Do not enter unless you know what you are doing. It is recommended you correct for doppler shifts by entering the source's radial velocity in the graphical frequency editor.
Select a MOPS configuration from the menu. MOPS refers to
the Mopra Spectrometer, the new polyphase digital filterbank. MOPS is now the standard mode. MOPS can operate in wideband mode (8.2 GHz bandwidth) or zoom mode (137.5 MHz bandwidth). There is an option for the wideband mode to observe with only 1024 channels and therefore reduce the size of the data files. This third option is rarely used.
Enter the centre
frequency of the 8 GHz covered by MOPS. If Doppler tracking is
enabled, the frequency here will be interpreted as the rest frequency
of the observed line. If Doppler tracking is disabled the frequency
here would be the actual observing frequency (sky frequency).
tracking. Note that this only adjusts the centre frequency, it does
NOT continuously track the Doppler shift during an observation. For
observing with MOPS it is recommended that Doppler tracking be
The radial velocity of
your source. Also choose the reference frame, LSR (local
standard of rest) or barycentric. The radial velocity
information provided here will be ignored if Doppler tracking is
* Note: If Doppler tracking is disabled (recommended for MOPS) and no radio velocity is
specified (also recommended) then you must adjust your sky frequency to account for
the velocity of both the source (LSR or barycentric) and the velocity of the observatory relative
to the rest frame. An online tool is available
to calculate this adjustment.
The number of seconds per integration cycle. Use 2 seconds for mops zoom and broadband observations, and 2.048 seconds for fast mapping observations. *
CHECK WITH SUPPORT STAFF BEFORE CHANGING THIS OPTION.
Please provide the source coordinates in the specified coordinate
system here. This determines the centre of the on-the-fly map. Please take care
of the format: Equatorial, RA: hh:mm:ss DEC: dd:mm:ss, Galactic
GLON: ddd.xxxxx GLAT: dd.xxxxx.
The size of the map in arcmin. Only square maps are supported at this stage. The maps always have
an odd number of rows so that one row passes through the map centre. Consequently the final map
width may vary from what you specified here.
Scanning direction of the map. You may choose to perform your map along RA/GLONG
(i.e. horizontal direction) or along DEC/GLAT (vertical direction). Scanning at arbitrary angles is
currently not supported.
For observing at 3-mm only. Approximate time in minutes between Tsys measurements, i.e., ambient load calibration using the paddle.
The true intervals between the Tsys measurements may slightly vary from the input due to
other constraints of the schedule.
For observing at 7- and 12-mm no Tsys measurement is required. In this case enter "0" for the time interval. This will ensure no Tsys measurements are entered into the output schedule file.
Spacing in arcsec betwen rows (orthogonal to the scanning direction). Default is calculated from the Nyquist frequency using an extra 0.9
oversampling factor and a 2" guard band to mitigate against tracking errors.
(Note: This option has not been tested.)Proper motion of the source, in arcsec/hour in the directions of specified coordinate system
(RA/Dec or GLON/GLAT). Two values separated by white space. Default is zero. Note: Proper motion
tracing is inexact and based on an estimate of how time passes during the map. The map centre is
updated at the beginning of each scan. You should give as the map centre the position of the source
at the start of the map. Coordinates and proper motions of the planets are available on JPL's HORIZONS