Hello, SMARTS, Chilean, and NOAO users! 01 JAN 2012 Welcome to SMARTS 2012A. You are being contacted because you have been granted service time on the CTIO 0.9m telescope in the 2012A observing semester, beginning 01 JAN 2012. This email is a brief overview of the SMARTS scheduling process for the 0.9m, the instrumentation, and tips on planning observations (in that order). For convenience, it is also online here: http://www.astro.gsu.edu/~thenry/SMARTS/smarts.0.9m.welcome ---------------------------------------------------------------------- C O N T A C T P E O P L E ---------------------------------------------------------------------- The responsible authorities for the SMARTS 0.9m are: Mr. Adric Riedel (GSU), SMARTS Fellow for the 0.9m. riedel@chara.gsu.edu Ms. Jennifer Winters (GSU), SMARTS Fellow for the 0.9m. winters@chara.gsu.edu Dr. Todd Henry (GSU), SMARTS 0.9m Coordinator. thenry@chara.gsu.edu Dr. Charles Bailyn (Yale), Director of the SMARTS Consortium. charles.bailyn@yale.edu Questions about 0.9m operations should be directed to Mr. Riedel, Ms. Winters, and Dr. Henry; GSU has been using the 0.9m since 1999 and has been coordinating the 0.9m since the beginning of SMARTS in 2003. ---------------------------------------------------------------------- S C H E D U L I N G ---------------------------------------------------------------------- Time on the SMARTS 0.9m is a mix of classical user observing and service observing, divided into (generally) alternating blocks of nights the CTIO staff call 'turnos'. Within any given turno, time is alloted on specific nights (or half-nights, but not less). As such, we cannot guarantee weather conditions. Note that as of 2012A, the CTIO 0.9m 'turnos' are no longer uniformly seven nights starting on a Thursday, as SMARTS is now running the user-only CTIO 1.0m and the user/service CTIO 0.9m on an alternating schedule. The overall SMARTS 0.9m page can be found at: http://www.astro.gsu.edu/~thenry/SMARTS The observing schedule for 2012A is posted (and updated) here: http://www.astro.gsu.edu/~thenry/SMARTS/schedule2012A.htm Under the 'TIMES' link for your night(s), you will also find a listing of precisely what hours you have been given. This will aid in planning your programs. Notice that, after the southern autumnal equinox, 20 MAR 2012, a one-hour break mandated by the Chilean federal government has been explicitly programmed into the schedule. Unless you wish to keep your program completely confidential, this is also where it will be posted for the service observers to see. Three weeks before your scheduled observations' turno, you will be contacted by Adric Riedel or Jen Winters, who will send you a template (also available at http://www.astro.gsu.edu/~thenry/SMARTS/smarts.template and attached to this email) to use to plan your program. Reminders will be sent two weeks before, and 10 days before, as needed. ***** IF YOU DO NOT RESPOND WITH AN OBSERVING LIST BY 7 DAYS ***** ***** BEFORE YOUR TURNO BEGINS, YOU WILL FORFEIT YOUR TIME. ***** You are welcome to contact Mr. Riedel or Ms. Winters with questions about your observing program. Also, example telescope setups from regular users may be found here: http://www.astro.gsu.edu/~thenry/SMARTS/setups.dir/index.htm You will also need to fill out the instrument form at http://www.ctio.noao.edu/forms/supportforms/ccd_direct.php (using 0.9M+Tek 2048 CCD) to confirm your time and request the filters you will need. This is critical for the 0.9m in order to be sure that your desired filters are available. After your observations are complete, Mr. Riedel or Ms. Winters will contact you again with the night reports from your scheduled nights and instructions on how to download the data from GSU's FTP server. Data will be held there for 30 days as bzip2-compressed fits files plus a text file with brief header information. ---------------------------------------------------------------------- I N S T R U M E N T A T I O N ---------------------------------------------------------------------- ---------------------------THE INSTRUMENT----------------------------- Pictures of the instrument: http://www.astro.gsu.edu/~thenry/SMARTS/smarts.0.9m.pictures The SMARTS 0.9m is a 36-inch (91-cm) Boller & Chivens telescope, built in 1965 and currently operated by the SMARTS Consortium for NOAO. The only available instrument on the 0.9m is a Tektronix 2048x2046 CCD with 65K pixel/ADU depth (linear to 60K ADU), and a FOV of 13.69' on the sky (north down, east left), with a pixel scale of 0.401"/pix (not 0.396"/pix as listed on the CTIO page below). This arrangement