Reading in and writing out observations

Loading SDFITS files

Classes and functions for importing SDFITS files

SDFITSLoad

Load generic SDFITS files - Not typically used directly. Sub-class for specific telescope SDFITS flavors.

class dysh.fits.sdfitsload.SDFITSLoad(filename, source=None, hdu=None, **kwargs)[source]

Bases: object

Generic Container for a bintable(s) from selected HDU(s) for a single SDFITS file. For multiple SDFITS files, see GBTFITSLoad.

Parameters:

filenamestr: input file name
sourcestr: target source to select from input file. Default: all sources
hduint or list: Header Data Unit to select from input file. Default: all HDUs

Attributes:

bintable: The list of bintables
filename: The input SDFITS filename

Methods

`binheader`()	The list of bintable headers
`create_index`([hdu])	Create the index of the SDFITS file.
`fix_meta`(meta)	Do any repair to the meta/header for peculariaties in definitions from a particular observatory The passed-in dictionary will be repaired in place.
`getrow`(i[, bintable])	Get a FITS_record from the input bintable
`getspec`(i[, bintable, observer_location])	Get a row (record) as a Spectrum
`index`([hdu, bintable])	Return The index table.
`info`()	Return the `HDUList` info()
`load`([hdu])	Load the bintable for given hdu.
`naxis`(naxis, bintable)	The NAXISn value of the input bintable.
`nchan`(bintable)	The number of channels per row of the input bintable.
`nintegrations`(bintable[, source])	The number of integrations on a given source divided by the number of polarizations
`npol`(bintable)	The number of polarizations present in the input bintable.
`nrows`(bintable)	The number of rows of the input bintable
`rawspectra`(bintable)	Get the raw (unprocessed) spectra from the input bintable.
`rawspectrum`(i[, bintable])	Get a single raw (unprocessed) spectrum from the input bintable.
`scans`(bintable)	The number of scans resent in the input bintable.
`sources`(bintable)	The number of sources present in the input bintable.
`summary`()	Print a summary of each record of the data
`udata`(key[, bintable])	The unique list of values of a given header keyword
`ushow`(key[, bintable])	Print the unique list of values of a given header keyword
`velocity_convention`(veldef, velframe)	Compute the velocity convention string use for velocity conversions, given the VELDEF and VELFRAME values.
`write`(fileobj[, rows, bintable, ...])	Write the `SDFITSLoad` to a new file, potentially sub-selecting rows or bintables.

add_primary_hdu

add_primary_hdu()[source]

binheader()[source]: The list of bintable headers

property bintable: The list of bintables

create_index(hdu=None)[source]

Create the index of the SDFITS file.

Parameters:

hduint or list: Header Data Unit to select from input file. Default: all HDUs

property filename: The input SDFITS filename

fix_meta(meta)[source]

Do any repair to the meta/header for peculariaties in definitions from a particular observatory The passed-in dictionary will be repaired in place. At minimum this method must populate meta[‘VELDEF’] and meta[‘VELFRAME’]

Parameters:

metadict: The header of the Spectrum to be fixed, corresponding to the meta attribute of the Spectrum.

getrow(i, bintable=0)[source]

Get a FITS_record from the input bintable

Parameters:

iint: The record (row) index to retrieve
bintableint: The index of the bintable attribute

Returns:

rowFITS_record: The i-th record of the input bintable

getspec(i, bintable=0, observer_location=None)[source]

Get a row (record) as a Spectrum

Parameters:

iint: The record (row) index to retrieve
bintableint, optional: The index of the bintable attribute. default is 0.
observer_locationEarthLocation: Location of the observatory. See Observatory. This will be transformed to ITRS using the time of observation DATE-OBS or MJD-OBS in the SDFITS header. The default is None.

Returns:

sSpectrum: The Spectrum object representing the data row.

index(hdu=None, bintable=None)[source]

Return The index table.

