U-band Imaging Polarimetry of the Blue Optical Lobes in the Abell 1795 Central Cluster Galaxy

Details U-band Imaging Polarimetry of the Blue Optical Lobes in the Abell 1795 Central Cluster Galaxy U-band Imaging Polarimetry of the Blue Optical Lobes in the Abell 1795 Central Cluster Galaxy

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...18711006m&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #110.06; Bulletin of the American Astronomical Society, Vol. 27, p.1443

Astronomy and Astrophysics

Astronomy

Scientific paper

We have obtained U-band polarimetry of the blue optical lobes located along the radio lobes of the FR I radio source in the Abell 1795 cluster central galaxy (z=0.063) [McNamara & O'Connell 1993, AJ, 105, 417]. We find an upper limit to the degree of polarization of the light emitted from the lobes to be <7%. The accuracy of this measurement is limited by the presence of diluting background starlight. This limit is inconsistent with scattered light that originated in an obscured, anisotropically radiating nucleus, unless the radiation is beamed by <20deg to the line of sight, which is unlikely. The absence of a detailed correspondence between the radio lobes and optical lobes and the absence of a polarized signal is likewise inconsistent with synchrotron light. The blue optical lobes are probably regions of vigorous star formation. If a burst of star formation was triggered by the expanding radio lobes, the age of the burst population should be comparable to the radio age of ~ 10(7) yr. Then, the star formation rate in both lobes, assuming the Local IMF, is ~ 20 Msun yr(-1) and the stellar mass of the lobes is ~ 10(8) Msun. The material fueling the star formation and the radio source may have originated from the cooling flow or accretion from one or more gaseous cluster galaxies.

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