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CO (J=3-2) Emission in the Radio Galaxy 53W002 at z=2.394 | | N.Z. Scoville
; M.S. Yun
; R.A. Windhorst W.C. Keel
; L. Armus
; | | Date: |
29 Jun 1997 | | Journal: | ApJ,485,L21 | | Subject: | astro-ph | | Affiliation: | Caltech), M.S. Yun (NRAO), R.A. Windhorst (Arizona State University) W.C. Keel (University of Alabama) and L. Armus (Caltech | | Abstract: | We report a sensitive search for redshifted CO (3-2) emission from the weak radio galaxy 53W002 at z=2.394. Maps at resolutions of 3 arcsec and 235km/s show a significant emission peak within 0.5 arcsec of the optical and radio continuum peaks. The measured narrow band flux is approximately ten times the extrapolated cm-wavelength non-thermal radio continuum expected at 101.9 GHz and exhibits a spectral profile implying a 540 km/s width (FWHM) at a systemic redshift z=2.394 for CO (3-2). This emission has a total integrated flux of 1.51(+/-0.2) Jy km/s, approximately four times weaker than that previously seen in the lensed systems FSC10214+4724 and the Cloverleaf QSO. For a Galactic CO-to-H2 conversion ratio, the implied molecular gas mass is 7.4x10^10 solar masses (H=75 km/s/Mpc and q=0.5). The CO emission is elongated at P.A.=120 degrees with a deconvolved major axis radius of 15 kpc (2.8 arcsec). This extension is along a similar direction to that seen in the cm-wave radio continuum and the optical but approximately three times larger. A velocity gradient is seen along the major axis, and if this structure is a (forming) disk, the implied dynamical mass is 9-22x10^10 solar masses at radii less than or equal to 15 kpc, assuming inclination i=0 degrees (edge-on). The magnitude of these masses and the similarity of the high gas-mass fraction are consistent with the host galaxy of 53W002 being a young galactic system, but the metallicity (probably greater than or equal to 0.1 solar in order to produce the CO lines) implies significant heavy element production prior to z=2.4. This constitutes the first high redshift molecular gas which is detected in emission where there is probably no gravitational magnification. | | Source: | arXiv, astro-ph/9706291 | | Services: | Forum | Review | PDF | Favorites | |
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