Why Can We Detect the High-Redshift Quasar BR 1202-0725 in CO?

Details Why Can We Detect the High-Redshift Quasar BR 1202-0725 in CO? Why Can We Detect the High-Redshift Quasar BR 1202-0725 in CO?

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997pasj...49..647i&link_type=abstract

Publications of the Astronomical Society of Japan, v.49, p.647-651.

Astronomy and Astrophysics

Astronomy

1

Cosmology: Observations, Galaxies: Evolution, Galaxies: Formation, Galaxies: Nuclei Of, Radio Lines: Co, Radio Sources: Agns

Scientific paper

We present CO luminosity evolutions of both elliptical and spiral galaxies based on a galactic-wind model and a bulge-disk model, respectively. We have found that the CO luminosity peaks at around the epoch of the galactic wind caused by collective supernovae ~ 0.85 Gyr after the birth of the elliptical with M = 2 * 10(12) MO , while ~ 0.36 Gyr after the birth of the bulge with M = 2 * 10(11) MO . After these epochs, the CO luminosity decreased abruptly because the majority of the molecular gas was expelled from the galaxy system as wind. Taking account of typical masses of elliptical galaxies and the bulges of spiral galaxies, we suggest that CO emission can be hardly detected from galaxies with a redshift of z ~ 1--4 unless some amplification either by galaxy mergers and/or by gravitational lensing is working. Therefore, our study explains reasonably well why CO emission was detected from the high-redshift quasar BR 1202-0725 at z =4.7, while it was not detected from powerful radio galaxies with 1 < z < 4.

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