measures¶
-
class
measures
[source]¶ measures tool
Methods Summary
get some additional measure information
define a baseline from a position measure
define a baseline measure
get the angular diameter of the current comet in the current frame
get the distance of the current comet in the current frame
get the current comet name
get the current comet table coordinates
get the current comet table type
define a direction measure
Show direction measure as a string.
save a measure as frame reference
free resources used by tool.
define a doppler measure
define an earthmagnetic measure
define an epoch measure
expand n positions to n*(n-1)/2 baselines
set the current comet table
set the active frame time at now
define a frequency measure
get the offset of a measure
get the reference code of a measure
get the type of a measure
get the value of a measure
Check if measure
get a list of known spectral lines
get known reference code names (list indices do not necessarily correspond to enumeration indices)
convert a measure to another reference
Construct measures tool
get position of an observatory
get a list of known observatories
get position angle of two directions
define a position measure
define a radialvelocity measure
get rise and set sidereal time
get rise and set times
get separation angle between two directions
Shift a direction measure by an offset angle at a position angle.
Show a measure as a string
show the currently active frame reference
get direction of a source
get a list of known sources
get frequency of a spectral line
convert a frequency or radialvelocity measure to a doppler measure
convert a doppler type value to a frequency
convert a doppler type value to a real radial velocity
convert a frequency and doppler measure to a rest frequency
calculate a uvw measure from a baseline
type of tool
define a uvw measure
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addxvalue
(a='')[source]¶ get some additional measure information
addxvalue will give some additional information about some measures as a vector of quantities. It is used internally to get the rectangular coordinates of measures that are normally given in angles. The casual user will probably in general not interested in this function.
Parameters
a (record='')
- measures for which extra information is to be gotten
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asbaseline
(pos='')[source]¶ define a baseline from a position measure
asbaseline converts a position measure into a baseline measure. No actual baseline is calculated, since operations can be done on positions, with subtractions to obtain baselines at a later stage.
Parameters
pos (record='')
- position measure
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baseline
(rf='ITRF', v0='', v1='', v2='', off='')[source]¶ define a baseline measure
baseline defines a baseline measure from the CLI. It has to specify a reference code, baseline quantity values (see introduction for the action on a scalar quantity with either a vector or scalar value, and when a vector of quantities is given), and optionally it can specify an offset, which in itself has to be a baseline. Allowable reference codes are ITRF and the direction ones.Note that additional ones may become available. Check in casawith:
print ” —- baseline Ex 1 —-” print me.listcodes(me.baseline()) # {‘normal’: array([‘J2000’, ‘JMEAN’, ‘JTRUE’, ‘APP’, ‘B1950’, ‘B1950_VLA’, ‘BMEAN’, # ‘BTRUE’, ‘GALACTIC’, ‘HADEC’, ‘AZEL’, ‘AZELSW’, ‘AZELNE’, ‘AZELGEO’, # ‘AZELSWGEO’, ‘AZELNEGEO’, ‘JNAT’, ‘ECLIPTIC’, ‘MECLIPTIC’, # ‘TECLIPTIC’, ‘SUPERGAL’, ‘ITRF’, ‘TOPO’, ‘ICRS’], # dtype=’|S10’), ‘extra’: array([], # dtype=’|S1’)}
The baseline quantity values should be either longitude (angle), latitude(angle) and height(length); or x,y,z (length). See quantity for possible angle formats.
Parameters
rf (string='ITRF')
- reference codev0 (variant='')
- longitude or xv1 (variant='')
- latitude or yv2 (variant='')
- height or zoff (record='')
- optional offset baseline measure
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cometangdiam
()[source]¶ get the angular diameter of the current comet in the current frame
- cometdist returns the angular diameter (as seen from Earth) in AU of the current
comet in the current frame, as a quantity. It will return -1 radians on failure!
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cometdist
()[source]¶ get the distance of the current comet in the current frame
- cometdist returns the distance in AU of the current comet in the current frame,
as a quantity. It will return -1 AU on failure!
-
cometname
()[source]¶ get the current comet name
cometname gets the name of the current comet (if any).
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comettopo
()[source]¶ get the current comet table coordinates
comettopo gets the comet table’s topographic coordinates used.
