General Utilities¶
- gatherDebugging.py
- Description
Script to gather information about the Pytho/numpy/LSL install to help with troubleshooting.
- Usage
gatherDebugging.py
- Options
None
- lslTelemetry.py
- Description
Script to change the LSL telemetry setting.
- Usage
lslTelemetry.py [options]
- Options
- -h, --help
Display this help information
- -e, --enabled
Enable telemetry for LSL
- -d, --disable
Disable telemetry for LSL
- -k, --key
Show install identification key
- makeWisdom.py
- Description
Build LSL-specific FFTW wisdom and save it to a file within the LSL distribution.
- Usage
makeWisdom.py
- Options
None
- updateLSLSSMIF.py
- Description
Update the internal LWA1 SSMIF used by LSL.
- Usage
updateLSLSSMIF.py [options]
- Options
- -h, --help
Display this help information
- -u, --update
Update the default LWA1 SSMIF
- -r, --revert
Revert the default LWA1 SSMIF to an older version
- astroevents.py
- Description
Application to display rise, transit, and set times for various astronomical sources from LWA-1 for the current date.
- Usage
astroevents.py
- Options
None
- astrostatus.py
- Description
Application to calculate real-time ephemeris for a LWA site.
- Usage
astrostatus.py [options]
- Options
- -h, --help
show this help message and exit
- -s SITE, --site=SITE
site name (default LWA-1)
- driftcurve.py
- Description
Generate a drift curve for a dipole at LWA-1 observing at a given frequency in MHz.
- Usage
driftcurve.py [OPTIONS]
- Options
- -h, --help
Display this help information
- -f, --freq
Frequency of the observations in MHz (default = 74 MHz)
- -p, --polarization
Polarization of the observations (NS or EW; default = EW)
- -l, --lf-map
Use LF map instead of GSM
- -t, --time-step
Time step of simulations in minutes (default = 10)
- -x, --do-plot
Plot the driftcurve data
- -v, --verbose
Run driftcurve in vebose mode
- getIonosphericRM.py
- Description
Estimate the ionospheric contribution to the RM for an observation using the IGS final product and the IGRF.
- Usage
getIonosphericRM.py [options] RA Dec Start Stop
RA: J2000 right ascension in HH:MM:SS[.SSS]
Dec: J2000 declination in sDD:MM:SS[.SSS]
Start: YYYY/MM/DD HH:MM:SS start time in UTC
Stop: YYYY/MM/DD HH:MM:SS stop time in UTC
- Options
- -h, --help
Display this help information
- -n, --n-samples
Number of samples to take between the start and stop times (default = 11)
- lwa_cat_view.py
- Description
Simple LWDA astronomical source catalogue display application.
- Usage
lwa_cat_view.py [options]
- Options
- -h, --help
show this help message and exit
- -s SITE, --site=SITE
site name (default LWDA)
- -p PERIOD, --period=PERIOD
update period in seconds (default 5)
- inspectTarball.py
- Description
Given a MCS metadata tarball, print out details of the associated observations.
- Usage
inspectTarball.py metaData
- Options
None
- plotAntenna.py
- Description
Plot the relative dipole response for both polarizations of an isolated LWA-1 antenna at a particular frequency.
- Usage
plotAntenna.py [OPTIONS]
- Options
- -h, --help
Display this help information
- -f, --freq
Frequency of the observations in MHz (default = 74 MHz)
- -v, --verbose
Run plotAntenna in vebose mode
- plotStands.py
- Description
Plot the x, y, and z locations of stands at LWA-1. Also, mark and label particular stands, if requested.
- Usage
plotStands.py [OPTIONS] [stand1 [stand2 […]]]
- Options
- -h, --help
Display this help information
- -m, --metadata
Name of SSMIF or metadata tarball file to use for mappings
- -l, --label
Label the stands with their ID numbers (default = No)
- -v, --verbose
Run plotStands in vebose mode
- -o, --output
Filename to save the plot to (default = do not save)
- plotUVCoverage.py
- Description
Randomly select 20 antennae from LWA-1 and plot the uv-plane coverage for a zenith snapshot and the expected beam. Alternatively, select some FRACTION of the stands with installed FEEs to use or use the specified list of stands.
- Usage
plotUVCoverage.py [FRACTION | STAND LIST]
- Options
- -h, --help
Display this help information
- -f, --frequency
Frequency in MHz to compute the uv coverage (default 50 MHz)
- -m, --metadata
Name of SSMIF or metadata tarball file to use for mappings
- -o, --output
Filename to save the plot to (default = do not save)
Data Reading and Writing¶
- splitTBN.py
- Description
Split a TBN file containing multiple seconds into several files
- Usage
splitTBN.py [options] file
- Options
- -h, --help
Display this help information
- -c, --count
Number of seconds to keep
- -o, --offset
Number of seconds to skip before splitting
- -d, --date
Label the split files with a date rather than a squence number
Note
This script does not use a
lsl.reader.bufferbuffer to try to re-order or verify all packets and simply splits files based on size.- splitDRX.py
- Description
Split a DRX file containing multiple seconds into several files
- Usage
splitDRX.py [options] file
- Options
- -h, --help
Display this help information
- -c, --count
Number of seconds to keep
- -o, --offset
Number of seconds to skip before splitting
- -d, --date
Label the split files with a date rather than a squence number
- splitSession.py
- Description
Given a MCS metadata tarball and a session DRX recording, split the session recording into the individual observations.
