Low-Mass Star Formation in Cooling Flow Galaxies

Details Low-Mass Star Formation in Cooling Flow Galaxies Low-Mass Star Formation in Cooling Flow Galaxies

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...416l..61s&link_type=abstract

Astrophysical Journal Letters v.416, p.L61

Astronomy and Astrophysics

Astronomy

8

Galaxies: Cooling Flows, Galaxies: Photometry

Scientific paper

Observations are presented based on optical and near-IR imaging to support the idea that isolated and cluster cooling flow galaxies are enriched in low-mass stars, the result of recent, truncated IMF star formation from accreting gas. Galaxies with low accretion rates (M < 5 M_sun_ yr^-1^) have normal optical colors and gradients, but red V - K colors signaling an IMF enhanced in low-mass main-sequence stars. Cluster cooling flow ellipticals (M> 50 M_sun_ yr^-1^) selected to have blue optical colors indicative of recent star formation also show redder V - K colors with respect to expected values for a weak starburst. The strength of the starburst in the U - V, V - K diagram indicates an efficiency which places only 5% of the accreting matter into an IMF similar to that found in the Galactic disk and the remaining mass is again sited in low-mass stars.

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