Parameters:

hduint or list: Header Data Unit to select from the index. Default: all HDUs
bintableint: The index of the bintable attribute, None means all bintables

Returns:

index~pandas.DataFrame: The index of this SDFITS file

info()[source]: Return the HDUList info()

load(hdu=None, **kwargs)[source]

Load the bintable for given hdu. Note mmHg and UTC are unrecognized units. mmHg is in astropy.units.cds but UTC is just wrong.

Parameters:

hduint or list: Header Data Unit to select from input file. Default: all HDUs

naxis(naxis, bintable)[source]

The NAXISn value of the input bintable.

Parameters:

naxisint: The NAXIS whose length is requested
bintableint: The index of the bintable attribute

Returns:

naxisthe length of the NAXIS

nchan(bintable)[source]

The number of channels per row of the input bintable. Assumes all rows have same length.

Parameters:

bintableint: The index of the bintable attribute

Returns:

nchanint: Number channels in the first spectrum of the input bintbale

nintegrations(bintable, source=None)[source]

The number of integrations on a given source divided by the number of polarizations

Parameters:

bintableint: The index of the bintable attribute
source: str: The source name (OBJECT keyword) or None for all sources. Default: None

Returns:

nintegrationsthe number of integrations

npol(bintable)[source]

The number of polarizations present in the input bintable.

Parameters:

bintableint: The index of the bintable attribute

Returns:

npol: int: Number of polarizations as given by CRVAL4 FITS header keyword.

nrows(bintable)[source]

The number of rows of the input bintable

Parameters:

bintableint: The index of the bintable attribute

Returns:

nrowsint: Number of rows, i.e., the length of the input bintable

rawspectra(bintable)[source]

Get the raw (unprocessed) spectra from the input bintable.

Parameters:

bintableint: The index of the bintable attribute

Returns:

rawspectra~numpy.ndarray: The DATA column of the input bintable

rawspectrum(i, bintable=0)[source]

Get a single raw (unprocessed) spectrum from the input bintable.

Parameters:

iint: The row index to retrieve.
bintableint or None: The index of the bintable attribute. If None, the underlying bintable is computed from i

Returns:

rawspectrum~numpy.ndarray: The i-th row of DATA column of the input bintable

scans(bintable)[source]

The number of scans resent in the input bintable. TODO: move this to GBTFISLoad?

Parameters:

bintableint: The index of the bintable attribute

Returns:

scans: int: Number of scans as given by SCAN FITS header keyword.

sources(bintable)[source]

The number of sources present in the input bintable.

Parameters:

bintableint: The index of the bintable attribute

Returns:

sources: int: Number of sources as given by OBJECT FITS header keyword.

summary()[source]: Print a summary of each record of the data

udata(key, bintable=None)[source]

The unique list of values of a given header keyword

Parameters:

keystr: The keyword to retrieve
bintableint: The index of the bintable attribute, None means all bintables

Returns:

udatalist: The unique set of values for the input keyword.

ushow(key, bintable=None)[source]

Print the unique list of values of a given header keyword

Parameters:

keystr: The keyword to retrieve
bintableint: The index of the bintable attribute, None means all bintables

velocity_convention(veldef, velframe)[source]

Compute the velocity convention string use for velocity conversions, given the VELDEF and VELFRAME values. Return value must be a recognized string of Spectrum1D, one of {“doppler_relativistic”, “doppler_optical”, “doppler_radio”} Sub-classes should implement, because different observatories use VELDEF and VELFRAME inconsistently. This base class method hard-coded to return “doppler_radio.”

Parameters:

veldefstr: The velocity definition string (VELDEF FITS keyword)
velframestr: The velocity frame string (VELFRAME FITS keyword)

write(fileobj, rows=None, bintable=None, output_verify='exception', overwrite=False, checksum=False)[source]

Write the SDFITSLoad to a new file, potentially sub-selecting rows or bintables.

