Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.naic.edu/~astro/aotms/backends/96-01.pdf Дата изменения: Mon Apr 26 02:34:08 1999 Дата индексирования: Sat Dec 22 05:19:36 2007 Кодировка: Поисковые слова: arp 220

Arecibo Upgrade Notes

INSTRUMENTAL POLARIZATION: POLARIZATION ISOLATION & ERRORS IN STOKES PARAMETERS
Jim Cordes & Joe Lazio 22 May 1996

Summary
The purpose of this memo is to: 1 demonstrate how polarization isolation is related to errors in Stokes parameters; 2 estimate a tolerable level of errors in Stokes parameters due to amplitude and phase mismatch in and before the hybrid; 3 emphasize that Stokes parameters will have to be corrected after the fact no matter how good the hardware. 4 estimate that isolation of 25 dB is needed, corresponding to phase errors 5 and power ratio 0:8 dB; it probably is not worth making heroic e orts to obtain increased isolation, because software correction can better address the totality of systematic errors that contaminate raw polarization data.

Stokes Parameter Matrix
In our 1992 Memo Instrumental Polarization: Cross Coupling and Hybrid Conversion Issues we showed that the measured primes and true Stokes parameters are related in the following way:

0 B B B @
where

I Q U V

0 0 0 0

1 C C C A

0 G G 2 B 2G G B =B 0 0 @
0 0
G

0 0 cos sin

0 0 , sin + cos

1 C C C A

0 B B B @

I Q U V

1 C C C A

;

1

= 1 Gx + Gy 2 Gx;y = jgx;y j2 G = Gx , Gy


2 =GxGy 1=2 = x, y, ; gx;y are the complex gains of the x; y signals going into the hybrid, gain gx;y and is the phase error in the hybrid.

x;y

is the phase of the complex

Polarization Error
Consider pure RHCP of unit amplitude incident on Stokes parameters are using the V = LH C P , RH C P 0I1 0 1 1 0 I0 1 BQC B 0 C B Q0 C B C = B C; BC BU C B 0 C BU 0C @A@ A @A V ,1 V0 The polarization error, de ned as the error in the p Q2 +U 2 +V 2 1=2, where Q = Q0 , Q, etc. is Ipol = hG=22 + sin 2 De ning a gain ratio R =
I Gy =G
x

the telescope. The true and measured convention

and setting Gx 1 h1 + R2 , 8pR cos +4i1=2 = 2 For a pure phase error, the polarization error reduces to =2j sin

i1=2 +1 , cos 2 : = 1, the polarization error is
: =

olarized intensity Ipol = divided by the total intensity, I , 3 4 2j.

0G B G= = B , sin B @ , cos

1 2C C C A

:

2

Polarization Isolation
De ne the degree of isolation in terms of the pseudo LHCP that is measured in response to the incident RHCP: I0 I0 + V 0 i L = 5 I0 2I 0 : Substituting the gain ratio R Gy =Gx, the isolation becomes p 1+ R , 2 R cos : i= 6 21 + R For a 1 dB amplitude mismatch and no phase error, Eq. 6 gives i =0:0033 or ,24:8 dB of isolation. However, the errors in Stokes parameters are not so small: Eq. 4 indicates that the polarized ux p is in error by 22. Each Stokes parameter is in error by an amount = 3. Scienti cally useful results require precisions in Stokes parameters better than 1. It does not appear practial to strive for this precision in hardware because other e ects, such as cross coupling in the feed, require correction in software using a variety of calibration measurements using celestial sources.


3

Figures
Figure 1 shows the polarization error plotted against the gain ratio R for di erent values of phase error, . Note that as R gets larger, the polarization error becomces increasingly less sensitive to phase errors. Also, for realistically achievable gain and phase mismatches, the polarization error does not get better than -15 dB. Figure 2 shows contours of constanti against phase error and the amplitude ratio, R.

What Level of Instrumental Polarization is Tolerable?
way to achieve 1 errors is to correct Stokes parameters in software by inverting Eq. 1. More accurately, one needs to invert a similar matrix given in our 1992 memo that includes cross coupling in the horn + OMT as well as hyrbrid errors. A workable situation may be de ned in terms of our experience with the line feed antennas. There we had a level of cross coupling that gave about 10 errors in Stokes parameters. Through tracking of polarized sources across parallactic angle, the cross coupling parameters could be determined and the Stokes parameters corrected to about 1. With the more complicated situation involving the hybrid combined with cross coupling, the hardware should be designed to yield 10 errors in Stokes parameters. This corresponds to an amplitude ratio of 0.8 dB or less 0:8 R = Gy =Gx 1:2 or a phase error j j 0:1 rad = 5: 7, corresponding to an isolation i ,26 dB. If this can be achieved, then the remaining correction can be made in software. How bad can the instrumental polarization be and still allowinversion of the matrix relation? The bigger the o -diagonal terms in the 4 4 matrix, the more unstable the correction and the more accurately that the matrix elements need to be determined. For example, inversion of the 2 2 submatrix involving I; Q in Eq. 1 involves the determinant D = G2 , G=22 in the denominator of the matrix elements. The elements become unwieldy as G=2G ! 1.

,30:8 dB isolation or R of 0.5 dB still gives 6 errors in individual Stokes parameters. The only

Examples given above suggest that better than 25 dB of isolation is needed. However, even