Mopra Schedule File Creator: On-the-Fly (OTF) Map V6.0
To refresh the screen using the default entries, press SHIFT and click the 'reload' button simultaneously.
Note that this schedule file creator assumes a cycle time of 2s.
This output should be saved on your local computer (.sch) and then uploaded to the Mopra control
computer bigrock.
The project number assigned to your proposal.
Example: M007
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Initials or short name of the observer(s).
Example: ZOZ
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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.
Example: MOPS zoom
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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).
Make sure your frequency is within these limits:
- 12-mm: 16000 - 25000 MHz
- 7-mm: 30000 - 50000 MHz
- 3-mm: 77500 - 117000 MHz
Example: 92900
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For MOPS zoom mode
use the mops_vis.pl script available on pyroclast to determine
which values to enter into the 4 spectral windows of each band. For
unused windows leave blank.
Example: 33,44,51,56
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Enable/disable Doppler
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
disabled.
Example: disabled
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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
disabled.
* 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
Frequency Calculator
to calculate this adjustment.
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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.
The coordinate system of your coordinates. You may choose between
equatorial (J2000 or B1950) or Galactic coordinates.
Example: J2000
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Specify the name of your source here. If left blank the source name defaults to "source".
Example: Orion
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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.
Example: RA: 23:41:32
DEC: -82:43:09
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You may choose only absolute positioning for the reference position.
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The position
of the reference integration (2 values separated by a comma). Please take care
of the format: Equatorial, RA: hh:mm:ss DEC: dd:mm:ss, Galactic
GLON: ddd.xxxxx GLAT: dd.xxxxx.
Example 1: 12:33:15.3, -72:54:04.8
Example 2: 366.4988, -54.0000
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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.
Example: 5
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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.
Example: RA/GLON
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Starting point of the map. Values may be the north-eastern, north-western,
south-eastern, or south-western corner.
Example: north-east
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Number of OTF rows before returning to the OFF position. You may choose 1 row for large maps (say more than 2 arcmin in size) and 2 for small maps.
Example: 1
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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.
Example: 15
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This frequency value (in MHz) is used to calculate the Nyquist sampling rate for the scanning. Default
is the value given in Observing Frequency.
Example: 88000
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Time spent on OFF scans in seconds. Default is calculated from the time spent on each row. Please
seek advice from support staff if you require no reference scans.
Example: 120
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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.
Example: 40
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Beam size in arcsec (FWHM). Default is calculated from the Nyquist/Observing frequency with a
Nyquist sampling rate (lambda/2D, where D=22 m). This value is then used to determine the scanrate.
Example: 40
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(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
website.
Example: 10.2 -3.5
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Original: Balthasar Indermuehle (10-OCT-2009)
Modified: Balthasar Indermuehle (14-OCT-2009)