FM Walter 1/31/08 rev 2/17 SMARTS 1.5m Service Observing Program 080217 --- EPHEMERIS INFORMATION --- For the night of: Sun, 2008 Feb 17 ---> Mon, 2008 Feb 18 Local midnight = 2008 Feb 18, 3 hr UT, or JD 2454514.625 Local Mean Sidereal time at midnight = 8 06 35.7 Sunset ( 2215 m horizon): 20 37 CDT; Sunrise: 7 18 CDT Evening twilight: 21 54 CDT; LMST at evening twilight: 6 00 Morning twilight: 6 01 CDT; LMST at morning twilight: 14 08 Moonrise: 18 10 CDT Moonset : 4 43 CDT Moon at civil midnight: illuminated fraction 0.892 4.0 days since first quarter, RA and dec: 7 31 48, 25 45.5 The sun is down for 10.7 hr; 8.1 hr from eve->morn 18 deg twilight. .......................................................................... Civil date Setup Program(s) Feb 17 9/Ic NOAO 08a-207 ** SUNY 08a-01 SUNY 08a-02 SUNY 08a-10 SUNY 08a-11 ** Please read the investigator's detailed instructions, which follow at end .............................................................................. Name Slit Filter Coll Grating Tilt & Comp,exp Ystart Ysize Yspec Blaze w.l. cov. (sec) Res (A) 9/Ic 110.5 clear 560 9 13.09 He-Ar 30 214 280 4000 3330-6800 8.6 .............................................................................. In afternoon or during dinner: - Install 9/Ic grating setup - check focus if necessary - obtain at least 25 Zero frames - obtain at least 10, preferably 25, flat-field frames (projector or dome) Get well-exposed TWILIGHT SPECTRA at zenith at beginning of night. Aim for three spectra, each with between 5,000 and 30,000 counts per pixel. Remember to take a comp spectrum too. Program Pri Target RA (J2000) Dec mag Exp Cmp T CDT Rem NOAO 8a-207 1 REF1 3 20 12.9 -85 34 56 9.9 1x 60 1 8 21 15 NOAO 8a-207 1 REF2 3 18 52.0 -85 35 21 12.2 2x 420 0 21 21 23 NOAO 8a-207 1 REF3 3 18 03.1 -85 36 02 14.6 2x 960 0 39 21 44 NOAO 8a-207 1 REF6 3 13 59.7 -85 30 16 14.0 2x 720 1 32 22 23 NOAO 8a-207 2 REF7 3 15 55.6 -85 30 20 15.0 2x1080 1 43 22 55 W NOAO 8a-207 1 REF8 3 16 46.3 -85 29 48 14.3 2x 720 0 31 23 38 W NOAO 8a-207 1 REF9 3 18 55.1 -85 36 42 14.3 2x 720 1 32 0 9 W cal 1 LTT 3218 8 41 33.6 -32 56 55 11.8 3x 200 1 19 0 41 cal 2 LTT 4364 11 45 37.7 -64 50 25.1 11.5 3x 200 1 19 1 0 SUNY 08a-11 2 N LMC 2005 5 10 32.2 -69 12 35 11.5 3x1200 1 69 1 19 N,W SUNY 08a-10 2 TW Hya 11 01 51.9 -34 42 17.0 11 3x 100 1 14 2 28 SUNY 08a-11 2 DE Cir 15 17 52.5 -61 57 16.4 16 3x1200 1 69 2 42 N cal 1 LTT 4364 11 45 37.7 -64 50 25.1 11.5 3x 200 1 19 3 51 cal 1 LTT 3218 8 41 33.6 -32 56 55 11.8 3x 200 1 19 4 10 SUNY 08a-02 1 EX Lup 16 03 05.48 -40 18 25.9 11.4 3x 100 1 14 4 29 SUNY 08a-10 2 RU Lup 15 56 42.3 -37 49 15.5 11 3x 100 1 14 4 43 cal 1 LTT 3218 8 41 33.6 -32 56 55 11.8 3x 200 1 19 4 57 W SUNY 08a-11 1 V1280 Sco 16 57 40.91 -32 20 36.4 13 3x 500 1 34 5 16 N cal 1 LTT 4364 11 45 37.7 -64 50 25.1 11.5 3x 200 1 19 5 50 SUNY 08a-11 1 V5558 Sgr 18 10 18.27 -18 46 52.1 8 3x 500 1 34 6 9 N end 32/I 6 43 ---------------------------------------------------------------------------- If there is any time left before dawn, or you get ahead and have to wait for targets to rise, or if some targets are too faint to acquire, please select from among the following 32/I targets: standard 3 HD103932 11 57 56.2 -27 42 25 7.0 3x 4 1 9 standard 3 HD108903 12 31 9.8 -57 6 34.4 1.6 3x 1 1 9 standard 3 HD120052 13 47 25.2 -17 51 34.1 5.4 3x 3 1 9 standard 3 HD120323 13 49 26.9 -34 26 59.9 4.2 3x 2 1 9 standard 3 HD122250 14 5 21.2 -76 47 46.7 5.5 3x 2 1 9 standard 3 HD120447 13 49 28.9 +15 47 50.3 4.1 3x 2 1 9 standard 3 HD146051 16 14 20.9 -03 41 32.4 2.7 3x 1 1 9 standard 3 HD149161 16 32 36.3 +11 29 16.9 4.8 3x 2 1 9 Just before sunrise, get well-exposed TWILIGHT SPECTRA at zenith IF you could not obtain them at dusk. Aim for 3-5 spectra, each with between 5,000 and 30,000 counts per pixel. Remember to take a comp spectrum too. -------------------------------------------------------------------- Remarks: M: moon within 10 degrees. Skip if not visible in the acquisition TV B: very bright target. Best observed through clouds. C: cataclysmic variable. May be fainter than in