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comettype
()[source]¶ get the current comet table type
comettype gets the comet table type (apparent or topocentric)
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direction
(rf='J2000', v0='', v1='', off='')[source]¶ define a direction measure
direction defines a direction measure from the CLI. It has to specify a reference code, direction quantity values (see introduction for the action on a scalar quantity with either a vector or scalar value),
and optionally it can specify an offset, which in itself has to be a direction. Allowable reference codes are: {em J2000 JMEAN JTRUE APP B1950 BMEAN BTRUE GALACTIC HADEC AZEL SUPERGAL ECLIPTIC MECLIPTIC TECLIPTIC MERCURY VENUS MARS JUPITER SATURN URANUS NEPTUNE PLUTO MOON SUN COMET}.Note that additional ones may become available. Check in casawith:
egin{verbatim} print ” —- direction Ex 1 —-” print me.listcodes(me.direction()) #{‘normal’: [‘J2000’, ‘JMEAN’, ‘JTRUE’, ‘APP’, ‘B1950’, ‘BMEAN’, #’BTRUE’, ‘GALACTIC’, ‘HADEC’, ‘AZEL’, ‘AZELSW’, ‘AZELNE’, ‘AZELGEO’, #’AZELSWGEO’, ‘AZELNEGEO’, ‘JNAT’, ‘ECLIPTIC’, ‘MECLIPTIC’, #’TECLIPTIC’, ‘SUPERGAL’, ‘ITRF’, ‘TOPO’, ‘ICRS’], ‘extra’: [‘MERCURY’, #’VENUS’, ‘MARS’, ‘JUPITER’, ‘SATURN’, ‘URANUS’, ‘NEPTUNE’, ‘PLUTO’, #’SUN’, ‘MOON’, ‘COMET’]} end{verbatim}
The direction quantity values should be longitude(angle) and latitude(angle) (none needed for planets: the frame epoch defines coordinates). See quantity for possible angle formats.
Parameters
rf (string='J2000')
- reference codev0 (variant='')
- longitudev1 (variant='')
- latitudeoff (record='')
- optional offset direction measure
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dirshow
(v='')[source]¶ Show direction measure as a string.
dirshow will convert a direction measure to a string
Parameters
v (record='')
- a direction measure value to be converted to string
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doframe
(v='')[source]¶ save a measure as frame reference
doframe will set the measure specified as part of a frame.
If conversion from one type to another is necessary, with the measure function,
the following frames
should be set if one of the reference types involved in the conversion is as in the following lists.{em Epoch}
UTC TAI LAST position LMST position GMST1 GAST UT1 UT2 TDT TCG TDB TCD
{em Direction}
J2000 JMEAN epoch JTRUE epoch APP epoch B1950 BMEAN epoch BTRUE epoch GALACTIC HADEC epoch position AZEL epoch position SUPERGALACTIC ECLIPTIC MECLIPTIC epoch TECLIPTIC epoch PLANET epoch [position]
{em Position}
WGS84 ITRF
{em Radial Velocity}
LSRK direction LSRD direction BARY direction GEO direction epoch TOPO direction epoch position GALACTO direction
{em Doppler}
RADIO OPTICAL Z RATIO RELATIVISTIC BETA GAMMA
{em Frequency}
REST direction radialvelocity LSRK direction LSRD direction BARY direction GEO direction epoch TOPO direction epoch position GALACTO
Parameters
v (record='')
- measure to be set in frame
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done
()[source]¶ free resources used by tool.
In general you will not want to call this method. It removes and then recreates the default measures tool.
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doppler
(rf='RADIO', v0='', off='')[source]¶ define a doppler measure
doppler defines a doppler measure from the CLI. It has to specify a reference code, doppler quantity value (see introduction for the action on a scalar quantity with either a vector or scalar value),
and optionally it can specify an offset, which in itself has to be a doppler. Allowable reference codes are: {em RADIO Z RATIO BETA GAMMA OPTICAL TRUE RELATIVISTIC}.Note that additional ones may become available. Check in casawith:
egin{verbatim} print ” —- doppler Ex 1 —-” print me.listcodes(me.doppler()) #{‘normal’: [‘RADIO’, ‘Z’, ‘RATIO’, ‘BETA’, ‘GAMMA’, ‘OPTICAL’, # ‘TRUE’, ‘RELATIVISTIC’], ‘extra’: []} end{verbatim}
The doppler quantity values should be either non-dimensioned to specify a ratio of the light velocity, or in velocity.
