Time

class astropy.time.Time(val, val2=None, format=None, scale=None, precision=None, in_subfmt=None, out_subfmt=None, location=None, copy=False)

Bases: TimeBase

Represent and manipulate times and dates for astronomy.

A Time object is initialized with one or more times in the val argument. The input times in val must conform to the specified format and must correspond to the specified time scale. The optional val2 time input should be supplied only for numeric input formats (e.g. JD) where very high precision (better than 64-bit precision) is required.

The allowed values for format can be listed with:

>>> list(Time.FORMATS)
['jd', 'mjd', 'decimalyear', 'unix', 'unix_tai', 'cxcsec', 'gps', 'plot_date',
 'stardate', 'datetime', 'ymdhms', 'iso', 'isot', 'yday', 'datetime64',
 'fits', 'byear', 'jyear', 'byear_str', 'jyear_str']

See also: http://docs.astropy.org/en/stable/time/

Parameters:

valsequence, ndarray, number, str, bytes, or Time object

Value(s) to initialize the time or times. Bytes are decoded as ascii.

val2sequence, ndarray, or number; optional

Value(s) to initialize the time or times. Only used for numerical input, to help preserve precision.

formatstr, optional

Format of input value(s), specifying how to interpret them (e.g., ISO, JD, or Unix time). By default, the same format will be used for output representation.

scalestr, optional

Time scale of input value(s), must be one of the following: (‘tai’, ‘tcb’, ‘tcg’, ‘tdb’, ‘tt’, ‘ut1’, ‘utc’)

precisionint, optional

Digits of precision in string representation of time

in_subfmtstr, optional

Unix glob to select subformats for parsing input times

out_subfmtstr, optional

Unix glob to select subformat for outputting times

locationEarthLocation or tuple, optional

If given as an tuple, it should be able to initialize an an EarthLocation instance, i.e., either contain 3 items with units of length for geocentric coordinates, or contain a longitude, latitude, and an optional height for geodetic coordinates. Can be a single location, or one for each input time. If not given, assumed to be the center of the Earth for time scale transformations to and from the solar-system barycenter.

copybool, optional

Make a copy of the input values

Attributes Summary

FORMATS	Dict of time formats
SCALES	List of time scales
T	Return an instance with the data transposed.
cache	Return the cache associated with this instance.
delta_tdb_tt	TDB - TT time scale offset
delta_ut1_utc	UT1 - UTC time scale offset
format	Get or set time format.
in_subfmt	Unix wildcard pattern to select subformats for parsing string input times.
info	Container for meta information like name, description, format.
isscalar
jd1	First of the two doubles that internally store time value(s) in JD.
jd2	Second of the two doubles that internally store time value(s) in JD.
mask
masked
ndim	The number of dimensions of the instance and underlying arrays.
out_subfmt	Unix wildcard pattern to select subformats for outputting times.
precision	Decimal precision when outputting seconds as floating point (int value between 0 and 9 inclusive).
scale	Time scale.
shape	The shape of the time instances.
size	The size of the object, as calculated from its shape.
unmasked	Get an instance without the mask.
value	Time value(s) in current format.
writeable