Parameters:

fileobjstr, file-like or pathlib.Path: File to write to. If a file object, must be opened in a writeable mode.
rows: int or list-like: Range of rows in the bintable(s) to write out. e.g. 0, [14,25,32]. Default: None, meaning all rows Note: Currently rows, if given, must be contained in a single bintable and bintable must be given
bintableint: The index of the bintable attribute or None for all bintables. Default: None
output_verifystr: Output verification option. Must be one of "fix", "silentfix", "ignore", "warn", or "exception". May also be any combination of "fix" or "silentfix" with "+ignore", +warn, or +exception" (e.g. ``"fix+warn"). See https://docs.astropy.org/en/latest/io/fits/api/verification.html for more info
overwritebool, optional: If True, overwrite the output file if it exists. Raises an OSError if False and the output file exists. Default is False.
checksumbool: When True adds both DATASUM and CHECKSUM cards to the headers of all HDU’s written to the file.

GBTFITSLoad

Load SDFITS files produced by the Green Bank Telescope

class dysh.fits.gbtfitsload.GBTFITSLoad(fileobj, source=None, hdu=None, **kwargs)[source]

Bases: SDFITSLoad

GBT-specific container to reprensent one or more SDFITS files

Parameters:

fileobjstr or pathlib.Path: File to read or directory path. If a directory, all FITS files within will be read in.
sourcestr: target source to select from input file(s). Default: all sources
hduint or list: Header Data Unit to select from input file. Default: all HDUs

Attributes:

bintable: The list of bintables
filename: The input SDFITS filename
files: The list of SDFITS file(s) that make up this GBTFITSLoad object
final_selection: The merged selection rules in the Selection object.
selection: The data selection object

Methods

`binheader`()	The list of bintable headers
`calonoff_rows`([scans, bintable, fitsindex])	Get individual scan row numbers sorted by whether the calibration (diode) was on or off, and selected by ifnum,plnum, fdnum,subref,bintable.
`create_index`([hdu])	Create the index of the SDFITS file.
`fix_meta`(meta)	Do any repair to the meta/header for peculariaties in definitions from a particular observatory The passed-in dictionary will be repaired in place.
`getfs`([calibrate, fold, use_sig, ...])	Retrieve and calibrate frequency-switched data.
`getps`([calibrate, timeaverage, polaverage, ...])	Retrieve and calibrate position-switched data.
`getrow`(i[, bintable])	Get a FITS_record from the input bintable
`getspec`(i[, bintable, observer_location, ...])	Get a row (record) as a Spectrum
`gettp`([sig, cal, calibrate, timeaverage, ...])	Get a total power scan, optionally calibrating it.
`index`([hdu, bintable, fitsindex])	Return The index table
`info`()	Return information on the HDUs contained in this object. See :meth:`~astropy.HDUList/info().
`load`([hdu])	Load the bintable for given hdu.
`naxis`(naxis, bintable)	The NAXISn value of the input bintable.
`nchan`(bintable)	The number of channels per row of the input bintable.
`nintegrations`(bintable[, source])	The number of integrations on a given source divided by the number of polarizations
`npol`(bintable)	The number of polarizations present in the input bintable.
`nrows`(bintable)	The number of rows of the input bintable
`onoff_rows`([scans, ifnum, plnum, bintable, ...])	Get individual ON/OFF (position switch) scan row numbers selected by ifnum,plnum, bintable.
`onoff_scan_list`([scans, ifnum, plnum, ...])	Get the scans for position-switch data sorted
`rawspectra`(bintable, fitsindex)	Get the raw (unprocessed) spectra from the input bintable.
`rawspectrum`(i[, bintable, fitsindex])	Get a single raw (unprocessed) spectrum from the input bintable.
`scan_rows`(scans[, ifnum, plnum, bintable, ...])	Get scan rows selected by ifnum,plnum, bintable.
`scans`(bintable)	The number of scans resent in the input bintable.
`select`([tag])	Add one or more exact selection rules, e.g., `key1 = value1, key2 = value2, ...` If `value` is array-like then a match to any of the array members will be selected.
`select_channel`(chan[, tag])	Select channels and/or channel ranges.
`select_range`([tag])	Select a range of inclusive values for a given key(s).
`select_within`([tag])	Select a value within a plus or minus for a given key(s).
`sources`(bintable)	The number of sources present in the input bintable.
`subbeamnod`([method, sig, cal, calibrate, ...])	Get a subbeam nod power scan, optionally calibrating it.
`summary`([scans, verbose, show_index])	Create a summary list of the input dataset.
`udata`(key[, bintable])	The unique list of values of a given header keyword
`ushow`(key[, bintable])	Print the unique list of values of a given header keyword
`velocity_convention`(veldef)	Given the GBT VELDEF FITS string return the specutils velocity convention, e.g., "doppler_radio"
`velocity_frame`(veldef)	Given the GBT VELDEF FITS string return the velocity frame, e.g., "heliocentric".
`write`(fileobj[, rows, bintable, ...])	Write the `SDFITSLoad` to a new file, potentially sub-selecting rows or bintables.
`write_scans`(fileobj, scans[, output_verify, ...])	Write specific scans of the `GBTFITSLoad` to a new file.

