suncasa.eovsa.eovsa_synoptic_imaging_pipeline
Attributes
Classes
Manages frequency setup based on observation date for radio astronomy imaging. |
Functions
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Compute the SNR for each image. |
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Compute the standard deviation for each image. |
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Compute residuals between each image and the mean image. |
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Check if tdt is a factor of 60 minutes or a harmonic of 60 minutes. |
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Generate a list of time ranges using pandas.date_range, with options to snap the ranges to full hours and |
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Convert a time range tuple in datetime format to a string representation. |
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Rotate an image around a specified point (xc_centre, yc_centre) by a given angle. |
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Rotate a SunPy map from helioprojective to RA-DEC coordinates and write it to a CASA image format. |
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Reproject a SunPy map to account for solar differential rotation to a new observation time. |
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Calculate the beam size at given frequencies based on a reference beam size at a reference frequency. |
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Create a blank solar disk model image (or optionally a data cube) |
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Calculate the upper limit of the UV range from frequency using linear interpolation. |
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Perform disk self-calibration on measurement set data. |
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Corrects smearing effects in solar observation data by aligning them with a model image. |
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Splits a measurement set into multiple subsets based on specified time ranges. |
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Figure out nominal times for tracking of old EOVSA antennas, and return time |
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Formats the spectral window (spw) string for file naming, ensuring start and end values are separated by a dash and zero-padded to two digits. |
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Remove directories and files that match the base image name (imname) with specific extensions. |
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Check if the image contains non-zero data. |
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Wrapper function for the tclean task in CASA. |
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Generates full-disk images, optionally cleans up interim images, and performs image registration. |
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Merges multiple FITS files into a single output file by calculating the mean of stacked data. |
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Executes the EOVSA data processing pipeline for solar observation data. |
Module Contents
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.compute_snr(images, rsun_pix, crpix1, crpix2)[source]
Compute the SNR for each image.
- Parameters:
images – 3D array of images (n_images, height, width).
rsun_pix – Radius of the circular region in pixels.
crpix1 – X-coordinate of the circle center.
crpix2 – Y-coordinate of the circle center.
- Returns:
Array of SNR values for each image.
- Return type:
snrs
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.compute_standard_deviation(images)[source]
Compute the standard deviation for each image.
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.compute_mean_residuals(images)[source]
Compute residuals between each image and the mean image.
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.detect_noisy_images(data_stack, rsun_pix, crpix1, crpix2, std_threshold=2.0, residual_threshold=2.0, snr_threshold=80.0, showplt=False)[source]
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.is_factor_of_60_minutes(tdt)[source]
Check if tdt is a factor of 60 minutes or a harmonic of 60 minutes.
- Parameters:
tdt (timedelta) – Time duration to check.
- Returns:
True if tdt is a factor or harmonic of 60 minutes, False otherwise.
- Return type:
bool
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.generate_trange_series(tbg, ted, tdt, snap_to_full_hour=False)[source]
Generate a list of time ranges using pandas.date_range, with options to snap the ranges to full hours and adjust the first and last time range based on specific conditions.
- Parameters:
tbg (str or datetime-like) – The start time.
ted (str or datetime-like) – The end time.
tdt (timedelta) – The duration of each time range.
snap_to_full_hour (bool) – Whether to snap the time series to full hours, defaults to False.
- Returns:
A list of tuples, each representing the start and end time of a range.
- Return type:
list of tuple
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.trange2timerange(trange)[source]
Convert a time range tuple in datetime format to a string representation.
- Parameters:
trange (tuple) – A tuple containing start and end times as datetime objects.
- Returns:
A string representation of the time range.
- Return type:
str
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.rotateimage(data, xc_centre, yc_centre, p_angle)[source]
Rotate an image around a specified point (xc_centre, yc_centre) by a given angle.
- Parameters:
data (numpy.ndarray) – The image data.
xc_centre (int) – The x-coordinate of the rotation center.
yc_centre (int) – The y-coordinate of the rotation center.
p_angle (float) – The rotation angle in degrees.
