Structure and age of the radiogalaxy 3C 435A (z = 0.471) with the integral field spectrograph TIGER

Details Structure and age of the radiogalaxy 3C 435A (z = 0.471) with the integral field spectrograph TIGER Structure and age of the radiogalaxy 3C 435A (z = 0.471) with the integral field spectrograph TIGER

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...292...20r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 292, no. 1, p. 20-26

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14

Astronomical Maps, Computational Astrophysics, Elliptical Galaxies, Radio Astronomy, Radio Galaxies, Radio Jets (Astronomy), Relativistic Particles, Star Formation, Stellar Physics, Accretion Disks, Red Shift, Spectrophotometers, Spectroscopy, Stellar Magnitude, Stellar Mass, Stellar Models

Scientific paper

Bidimensional spectroscopy of the distant (z = 0.471) radio-galaxy 3C 435A has been performed with the integral field spectrograph TIGER at the Canada-France-Hawaii Telescope (CFHT). The (O II) 3727 A and (O III) 4959, 5007 A maps are remarkably superimposed with the 1.4 GHz radio lobe isophotes, showing the narrow relationship between the radio plasma and the ionized component, while the 4.8 GHz radio emission traces a shock region. The (O II)/(O III) ratio map follows the external part of the radio lobe rather than the central jet, and is strongly distorted by multiple components. This high number density is confirmed by the velocity field. The maximum ratio value (approximately equal to 8) indicates a low level of ionization. For the first time, stellar and nebular components are separated at a large redshift, indicating that the alignment effect is mainly due to nebular (O II) and (O III) emission. With the help of our spectrophotometric model, the stellar continuum of the central component A is well fitted with an old (more than 15 Gyrs at z = 0) elliptical galaxy model, while nebular lines witness a faint star formation process. Two companions B and D, located near the radio-axis, fit evolved (greater than or equal to 10 Gyrs) models, ruling out a current star formation activity induced by the radio-jet. Another companion, C, located in a direction roughly perpendicular to the radio-axis, has a blue color of irregular type, a few Gyr age, detectable emission lines and high velocity. Component E, roughly aligned with A and C, is essentially emitting in the (O II) line.

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