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4. Planning Your Observations
|4.1 Applying for Observing Time|
|4.2 Observing Modes|
|4.3 Creating Schedule Files|
|4.4 Radio-Frequency Interference Considerations|
|4.5 Standing Wave Reduction|
|4.6 Dish Surface Quality|
4.1 Applying for Observing Time
Information regarding system capabilities not listed in the above can be addressed to email@example.com
4.2 Observing Modes
Spectral and continuum-line observations can be performed with all currently-available receivers and back-ends. Possible observing modes include:
Simply track the position for the specified length of time.
Execute a 5-point pattern about a target, along with one off-source position for bandpass reference (not currently implemented).
The position is tracked in turn by each beam (Multibeam receiver only.)
Observe a calibrator with each beam in turn (Multibeam receiver only.)
The telescope scans from one end to the other at a requested rate.
Perform a four-point scan (forward/reverse in RA, forward/reverse in DEC), across a source for the purposes of defining pointing offsets and calibration purposes.
- Equatorial-Horizontal Mixed Scans
Here the telescope can perform AZ-EL "spider" scans (..., -90, -45, 0, 45, 90, ...) referenced to an RA/DEC position. The scans are conducted along the Great Circle passing through the source. Mapping an area in AZ-EL centred on the RA/DEC position is also possible.
RSCAN is the TCS equivalent to the ATCA RSCAN, where the telescope is continuously in scanning mode between to Azmiuth limits. It has some precision synchronisation so that scans on subsequent days interleave correctly.
PSCAN is a variant of RSCAN in that an RSCAN is executed, in Azimuth, followed by a calibration observation. Note that strict LST synchronisation is required. A file defining the cal source and the Azimuth scan details needs to be consulted before each set.
There are three methods of switching. Not all methods are available with all receivers/back-ends.
- Position Switching
Using the TRACK mode, the telescope alternates between an on and off-source position where the latter is assumed to be free of line emission. This mode is typically used for observing molecular lines such as Ammonia and Maser lines. Point-by-point mapping can be done with this mode.
- Frequency Switching
During an observation, the observing frequency alternates between a pair of frequencies. Both slow and fast modes are available. This mode is often used for SCANNING on-the-fly observations which look at spatially-extended emission such as wide (Galactic HI) and narrow hydrogen recombination spectral lines. The second (switched) frequency is used as a reference spectrum which aids in data reduction and can increase signal to noise by at least a factor of two over the position-switching mode. The total frequency switch can be either “in-band” or “out-of-band”. The size of the throw depends on the nature of the emission you are seeking. The throw should be at least 2-3 times the width of the widest profile you might expect in your data. You should also be aware if you are observing multiple spectral lines within a bandpass, some of the data processing applications such as LIVEDATA produce ghosts which may overlap and be confused with real spectra. For estimating the size of the required throw, for wide Galactic HI observations, a frequency throw of about 3 MHz with an 8 MHz bandwidth is the norm.
- Beam Switching
This is currently restricted to Multibeam receivers (MX mode). The position is tracked in turn by each required beam of the Multibeam system. This mode is ideal for observing sources such as single galaxies (or multiple if all lie within the beam). When a beam is not looking at the source we assume it’s collecting a reference spectrum from blank sky. The prior and following scans are used to form the bandpass calibration.
4.3 Creating Schedule Files
For the majority of programs, you will be using the Telescope Control Software (TCS). The TCS graphical user interface (TCS GUI) is written in Glish/Tk and runs on a Linux workstation. A Glish client runs on the same host as the TCS GUI which serves as a communications channel between the TCS GUI and the (Linux) controller.
There are two ways to use TCS. The first is to select observing parameters from the TCS GUI via widgets and entry boxes. The second (and recommended) is to use schedule files (simple text-files) which contain lists of keys and assosiated values which become the default parameters on the TCS GUI. In this way, it is possible to control the numerous components of the observing system. These systems include:
- Antenna Control (coord system, observation type)
- Tracking parameters (position, offset type, duration)
- Scanning parameters (scan center, scan range, duration/rate)
- Receiver control (receiver, focus, parallactic angle, feed angle)
- Correlator (mode, configuration)
- Local Oscillator (rest/sky frequency, bandwidth, channels, frequency switching/offset, frame)
- Cal Control Unit (enable/disable cal injection for receiver)
- Back End Controller Computer (enable Tsys logging)
Until accustomed with the system, first-time users are strongly urged to use schedule files. Detailed information on keywords used in schedule files and some examples can be found in the TCS documentation However, please note this is seriously out-of-date and you should consult this manual or note there are a number of online utilities which allow you to create a TCS schedule file for spectral-line, continuum and pulsar observations.
For spectral-line and continuum observations there are online tools for position–switching, tracking (with/without frequency-switching), beam–switching, on-the-fly mapping, scanning (with/without frequency-switching), or spot calibration.
For each form, there is help associated with each field, which the user fills in according to requirements. Below, we show two mapping examples as part of a ficticious project to characterise the RCW41 HII region; one for continuum/polarisation at 2.8GHz and the other spectral-line, looking at the first four transitions of the ammonia line.
For Pulsar observations, there is an online tool for creating a PDFB pulsar schedule here. It contains instructions on how to go about producing a schedule from scratch.
4.3.1 Pulsar Observations
A PDFB pulsar schedule can be created on the following web page here. The web page contains instructions on how to go about producing a schedule from scratch. When completed, save the schedule and transfer it to a location that TCS can access and load. In filling out the form, the valid PDFB correlator configurations for both FOLD and SEARCH modes are listed in the online tool.
4.4 Radio-Frequency Interference Considerations
An introduction to RFI observed at the observatory and surveys performed is available here.
4.5 Standing Wave Reduction
For Parkes, characteristic small-scale ripple with periodicity 5.7 MHz arises from multiple reflections in the 26m space between the vertex at one end, and the focus and/or underside of the focus cabin at the other. fig:standwave shows 22 GHz observations of a strong Ammonia source, G316.819, showing strong (1,1) and (2,2) transitions for 4 minutes (exact multiple of 60 seconds). The two observations were taken one after the other, the first (upper panel) with no special ’de-rippling’ measures, the lower taken in a mode where the receiver is moved cyclically up and down in the translator Y-axis to ’smear out’ the ripple with amplitude 6.3mm peak-to-peak (/2) and period 60 seconds. This technique is available for use with higher-frequency receivers only and proposers should contact Parkes Operations (firstname.lastname@example.org) before submitting proposals.
Figure 4.1: Upper panel showing characteristic 5.7 MHz standing wave interference with lower panel showing a cleaner spectrum obtained with receiver cycling.
4.6 Dish Surface Quality
A 4 GHz holographic survey of the dish surface was performed prior to the 1995 upgrade of the focus cabin. Other surveys at 3.95 GHz (June 1996) and 12.75 GHz (July 1996) were performed after the installation of the new focus cabin. Details of the readjustment of the inner 44m of the Parkes reflector in December 1996 is also also available here. As part of the NASA Mars tracking contract in 2003/2004, the Parkes Telescope’s surface was upgraded to make it more reflective and sensitive at X-band ( 8.5 GHz). The surface upgrade improved the telescope’s performance by about 1 dB (or 25%). A technical guide is available.
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