Figaro includes a large number of standard files supplied by Roderick Johnstone, IoA Cambridge. This section reproduces the document he supplied with those files and which dates from December 1987. The files are kept in the standard Figaro directory FIGARO_PROG_S (see Section 3.4), which on a normal Starlink system corresponds to directory:
The files were prepared on a VAX/VMS system, where file names were in upper-case only. Consequently they are listed in upper-case in the note, but following the normal convention the corresponding Unix file names are lower-case. SPICA was a spectroscopic data reduction system, now long-defunct, which was in some ways a precursor of Figaro.
The files listed contain stellar fluxes in milli-Jansky. AB magnitude files have the same name, but with an A before the ‘.’ as in standard Figaro style. I have tried to conform to the systematic naming used by Figaro so files are called after the star with positive and negative signs replaced by P and M respectively. Note that some files have been included more than once under aliases of the star name.
Numerical values of wavelength, flux, bandwidth and order changeover wavelengths have been checked and are believed to be correct. Some errors in the SPICA tables were found. Where existing Figaro files are correct these have not been duplicated.
Note that there are several different magnitude systems which determine the fluxes presented in these tables. These are defined through different calibrations of the primary standard Vega and use different ways of transferring the magnitude system from Vega to the fainter secondary standards. In general the stars listed here are not actual standards but are just good calibrations of non-variable stars. The user is strongly advised to read the paper from which the numbers come (listed at the top of each file) to gain an idea of both the random and the systematic errors in the fluxes as well as the magnitude system from which the fluxes derived.
I am most grateful to Doreen Oliver at RGO who I believe typed in most of the original SPICA files and to Carolin Crawford who gave invaluable help checking the numbers.
In 1991 Jeremy Walsh provided two new sets of spectrophotometric flux tables for use with Figaro. One comprised a set of stars observed by Oke, the other a set of HST standard stars. Copies of these data can be retrieved by anonymous ftp. The details are as follows.
| ftp site: | ftp.roe.ac.uk |
| directory: | /pub/acd/fluxstandards |
| files: | 0README.LIS |
hst.tar.Z |
|
oke.tar.Z |
|
The data files are compressed tar archives. Remember to use ftp in binary mode when retrieving them. Once you have retrieved copies of the files they can be decompressed using Unix command uncompress, for example:
Then extract the individual files from the tar archive:
Brief details of the two datasets follow. For details of the processing of these files please refer to Jeremy Walsh at the ST-ECF.
These standards comprise 25 stars observed by Oke6 in the wavelength range 3200 to 9200 Å. Table 2 gives summary details for these stars.
| Star | Name | R.A. | Dec. | Sp. | V | AB | HST |
| No. | (2000) | (2000) | Type | (5460 Å) | |||
| 1 | G158-100 | 00 33 54.3 | -12 07 57 | sdG | 14.89 | 14.82 | |
| 2 | HZ 4 | 03 55 21.7 | +09 47 19 | DA4 | 14.52 | 10.47 | |
| 3 | G191B2B | 05 05 30.6 | +52 49 54 | DAO | 11.78 | 11.72 | |
| 4 | G193-74 | 07 53 27.4 | +52 29 36 | DC | 15.70 | 15.58 | |
| 5 | BD+75 325 | 08 10 49.3 | +74 57 57 | O5p | 9.54 | 9.52 | |
| 6 | Feige 34 | 10 39 36.7 | +43 06 10 | DO | 11.18 | 11.13 | |
| 7 | HD 93521 | 10 48 23.5 | +37 34 13 | O9Vp | 7.04 | 6.96 | |
| 8 | HZ 21 | 12 13 56.4 | +32 56 31 | DO2 | 14.68 | 14.67 | |
| 9 | Feige 66 | 12 37 23.6 | +25 04 00 | sdO | 10.50 | 10.43 | |
| 10 | Feige 67 | 12 41 51.8 | +17 31 20 | sdO | 11.81 | 11.78 | |
| 11 | G60-54 | 13 00 09.5 | +03 28 56 | DC | 15.81 | 15.73 | |
| 12 | HZ 44 | 13 23 35.4 | +36 08 00 | sdO | 11.66 | 11.65 | |
| 13 | GRW+70 5824 | 13 38 51.8 | +70 17 08 | DA3 | 12.77 | 12.72 | |
| 14 | BD+33 2642 | 15 51 59.9 | +32 56 55 | B2IV | 10.81 | 10.74 | |
| 15 | G138-31 | 16 27 53.6 | +09 12 24 | DA7 | 16.14 | 16.07 | |
| 16 | G24-9 | 20 13 56.0 | +06 42 55 | DC | 15.72 | 15.77 | |
| 17 | BD+28 4211 | 21 51 11.1 | +28 51 52 | Op | 10.51 | 10.47 | |
| 18 | BD+25 4655 | 21 59 39.3 | +26 25 42 | 9.65 | |||
| 19 | LTT 9491 | 23 19 35.0 | -71 05 30 | DC | 14.04 | 14.06 | |
| 20 | Feige 110 | 23 19 58.4 | -05 09 56 | DOp | 11.82 | 11.81 | |
| 21 | GD 248 | 23 26 06.7 | +16 00 21 | DC | 15.09 | 15.08 | |
| 22 | GD 50 | 03 48 50.1 | -00 58 30 | DA2 | 14.06 | 14.06 | |
| 23 | SA95-42 | 03 53 43.7 | -00 04 33 | 15.61 | 15.60 | ||
| 24 | GD 108 | 10 00 47.3 | -07 33 31 | sdB? | 13.56 | 13.57 | |
| 25 | NGC 7293 | 22 29 38.5 | -20 50 13 | 13.51 | 13.48 | ||
These standards comprise 27 stars selected to be standards for the HST. The basic reference is Turnshek et al,7 but see also Bohlin8 The observations cover the approximate wavelength range 800 to 12,000 Å. Table 3 gives summary details for these stars.
