ALFALFA Survey - Observations for A2010

ALFALFA Survey - Notes on Zenith Strip Observing

Version date: Fall 2011 Sep 6th update)

Previous page Fall2010 version

This page is designed to provide the background needed to understand the changes in observing strategy being adopted in 2011 to accomodate zenith strip, off-meridian observing for the Fall 2011 A2010 observing season. It will be best if observers' understand the need for the changes, the limits on telescope motion and how to arrive at the solution, especially since the observing schedule may change unexpectedly.

Changes to observing protocol
Here is a quick summary:

We run TOGS **only** at the start.
We will use one of several new configuration files including a2010_az85_2010.conf or a2010_az265_2010.conf depending on whether we are using an azimuth near 90 or near 270 degrees or something else. Choose the one specified for a particular date and drift (chosen to be close to the Az for that night).
Unlike the circumstance of meridian observing, the configuration file only provides a basic setup of the backend, LO and observing mode.
Unlike the circumstance of meridian observing, the "start time" for the observing (in RA) will be offset from the actual LST time by 20-30 minutes. The hour angle is non-zero (i.e., we are **real** astronomers!). See the A2010 current schedule page.
Once the configuration file is loaded, the observer will have to update
1. the ALFA rotation angle, in the "fixed azimuth drift" widget of the CIMA observing observing menu
2. the azimuth, in the "fixed azimuth drift" widget
3. the starting R.A., in the "fixed azimuth drift" widget. The RA will be offset from the LST by a predictable amount.
and then rotate ALFA to the proper rotation angle using the pointing control widget off the main menu.

The tentative plan for how to accomplish this can be found here without regard to the date of the observations. You should use that as a guide, but please double check according to the date when observations are actually conducted.

Restricted ZA "almost fixed azimuth" observing mode: the basics
In the normal mode of A2010 observing, we fix the azimuth at 180 or 360, and then adjust the ZA according to the declination of the drift. Close to zenith, we run into the constraint that the Gregorian cannot come with 1.1 deg of zenith, so we have always known that we would have to observe those drifts at some different azimuth. The exact azimuth we might choose depends on the zenith angle and the hour angle of the target drift (and thus, the declination and the RA range we want to cover). As analyzed by Shan and Manolis, once the zenith angle of a source very close to Dec =~ +18 deg exceeds a few degrees, the required azimuth changes only a little even if the zenith angle changes a lot. For those sources, the azimuth needs to be close to either 90 deg or 270 deg, once the source is beyond a ZA of a few degrees. Restricting the ZA to a range between 3.5 and 12 degrees (the current limits) introduces further constraints/considerations:

Obviously, when we observe at an AZ off the meridian, the RA of Beam 0 does not match the LST. Hence the observed range of RA will not correspond to the LST range of the observations.
The position in AZ, ZA to which the telescope is commanded to point does not ever correspond exactly to the position corresponding to RA, Dec, because of (a) precession and (b) the telescope pointing model. Moreover, the position we specify corresponds to the mapping of the RA,Dec at the center of ALFA Beam 0 to Az,ZA, but the limits refer to the encoder position tracking the center of the dome. In particular, you will notice that the Z.A. changes during the night. Remember that we are tracking in J2000 coords and it is now 2010.7 (Sep 2010). Close to 90,270 a small change in Decl translates to a larger change in Z.A. Refer to the ALFALFA notes on precession. As long as we are within the limits of 3.5 < Z.A. < 12 degrees, we are ok.
Phil thinks that CIMA may have divide by zero errors if AZ = 90 or 270 exactly, so he urges us to stay a few degrees away from 90.0 and 270.0. (Indeed, after our experience last spring, we are sure of this.)
Very close to zenith, the value of ZA for a given azimuth is double valued. CIMA will always select the lower ZA, so we have to think most carefully about these drifts (for this reason, they will be done by the EGGs from Ithaca). See Phil's notes.
We require that the ALFA beams tracks be equally spaced in declination and achieve that by rotating ALFA appropriately. The required rotation angle depends on AZ, and is 19 degrees only on the meridian. Hence if we elect different azimuths, we need to rotate ALFA accordingly. Note: the beam spacing also changes slightly; we have to live with that. You might want to refresh your knowledge; refer to our memo and links there.
The ALFA beam pattern has 6-fold symmetry, but we do not want to change the relative orientation of the beams. In particular, we always want beam 4 to be the one at highest ZA; remind yourself here.
ALFA can be rotated only over the range of (-100,+100) degrees; that turns out to be important and reduces our flexibility in choosing whether to use 90 or 270. That constraint, in turn, impacts the RA range we actually cover.

A note about TOGS
During the fall 2011 season, TOGS is scheduled only at the start of A2010. To accomodate the ZA restriction issues, the TOGS command file has been modified so that the A2010 observer no longer has to update the "galfasrc" entry in the "a2010.cat" file. Just run the special command_galfasrc_zenstrip.cmd script. Instead of RA,Dec, it takes an Az,ZA from the "galfa_togs.cat" file; that should be updated by the TOGS team prior to the start of the run. If something weird happens, check that "galfa_togs.cat" is set for an azimuth near ours; if not, skip it (or fix it yourself if you have time). If for some reason, the telescope runs into a limit, just let the script continue to collect data. Can't do much more than that on the fly.