Parameters
rf (string='RADIO')
- reference codev0 (variant='')
- doppler ratio/velocityoff (record='')
- optional offset doppler measure
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earthmagnetic
(rf='IGRF', v0='', v1='', v2='', off='')[source]¶ define an earthmagnetic measure
earthmagnetic defines an earthmagnetic measure from the CLI. It needs a reference code, earthmagnetic quantity values (see introduction for the action on a scalar quantity with either a vector or scalar value) if the reference code is not for a model, and optionally it can specify an offset, which in itself has to be a earthmagnetic. In general you specify a model (IGRF is the default and the only one known) and convert it to an explicit field. (See
for information on the International Geomagnetic Reference Field). The earthmagnetic quantity values should be either longitude (angle), latitude(angle) and length(field strength); or x,y,z (field). See quantity for possible angle formats.
Parameters
rf (string='IGRF')
- reference codev0 (variant='')
- Field strengthv1 (variant='')
- longitudev2 (variant='')
- latitudeoff (record='')
- optional offset earthmagnetic measure
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epoch
(rf='UTC', v0='', off='')[source]¶ define an epoch measure
epoch defines an epoch measure from the CLI. It has to specify a reference code, an epoch quantity value (see introduction for the action on a scalar quantity with either a vector or scalar value),
and optionally it can specify an offset, which in itself has to be an epoch. Allowable reference codes are: {em UTC TAI LAST LMST GMST1 GAST UT1 UT2 TDT TCG TDB TCB}.Note that additional ones may become available. Check in casawith:
egin{verbatim} print ” —- epoch Ex 1 —-” print me.listcodes(me.epoch()) #{‘normal’: [‘LAST’, ‘LMST’, ‘GMST1’, ‘GAST’, ‘UT1’, ‘UT2’, ‘UTC’, ‘TAI’, # ‘TDT’, ‘TCG’, ‘TDB’, ‘TCB’, ‘IAT’, ‘GMST’, ‘TT’, ‘ET’, ‘UT’], ‘extra’: []} # end{verbatim}
See quantity for possible time formats.
Parameters
rf (string='UTC')
- reference codev0 (variant='')
- epoch valueoff (record='')
- optional offset epoch measure
-
expand
(v='')[source]¶ expand n positions to n*(n-1)/2 baselines
expand calculates the differences between a series of given measure values: it calculates baseline values from position values. The returned value is a measure, but the value of the optional output variable {em xyz} will be set to an array of values.
Parameters
v (record='')
- measure (baseline, position or uvw measure)
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framecomet
(v='')[source]¶ set the current comet table
framecomet will put the specified comet table in the frame.
Parameters
v (string='')
- name of a table
-
framenow
()[source]¶ set the active frame time at now
framenow will fill the active frame time with the current date and time. The different frame values necessary are described in the doframe function
-
frequency
(rf='LSRK', v0='', off='')[source]¶ define a frequency measure
frequency defines a frequency measure from the CLI. It has to specify a reference code, frequency quantity value (see introduction for the action on a scalar quantity with either a vector or scalar value),
and optionally it can specify an offset, which in itself has to be a frequency. Allowable reference codes are: {em REST LSRK LSRD BARY GEO TOPO GALACTO LGROUP CMB}.Note that additional ones may become available. Check in casawith: egin{verbatim} print ” —- frequency Ex 1 —-” print me.listcodes(me.frequency()) #{‘normal’: [‘REST’, ‘LSRK’, ‘LSRD’, ‘BARY’, ‘GEO’, ‘TOPO’, # ‘GALACTO’, ‘LGROUP’, ‘CMB’], ‘extra’: []} end{verbatim}
The frequency quantity values should be in one of the recognised units (examples all give same frequency): egin{itemize} item value with time units: a period (0.5s) item value as frequency: 2Hz item value in angular frequency: 720deg/s item value as length: 149896km item value as wave number: 4.19169e-8m-1 item value as energy (h.nu): 8.27134e-9ueV item value as momentum: 4.42044e-42kg.m end{itemize}
Parameters
rf (string='LSRK')
- reference codev0 (variant='')
- frequency/wavelength/ldotsoff (record='')
- optional offset frequency measure
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getoffset
(v='')[source]¶ get the offset of a measure
getoff gets the actual offset of the measure (as a measure) or F if no offset given.
Parameters
v (record='')
- measure (array of measures)
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getref
(v='')[source]¶ get the reference code of a measure
gettype gets the actual reference code of the measure.