add_primary_hdu
select_track

calonoff_rows(scans=None, bintable=None, fitsindex=0, **kwargs)[source]

Get individual scan row numbers sorted by whether the calibration (diode) was on or off, and selected by ifnum,plnum, fdnum,subref,bintable.

Parameters:

scansint or list-like: The scan numbers to find the rows of
ifnumint: the IF index
plnumint: the polarization index
fdnumint: the feed index
subrefint: the subreflector state (-1,0,1)
bintableint: the index for BINTABLE containing the scans
fitsindex: int: the index of the FITS file contained in this GBTFITSLoad. Default:0

Returns:

rowsdict: A dictionary with keys ‘ON’ and ‘OFF’ giving the row indices of CALON and CALOFF data for the input scan(s)

property files

The list of SDFITS file(s) that make up this GBTFITSLoad object

Returns:

fileslist: list of PosixPath objects

property final_selection

The merged selection rules in the Selection object. See final()

Returns:

~pandas.DataFrame: The final merged selection

getfs(calibrate=True, fold=True, use_sig=True, timeaverage=True, polaverage=False, weights='tsys', bintable=None, observer_location=<EarthLocation (882593.9465029, -4924896.36541728, 3943748.74743984) m>, **kwargs)[source]

Retrieve and calibrate frequency-switched data.

Parameters:

calibrateboolean, optional: Calibrate the scans. The default is True.
foldboolean, optional: Fold the sig and ref scans. The default is True.
use_sigboolean, optional: Return the sig or ref based spectrum. This applies to both the folded and unfolded option. The default is True. NOT IMPLEMENTED YET
timeaverageboolean, optional: Average the scans in time. The default is True.
polaverageboolean, optional: Average the scans in polarization. The default is False.
weightsstr or None, optional: How to weight the spectral data when averaging. tsys means use system temperature weighting (see e.g., timeaverage()); None means uniform weighting. The default is “tsys”.
fold: boolean, optional: The default is True
bintableint, optional: Limit to the input binary table index. The default is None which means use all binary tables.
observer_locationEarthLocation: Location of the observatory. See Observatory. This will be transformed to ITRS using the time of observation DATE-OBS or MJD-OBS in the SDFITS header. The default is the location of the GBT.
**kwargsdict: Optional additional selection (only?) keyword arguments, typically given as key=value, though a dictionary works too. e.g., ifnum=1, plnum=[2,3] etc.

Returns:

scanblockScanBlock: ScanBlock containing the individual `~spectra.scan.FSScan`s

Raises:

Exception: If no scans matching the selection criteria are found.

getps(calibrate=True, timeaverage=True, polaverage=False, weights='tsys', bintable=None, **kwargs)[source]

Retrieve and calibrate position-switched data.