finding chart. Skip if not visible. E: target far to the east. If running ahead, give extra time to the previous target, or observe a backup target if time permits. FC: target has proper motion. Check finding chart under SUNY 07a-04 program. N: Nova. Will be fainter than on finding chart. NN: new nova. No finding chart available. Should be the brightest star near the coordinates (positional uncertainty +/- 2 arcsec). R: radial velocity standard. ST: if you cannot observe the standard, please try to observe another cal star (in the backup list) at some other time during the night. S4: set slit width to 4.0 arcsec. Center on the nucleus of the galaxy. S5: set slit width to 5.0 arcsec. Center on the nucleus of the galaxy. S2: set slit width to 2.0 arcsec. Center on the nucleus of the galaxy. Reset the slit to the normal width for the wavecal. S10: set slit width to 10.0 arcsec. Please reset at the end of the observation. No wavecal is necessary with this exposure. PM: may have significant proper motion. W: star very close to 2 air masses at end of observation. Don't start late; do the calibration lamp at the end if it helps. Y: 5 arcsec SE of brighter star. Try to keep the brighter star out of the slit. Skip if the seeing is really bad. Z: monitoring target. Try to maintain spacing between observations. -------------------------------------------------------------------- General Notes: Astronomical ephemerides are from SKYCAL,by John Thorstensen Pri: Target priority. + = absolute highest priority 1 = observe object if possible 2 = extra targets; observe only if no Priority 1 target is available 3 = backup/filler targets; low priority Cmp: 1 means take comparison spectrum only before target exposures; 2 means before and after; 3 means before, after, and between each exposure. 0 means NO wavecal should be taken. .............................................................................. Notes about finding charts: RA & Dec: all coordinates are accurate to 1"; charts can be generated by operator as necessary using LEDAS or DSS. Many charts are available via the link from the main 1.5m scheduling page. Charts for many objects should be available at the telescope. .............................................................................. Questions may be addressed to: Howard Bond bond@stsci.edu (STSI programs) Fred Walter fwalter@astro.sunysb.edu (SUNY programs) ----------------------------------------------------------------------- ----------------------------------------------------------------------- Investigator's Detailed Instructions for NOAO 08a-207 NOAO 0207 P.I. Martin Altmann, Heidelberg, Germany SMARTS 1.5m Service Observing Program 080217 Synopsis of the programme: ========================== This programme aims at securing spectra for the determination of spectroscopic parallaxes of reference stars for a HST-parallax programme. Since unlike the ideal case the distances of background stars are non-negligible their approximate distances need to be determined so that the measured parallax can be corrected accordingly. Therefore the main aim of the observations to be carried out here is to measure the overall SED of the optical spectrum, as well as lines - this will be used to classify the stars . Radial velocities are of no importance therefore we work with a minimum of emission line spectra. A major difficulty is the hour angle limited time during which we have to carry out the observations. Grating setup for night: ======================== 9/Ic (or 32/Ib) Note: Both setups need to be observed. For this night we would prefer 9/Ic, if the previous night was 32/Ib - if the first night was lost, use 32/Ib. EPHEMERIS INFORMATION Critically important!!!!!!!! All times local , i.e. Chilean time Night of Feb. 17 ---> 18, 2008 Sun: set: 20:37; (12-): 21:24; (18-): 21:54; (18+): 6:01; Rise: 7:18 LST(midnight): 8:06:36 LST(12-): 05:30 Notes: 12-: end of evening nautical twilight (-12 degrees setting) 18-: " " " astron. " " (-18 degrees setting) 18+: beg. of morning astron. twilight (-18 degrees rising) LST(): local sidereal time at x local time Important notice: ================= H.A. range, start and ending of observations (CRITICAL!!!!!) ------------------------------------------------------------ Since our target area is at R.A.