interferometric gain calibration for alma
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Interferometric Gain Calibration for ALMA
Jim Gibson and Jack Welch
UC Berkeley RAL
Major Features
• Accuracy comes from (a) a well understood standard horn gain calculation: e<1% (Schelkunoff and Frijs), and (b) accurate two load ALMA Tsys calibration
• Use simple ambient temperature cal receiver• Use wideband natural source, flux need not be known• Decorrelation delay path with 1GHz band > 40cm• Use the system correlator as the power meter• Use the two load cal system for the gain transfer
antenna
Single Antenna
ki
Interferometer Pair
jiij kkk with
form the fraction
Gain Determination
Jovian Spectrumnear λ 1 cm
Tk R
10 1.42
15 2.00
20 2.38
25 2.63
30 2.83
35 2.99
40 3.09
45 3.18
50 3.25
CO Line Ratio vs. Kinetic Temperature
Derived Tk from different Brightness ratio accuracies
• A. 20% : R=2.5: range: 1.75 – 3.25• 13K ≤ Tk ≤ 51K
• B. 10% : R=2.5: range :2.15 – 2.85• 17K ≤ Tk ≤ 32K
• C. 5%: R=2.5: range: 2.3 – 2.7• 20K ≤ Tk ≤ 27K
Saturn as a transfer standard at 2.8 mm
• Assumptions:• ALMA rcvr Tsys = 50k• Cal rcvr Tsys = 1000k• Receiver bandwidth = 1 GHz• Cal antenna: 20x2.7x2.0 cm ~30db gain (exactly known)• Horn loss: 2% +/- .2%• Saturn flux ~ 220 Jy• Saturn diameter: ~16”• Geom mean Tsys = 220k• Geom mean effective area: (68 x 5.4 x10 -4)1/2 =0.2m2
• S/N = 150 in 1000 seconds with four antenna pairs
Proposed Calibration Receiver
LO1 ref
LO2 ref
IF
Mixer and IF amplifiers
Issues/Alternatives
• Mount cal receiver on an ACA antenna• Use an STI 65K cooler on cal receiver for
better Tsys. 5000$, 106 hours life.• Horn gain: Shelkunoff and Frijs: Advanced
Antenna Theory; Wrixon and Welch, IEEE Trans AP, AP20, 1972; Chiu and Semplak, BSTJ, 44,,527, 1965; Gibson et al, 2005, Icarus, 173, 439.
• Transfer of Tsys to cal horn
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