Parameters:

calibrateboolean, optional: Calibrate the scans. The default is True.
timeaverageboolean, optional: Average the scans in time. The default is True.
polaverageboolean, optional: Average the scans in polarization. The default is False.
weightsstr or None, optional: How to weight the spectral data when averaging. tsys means use system temperature weighting (see e.g., timeaverage()); None means uniform weighting. The default is “tsys”.
bintableint, optional: Limit to the input binary table index. The default is None which means use all binary tables. (This keyword should eventually go away)
**kwargsdict: Optional additional selection (only?) keyword arguments, typically given as key=value, though a dictionary works too. e.g., ifnum=1, plnum=[2,3] etc.

Returns:

scanblockScanBlock: ScanBlock containing the individual `~spectra.scan.PSScan`s

Raises:

Exception: If scans matching the selection criteria are not found.

getspec(i, bintable=0, observer_location=<EarthLocation (882593.9465029, -4924896.36541728, 3943748.74743984) m>, fitsindex=0)[source]

Get a row (record) as a Spectrum

Parameters:

iint: The record (row) index to retrieve
bintableint, optional: The index of the bintable attribute. default is 0.
observer_locationEarthLocation: Location of the observatory. See Observatory. This will be transformed to ITRS using the time of observation DATE-OBS or MJD-OBS in the SDFITS header. The default is the location of the GBT.
fitsindex: int: the index of the FITS file contained in this GBTFITSLoad. Default:0
Returns
——-
sSpectrum: The Spectrum object representing the data row.

gettp(sig=None, cal=None, calibrate=True, timeaverage=True, polaverage=False, weights='tsys', bintable=None, **kwargs)[source]

Get a total power scan, optionally calibrating it.

Parameters:

sigbool or None: True to use only integrations where signal state is True, False to use reference state (signal state is False). None to use all integrations.
cal: bool or None: True to use only integrations where calibration (diode) is on, False if off. None to use all integrations regardless calibration state. The system temperature will be calculated from both states regardless of the value of this variable.
calibrate: bool: whether or not to calibrate the data. If True, the data will be (calon - caloff)*0.5, otherwise it will be SDFITS row data. Default:True
timeaverageboolean, optional: Average the scans in time. The default is True.
polaverageboolean, optional: Average the scans in polarization. The default is False.
weights: str or None: None or ‘tsys’ to indicate equal weighting or tsys weighting to use in time averaging. Default: ‘tsys’
bintableint, optional: Limit to the input binary table index. The default is None which means use all binary tables.
**kwargsdict: Optional additional selection (only?) keyword arguments, typically given as key=value, though a dictionary works too. e.g., ifnum=1, plnum=[2,3] etc.

Returns:

dataScanBlock: A ScanBlock containing one or more TPScan

index(hdu=None, bintable=None, fitsindex=None)[source]

Return The index table

Parameters:

hduint or list: Header Data Unit to select from the index. Default: all HDUs
bintableint: The index of the bintable attribute, None means all bintables
fitsindex: int: The index of the FITS file contained in this GBTFITSLoad. Default:None meaning return one index over all files.

Returns:

index~pandas.DataFrame: The index of this GBTFITSLoad

info()[source]: Return information on the HDUs contained in this object. See :meth:`~astropy.HDUList/info()

onoff_rows(scans=None, ifnum=0, plnum=0, bintable=None, fitsindex=0)[source]

Get individual ON/OFF (position switch) scan row numbers selected by ifnum,plnum, bintable.