Methods Summary

argmax([axis, out])	Return indices of the maximum values along the given axis.
argmin([axis, out])	Return indices of the minimum values along the given axis.
argsort([axis, kind])	Returns the indices that would sort the time array.
copy([format])	Return a fully independent copy the Time object, optionally changing the format.
diagonal(*args, **kwargs)	Return an instance with the specified diagonals.
earth_rotation_angle([longitude])	Calculate local Earth rotation angle.
filled(fill_value)	Get a copy of the underlying data, with masked values filled in.
flatten(*args, **kwargs)	Return a copy with the array collapsed into one dimension.
get_delta_ut1_utc([iers_table, return_status])	Find UT1 - UTC differences by interpolating in IERS Table.
insert(obj, values[, axis])	Insert values before the given indices in the column and return a new Time or TimeDelta object.
isclose(other[, atol])	Returns a boolean or boolean array where two Time objects are element-wise equal within a time tolerance.
light_travel_time(skycoord[, kind, ...])	Light travel time correction to the barycentre or heliocentre.
max([axis, out, keepdims])	Maximum along a given axis.
mean([axis, dtype, out, keepdims, where])	Mean along a given axis.
min([axis, out, keepdims])	Minimum along a given axis.
now()	Creates a new object corresponding to the instant in time this method is called.
ptp([axis, out, keepdims])	Peak to peak (maximum - minimum) along a given axis.
ravel(*args, **kwargs)	Return an instance with the array collapsed into one dimension.
replicate([format, copy, cls])	Return a replica of the Time object, optionally changing the format.
reshape(*args, **kwargs)	Returns an instance containing the same data with a new shape.
sidereal_time(kind[, longitude, model])	Calculate sidereal time.
sort([axis])	Return a copy sorted along the specified axis.
squeeze(*args, **kwargs)	Return an instance with single-dimensional shape entries removed.
strftime(format_spec)	Convert Time to a string or a numpy.array of strings according to a format specification.
strptime(time_string, format_string, **kwargs)	Parse a string to a Time according to a format specification.
swapaxes(*args, **kwargs)	Return an instance with the given axes interchanged.
take(indices[, axis, out, mode])	Return a new instance formed from the elements at the given indices.
to_datetime([timezone, leap_second_strict])	Convert to (potentially timezone-aware) datetime object.
to_string()	Output a string representation of the Time or TimeDelta object.
to_value(format[, subfmt])	Get time values expressed in specified output format.
transpose(*args, **kwargs)	Return an instance with the data transposed.

Attributes Documentation

FORMATS = {'byear': <class 'astropy.time.formats.TimeBesselianEpoch'>, 'byear_str': <class 'astropy.time.formats.TimeBesselianEpochString'>, 'cxcsec': <class 'astropy.time.formats.TimeCxcSec'>, 'datetime': <class 'astropy.time.formats.TimeDatetime'>, 'datetime64': <class 'astropy.time.formats.TimeDatetime64'>, 'decimalyear': <class 'astropy.time.formats.TimeDecimalYear'>, 'fits': <class 'astropy.time.formats.TimeFITS'>, 'gps': <class 'astropy.time.formats.TimeGPS'>, 'iso': <class 'astropy.time.formats.TimeISO'>, 'isot': <class 'astropy.time.formats.TimeISOT'>, 'jd': <class 'astropy.time.formats.TimeJD'>, 'jyear': <class 'astropy.time.formats.TimeJulianEpoch'>, 'jyear_str': <class 'astropy.time.formats.TimeJulianEpochString'>, 'mjd': <class 'astropy.time.formats.TimeMJD'>, 'plot_date': <class 'astropy.time.formats.TimePlotDate'>, 'stardate': <class 'astropy.time.formats.TimeStardate'>, 'unix': <class 'astropy.time.formats.TimeUnix'>, 'unix_tai': <class 'astropy.time.formats.TimeUnixTai'>, 'yday': <class 'astropy.time.formats.TimeYearDayTime'>, 'ymdhms': <class 'astropy.time.formats.TimeYMDHMS'>}

Dict of time formats

SCALES = ('tai', 'tcb', 'tcg', 'tdb', 'tt', 'ut1', 'utc', 'local')

List of time scales

T

Return an instance with the data transposed.

Parameters are as for T. All internal data are views of the data of the original.

cache

Return the cache associated with this instance.

delta_tdb_tt

TDB - TT time scale offset

delta_ut1_utc

UT1 - UTC time scale offset

format

Get or set time format.

The format defines the way times are represented when accessed via the .value attribute. By default it is the same as the format used for initializing the Time instance, but it can be set to any other value that could be used for initialization. These can be listed with:

>>> list(Time.FORMATS)
['jd', 'mjd', 'decimalyear', 'unix', 'unix_tai', 'cxcsec', 'gps', 'plot_date',
 'stardate', 'datetime', 'ymdhms', 'iso', 'isot', 'yday', 'datetime64',
 'fits', 'byear', 'jyear', 'byear_str', 'jyear_str']

in_subfmt

Unix wildcard pattern to select subformats for parsing string input times.

info

Container for meta information like name, description, format. This is required when the object is used as a mixin column within a table, but can be used as a general way to store meta information.

isscalar

jd1

First of the two doubles that internally store time value(s) in JD.

jd2

Second of the two doubles that internally store time value(s) in JD.

mask

masked

ndim

The number of dimensions of the instance and underlying arrays.

out_subfmt

Unix wildcard pattern to select subformats for outputting times.

precision

Decimal precision when outputting seconds as floating point (int value between 0 and 9 inclusive).

scale

Time scale.

shape

The shape of the time instances.