- Usage
splitSession.py metaData data
- Options
None
- plotMapper.py
- Description
Read and plot the NOSTA_MAPPER table in a FITS IDI file writen by
lsl.writer.fitsidiif it exists.- Usage
plotMapper.py file
- Options
None
Data Analysis¶
- tbwSpectra.py
- Description
Given a TBW file, plot the time averaged spectra for each digitizer input.
- Usage
tbwSpectra.py [OPTIONS] file
- Options
- -h, --help
Display this help information
- -m, --metadata
Name of SSMIF or metadata tarball file to use for mappings
- -t, --bartlett
Apply a Bartlett window to the data
- -b, --blackman
Apply a Blackman window to the data
- -n, --hanning
Apply a Hanning window to the data
- -q, --quiet
Run tbwSpectra in silent mode
- -l, --fft-length
Set FFT length (default = 4096)
- -g, --gain-correct
Correct signals for the cable losses
- -s, --stack
Stack spectra in groups of 6 (if ‘-g’ is enabled only)
- -d, --disable-chunks
Display plotting chunks in addition to the global average
- -o, --output
Output file name for spectra imag
Warning
tbwSpectra.py currently assumed that the system it is running on has enough memory to read in a full TBW capture. Due to data representation and processing overheads this amounts to about 16 GB.
- tbnSpectra.py
- Description
Given a TBN file, plot the time averaged spectra for each digitizer input.
- Usage
tbnSpectra.py [OPTIONS] file
- Options
- -h, --help
Display this help information
- -m, --metadata
Name of SSMIF or metadata tarball file to use for mappings
- -t, --bartlett
Apply a Bartlett window to the data
- -b, --blackman
Apply a Blackman window to the data
- -n, --hanning
Apply a Hanning window to the data
- -s, --skip
Skip the specified number of seconds at the beginning of the file (default = 0)
- -a, --average
Number of seconds of data to average for spectra (default = 10)
- -q, --quiet
Run tbwSpectra in silent mode
- -l, --fft-length
Set FFT length (default = 4096)
- -d, --disable-chunks
Display plotting chunks in addition to the global average
- -o, --output
Output file name for spectra image
- drxSpectra.py
- Description
Given a DRX file, plot the time averaged spectra for each beam output.
- Usage
drxSpectra.py [OPTIONS] file
- Options
- -h, --help
Display this help information
- -t, --bartlett
Apply a Bartlett window to the data
- -b, --blackman
Apply a Blackman window to the data
- -n, --hanning
Apply a Hanning window to the data
- -s, --skip
Skip the specified number of seconds at the beginning of the file (default = 0)
- -a, --average
Number of seconds of data to average for spectra (default = 10)
- -q, --quiet
Run tbwSpectra in silent mode
- -l, --fft-length
Set FFT length (default = 4096)
- -d, --disable-chunks
Display plotting chunks in addition to the global average
- -o, --output
Output file name for spectra image
- drSpecSpectra.py
- Description
Given a DR spectrometer file, plot the time averaged spectra for each beam output.
- Usage
drSpecSpectra.py [OPTIONS] file
- Options
- -h, --help
Display this help information
- -s, --skip
Skip the specified number of seconds at the beginning of the file (default = 0)
- -a, --average
Number of seconds of data to average for spectra (default = 10)
- -q, --quiet
Run drSpecSpectra in silent mode
- -d, --disable-chunks
Display plotting chunks in addition to the global average
- -o, --output
Output file name for spectra image
- correlateTBW.py
- Description
Cross-correlate data in a TBW file
- Usage
correlateTBW.py [OPTIONS] file
- Options
- -h, --help
Display this help information
- -m, --metadata
Name of SSMIF or metadata tarball file to use for mappings
- -l, --fft-length
Set FFT length (default = 2048)
- -q, --quiet
Run correlateTBW in silent mode
- -x, --xx
Compute only the XX polarization product (default)
- -y, --yy
Compute only the YY polarization product
- -2, --two-products
Compute both the XX and YY polarization products
- correlateTBN.py
- Description
Example script that reads in TBN data and runs a cross-correlation on it. The results are saved in the Miriad UV format.
- Usage
correlateTBN.py [OPTIONS] file
- Options
- -h, --help
Display this help information
- -m, --metadata
Name of SSMIF or metadata tarball file to use for mappings
- -f, --fft-length
Set FFT length (default = 256)
- -t, --avg-time
Window to average visibilities in time (seconds; default = 6 s)
- -s, --samples
Number of average visibilities to generate (default = 10)
- -o, --offset
Seconds to skip from the beginning of the file
- -q, --quiet
Run correlateTBN in silent mode
- -x, --xx
Compute only the XX polarization product (default)
- -y, --yy
Compute only the YY polarization product
- -2, --two-products
Compute both the XX and YY polarization products
- -4, --four-products
Compute all for polariation products: XX, YY, XY, and YX.
- possm.py
- Description
Script that takes a FITS IDI file and mimics the AIPS task POSSM by plotting average cross-power spectra for all baselines in the FITS IDI file.
- Usage
possm.py file
- Options
None
- imageIDI.py
- Description
Script that takes a FITS IDI file and images the data.
- Usage
imageIDI.py file
- Options
- -h, --help
Display this help information
- -1, --freq-start
First frequency to image in MHz (Default = 10 MHz)
- -2, --freq-stop
Last frequency to image in MHz (Default = 88 MHz)
- -s, --dataset
Data set to image (Default = All)
- -m, --uv-min
Minimun baseline uvw length to include (Default = 0 lambda at midpoint frequency)
- -n, --no-labels
Disable source and grid labels
- -g, --no-grid
Disable the RA/Dec grid