Note for future reference: we have commented out the "galfasrc" entry in the a2010.cat file, so you cannot run the other mode of TOGS calibration (via command_galfasrc10.cmd) unless you (a) edit a2010.cat to uncomment that line; (2) make a new version of command_galfasrc10.cmd which does not rotate ALFA (comment out the "ALFAANG 19" line); and (3) change the RA of the galfasrc in a2010.cat as before.

What needs to be observed:
The missing drifts can be identified here, assuming that someone keeps that file updated. Check also the A2010 team schedule (likewise, assuming someone keeps it updated).

Useful software for planning
There are two programs in eggidl/gen which I use to help with scheduling: blocksched, lsttoazRT and azdectozaha (which is a function, written by Phil, modified by us). These programs are accessible when you call @egggeninit (assuming you have the path to eggidl/gen in your .idl_startup file).Note, that these programs are neither elegant nor flexible, so be sure you understand their limitations.

blocksched Calculates LST start/stop times for AST time block on a given date
SYNTAX: blocksched, yymmdd,ast1HHMM,ast2HHMM
EXAMPLE: blocksched,100316L,2215,2359
Use this to figure out the LST range corresponding to a given block in AST on a given date. Note that if your block crosses midnight, you need to run it twice (or just add 4 minutes). Also, precision only to nearest minute.

lsttoazrt Computes the az, za and optimal rotation angles for a succession of drifts of length DRIFTTIME, starting on a given day yymmdd at a given LST and assuming the ALFALFA beam configuration. Performs simple error check on slew times between drifts, ALFA rotation limits, and optimization algorithm iteration boundaries. Was written for the NGC 2903 ALFA precursor program (A1963). Note: Since this routine was not written for A2010, it does more than we need it to do but I am too lazy to change it. Just ignore the DRIFTTIME (set it to 480.) and the info on drifts other than the first one.
SYNTAX: lsttoazrt, yymmdd,lmstHHMMSS,raHHMMSS,decDDMMSS,driftTime
EXAMPLE: lsttoazRT,100312L,092000L,084500L,162530L,480.

Use a standard value of the LST (I am using 092000L) and then adjust raHHMMSS so that the resultant Az and ZA yield (1) ZA within (6:9) and Az differs from 90 or 270 by a few degrees. The result also then can be used to see the approx difference between the LST and RA at the actual LST of the observation (which will vary from night to night).

Daily chores: (IF NOT PERFORMED BY MARTHA -- not needed now!)
Every day, the following tasks need to be performed. It is not necessary that a single person perform all of them, but the tasks need to be performed every day (or at most, within 2 days).

Check the posted schedule for unexpected changes. (Task should take <2 minutes.)
Update the schedule files (see below). (Task should take <10 minutes.)
Double check that the a2010.cat file is set up properly for the next observer. It's always a good idea that this task be performed by someone other than the observer who may have been seriously sleep deprived. (Task should take <5 minutes.)
(1) check that the data were properly converted to IDL save files. (Task should take <5 minutes.)
(2) transfer the IDL save files to the dorado13/idlraw area. (Task should take <5 minutes to set up, and files should take about 2 hour to transfer.)
Edit and "source" /home/dorado3/dorado13/galaxy/idlraw/rsync.csh to perform the transfer.
Once the data are successfully transfered, then someone should run NCALIB1, NCALIB2 and BPD on the files to make sure that everything is ok. Do this as "galaxy" on the machine called "arecibo" in the disk area /home/arecibo/galaxy/mar2010. Make a subdirectory with the appropriate block name and follow the log.spring file, filling in to make log_processing_YYMMDD. You only need to get through BPD, but be sure to check the pos file and one drift to make sure everything is ok. If you find something wrong (especially unfamiliar or gross rfi), notify the folks at AO (especially Phil phil@naic.edu). If problem is serious, call someone like Robert, Phil, Ganesh, etc. on the phone. (Task should take <15 minutes to get to point when BPD starts: BDP should then run for about 90 min.)

The schedule files:
There are 4 files which we use to keep track of the planned and executed observations. They are designed to be, in some ways, redundant; instilling redundancy is a good way to minimize errors. The files are located in camuy:/home/web/research/projects/egg/alfalfa/scheds/asttimes/

a2010_schedcurrent.txt containing the past and future observing plan
a2010_schedupcoming.txt containing only the future observing plan
a2010_schedspr_needed.txt indicates what RA coverage is still needed per drift
a2010_schedsprstatus.txt indicates what RA coverage has been completed

To update, follow the instructions in /home/web/research/projects/egg/alfalfa/scheds/asttimes/upsched_process.txt.

Last updated Tue Aug 31 09:00:14 EDT 2010 by martha