Like shape, can be set to a new shape by assigning a tuple. Note that if different instances share some but not all underlying data, setting the shape of one instance can make the other instance unusable. Hence, it is strongly recommended to get new, reshaped instances with the reshape method.

Raises:

ValueError

If the new shape has the wrong total number of elements.

AttributeError

If the shape of the jd1, jd2, location, delta_ut1_utc, or delta_tdb_tt attributes cannot be changed without the arrays being copied. For these cases, use the Time.reshape method (which copies any arrays that cannot be reshaped in-place).

size

The size of the object, as calculated from its shape.

unmasked

Get an instance without the mask.

Note that while one gets a new instance, the underlying data will be shared.

See also

astropy.time.Time.filled

value

Time value(s) in current format.

writeable

Methods Documentation

argmax(axis=None, out=None)

Return indices of the maximum values along the given axis.

This is similar to argmax(), but adapted to ensure that the full precision given by the two doubles jd1 and jd2 is used. See argmax() for detailed documentation.

argmin(axis=None, out=None)

Return indices of the minimum values along the given axis.

This is similar to argmin(), but adapted to ensure that the full precision given by the two doubles jd1 and jd2 is used. See argmin() for detailed documentation.

argsort(axis=-1, kind='stable')

Returns the indices that would sort the time array.

This is similar to argsort(), but adapted to ensure that the full precision given by the two doubles jd1 and jd2 is used, and that corresponding attributes are copied. Internally, it uses lexsort(), and hence no sort method can be chosen.

Parameters:

axisint, optional

Axis along which to sort. Default is -1, which means sort along the last axis.

kind‘stable’, optional

Sorting is done with lexsort() so this argument is ignored, but kept for compatibility with argsort(). The sorting is stable, meaning that the order of equal elements is preserved.

Returns:

indicesndarray

An array of indices that sort the time array.

copy(format=None)

Return a fully independent copy the Time object, optionally changing the format.

If format is supplied then the time format of the returned Time object will be set accordingly, otherwise it will be unchanged from the original.

In this method a full copy of the internal time arrays will be made. The internal time arrays are normally not changeable by the user so in most cases the replicate() method should be used.

Parameters:

formatstr, optional

Time format of the copy.

Returns:

tmTime object

Copy of this object

diagonal(*args, **kwargs)

Return an instance with the specified diagonals.

Parameters are as for diagonal(). All internal data are views of the data of the original.

earth_rotation_angle(longitude=None)

Calculate local Earth rotation angle.

Parameters:

longitudeQuantity, EarthLocation, str, or None; optional

The longitude on the Earth at which to compute the Earth rotation angle (taken from a location as needed). If None (default), taken from the location attribute of the Time instance. If the special string ‘tio’, the result will be relative to the Terrestrial Intermediate Origin (TIO) (i.e., the output of era00).

Returns:

Longitude

Local Earth rotation angle with units of hourangle.

See also

astropy.time.Time.sidereal_time

Notes

The difference between apparent sidereal time and Earth rotation angle is the equation of the origins, which is the angle between the Celestial Intermediate Origin (CIO) and the equinox. Applying apparent sidereal time to the hour angle yields the true apparent Right Ascension with respect to the equinox, while applying the Earth rotation angle yields the intermediate (CIRS) Right Ascension with respect to the CIO.

The result includes the TIO locator (s’), which positions the Terrestrial Intermediate Origin on the equator of the Celestial Intermediate Pole (CIP) and is rigorously corrected for polar motion. (except when longitude='tio').

References

IAU 2006 NFA Glossary (currently located at: https://syrte.obspm.fr/iauWGnfa/NFA_Glossary.html)

filled(fill_value)

Get a copy of the underlying data, with masked values filled in.

Parameters:

fill_valueobject

Value to replace masked values with. Note that if this value is masked

See also

astropy.time.Time.unmasked

flatten(*args, **kwargs)

Return a copy with the array collapsed into one dimension.

Parameters are as for flatten().

get_delta_ut1_utc(iers_table=None, return_status=False)

Find UT1 - UTC differences by interpolating in IERS Table.