has lasted for more than 14 years, and has been incredibly stable, both photometrically and astrometrically. More detailed (somewhat outdated) information about the following points may be found here: http://www.ctio.noao.edu/telescopes/36/0-9m.html The Tektronix CCD can be run in a number of modes: FULL chip (13.6'), ONE amp readout (3 min readout) FULL chip (13.6'), QUAD amp readout (0.8 min readout) Central QUARter (6.8'), ONE amp readout (0.8 min readout) Central QUARter (6.8'), QUAD amp readout (0.3 min readout) Quad-readout frames will need to be processed with a tool like IRAF's quadproc, as each of the amplifiers has its own bias level. In single-amp mode, the lower left (ll) amplifier is usually used. Dual-amp mode and 2x2 binning are also possible, but not officially supported. There are also three available gain settings (read noise is for ll amp:) 1: (unavailable, failed in March 2009) 2: Read Noise ~ 1.5 ADU = 3.9 e- 3: Read Noise ~ 1.7 ADU = 3.1 e- 4: Read Noise ~ 2.6 ADU = 2.6 e- (values updated 2012A by Dr. John Subasavage, this supercedes the CTIO website) ----------------------------THE FILTERS------------------------------- The 0.9m accepts two filter wheels. There are two sizes available, 8-slot wheels for 3"x3" filters, and 5-slot wheels for 4"x4" filters. CTIO has a large assortment of filters available for use, listed here (many linked to their filter traces): http://www.ctio.noao.edu/instruments/filters/filters_34.html CTIO also has some old 2"x2" filters useable in the 0.9m, listed here: http://www.ctio.noao.edu/instruments/filters/index.html Using the 2"x2" filters is not recommended --- many of them are seriously degraded and all of them vignette on the 0.9m in FULL chip mode. In addition to those filters, CTIO has a set of 3x3 Neutral Density filters: ND1 attenuation by = 2.5 MAGNITUDES ND2 attenuation by = 5.0 MAGNITUDES ND3 attenuation by = 7.5 MAGNITUDES ND4 attenuation by = 10.0 MAGNITUDES it is also possible to combine two ND filters (e.g. ND2+ND4=15.0 mag attenuation). The 0.9m uses a 3x3 color-balance filter for dome flats (but not sky flats). It is not necessary to request this filter; it is used automatically. Please make your filter request as specific as possible when you fill out the instrument form. These filters are shared between telescopes so CTIO staff will need time to make sure the right ones are available for the 0.9m on your nights. http://www.ctio.noao.edu/forms/supportforms/ccd_direct.php The most common filters in use at the 0.9m are: * The Tektronix UBVRI 3"x3" filter set (roughly Johnson/Kron-Cousins), which is almost always comprised of the Tek #2 UBRI filters and the Tek #1 V filter. Filter traces for all three Tek filter sets are available at http://www.astro.gsu.edu/~thenry/SMARTS/smarts.0.9m.filters.pdf * An SDSS ugriz 4"x4" filter set (Sloan filters, not to be confused with our Thuan-Gunn griz set) -------------------------EXPOSURE TIMES------------------------------- Details about the common filters (e.g. exposure time estimates) are available here: http://www.astro.gsu.edu/~thenry/SMARTS/smarts.0.9m.filters.text However, note that you can request exposure to a certain number of peak ADU, rather than a specific exposure time. Exposure times will, of course, depend on seeing and cloud cover, and also on how recently the primary mirror of the 0.9m was cleaned. The 0.9m can take exposures as short as 0.5 seconds, but shutter effects (uneven illumination) are a concern up to 5 seconds. It is recommended to request defocusing or an ND filter if targets saturate in less than 5 seconds. Tests of astrometric (not photometric) stability show best results for exposures longer than 60 seconds. Tracking at the 0.9m is usually stable for up to 300 seconds. For longer exposures the observer will typically use the autoguider. ---------------------------------------------------------------------- K N O W N I S S U E S A T T H E 0 . 