FUSE Calibration Target List The information listed below includes the Program Identification (PID), the target name, J2000 coordinates, cumulative exposure time planned for Cycle 4 (which may include multiple visits), V magnitude, and an indicator of the spectral type. The PID permits cross-referencing of target to its primary calibration program, as indicated below. Cumulative Exposure Target PID Target Name RA(J2000) DEC(J2000) Time (s) V Type ---- ---------------- ----------- ----------- -------- ----- ------ M107 WD0005+5106 00 08 18.10 +51 23 17.0 10000 13.32 DO1 M105 JL_163 00 10 33.20 -50 15 24.70 5000 12.89 sdB M105 CD-48_106 00 31 41.65 -47 25 20.10 5000 12.45 sdB M101 GD659 00 53 17.20 -32 59 58.0 16000 13.37 DA1 M102 BPM70524 01 03 25.00 -06 32 12.0 13000 13.30 DB M105 LB_3241 02 13 11.90 -49 44 53.90 5000 12.72 sdOB M105 REJ0230-47 02 30 53.3 -47 55 25 5000 14.53 DA M105 CPD-71_172 02 53 30.70 -71 22 31.80 5000 12.05 sdOB M102 BPM17088 03 08 30.00 -56 34 0.0 13000 14.07 DB M107 LSV46-21 04 43 21.00 +46 42 4.0 10000 12.90 DAO M103 RE0503-289 05 03 55.90 -28 54 36.0 13000 13.90 DO1 M101 G191-B2B 05 05 30.60 +52 49 54.0 4000 11.78 DA1 M105 CD-61_1208 05 52 08.10 -61 07 13.80 5000 11.19 sdB M101 GD71 05 52 27.40 +15 53 23.0 25000 13.03 DA1 M105 WD0715-704 07 15 17.10 -70 25 08.01 5000 14.00 DA M104 BD+75D325 08 10 49.30 +74 57 57.5 2300 9.55 sdO M103 AGK+81D266 09 21 19.30 +81 43 30.5 2000 11.85 sdO M105 LSS1362 09 52 44.36 -46 16 48.30 5000 12.50 CSPN M103 FEIGE-34 10 39 36.70 +43 06 10.1 2000 11.12 sdO M105 HD100276 11 31 48.15 -60 36 22.50 5000 7.22 B0.5Ib M105 WD1202+608 12 04 38.71 +60 32 07.00 5000 13.61 DA M103 HZ21 12 13 56.50 +32 56 28.3 15000 14.22 DO1 M105 WD1234+481 12 36 45.30 +47 55 22.99 10000 14.40 DA M103 FEIGE-66 12 37 23.60 +25 04 0.3 2000 10.51 sdO M103 FEIGE-67 12 41 51.80 +17 31 20.5 2000 11.81 sdO M101 GD153 12 57 2.40 +22 01 56.0 12000 13.35 DA1 M101 HZ43 13 16 22.00 +29 05 57.0 6000 12.91 DA1 M104 HZ44 13 23 35.40 +36 08 0.0 20880 11.71 sdO M105 Feige_87 13 40 14.70 +60 52 47.61 5000 11.71 sdB M105 LSE44 13 52 40.80 -48 08 23.39 5000 12.46 sdO M105 WD1501+664 15 02 09.62 +66 12 18.61 10000 15.90 DOZ M105 HD134411 15 11 08.89 -39 51 50.60 5000 9.56 B2Vn M105 WD1529+486 15 29 43.50 +48 36 21.99 10000 14.70 DA M102 GD190 15 44 19.00 +18 16 18.0 20000 14.72 DB M105 WD1631+781 16 29 10.71 +78 04 39.11 5000 13.10 DA M103 HD149499B 16 38 30.50 -57 28 11.0 15000 11.70 DO1 M105 RE_J1738+669 17 38 02.47 +66 53 47.81 10000 16.4 DA M105 WD1800+685 18 00 09.50 +68 35 54.01 10000 14.70 DA M105 HD177566 19 07 07.73 -41 43 10.00 5000 10.20 PAGB M107 GCRV12336 19 59 36.37 +22 43 16.10 15000 13.94 CSPN M105 WD2004-605 20 09 05.46 -60 25 41.00 5000 13.60 DA M105 WD2013+400 20 13 09.20 +40 02 24.00 10000 14.40 DA M104 BD+28D4211 21 51 11.10 +28 51 51.8 2400 10.51 sdO M105 WD2111+498 21 12 44.09 +50 06 18.00 5000 13.09 DA M105 BD+28D4211 21 51 11.10 +28 51 51.80 5000 10.53 sdO M105 WD2156-546 21 56 21.10 -54 38 23.00 10000 14.40 DA M103 WD2211-495 22 14 12.30 -49 19 2.0 15000 11.50 DA1 M105 WD2247+583 22 49 52.27 +58 34 32.85 10000 14.26 DA M105 WD2331-475 23 34 02.33 -47 14 27.60 5000 13.19 DA M101 GD246 23 12 21.40 +10 47 5.0 5000 13.08 DA1 M103 FEIGE-110 23 19 58.40 -05 09 55.8 2000 11.50 sdO ------------------------------------------------------------------------ Notes: 1. With the exception of targets most often used in program M103 (G191-B2B, HD149499B, WD2211-495), not all stars shown may be observed. 2. In the other programs a large number of stars are included for purposes of scheduling convenience. Some of the stars are likely to be observed repeatedly (especially stars in M105 program). 3. M105 stars are used to monitor possible sensitivity degradation as we start pointing closer to the RAM direction and will be observed as needed. 4. Stars identified with a given program may be used for other programs, but are listed only once in the target list. 5. Many of the objects shown will also be used for additional calibration programs, such as measurements of mirror and grating scattering, focusing, FES photometric calibration, etc. 6. The estimate of cumulative exposure time is provided only as an indication of the amount of exposure time that may be obtained for calibration purposes. The actual exposure times may revised upward or downward to accommodate requirements of the instrument calibration program. The calibration program IDs are the following: M101: Photometric calibration, defined by DA white dwarfs. M102: Photometric calibration, objects without Lyman lines (DB white dwarfs). M103: Photometric calibration, monitoring by DO white dwarfs, G191, sdO stars. M104: Flat field, done by FP-splits of DO white dwarfs, sdO stars, etc. M105: Photometric calibration, expanded pool of targets for monitoring of sensitivity degradation. M107: Wavelength calibration, absorption-line objects.