Parameters:

scansint or list-like: The scan numbers to find the rows of
ifnumint: the IF index
plnumint: the polarization index
bintableint: the index for BINTABLE in sdfits containing the scans
fitsindex: int: the index of the FITS file contained in this GBTFITSLoad. Default:0

Returns:

rowsdict: A dictionary with keys ‘ON’ and ‘OFF’ giving the row indices of the ON and OFF data for the input scan(s)

onoff_scan_list(scans=None, ifnum=0, plnum=0, bintable=None, fitsindex=0)[source]

Get the scans for position-switch data sorted: by ON and OFF state

Parameters:

scansint or list-like: The scan numbers to find the rows of
ifnumint: the IF index
plnumint: the polarization index

Returns:

rowsdict: A dictionary with keys ‘ON’ and ‘OFF’ giving the scan numbers of ON and OFF data for the input scan(s)

rawspectra(bintable, fitsindex)[source]

Get the raw (unprocessed) spectra from the input bintable.

Parameters:

bintableint: The index of the bintable attribute
fitsindex: int: the index of the FITS file contained in this GBTFITSLoad. Default:0

Returns:

rawspectra~numpy.ndarray: The DATA column of the input bintable

rawspectrum(i, bintable=0, fitsindex=0)[source]

Get a single raw (unprocessed) spectrum from the input bintable.

Parameters:

iint: The row index to retrieve.
bintableint or None: The index of the bintable attribute. If None, the underlying bintable is computed from i
fitsindex: int: the index of the FITS file contained in this GBTFITSLoad. Default:0

Returns:

rawspectrum~numpy.ndarray: The i-th row of DATA column of the input bintable

scan_rows(scans, ifnum=0, plnum=0, bintable=None, fitsindex=0)[source]

Get scan rows selected by ifnum,plnum, bintable.

Parameters:

scansint or list-like: The scan numbers to find the rows of
ifnumint: the IF index
plnumint: the polarization index
bintableint: the index for BINTABLE in sdfits containing the scans. Default:None
fitsindex: int: the index of the FITS file contained in this GBTFITSLoad. Default:0

Returns:

rowslist: Lists of the rows in each bintable that contain the scans. Index of rows is the bintable index number

select(tag=None, **kwargs)[source]

Add one or more exact selection rules, e.g., key1 = value1, key2 = value2, ... If value is array-like then a match to any of the array members will be selected. For instance select(object=['3C273', 'NGC1234']) will select data for either of those objects and select(ifnum=[0,2]) will select IF number 0 or IF number 2. See Selection.

Parameters:

tagstr: An identifying tag by which the rule may be referred to later. If None, a randomly generated tag will be created.
keystr: The key (SDFITS column name or other supported key)
valueany: The value to select

select_channel(chan, tag=None)[source]

Select channels and/or channel ranges. These are NOT used in final() but rather will be used to create a mask for calibration or flagging. Single arrays/tuples will be treated as channel lists; nested arrays will be treated as ranges, for instance

`` # selects channels 1 and 10 select_channel([1,10]) # selects channels 1 thru 10 inclusive select_channel([[1,10]]) # select channel ranges 1 thru 10 and 47 thru 56 inclusive, and channel 75 select_channel([[1,10], [47,56], 75)]) # tuples also work, though can be harder for a human to read select_channel(((1,10), [47,56], 75)) ``

See Selection.

Parameters:

channumber, or array-like: The channels to select

Returns:

None.

select_range(tag=None, **kwargs)[source]

Select a range of inclusive values for a given key(s). e.g., key1 = (v1,v2), key2 = (v3,v4), ... will select data v1 <= data1 <= v2, v3 <= data2 <= v4, ... ` Upper and lower limits may be given by setting one of the tuple values to None. e.g., `key1 = (None,v1) for an upper limit data1 <= v1 and key1 = (v1,None) for a lower limit data >=v1. Lower limits may also be specified by a one-element tuple key1 = (v1,). See Selection.

Parameters:

tagstr, optional: An identifying tag by which the rule may be referred to later. If None, a randomly generated tag will be created.
keystr: The key (SDFITS column name or other supported key)
valuearray-like: Tuple or list giving the lower and upper limits of the range.