- Returns:
The rotated image.
- Return type:
numpy.ndarray
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.sunpymap2helioimage(sunmap, out_image)[source]
Rotate a SunPy map from helioprojective to RA-DEC coordinates and write it to a CASA image format.
- Parameters:
sunmap (sunpy.map.Map) – The input SunPy Map object to be rotated.
out_image (str) – The filepath for the output CASA image.
- Returns:
The filepath to the output CASA image format.
- Return type:
str
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.solar_diff_rot_image(in_map, newtime, out_image, showplt=False)[source]
Reproject a SunPy map to account for solar differential rotation to a new observation time.
- Parameters:
in_map (sunpy.map.Map) – The input SunPy Map object to be reprojected.
newtime (astropy.time.Time) – The new time to which the map is reprojected.
out_image (str) – The path for the output image file in CASA format.
showplt (bool) – Boolean flag to show plots of the original and reprojected maps, defaults to False.
- Returns:
The path to the output CASA image format.
- Return type:
str
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.get_bmsize(cfreq, refbmsize=70.0, reffreq=1.0, minbmsize=4.0)[source]
Calculate the beam size at given frequencies based on a reference beam size at a reference frequency. This function supports both single frequency values and lists of frequencies.
- Parameters:
cfreq (float or list) – Input frequencies in GHz, can be a float or a list of floats.
refbmsize (float, optional) – Reference beam size in arcsec, defaults to 70.0.
reffreq (float, optional) – Reference frequency in GHz, defaults to 1.0.
minbmsize (float, optional) – Minimum beam size in arcsec, defaults to 4.0.
- Returns:
Beam size at the given frequencies, same type as input (float or numpy array).
- Return type:
float or numpy.ndarray
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.calc_diskmodel(slashdate, nbands, freq, defaultfreq)[source]
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.writediskxml(dsize, fdens, freq, xmlfile='SOLDISK.xml')[source]
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.gaussian2d(x, y, amplitude, x0, y0, sigma_x, sigma_y, theta)[source]
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.image_adddisk(eofile, diskinfo, edgeconvmode='frommergeddisk', caltbonly=False, bmfactor=2.0, overwrite=True)[source]
- Parameters:
eofile – input image FITS file
diskinfo – disk information file
edgeconvmode – edge convolve mode, ‘frommergeddisk’ or ‘frombeam’
caltbonly – calculate the Tb of the disk and return the value
bmfactor – factor to multiply the beam major and minor axes to get the sigma of the Gaussian kernel
overwrite – whether to overwrite the output fits file if it already exists
- Returns:
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.mk_diskmodel(outname='disk', direction='J2000 10h00m00.0s 20d00m00.0s', reffreq='2.8GHz', flux=660000.0, eqradius='16.166arcmin', polradius='16.166arcmin', pangle='21.1deg', overwrite=True)[source]
Create a blank solar disk model image (or optionally a data cube) outname String to use for part of the image and fits file names (default ‘disk’) direction String specifying the position of the Sun in RA and Dec. Default
means use the standard string “J2000 10h00m00.0s 20d00m00.0s”
- reffreq The reference frequency to use for the disk model (the frequency at which
the flux level applies). Default is ‘2.8GHz’.
flux The flux density, in Jy, for the entire disk. Default is 66 sfu. eqradius The equatorial radius of the disk. Default is
16 arcmin + 10” (for typical extension of the radio limb)
- polradius The polar radius of the disk. Default is
16 arcmin + 10” (for typical extension of the radio limb)
- pangle The solar P-angle (geographic position of the N-pole of the Sun) in
degrees E of N. This only matters if eqradius != polradius
- index The spectral index to use at other frequencies. Default None means
use a constant flux density for all frequencies.
- cell The cell size (assumed square) to use for the image. The image size
is determined from a standard radius of 960” for the Sun, divided by cell size, increased to nearest power of 512 pixels. The default is ‘2.0arcsec’, which results in an image size of 1024 x 1024.