9 M ---------------------------------------------------------------------- HEADERS --- The "new" TCS installed in 2005 cannot communicate with the ARCON data acquisition computer, and as such several header fields (including RA, DEC and EPOCH) are now garbage. Many attempts to solve this problem have been unsuccessful. Given the actual pointing accuracy (see below), a first step would be to use the input J2000 coordinates instead. For details, see http://www.astro.gsu.edu/~thenry/SMARTS/smarts.0.9m.tcs POINTING --- pointing is typically good to 20 arcseconds, which means it is reliable enough that you should be able to use the J2000 coordinates of your intended field center. However, we HIGHLY recommend that you provide an electronic finder (with orientation and scale labels!) on a working website for every target. BAD COLUMNS --- Like many CCDs, the Tek 2k CCD on the 0.9m has bad columns. These can be avoided. Similarly, in quad-readout mode, each quadrant is bordered by overscan regions that can be avoided. PHANTOM OF THE 0.9M --- occasionally, the dome will spin 360 degrees seemingly without cause. Many tests have been done to determine the cause, and no convincing gotcha has been found. ---------------------------------------------------------------------- P L A N N I N G O B S E R V A T I O N S ---------------------------------------------------------------------- Attached to this email is the sample template (ASCII format). YOU MUST USE THIS TEMPLATE FOR YOUR OBSERVATIONS. IT HAS A LABEL OF 2012A AT THE TOP. The closer you adhere to the format, the smoother your observations will go. A few tips and requests, because we at the 0.9m like to under-promise and over-deliver: * No non-sidereal programs in service mode. The timing and instrument changes make this better suited to user mode. If you must track a moving target, do it with many short exposures. * No polarimetry programs in service mode. As this is a non-standard instrument setup for the 0.9m, it is better handled as user time. * Assume you are proposing for automated observing. None of us are familiar with your program, so everything you need must be spelled out. * You may only have TWO possible programs (photometric, nonphotometric backup) per night, and each must be entirely self-contained. A single program that can be done in either case (ignoring standard star observations if nonphotometric, for example) is also fine. * Include links to finder charts, with the target labeled and some idea of the image scale and orientation. If you do not, we have no way to spot any pointing errors. * Assume your program will be set in stone once started. We do not have the facility to change target lists for night #2 based on what was observed on night #1. * If there are time-sensitive observations that would happen during a scheduled break, the one-hour break can be moved (but not REmoved). * Assume the observer is going to go straight down your list as the night progresses. Use the priority system to make sure the observer knows which targets can be skipped if time is short. * For best results when requesting absolute photometry, use an airmass calculator (such as http://www.briancasey.org/artifacts/astro/airmass.cgi) to determine the exact times (UT) you want your standards observed, and list each visit as a separate observation. * The weather at CTIO is worst in winter. Programs scheduled for December or January (Chilean summer) can likely expect to get more than 70% photometric nights, but the odds of photometric weather in August are low. * Plan for overhead, as detailed for service mode at: http://www.astro.gsu.edu/~thenry/SMARTS/smarts.overheads * Keep it simple. Our observers are Chilean CTIO employees. They are not scientists, nor is English their first language, and neither Mr. Riedel nor Ms. Winters want to reword parts of your program to make it clearer for them. The following requests work well: * integrating for a certain amount of time * integrating to X number of peak counts on a target object (marked on a finder) * observing a target continuously for an entire night/ until UT time X * dithering between observations (this goes for sky flats as well) * moving the target off the center of a quad-readout frame * explicit timing of observations (put UT times in the notes) * listing objects, such as standard stars, multiple times if you want them observed at different airmasses * "use ND filter if (object) saturates in less than X seconds" * "observations may begin in twilight" ---------------------------------------------------------------------- W H A T Y O U N E E D T O D O N O W ---------------------------------------------------------------------- Once you have read this message, please email Mr. Riedel at riedel@chara.gsu.edu and you will be placed on the "confirmed" list for observations in 2012A. ---------------------------------------------------------------------- If there are any further questions about anything in this email, feel free to contact Mr. Riedel, Ms. Winters, or Dr. Henry. Clear Skies, Adric Riedel SMARTS Fellow Graduate Student, Georgia State University Jennifer Winters SMARTS Fellow Graduate Student, Georgia State University Dr. Todd J. Henry Director, RECONS Professor of Astronomy, Georgia State University