| Star | R.A. | Dec. | V | Sp. | Oke |
| Name | (2000) | (2000) | Type | ||
| AG+81 266 | 09 21 19.1801 | +81 43 27.642 | 12.10 | B2 | |
| Alpha Lyr | 18 36 56.3364 | +38 47 01.291 | 0.03 | A0V | |
| BD+28 4211 | 21 51 11.0222 | +28 51 50.364 | 10.54 | Op | |
| BD+33 2642 | 15 51 59.8855 | +32 56 54.324 | 10.81 | B2IVp | |
| BD+75 325 | 08 10 49.4903 | +74 57 57.929 | 9.50 | O5pvar | |
| BPM 16274 | 00 50.1 | -52 09 | 14.16 | DA... | |
| Eta UMA | 13 47 32.4377 | +49 18 47.754 | 1.852 | B3V | |
| Feige 110 | 23 19 58.3977 | -05 09 56.207 | 11.4 | DA: | |
| Feige 34 | 10 39 36.7400 | +43 06 09.252 | 11.0 | DA: | |
| G 191-B2B | 05 05 30.6119 | +52 49 51.945 | 11.79 | DAw... | |
| G 93-48 | 21 52 25.3835 | +02 23 19.556 | 12.73 | DA | |
| Gamma UMa | 11 53 49.8475 | +53 41 41.136 | 2.427 | A0V | |
| GD 108 | 10 00 47 | -07 33.5 | 13.56 | B | |
| GD 50 | 03 48 50.10 | -00 58 28.5 | 13.98 | DAw... | |
| GRW+70 5824 | 13 38 50.4743 | +70 17 07.619 | 12.80 | DA: | |
| HD 49798 | 06 48 04.6995 | -44 18 58.431 | 8.27 | sdO6p | |
| HD 60753 | 07 33 27.3188 | -50 35 03.319 | 6.682 | B2III | |
| HD 93521 | 10 48 23.5112 | +37 34 13.090 | 7.06 | O9Vp | |
| HZ 21 | 12 13 56.27 | +32 56 31.4 | 14.22 | DA: | |
| HZ 2 | 04 12 43.49 | +11 51 50.6 | 13.86 | DA: | |
| HZ 44 | 13 23 35.258 | +36 07 59.51 | 11.3 | B2 | |
| HZ 4 | 03 55 21.77 | +09 47 18.4 | 14.47 | DA: | |
| LB 227 | 04 09 28.50 | +17 07 55.2 | 15.35 | DA | |
| LDS 749B | 21 32 16.1 | +00 15 15 | 14.58 | DB | |
| Mu Col | 05 45 59.8950 | -32 18 23.166 | 5.148 | O9.5V | |
| NGC 7293 | 22 29 48.4 | -20 49 26 | 13.54 | ||
| Zeta Cas | 00 36 58.2846 | +53 53 48.874 | 3.666 | B2IV | |
6J.B. Oke, 1990, Astron. J, 99, pp1621-1631.
7D.A. Turnshek, R.C. Bohlin, R.L. Williamson II, O.L. Lupie, J. Koornneef and D.H. Morgan, 1990, Astron. J, 99, pp1243-1261, 1344-1377.
8R.C. Bohlin, September 1992, STScI Newsletter, 9, No. 2.