- Note that the frequency increment used is ‘325MHz’, which is the width of EOVSA bands
(not the width of individual science channels)
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.insertdiskmodel(vis, sizescale=1.0, fdens=None, dsize=None, xmlfile='SOLDISK.xml', writediskinfoonly=False, active=False, overwrite=False)[source]
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.uvrange_uplim_from_freq(x, x0, x1, y0, y1)[source]
Calculate the upper limit of the UV range from frequency using linear interpolation.
- Parameters:
x (float) – The frequency for which the UV range upper limit is calculated.
x0 (float) – The start frequency of the interpolation range.
x1 (float) – The end frequency of the interpolation range.
y0 (float) – The UV range upper limit at the start frequency.
y1 (float) – The UV range upper limit at the end frequency.
- Returns:
The calculated UV range upper limit for the given frequency.
- Return type:
float
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.disk_slfcal(msfile, tbg, ted, disk_params, workdir='./', overwrite=True, iterbands=False)[source]
Perform disk self-calibration on measurement set data.
- Parameters:
msfile (str) – The measurement set file to be calibrated.
tbg (datetime) – The beginning time of the calibration range.
ted (datetime) – The end time of the calibration range.
disk_params (dict) – A dictionary containing disk model parameters.
iterbands (bool) – Boolean flag to run gaincal iterating over frequency bands, defaults to False. iterbands = True is only useful when uvrange_uplim is used, which is currently not implemented.
- Returns:
The filepath of the self-calibrated measurement set.
- Return type:
str
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.shift_corr(mmsfiles, trange_series, spws, imagemodel, imagemodel_fits, reftime_master, workdir='./', pols='XX', overwrite=False, do_featureslfcal=False, do_diskslfcal=True, disk_params={}, do_sbdcal=True, verbose=True)[source]
Corrects smearing effects in solar observation data by aligning them with a model image.
- Parameters:
mmsfiles (list of str) – Paths to the measurement set files to be corrected.
trange_series (list of tuple) – Each tuple contains start and end times for the measurement set files.
spws (list of string) – Spectral window indices to be considered.
imagemodel (str) – Path to the model image in CASA measurement set format.
imagemodel_fits (str) – Path to the model image in FITS format.
reftime_master (astropy.time.Time) – Reference time for the rotation of the model image.
workdir (str) – Working directory for output files, defaults to ‘./’.
do_featureslfcal (bool) – Boolean flag to perform feature self-calibration, defaults to False.
pols (str) – Polarization types to be considered, defaults to ‘XX’.
overwrite (bool) – Boolean flag to overwrite existing files, defaults to False.
do_diskslfcal (bool) – Boolean flag to perform disk self-calibration, defaults to True.
disk_params (dict) – Dictionary containing parameters for disk self-calibration.
do_sbdcal (bool) – Boolean flag to perform single-band delay calibration, defaults to True.
verbose (bool) – Boolean flag to enable verbose output, defaults to True.
- Returns:
Paths to the corrected measurement set files.
- Return type:
list of str
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.split_mms(msname, timerange_series, spw='', workdir='./', overwrite=False, verbose=True)[source]
Splits a measurement set into multiple subsets based on specified time ranges.
- Parameters:
msname (str) – Path to the original measurement set.
timerange_series (list of tuple) – Time ranges for each split, with each tuple containing start and end datetime objects.
spw (str) – Spectral window specification for the splitting process, defaults to ‘’.
workdir (str) – Target directory for saving the split measurement sets, defaults to ‘./’.
overwrite (bool) – Boolean flag to overwrite existing files, defaults to False.
verbose (bool) – Boolean flag to enable verbose output, defaults to True.
- Returns:
Paths to the created split measurement sets, corresponding to each specified time range.
- Return type:
list of str
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.ant_trange(vis)[source]
Figure out nominal times for tracking of old EOVSA antennas, and return time range in CASA format
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.format_spw(spw)[source]
Formats the spectral window (spw) string for file naming, ensuring start and end values are separated by a dash and zero-padded to two digits.
- Parameters:
spw (str) – The spectral window in the format “start~end”, where start and end are integers.