Parameters
v (record='')
- measure (array of measures)
-
gettype
(v='')[source]¶ get the type of a measure
gettype gets the actual type of the measure.
Parameters
v (record='')
- measure (array of measures)
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getvalue
(v='')[source]¶ get the value of a measure
getvalue gets the actual implementation value of the measure.
Parameters
v (record='')
- measure (array of measures)
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ismeasure
(v='')[source]¶ Check if measure
Checks if the operand is a correct measure
Parameters
v (record='')
- value to be tested
-
linelist
()[source]¶ get a list of known spectral lines
linelist will give you a string with a space separated list of spectral lines known in the Lines table.
A number of lines are available now, but tables with many lines are already online, and will be interfaced once a nomenclature can be defined for the tens of thousands of lines.
-
listcodes
(ms='')[source]¶ get known reference code names (list indices do not necessarily correspond to enumeration indices)
listcodes will produce the known reference codes for a specified measure type. It will return a record with two entries. The first is a string vector of all normal codes; the second a string vector (maybe empty) with all extra codes (like planets). NOTE: Synonyms and different code groups may be present in the code name lists. The indices in these lists therefore do not necessarily correspond to the internal CASA enumeration indices.
Parameters
ms (record='')
- the measure type for which to list
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measure
(v='', rf='', off='')[source]¶ convert a measure to another reference
measure converts measures (epoch, direction etc.) from one reference to another. It will, for instance, convert a direction from J2000 to AZEL representation. Its arguments are a measure, an output reference code (see the individual measures for the allowable codes (direction, position, epoch, frequency, doppler, radialvelocity, baseline, uvw, earthmagnetic)), and an optional offset of the same type as the main measure. The offset will be subtracted from the result before it is returned.In some cases (see the individual measures for when), more information than just a reference code is necessary. E.g. the above example of a conversion to AZEL, needs to know for when, and where on Earth we want it. This information is stored in a reference frame. Measures are set in the reference frame with the doframe function. The frame is tool
wide.
{f IMPORTANT NOTE:}To get an accurate conversion of solar system objects direction to a celestial frame, one should convert to AZEL or HADEC before to get parallax accounted for. Thus if you want to get the moon’s position in J2000..one would do it in 2 stagesi.e (after setting the appropriate frames)
moonazel=me.measure(me.direction(‘moon’), ‘AZELGEO’) moonJ2000=me.measure(moonazel, ‘J2000’)
Parameters
v (record='')
- measure to be convertedrf (string='')
- output reference codeoff (record='')
- optional output offset measure
-
measures
()[source]¶ Construct measures tool
Create a measures tool on the specified host (or by default the host you are running on).
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observatory
(name='ALMA')[source]¶ get position of an observatory
observatory will give you the position of an observatory as given in the system. At the time of writing the following observatories are recognised (but check e.g. the position GUI for currently known ones, or the me.obslist() tool function): {em’ALMA’ ‘ARECIBO’ ‘ATCA’ ‘BIMA’ ‘CLRO’ ‘DRAO’ ‘DWL’ ‘GB’ ‘GBT’ ‘GMRT’
‘IRAM PDB’ ‘IRAM_PDB’ ‘JCMT’ ‘MOPRA’ ‘MOST’ ‘NRAO12M’ ‘NRAO_GBT’ ‘PKS’ ‘SAO SMA’ ‘SMA’ ‘VLA’ ‘VLBA’ ‘WSRT’ ‘ATF’ ‘ATA’ ‘CARMA’ ‘ACA’ ‘OSF’ ‘OVRO_MMA’ ‘EVLA’ ‘ASKAP’ ‘APEX’ ‘SMT’ ‘NRO’ ‘ASTE’ ‘LOFAR’ ‘MeerKAT’ ‘KAT-7’ ‘EVN’ ‘LWA1’ ‘PAPER_SA’ ‘PAPER_GB’ ‘e-MERLIN’ ‘MERLIN2’ ‘Effelsberg’ ‘MWA32T’ }.
Parameters
name (string='ALMA')
- observatory name - case insensitive
-
obslist
()[source]¶ get a list of known observatories
obslist will give you an array of strings of the observatories known in the Observatories table.
