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4. Planning Your Observations

4.1 Applying for Observing Time

Parkes-specific information for upcoming semsters and submission deadlines can be found here, while current and archived observing schedules can be found here.

Information regarding system capabilities not listed in the above can be addressed to parkes-operations@csiro.au

4.2 Observing Modes

Spectral and continuum-line observations can be performed with all currently-available receivers and back-ends. Possible observing modes include:

There are three methods of switching. Not all methods are available with all receivers/back-ends.

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:

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used in schedule files and some examples can be found in the TCS documentation However, please note this is seriously out-of-date and you should consult this manual or note there are a number of online utilities which allow you to create a TCS schedule file for spectral-line, continuum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 Spectral-line and Continuum Observations (non-pulsar) Continuum/Polarisation Example

In this example, we will be using the 10CM concentric receiver (part of the 1050CM package) to create a 30x30 arcmin full stokes (allowing polarisation analysis) continuum map of the RCW41 HII region at 2.8GHz, using DFB3 with a bandwidth of 128MHz with 8192 channels. We disable Tsys logging here as it contributes to the system noise. Actually, we should create two maps, the first consisting of a series of scans in RA (constant DEC), as done here, and the second map consisting of a series of scans in DEC (constant RA). This basket-weaving allows for the removal of scan-line patterns (“stripes”) from single-dish radio maps. The width between adjacent scans in both maps is 60 arcseconds (1/6th of the 10CM beam). We will be using the scanning map online schedule tool.

The input parameters to the online tool are shown below.


Figure 4.1: TCS schedule continuum example: Full-stokes, 2.8GHz continuum map for the RCW41 region.

Note this is only for the RA (constant DEC) scans. You can view the complete RA scans schedule file here. This is saved to your computer as a text file then uploaded to the Parkes computers before you start observing. According to the output, it will take approximately 70 minutes to complete the RA scans, plus another 70 minutes for the DEC scans. Spectral-line Example

In this example, we will again map the RCW41 region, but this time, we will use the 13MM receiver to map the Ammonia (1,1), (2,2), (3,3) and (4,4) transitions. Again we will be using DFB3, but instead of a single IF, DFB3 can have two input IFs. The configuration will use 256MHz/8192 channels for the first IF (to record the first three transitions), and 64MHz/8192 chanels in the second (to record the fourth transition). The observing method is the On-The-Fly Mapping. Here, the map is created by interleaving a reference position (done in TRACK mode), with scans across the region of interest. Note the reference position is assumed to be free of line-emission! In addition, we are only mapping a 10x10 arcminute region of RCW41. The width between adjacent scans is 20 arcseconds, or 1/3rd of the 13MM beamwidth. We assume the RCW41 core is moving 3.7 km/s with respect to the LSR and so doppler tracking is enabled for both IFs.

The input parameters to the online tool are shown below.


Figure 4.2: TCS schedule spectral-line example: Four ammonia transitions map for the RCW41 region.

Note, again, this is only for the RA (constant DEC) scans. You can view the complete RA scans schedule file here. Again, this is saved to your computer and uploaded to the Parkes local observing computers prior to observing. According to the output, the RA scans will take around 180 minutes to do, plus another 180 if we also (should) do the DEC scans.

4.3.2 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 $\sim$5.7 MHz arises from multiple reflections in the 26m space between the vertex at one end, and the focus and/or underside of the focus cabin at the other. fig:standwave shows 22 GHz observations of a strong Ammonia source, G316.819, showing strong (1,1) and (2,2) transitions for 4 minutes (exact multiple of 60 seconds). The two observations were taken one after the other, the first (upper panel) with no special ’de-rippling’ measures, the lower taken in a mode where the receiver is moved cyclically up and down in the translator Y-axis to ’smear out’ the ripple with amplitude 6.3mm peak-to-peak ($\lambda$/2) and period 60 seconds. This technique is available for use with higher-frequency receivers only and proposers should contact Parkes Operations (parkes-operations@csiro.au) before submitting proposals.


Figure 4.3: 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 ($\sim$ 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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Last updated by Stacy Mader on July 2, 2015