- Returns:
A formatted string with start and end values zero-padded to two digits, separated by a dash.
- Return type:
str
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.rm_imname_extensions(imname, keep_ext=[], verbose=False)[source]
Remove directories and files that match the base image name (imname) with specific extensions.
- Parameters:
imname (str) – The base name of images/directories to remove specific extensions for.
keep_ext (list) – A list of extensions to keep. Default is an empty list.
verbose (bool) – If True, print detailed information about the removal process. Default is False.
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.check_image_zeros(imname)[source]
Check if the image contains non-zero data.
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.run_tclean_automasking(vis, sp, trange, uvrange, datacolumn, imname, imsize, cell, stokes, scales, niter, reffreq, pbcor, savemodel, usemask, restoringbeam, sidelobethreshold, noisethreshold, lownoisethreshold, minbeamfrac, negativethreshold, growiterations)[source]
Wrapper function for the tclean task in CASA.
- Parameters:
vis (str) – Name of the visibility data set to be imaged.
sp (str) – Spectral window selection.
trange (str) – Time range selection.
uvrange (str) – UV range selection.
datacolumn (str) – Specifies which data column to use.
imname (str) – Name of the output image.
imsize (list) – Image size in pixels.
cell (list) – Cell size specification.
stokes (str) – Stokes parameters to image.
scales (list) – Scales for multi-scale clean.
niter (int) – Maximum number of iterations.
reffreq (float) – Reference frequency for the image.
pbcor (bool) – Specifies whether to perform primary beam correction.
savemodel (str) – Specifies whether to save the model.
usemask (bool) – Specifies whether to use auto-masking.
restoringbeam (list) – Restoring beam parameters.
sidelobethreshold (float) – Side lobe threshold for auto-masking.
noisethreshold (float) – Noise threshold for auto-masking.
lownoisethreshold (float) – Low noise threshold for auto-masking.
negativethreshold (float) – Negative threshold for auto-masking.
growiterations (int) – Number of grow iterations for auto-masking.
- class suncasa.eovsa.eovsa_synoptic_imaging_pipeline.FrequencySetup(tim=None)[source]
Manages frequency setup based on observation date for radio astronomy imaging.
This class is initialized with an observation time and calculates essential frequency parameters such as effective observing frequencies (eofreq) and spectral windows (spws) based on the observation date. It provides methods to calculate reference frequency and bandwidth for given spectral windows.
- Parameters:
tim (astropy.time.Time) – Observation time used to determine the frequency setup.
Attributes: - tim (astropy.time.Time): The observation time. - spw2band (numpy.ndarray): An array mapping spectral window indices to band numbers. - bandwidth (float): The bandwidth in GHz. - defaultfreq (numpy.ndarray): The default effective observing frequencies in GHz. - nbands (int): Number of bands. - eofreq (numpy.ndarray): Effective observing frequencies based on the observation time. - spws (list of str): Spectral window selections based on the observation time.
- Example:
>>> from astropy.time import Time >>> tim = Time('2022-01-01T00:00:00', format='isot') >>> freq_setup = FrequencySetup(tim) >>> crval, cdelt = freq_setup.get_reffreq_and_cdelt('5~10') >>> print(crval, cdelt)
- get_reffreq_and_cdelt(spw)[source]
Calculates the reference frequency (CRVAL) and the frequency delta (CDELT) for a given spectral window range.
This method takes a spectral window selection and computes the mean of the effective observing frequencies (eofreq) within that range as the reference frequency. It also calculates the bandwidth covered by the spectral window range as the frequency delta.
- Parameters:
spw (str) – Spectral window selection, specified as a range ‘start~end’ or a single value.
- Returns:
A tuple containing the reference frequency and frequency delta, both in GHz.