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posangle
(m1='', m2='')[source]¶ get position angle of two directions
posangle will give the position angle from a direction to another. I.e. the angle in a direction between the direction to the North pole and the other direction. The posiation angle is calculated in the frame of the first argument. m2 is thus converted to the frame of m1 before calculating the position angle.
Parameters
m1 (record='')
- direction of source (direction measure)m2 (record='')
- direction of other source (direction measure)
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position
(rf='WGS84', v0='', v1='', v2='', off='')[source]¶ define a position measure
position defines a position measure from the CLI. It has to specify a reference code, position quantity values (see introduction for the action on a scalar quantity with either a vector or scalar value),
and optionally it can specify an offset, which in itself has to be a position. Allowable reference codes are: {em WGS84 ITRF} (World Geodetic System and International Terrestrial Reference Frame). Note that additional ones may become available. Check in casawith:
egin{verbatim} print ” —- position Ex 1 —-” print me.listcodes(me.position()) #{‘normal’: [‘ITRF’, ‘WGS84’], ‘extra’: []} end{verbatim}
The position quantity values should be either longitude
(angle), latitude(angle) and height(length); or x,y,z (length). See quantity for possible angle formats.
Parameters
rf (string='WGS84')
- reference codev0 (variant='')
- longitude or xv1 (variant='')
- latitude or yv2 (variant='')
- height or zoff (record='')
- optional offset position measure
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radialvelocity
(rf='LSRK', v0='', off='')[source]¶ define a radialvelocity measure
radialvelocity defines a radialvelocity measure from the CLI. It has to specify a reference code, radialvelocity quantity value (see introduction for the action on a scalar quantity with either a vector or scalar value),
and optionally it can specify an offset, which in itself has to be a radialvelocity. Allowable reference codes are: {em LSRK LSRD BARY GEO TOPO GALACTO LGROUP CMB}. Note that additional ones may become available. Check in casawith:
egin{verbatim} print ” —- radialvelocity Ex 1 —-” print me.listcodes(me.radialvelocity()) # Out[17]: #{‘extra’: [], # ‘normal’: [‘LSRK’, ‘LSRD’, ‘BARY’, ‘GEO’, ‘TOPO’, ‘GALACTO’, # ‘LGROUP’, ‘CMB’]} end{verbatim} The radialvelocity quantity values should be given as velocity.
Parameters
rf (string='LSRK')
- reference codev0 (variant='')
- radial velocityoff (record='')
- optional offset radialvelocity measure
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rise
(crd='', ev='0.0deg')[source]¶ get rise and set sidereal time
rise will give the rise/set hour-angles of a source. It needs the position in the frame, and a time. If the latter is not set, the current time will be used.
Parameters
crd (variant='')
- direction of source (direction measure)ev (variant='0.0deg')
- elevation angle limit
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riseset
(crd='', ev='0.0deg')[source]¶ get rise and set times
rise will give the rise/set times of a source. It needs the position in the frame, and a time. If the latter is not set, the current time will be used. The returned value is a record with a ‘solved’ field, which is F if the source is always below or above the horizon. In that case the rise and set fields will all have a string value. The record also returns a rise and set record, with ‘last’ and ‘utc’ fields showing the rise and set times as epochs.
Parameters
crd (variant='')
- direction of source (direction measure)ev (variant='0.0deg')
- elevation limit
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separation
(m1='', m2='')[source]¶ get separation angle between two directions
separation will give the separation of a direction from another as an angle.
Parameters
m1 (record='')
- direction of source (direction measure)m2 (record='')
- direction of other source (direction measure)
-
shift
(v='', offset='0deg', pa='0deg')[source]¶ Shift a direction measure by an offset angle at a position angle.
- This method calculates the direction measure located at the specified offset angular amount along the specified
position angle from the specified direction measure.
Parameters
v (record='')
- The direction measure to shift, represented as a record.offset (variant='0deg')
- The angular offset, represented as a quantity record or string.pa (variant='0deg')
- Position angle of the offset, measured from the positive latitude axis through the positive longitude axis.
-
show
(v='', refcode=True)[source]¶ Show a measure as a string
show will convert a measure to a string.
All measures are catered for (at this moment {em direction, position, epoch, radialvelocity, frequency, doppler, baseline, uvw, earthmagnetic} ).
Parameters
v (record='')
- measure value to be converted to stringrefcode (bool=True)
- add the reference code to output
-
showframe
()[source]¶ show the currently active frame reference
showframe will display the currently active reference frame values on the terminal. The different frame values necessary are described in the doframe function. The frame is displayed on the terminal using the formatting as done for the show function.
