abell 2218/smm1 co(3-2)
DESCRIPTION
ABELL 2218/SMM1 CO(3-2). J.-P.Kneib et al. A&A 2004, submitted. ASTRO> uv_tracks w05 w00 e03 n05 n09 n13 /frame /hour -4 4 /table d.uvt new. Correlator Modes http://www.iram.fr/IRAMFR/TA/backend/cor6A/index.html. Looking forward to seeing proposals from YOU!. - PowerPoint PPT PresentationTRANSCRIPT
ABELL 2218/SMM1 CO(3-2)J.-P.Kneib et al. A&A 2004, submitted
computer neri
left: triple lensed image of a single source SMM1, with B the strongest of the three images; right: the spectra of redshifted CO at the three positions. The magnification is 22 for B - this translates to a peak CO flux less than 0.2 mJy, and 0.9 mJy for the dust. So it's the deepest (i.e. faintest) submillimeter detection up to now. The double-peak profile is typical for many of the massive galaxies detected at z>2 and very likely witnesses the presence of a merger system with separated by less than 3 kpc. Sheth et al. have obtained the same result with OVRO, though with much less SNR (less than half). They have invested 53 hours on-source, we have 16 hours with Bure. Note: the Sheth group except Sheth himself, were also on the Plateau de Bure proposal asking for the same target. OVRO is closed now, but we have to watch about CARMA at the horizon. In a few years from now, when the two instruments will have similar collecting area, many proposals will be submitted in parallel to both observatories.
ASTRO> uv_tracks w05 w00 e03 n05 n09 n13 /frame /hour -4 4 /table d.uvt new
Correlator Modeshttp://www.iram.fr/IRAMFR/TA/backend/cor6A/index.html
Bandwidth Subband Clock Multiplex
Factor
Lags no. Channels Spacing
320 MHz DSB 80 MHz 4 2 x 128 2 x 64 2.5 MHz
160 MHz SSB 80 MHz 4 1 x 256 1 x 128 1.25 MHz
160 MHz DSB 80 MHz 2 2 x 256 2 x 128 0.625 MHz
80 MHz SSB 80 MHz 2 1 x 512 1 x 256 0.312 MHz
80 MHz DSB 80 MHz 1 2 x 512 2 x 256 0.156 MHz
40 MHz SSB 80 MHz 1 1 x 1024 1 x 512 0.078 MHz
20 MHz SSB 40 MHz 1 1 x 1024 1 x 512 0.039 MHz
Looking forward to seeing proposals from YOU!