- Return type:
(str, str)
- Example:
>>> crval, cdelt = freq_setup.get_reffreq_and_cdelt('5~10') >>> print(crval, cdelt)
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.fd_images(vis, cleanup=False, image_marker='', timerange='', niter=None, cell=['2.5arcsec'], imsize=[1024], spws=['0~1', '2~4', '5~10', '11~20', '21~30', '31~43'], imgoutdir='./', bright=None, stokes='XX', uvrange='', toTb=True, pbcor=True, datacolumn='data', savemodel='none', usemask='auto-multithresh', overwrite=False, compress=False, dryrun=False)[source]
Generates full-disk images, optionally cleans up interim images, and performs image registration.
This function creates full-disk solar images based on visibility data, performs an optional cleanup of interim images, and aligns the resulting images to a standard solar disk model. It supports dynamic image size, cell size, and spectral window (SPW) selection. The function also handles the creation of FITS files from the generated images, ensuring the reference frequency in the FITS header is calculated as the middle of the selected frequency range.
- Parameters:
vis (str) – Path to the visibility data.
cleanup (bool) – If True, deletes interim images after processing. Default is False.
image_marker (str) – Additional identifier for the image name. Default is ‘’.
timerange (str) – Range of time to select from data. Default is ‘’.
niter (int) – Number of iterations for the cleaning algorithm. If None, defaults to 5000.
cell (list) – Size of the image cell, e.g., [‘2.5arcsec’].
imsize (list) – Dimensions of the output image, e.g., [1024].
spws (list) – Spectral windows to process, specified as ranges, e.g., [‘0~1’, ‘2~5’].
imgoutdir (str) – Output directory for the resulting images and FITS files. Defaults to ‘./’.
bright (list) – Flags to indicate brightness processing per SPW. Defaults to all True.
stokes (str) – Stokes parameter to use. Default is “XX”.
uvrange (str) – UV range to select from data. Default is ‘’.
toTb (bool) – If True, converts image to temperature scale. Default is True.
pbcor (bool) – If True, applies primary beam correction. Default is True.
datacolumn (str) – Data column to use from the visibility data. Default is ‘data’.
savemodel (str) – Options for saving the model visibilities. Choices are ‘none’, ‘virtual’, and ‘modelcolumn’. Default is ‘none’.
overwrite (bool) – If True, overwrites existing FITS files. Default is False.
dryrun (bool) – If True, only returns the paths to the generated images. No actual image processing is performed. Default is False.
- Returns:
A tuple containing two lists: paths to the generated FITS files and paths to the CASA image files.
- Return type:
(list of str, list of str)
Note
1. The reference frequency in the FITS header is calculated as the middle of the selected frequency range. This ensures accurate representation of the frequency information in the generated images. 2. The function internally manages directory creation for images, applies multiscale cleaning based on initial beam size determination, and uses default or specified scales for image cleaning. Errors in beam size determination lead to fallback on default scales. The function finally aligns and converts the images to FITS format, with options for temperature scale conversion and phase center alignment.
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.merge_FITSfiles(fitsfilesin, outfits, exptime_weight=False, snr_weight=None, deselect_index=None, suppress_ondiskres=False, suppress_thrshd=0.3, overwrite=True)[source]
Merges multiple FITS files into a single output file by calculating the mean of stacked data.
This function stacks the data from a list of input FITS files along a new axis, optionally applying exposure time weighting and suppression of on-disk residuals based on a threshold relative to the disk brightness temperature. The mean of the stacked data is then written to a specified output FITS file.
- Parameters:
fitsfilesin (list of str) – List of file paths to the input FITS files to be merged.
outfits (str) – File path for the output FITS file where the merged data will be saved.
exptime_weight (bool, optional) – If True, the exposure time is used as a weight for calculating the mean of the stacked data. Defaults to False.
snr_weight (list of float, optional) – List of signal-to-noise ratios (SNRs) to use as weights for calculating the mean of the stacked data. If both exposure time and SNR weights are provided, the weights will be the product of the two. Defaults to None.
deselect_index (list of int, optional) – index of the images to be deselected. Defaults to None.
suppress_ondiskres (bool, optional) – If True, suppresses on-disk residuals based on suppress_thrshd. Defaults to False.
suppress_thrshd (float, optional) – Threshold for suppression of on-disk residuals, expressed as a fraction of the disk brightness temperature. May suppress weak but real emission. Defaults to 0.3.
overwrite (bool, optional) – If True, the output file is overwritten if it already exists. Defaults to True.