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source
(name='1934-638')[source]¶ get direction of a source
source will give you the direction of a source. The known list can be obtained by me.sourcelist().
Parameters
name (variant='1934-638')
- name
-
sourcelist
()[source]¶ get a list of known sources
sourcelist will give you a string with the space separated list of sources known in the Sources table.
-
spectralline
(name='HI')[source]¶ get frequency of a spectral line
spectralline will give you the frequency of a spectral line. The known list can be obtained by me.linelist().
Parameters
name (string='HI')
- name
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todoppler
(rf='', v0='', rfq='')[source]¶ convert a frequency or radialvelocity measure to a doppler measure
todoppler will convert a radialvelocity measure or a frequency measure to a doppler measure. In the case of a frequency, a rest frequency has to be specified. The type of doppler wanted (e.g. RADIO) has to be specified.
Parameters
rf (string='')
- doppler reference typev0 (record='')
- radial velocity or frequency measurerfq (variant='')
- rest frequency (frequency measure or frequency quantity)
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tofrequency
(rf='', v0='', rfq='')[source]¶ convert a doppler type value to a frequency
tofrequency will convert a Doppler type value (e.g. in radio mode) to a frequency. The type of frequency (e.g. LSRK) and a rest frequency (either as a frequency quantity (e.g. qa.constants(‘HI’)) or a frequency measure (e.g. me.frequency(‘rest’,’5100MHz’)) should be specified
Parameters
rf (string='')
- frequency reference typev0 (record='')
- doppler measure valuerfq (record='')
- rest frequency (frequency measure or freuency quantity)
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toradialvelocity
(rf='', v0='')[source]¶ convert a doppler type value to a real radial velocity
toradialvelocity will convert a Doppler type value (e.g. in radio mode) to a real radialvelocity. The type of velocity (e.g. LSRK) should be specified
Parameters
rf (string='')
- radial velocity reference typev0 (record='')
- doppler value measure
-
torestfrequency
(v0='', d0='')[source]¶ convert a frequency and doppler measure to a rest frequency
torestfrequency will convert a frequency measure and a doppler measure (e.g. obtained from another spectral line with a known rest frequency) to a rest frequency.
Parameters
v0 (record='')
- frequency reference typed0 (record='')
- doppler measure value
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touvw
(v='')[source]¶ calculate a uvw measure from a baseline
touvw calculates a uvw measure from a baseline. Note that the baseline does not have to be a proper {em baseline}, but can be a series of positions (to call positions baselines see asbaseline ) for speed reasons: operations are linear and can be done on positions, which are converted to baseline values at the end (with expand ).
Whatever the reference code of the baseline, the returned {em uvw} will be given in J2000. If the {em dot} argument is given, that variable will be filled with a quantity array consisting of the time derivative of the uvw (note that only the sidereal rate is taken into account; not precession, earth tides and similar variations, which are much smaller). If the {em xyz} variable is given, it will be filled with the quantity values of the uvw measure.
The values of the input baselines can be given as a quantity vector per x, y or z value.
uvw coordinates are calculated for a certain direction in the sky; hence the frame has to contain the direction for the calculation to work. Since the baseline and the sky rotate with respect of each other, the time should be specified as well.
Parameters
v (record='')
- baseline measure
-
uvw
(rf='ITRF', v0='', v1='', v2='', off='')[source]¶ define a uvw measure
uvw defines a uvw measure from the CLI. It has to specify a reference code, uvw quantity values (see introduction for the action on a scalar quantity with either a vector or scalar value), and optionally it can specify an offset, which in itself has to be a uvw. Allowable reference codes are ITRF and the direction ones.Note that additional ones may become available. Check in casawith: print ” —- uvw Ex 1 —-” print me.listcodes(me.uvw()) # {‘normal’: array([‘J2000’, ‘JMEAN’, ‘JTRUE’, ‘APP’, ‘B1950’, ‘B1950_VLA’, ‘BMEAN’,
The uvw quantity values should be either longitude (angle), latitude(angle) and height(length); or x,y,z (length). See quantity for possible angle formats.
Parameters
rf (string='ITRF')
- reference codev0 (variant='')
- longitude or xv1 (variant='')
- latitude or yv2 (variant='')
- height or zoff (record='')
- optional offset uvw measure
-