Parameters:

iers_tableIERS, optional

Table containing UT1-UTC differences from IERS Bulletins A and/or B. Default: earth_orientation_table (which in turn defaults to the combined version provided by IERS_Auto).

return_statusbool

Whether to return status values. If False (default), iers raises IndexError if any time is out of the range covered by the IERS table.

Returns:

ut1_utcfloat or float array

UT1-UTC, interpolated in IERS Table

statusint or int array

Status values (if return_status=`True`):: astropy.utils.iers.FROM_IERS_B astropy.utils.iers.FROM_IERS_A astropy.utils.iers.FROM_IERS_A_PREDICTION astropy.utils.iers.TIME_BEFORE_IERS_RANGE astropy.utils.iers.TIME_BEYOND_IERS_RANGE

Notes

In normal usage, UT1-UTC differences are calculated automatically on the first instance ut1 is needed.

Examples

To check in code whether any times are before the IERS table range:

>>> from astropy.utils.iers import TIME_BEFORE_IERS_RANGE
>>> t = Time(['1961-01-01', '2000-01-01'], scale='utc')
>>> delta, status = t.get_delta_ut1_utc(return_status=True)  
>>> status == TIME_BEFORE_IERS_RANGE  
array([ True, False]...)

insert(obj, values, axis=0)

Insert values before the given indices in the column and return a new Time or TimeDelta object.

The values to be inserted must conform to the rules for in-place setting of Time objects (see Get and set values in the Time documentation).

The API signature matches the np.insert API, but is more limited. The specification of insert index obj must be a single integer, and the axis must be 0 for simple row insertion before the index.

Parameters:

objint

Integer index before which values is inserted.

valuesarray_like

Value(s) to insert. If the type of values is different from that of quantity, values is converted to the matching type.

axisint, optional

Axis along which to insert values. Default is 0, which is the only allowed value and will insert a row.

Returns:

outTime subclass

New time object with inserted value(s)

isclose(other, atol=None)

Returns a boolean or boolean array where two Time objects are element-wise equal within a time tolerance.

This evaluates the expression below:

abs(self - other) <= atol

Parameters:

otherTime

Time object for comparison.

atolQuantity or TimeDelta

Absolute tolerance for equality with units of time (e.g. u.s or u.day). Default is two bits in the 128-bit JD time representation, equivalent to about 40 picosecs.

light_travel_time(skycoord, kind='barycentric', location=None, ephemeris=None)

Light travel time correction to the barycentre or heliocentre.

The frame transformations used to calculate the location of the solar system barycentre and the heliocentre rely on the erfa routine epv00, which is consistent with the JPL DE405 ephemeris to an accuracy of 11.2 km, corresponding to a light travel time of 4 microseconds.

The routine assumes the source(s) are at large distance, i.e., neglects finite-distance effects.

Parameters:

skycoordSkyCoord

The sky location to calculate the correction for.

kindstr, optional

'barycentric' (default) or 'heliocentric'

locationEarthLocation, optional

The location of the observatory to calculate the correction for. If no location is given, the location attribute of the Time object is used

ephemerisstr, optional

Solar system ephemeris to use (e.g., ‘builtin’, ‘jpl’). By default, use the one set with astropy.coordinates.solar_system_ephemeris.set. For more information, see solar_system_ephemeris.

Returns:

time_offsetTimeDelta

The time offset between the barycentre or Heliocentre and Earth, in TDB seconds. Should be added to the original time to get the time in the Solar system barycentre or the Heliocentre. Also, the time conversion to BJD will then include the relativistic correction as well.

max(axis=None, out=None, keepdims=False)

Maximum along a given axis.

This is similar to max(), but adapted to ensure that the full precision given by the two doubles jd1 and jd2 is used, and that corresponding attributes are copied.

Note that the out argument is present only for compatibility with np.max; since Time instances are immutable, it is not possible to have an actual out to store the result in.

mean(axis=None, dtype=None, out=None, keepdims=False, *, where=True)

Mean along a given axis.

This is similar to mean(), but adapted to ensure that the full precision given by the two doubles jd1 and jd2 is used, and that corresponding attributes are copied.

Note that the out argument is present only for compatibility with np.mean; since Time instances are immutable, it is not possible to have an actual out to store the result in.

Similarly, the dtype argument is also present for compatibility only; it has no meaning for Time.

