Table 1: List of observational parameters for KOSMA.
Species Transition Frequency Receiver $\eta_{\rm mb}^{{\rm {\it a}}}$ HPBW $^{{\rm {\it a}}}$ Mode No. $^{{\rm {\it f}}}$ $\Delta v$ $^{{\rm {\it f}}}$ $\langle\tau^{\rm atm}_0\rangle$ $^{{\rm {\it f}}}$ Observing period
    [GHz]     ['']     [m s-1]    
13CO $^{{\rm {\it b}}}$ J=3-2 330.5880 DualSIS 0.68 80 OTF $^{{\rm {\it c}}}$ 693 308 0.26 01/2006
12C32S J=7-6 342.8829   0.68 80 OTF $^{{\rm {\it c}}}$ 525 294 0.08 12/2005
12CO J=3-2 345.7960   0.68 80 OTF $^{{\rm {\it c}}}$ 525 294 0.08 12/2005
12CO J=4-3 461.0408 SMART 0.5 57 OTF $^{{\rm {\it c}}}$ 3458 677 0.85-1.4 1/2005
[12C I] 3P1-3P0 492.1607   0.5 55 DBS $^{{\rm {\it d}}}$ 1380 630 0.5-1.6 1/2003-3/2004
13CO J=6-5 661.067   0.4 $\sim$40 PSw $^{{\rm {\it e}}}$ 33 307 1.0-1.3 1/1998
12CO J=6-5 691.473   0.4 $\sim$40 PSw $^{{\rm {\it e}}}$ 58 295 1.0-1.3 1/1998
12CO J=7-6 806.6518   0.31 42 DBS $^{{\rm {\it d}}}$ 964 775 0.4-1.6 1/2003-3/2004
[12C I] 3P2-3P1 809.3420   0.31 42 DBS $^{{\rm {\it d}}}$ 964 775 0.4-1.6 1/2003-3/2004
$^{{\rm {\it a}}}$ The main beam efficiency $\eta_{\rm mb}$ and the half power beam width (HPBW) were determined from cross scans of Jupiter. $^{{\rm {\it b}}}$ See Schneider et al. (2006) for a 13CO 3-2 map covering a larger part of Cygnus X. $^{{\rm {\it c}}}$ OTF - on-the-fly mapping mode with periodic switching to an emission-free reference position at $\alpha({\rm J2000})=20^{\rm h}37^{\rm m}10^{\rm s}$, $\delta({\rm J2000})=42^\circ30'00''$. $^{{\rm {\it d}}}$ DBS - dual beam switch observing mode with a chopping secondary mirror in azimuth. $^{{\rm {\it e}}}$The CO and 13CO 6-5 observations were carried out on a 35''grid (Köster 1998) in a position-switched observing mode (PSw). The OFF position was at $\alpha(J2000)=20^{\rm h}26^{\rm m}43~\hbox{$.\!\!^{\rm s}$ }56$, $\delta(J2000)=42^\circ09'39\hbox{$.\!\!^{\prime\prime}$ }5$. $^{{\rm {\it f}}}$These columns lists the number of mapped positions, the velocity channel width $\Delta v$ (the resolution is a factor of ${\sim}1.4$ larger), and the mean atmospheric zenith opacity $\langle\tau^{\rm atm}_0\rangle$.

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