=03:13 to 03:20 and the hard limit is at H.A.=05:30 (LST: 08:45, local time: 0:43, UTC 4:43), observing of the objects should start at Sun: -12 degrees, i.e. at the end of nautical twilight (or earlier if possible). The current schedule (see observing table below) is 206 minutes of total observing time (incl. Overheads), or 3:26. The timespan between end of nautical twilight and end of observations is approximately 3:20, i.e. 6 minutes less than the strict observing range. Therefore the slewing and acquisition phase for the first target (REF 1) which is a rather bright star should be done before -12 degrees. This also applies to the first emission line spectrum. We only need 3 emission line spectrums during the whole night, since: -all targets are in the same field - no large slews across the sky. -these spectra are intended for spectral classification purposes only. No RVs. The wavelength calibration only needs to be sufficient for unambiguous identification of spectral lines. The last emission line spectrum should be taken after the last stellar spectrum. If the guiding is switched off during this time it will buy us another minute. Spectrophotometric standards ----------------------------- We do need a spectrophotometric standard star, this must under all circumstances be done, after the actual object exposures have been done. Do not waste valuable time by taking the standard during the object time. Since we have a lot of time afterwards we would request to take spectra of two more standard stars - this can be used for extinction determination. Concerning the overheads: ------------------------- The overheads were calculated as indicated in the instructions, i.e. 5 min slew time, 1 minute readout for every exposure. For most targets we ask for two exposures and in for three emission line comparison spectra during the observing. Therefore the overhead is nominally 7 minutes, 8 minutes when a EM spectrum is required. Given that the targets are within a few minutes of each other eliminating the need for large slews, the acquisition time is most likely going to be shorter. This will allow us to fullfill the VERY tight schedule. The finding chart: ------------------ There is one finding chart for all objects. The numbers next to the arrows are the REF# numbers, e.g. arrow "1" points at REF1, etc. The arrow "WD" can be ignored - these are the actual white dwarfs. The chart's orientation is indicated in the lower right corner, the dimension of the shaded area is approximately 15'x15', i.e. that of the whole chart 20'x15'. Grating setup for night: ------------------------ 9/Ic (or 32/Ib) Note: Both setups need to be observed. For this night we would prefer 9/Ic, if the previous night was 32/Ib - if the first night was lost, use 32/Ib. Schedule for the night: ======================== During the afternoon: Installing the setup 9/Ic Standard calibrations (bias, flats, etc.) Twilight: twilight spectra at -9 degrees slew to first target (REF1 is a bright star) at -12 degrees, i.e. 21:24 local time the observations must start. (except for REF1) 2 exposures per star, one emission line spectrum before starting, one during the middle one after the last exposure. The objects do not have to be observed in the sequence as indicated by the object list, it is however prudent to start with the brightest object REF1, which is also the first entry in the list. At LST: 08:45, local time: 0:41, UTC 4:41, the hard H.A. criterium of 5:30 has been reached (while taking the last exposure, please check that it stops integrating before it reaches the switch, in necessary adjust the exposure time accordingly. After finishing the object observations: Spectrophotometric standard star, i.e. the season's default object and two others at different airmasses (to determine extinction). After finishing the standard stars, the targets we applied for cannot be observed anymore