- Raises:
ValueError – If any of the input FITS files cannot be read.
- Return type:
None
Notes
The suppression of on-disk residuals is achieved by applying a sigmoid function to pixels within a specified range of the disk brightness temperature, effectively reducing the contribution of residuals while preserving the overall structure.
Examples
Merge three FITS files without exposure time weighting and with on-disk residual suppression:
>>> merge_FITSfiles(['sun_01.fits', 'sun_02.fits', 'sun_03.fits'], 'sun_merged.fits', ... exptime_weight=False, suppress_ondiskres=True, suppress_thrshd=0.3, overwrite=True)
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.process_time_block(tidx_ted_tbg, msfile_in, msname, subdir, total_blocks, tdt, tdtstr, spws, niter_init, reftime_master, do_diskslfcal, disk_params, pols='XX', do_sbdcal=False, overwrite=False)[source]
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.process_imaging_timerange(tidx_ted_tbg, msfile_in, spws, subdir, overwrite)[source]
- suncasa.eovsa.eovsa_synoptic_imaging_pipeline.pipeline_run(vis, outputvis='', workdir=None, slfcaltbdir=None, imgoutdir=None, figoutdir=None, clearcache=False, clearlargecache=False, pols='XX', mergeFITSonly=False, verbose=True, do_diskslfcal=True, overwrite=False, niter_init=200, ncpu='auto', tr_series_imaging=None, spws_imaging=None, hanning=False, do_sbdcal=False)[source]
Executes the EOVSA data processing pipeline for solar observation data.
- Parameters:
vis (str) – Path to the input measurement set (MS) data.
outputvis (str, optional) – Output path for the processed MS, defaults to an empty string.
workdir (str, optional) – Working directory for intermediate data, defaults to None which sets it to ‘/data1/workdir’.
slfcaltbdir (str, optional) – Directory for storing calibration tables, defaults to None.
imgoutdir (str, optional) – Output directory for image files, defaults to None.
figoutdir (str, optional) – Output directory for figures, defaults to None.
clearcache (bool, optional) – If True, clears all cache files after processing, defaults to False.
clearlargecache (bool, optional) – If True, clears the large cache after processing, defaults to False. If True, clearcache is ignored.
pols (str, optional) – Polarization types to process, defaults to ‘XX’.
mergeFITSonly (bool, optional) – If True, skips processing and only merges FITS files, defaults to False.
verbose (bool, optional) – Enables verbose output during processing, defaults to True.
do_diskslfcal (bool, optional) – If True, performs disk self-calibration, defaults to True.
overwrite (bool, optional) – If True, overwrites existing files, defaults to False.
niter_init (int, optional) – Initial number of iterations for imaging, defaults to 200.
ncpu (str or int, optional) – Specifies the number of CPUs for parallel processing, defaults to ‘auto’.
tr_series_imaging (list of tuple, optional) – Time ranges for imaging, defaults to None.
spws_imaging (list of str, optional) – Spectral windows selected for imaging, defaults to None.
hanning (bool, optional) – If True, applies Hanning smoothing to the data, defaults to False.
do_sbdcal (bool) – Boolean flag to perform single-band delay calibration, defaults to False.
- Returns:
Path to the processed visibility data.
- Return type:
str
- Example:
## if you want to specify the spectral windows for imaging >>> spws_imaging = [‘5~10’, ‘11~20’, ‘21~30’] ## if you want to specify the time range for imaging >>> from datetime import datetime, timedelta >>> from suncasa.eovsa import eovsa_synoptic_imaging_pipeline as esip >>> tbg_imaging = datetime(2024, 4, 8, 16, 58, 0) >>> ted_imaging = datetime(2024, 4, 8, 19, 00, 0) >>> tdt_imaging = timedelta(minutes=2) >>> tr_series_imaging = esip.generate_trange_series(tbg_imaging, ted_imaging, tdt_imaging)