Returns:

None.

select_track(df)[source]

select_within(tag=None, **kwargs)[source]

Select a value within a plus or minus for a given key(s). e.g. key1 = [value1,epsilon1], key2 = [value2,epsilon2], ... Will select data value1-epsilon1 <= data1 <= value1+epsilon1, value2-epsilon2 <= data2 <= value2+epsilon2,...

See Selection.

Parameters:

tagstr, optional: An identifying tag by which the rule may be referred to later. If None, a randomly generated tag will be created.
keystr: The key (SDFITS column name or other supported key)
valuearray-like: Tuple or list giving the value and epsilon

Returns:

None.

property selection

The data selection object

Returns:

~dysh.util.Selection: The Selection object

subbeamnod(method='cycle', sig=None, cal=None, calibrate=True, timeaverage=True, polaverage=False, weights='tsys', bintable=None, **kwargs)[source]

Get a subbeam nod power scan, optionally calibrating it.

Parameters:

method: str: Method to use when processing. One of ‘cycle’ or ‘scan’. ‘cycle’ is more accurate and averages data in each SUBREF_STATE cycle. ‘scan’ reproduces GBTIDL’s snodka function which has been shown to be less accurate. Default:’cycle’
sigbool: True to indicate if this is the signal scan, False if reference
cal: bool: True if calibration (diode) is on, False if off.
calibrate: bool: whether or not to calibrate the data. If True, the data will be (calon - caloff)*0.5, otherwise it will be SDFITS row data. Default:True
timeaverageboolean, optional: Average the scans in time. The default is True.
polaverageboolean, optional: Average the scans in polarization. The default is False.
weights: str or None: None to indicate equal weighting or ‘tsys’ to indicate tsys weighting to use in time averaging. Default: ‘tsys’
bintableint, optional: Limit to the input binary table index. The default is None which means use all binary tables.
**kwargsdict: Optional additional selection (only?) keyword arguments, typically given as key=value, though a dictionary works too. e.g., ifnum=1, plnum=[2,3] etc.

Returns:

dataScanBlock: A ScanBlock containing one or more SubBeamNodScan

summary(scans=None, verbose=False, show_index=True)[source]

Create a summary list of the input dataset. If verbose=False (default), some numeric data (e.g., RESTFREQ, AZIMUTH, ELEVATIO) are averaged over the records with the same scan number.

Parameters:

scansint or 2-tuple: The scan(s) to use. A 2-tuple represents (beginning, ending) scans. Default: show all scans
verbose: bool: If True, list every record, otherwise return a compact summary
show_index: bool: If True, show the DataFrame index column. Default: False

Returns:

summary - DataFrame: Summary of the data as a DataFrame.

velocity_convention(veldef)[source]

Given the GBT VELDEF FITS string return the specutils velocity convention, e.g., “doppler_radio”

Parameters:

veldefstr: The FITS header VELDEF string

Returns:

conventionstr: The velocity convention

velocity_frame(veldef)[source]

Given the GBT VELDEF FITS string return the velocity frame, e.g., “heliocentric”.

Parameters:

veldefstr: The FITS header VELDEF string

Returns:

frame: str: The velocity frame

write_scans(fileobj, scans, output_verify='exception', overwrite=False, checksum=False)[source]

Write specific scans of the GBTFITSLoad to a new file. TBD: How does this work for multiple files??

Parameters:

fileobjstr, file-like or pathlib.Path: File to write to. If a file object, must be opened in a writeable mode.
scans: int or list-like: Range of scans to write out. e.g. 0, [14,25,32].
output_verifystr: Output verification option. Must be one of "fix", "silentfix", "ignore", "warn", or "exception". May also be any combination of "fix" or "silentfix" with "+ignore", +warn, or +exception" (e.g. ``"fix+warn"). See https://docs.astropy.org/en/latest/io/fits/api/verification.html for more info
overwritebool, optional: If True, overwrite the output file if it exists. Raises an OSError if False and the output file exists. Default is False.
checksumbool: When True adds both DATASUM and CHECKSUM cards to the headers of all HDU’s written to the file.