Parameters:

axisNone or int or tuple of int, optional

Axis or axes along which the means are computed. The default is to compute the mean of the flattened array.

dtypeNone

Only present for compatibility with mean(), must be None.

outNone

Only present for compatibility with mean(), must be None.

keepdimsbool, optional

If this is set to True, the axes which are reduced are left in the result as dimensions with size one. With this option, the result will broadcast correctly against the input array.

wherearray_like of bool, optional

Elements to include in the mean. See reduce for details.

Returns:

mTime

A new Time instance containing the mean values

min(axis=None, out=None, keepdims=False)

Minimum along a given axis.

This is similar to min(), but adapted to ensure that the full precision given by the two doubles jd1 and jd2 is used, and that corresponding attributes are copied.

Note that the out argument is present only for compatibility with np.min; since Time instances are immutable, it is not possible to have an actual out to store the result in.

classmethod now()

Creates a new object corresponding to the instant in time this method is called.

Note

“Now” is determined using the now function, so its accuracy and precision is determined by that function. Generally that means it is set by the accuracy of your system clock. The timezone is set to UTC.

Returns:

nowtimeTime

A new Time object (or a subclass of Time if this is called from such a subclass) at the current time.

ptp(axis=None, out=None, keepdims=False)

Peak to peak (maximum - minimum) along a given axis.

This is similar to ptp(), but adapted to ensure that the full precision given by the two doubles jd1 and jd2 is used.

Note that the out argument is present only for compatibility with ptp; since Time instances are immutable, it is not possible to have an actual out to store the result in.

ravel(*args, **kwargs)

Return an instance with the array collapsed into one dimension.

Parameters are as for ravel(). Note that it is not always possible to unravel an array without copying the data. If you want an error to be raise if the data is copied, you should should assign shape (-1,) to the shape attribute.

replicate(format=None, copy=False, cls=None)

Return a replica of the Time object, optionally changing the format.

If format is supplied then the time format of the returned Time object will be set accordingly, otherwise it will be unchanged from the original.

If copy is set to True then a full copy of the internal time arrays will be made. By default the replica will use a reference to the original arrays when possible to save memory. The internal time arrays are normally not changeable by the user so in most cases it should not be necessary to set copy to True.

The convenience method copy() is available in which copy is True by default.

Parameters:

formatstr, optional

Time format of the replica.

copybool, optional

Return a true copy instead of using references where possible.

Returns:

tmTime object

Replica of this object

reshape(*args, **kwargs)

Returns an instance containing the same data with a new shape.

Parameters are as for reshape(). Note that it is not always possible to change the shape of an array without copying the data (see reshape() documentation). If you want an error to be raise if the data is copied, you should assign the new shape to the shape attribute (note: this may not be implemented for all classes using NDArrayShapeMethods).

sidereal_time(kind, longitude=None, model=None)

Calculate sidereal time.

Parameters:

kindstr

'mean' or 'apparent', i.e., accounting for precession only, or also for nutation.

longitudeQuantity, EarthLocation, str, or None; optional

The longitude on the Earth at which to compute the Earth rotation angle (taken from a location as needed). If None (default), taken from the location attribute of the Time instance. If the special string ‘greenwich’ or ‘tio’, the result will be relative to longitude 0 for models before 2000, and relative to the Terrestrial Intermediate Origin (TIO) for later ones (i.e., the output of the relevant ERFA function that calculates greenwich sidereal time).

modelstr or None; optional

Precession (and nutation) model to use. The available ones are: - apparent: [‘IAU1994’, ‘IAU2000A’, ‘IAU2000B’, ‘IAU2006A’] - mean: [‘IAU1982’, ‘IAU2000’, ‘IAU2006’] If None (default), the last (most recent) one from the appropriate list above is used.

Returns:

Longitude

Local sidereal time, with units of hourangle.

See also

astropy.time.Time.earth_rotation_angle

Notes

The difference between apparent sidereal time and Earth rotation angle is the equation of the origins, which is the angle between the Celestial Intermediate Origin (CIO) and the equinox. Applying apparent sidereal time to the hour angle yields the true apparent Right Ascension with respect to the equinox, while applying the Earth rotation angle yields the intermediate (CIRS) Right Ascension with respect to the CIO.

For the IAU precession models from 2000 onwards, the result includes the TIO locator (s’), which positions the Terrestrial Intermediate Origin on the equator of the Celestial Intermediate Pole (CIP) and is rigorously corrected for polar motion (except when longitude='tio' or 'greenwich').

