Spectropolarimetry

Table of observations of spectropolarimetry. For a complete observation a set of 8 spectra at different polarisation states and position angles are required. This criteria was not met for several of the epochs below - see notes to Table.

Reduced data are produced by the TSP package of Bailey (jab@aaoepp.aao.gov.au). Converted FITS format files are available but hold less information than the original format.

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Age (d) Date Instrumental Setup Res. (A) Wavelength Range (A) Pol.
4 87:02:27 RGO 25cm+PC+IPCS 2.0 3402 - 5299 lin1
12 87:03:07 RGO 82cm+PC+GEC16 2.0 5986 - 6820 lin
71 87:05:05 RGO 25cm+PC+GEC16 2.9 6024 - 6846 lin
100 87:06:03 RGO 25cm+PC+GEC16 3.5 5440 - 6840 lin
  100 87:06:03   RGO 25cm+PC+GEC16   3.5  8220 - 9055 lin
125 87:06:28 RGO 25cm+PC+GEC16 2.9 6014 - 6834 lin, circ
130-2 87:07:03-05 RGO 25cm+PC+RCA 4.4 3616 - 6172 lin
135 87:07:08 RGO 82cm+PC+GEC16 2.0 6196 - 6600 lin, circ
135  87:07:08  RGO 82cm+PC+GEC16  2.0 8300 - 8800 lin, circ
147 87:07:20 RGO 82cm+PC+GEC16 3.3 6250 - 6750 lin2
168 87:08:10 RGO 82cm+PC+GEC16 4.0 5660 - 6762 lin
168  87:08:10  RGO 82cm+PC+GEC16 4.0  8328 - 8878 lin
190 87:09:01 RGO 25cm+PC+GEC17 6.0 4045 - 8989 lin
191 87:09:02 RGO 25cm+PC+GEC17 3.2 6031 - 6850 lin, circ
 191 87:09:02  RGO 25cm+PC+GEC17  3.2  8074 - 8899 lin
226 87:10:07 RGO 25cm+PC+GEC17 6.0 4565 - 9551 lin
252 87:11:02 RGO 82cm+PC+GEC17 2.5 5520 - 8880 lin2
281 87:12:01 RGO 25cm+PC+GEC17     Poor3
290 87:12:10 FORS+PC 20 5500 - 9600 lin2
315 88:01:04 RGO 82cm+PC+GEC17 2.4 6230 - 6508 lin
315   88:01:04    RGO 82cm+PC+GEC17   2.4  7030 - 7590 lin
 315  88:01:04   RGO 82cm+PC+GEC17     2.4 8345 - 8905 lin
350 88:02:08 RGO 25cm+PC+GEC17 5.3 4210 - 8990 lin
522-4 88:07:29-31 RGO 82cm+PC+GEC17 3.4 6210 - 6780 lin
 522-4 88:07:29-31  RGO 82cm+PC+GEC17  3.4   7000 - 7572 lin
522-4  88:07:29-31  RGO 82cm+PC+GEC17   3.4 8313 - 8884 lin
641-4 88:11:25-28 RGO 25cm+PC+GEC17 6.0 5600 - 8920 lin
1265 90:08:11 FORS+PC     Poor3

Notes

1. Too noisy for spectropolarimetry but summed polarisations form useful spectrum.                      2. Poor signal to noise ratio.                                                                                                                  3. Incomplete set due to poor weather.                                                                                                 4. All observations with CCDs have interference fringing. This fringing is cancelled out for spectropolarimetry measurements but needs to be removed if summed polarisations are to be used as normal spectra.

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Ray Stathakis (ras@aaoepp.aao.gov.au), last update 5 February 1998