of magnitude below values expected from the reported accretion rates (often M-dot greater than or equal to 100 solar mass/yr) and the measured star-formation time in spirals and ellipticals (tauSF approximately 1 Gyr). Even supposing that the whole process of star formation - from recombination of ionized gas into atoms and molecules to cloud gravitational condensation - is governed by the collapse time (approximately 4 107 yr) and that only part of the cold gas is included in the IRAM beam, our detection limits rule out the high values of M-dot proposed by the 'standard model' of cooling flows by a factor 5 on average.

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