References

IAU 2006 NFA Glossary (currently located at: https://syrte.obspm.fr/iauWGnfa/NFA_Glossary.html)

sort(axis=-1)

Return a copy sorted along the specified axis.

This is similar to sort(), but internally uses indexing with lexsort() to ensure that the full precision given by the two doubles jd1 and jd2 is kept, and that corresponding attributes are properly sorted and copied as well.

Parameters:

axisint or None

Axis to be sorted. If None, the flattened array is sorted. By default, sort over the last axis.

squeeze(*args, **kwargs)

Return an instance with single-dimensional shape entries removed.

Parameters are as for squeeze(). All internal data are views of the data of the original.

strftime(format_spec)

Convert Time to a string or a numpy.array of strings according to a format specification. See time.strftime documentation for format specification.

Parameters:

format_specstr

Format definition of return string.

Returns:

formattedstr or numpy.array

String or numpy.array of strings formatted according to the given format string.

classmethod strptime(time_string, format_string, **kwargs)

Parse a string to a Time according to a format specification. See time.strptime documentation for format specification.

>>> Time.strptime('2012-Jun-30 23:59:60', '%Y-%b-%d %H:%M:%S')
<Time object: scale='utc' format='isot' value=2012-06-30T23:59:60.000>

Parameters:

time_stringstr, sequence, or ndarray

Objects containing time data of type string

format_stringstr

String specifying format of time_string.

kwargsdict

Any keyword arguments for Time. If the format keyword argument is present, this will be used as the Time format.

Returns:

time_objTime

A new Time object corresponding to the input time_string.

swapaxes(*args, **kwargs)

Return an instance with the given axes interchanged.

Parameters are as for swapaxes(): axis1, axis2. All internal data are views of the data of the original.

take(indices, axis=None, out=None, mode='raise')

Return a new instance formed from the elements at the given indices.

Parameters are as for take(), except that, obviously, no output array can be given.

to_datetime(timezone=None, leap_second_strict='raise')

Convert to (potentially timezone-aware) datetime object.

If timezone is not None, return a timezone-aware datetime object.

Since the datetime class does not natively handle leap seconds, the behavior when converting a time within a leap second is controlled by the leap_second_strict argument. For example:

>>> from astropy.time import Time
>>> t = Time("2015-06-30 23:59:60.500")
>>> print(t.to_datetime(leap_second_strict='silent'))
2015-07-01 00:00:00.500000

Parameters:

timezone{tzinfo, None}, optional

If not None, return timezone-aware datetime.

leap_second_strictstr, optional

If raise (default), raise an exception if the time is within a leap second. If warn then issue a warning. If silent then silently handle the leap second.

Returns:

datetime

If timezone is not None, output will be timezone-aware.

to_string()

Output a string representation of the Time or TimeDelta object.

Similar to str(self.value) (which uses numpy array formatting) but array values are evaluated only for the items that actually are output. For large arrays this can be a substantial performance improvement.

Returns:

outstr

String representation of the time values.

to_value(format, subfmt='*')

Get time values expressed in specified output format.

This method allows representing the Time object in the desired output format and optional sub-format subfmt. Available built-in formats include jd, mjd, iso, and so forth. Each format can have its own sub-formats

For built-in numerical formats like jd or unix, subfmt can be one of ‘float’, ‘long’, ‘decimal’, ‘str’, or ‘bytes’. Here, ‘long’ uses numpy.longdouble for somewhat enhanced precision (with the enhancement depending on platform), and ‘decimal’ decimal.Decimal for full precision. For ‘str’ and ‘bytes’, the number of digits is also chosen such that time values are represented accurately.

For built-in date-like string formats, one of ‘date_hms’, ‘date_hm’, or ‘date’ (or ‘longdate_hms’, etc., for 5-digit years in TimeFITS). For sub-formats including seconds, the number of digits used for the fractional seconds is as set by precision.

Parameters:

formatstr

The format in which one wants the time values. Default: the current format.

subfmtstr or None, optional

Value or wildcard pattern to select the sub-format in which the values should be given. The default of ‘*’ picks the first available for a given format, i.e., ‘float’ or ‘date_hms’. If None, use the instance’s out_subfmt.

transpose(*args, **kwargs)

Return an instance with the data transposed.

Parameters are as for transpose(). All internal data are views of the data of the original.