pypeit.spectrographs.vlt_uves module

Module for VLT/UVES

class pypeit.spectrographs.vlt_uves.UVESMosaicLookUp[source]

Bases: object

Provides the geometry required to mosaic VLT/UVES data. Similar to GeminiGMOSMosaicLookUp

geometry = {'MSC01': {'default_shape': (4188.0, 4096), 'det1': {'rotation': 0.0, 'shift': (0.0, 0.0)}, 'det2': {'rotation': 0.0, 'shift': (2146.0, 0.0)}}}

class pypeit.spectrographs.vlt_uves.VLTUVESBlueSpectrograph[source]

Bases: VLTUVESSpectrograph

camera = 'VLT_UVES_blue': Name of the spectrograph camera or arm. This is used by specdb, so use that naming convention

config_specific_par(inp, inp_par=None)[source]

Modify the PypeIt parameters to hard-wired values used for specific instrument configurations.

Parameters:

inp (str, list, Path, astropy.io.fits.Header, astropy.table.Table) – Input filename, an astropy.io.fits.Header object, or a list of astropy.io.fits.Header objects. Or a row from the metadata table.
inp_par (ParSet, optional) – Parameter set used for the full run of PypeIt. If None, use default_pypeit_par().

Returns:

The PypeIt parameter set adjusted for configuration specific parameter values.

Return type:

ParSet

classmethod default_pypeit_par()[source]

Return the default parameters to use for this instrument.

Returns:: Parameters required by all of PypeIt methods.
Return type:: PypeItPar

get_detector_par(det, hdu=None)[source]

Return metadata for the selected detector.

Parameters:

det (int) – 1-indexed detector number.
hdu (astropy.io.fits.HDUList, optional) – The open fits file with the raw image of interest. If not provided, frame-dependent parameters are set to a default.

Returns:

Object with the detector metadata.

Return type:

DetectorContainer

get_echelle_angle_files()[source]

Pass back the files required to run the echelle method of wavecalib

Returns:: List of files
Return type:: list

init_meta()[source]

Define how metadata are derived from the spectrograph files.

That is, this associates the PypeIt-specific metadata keywords with the instrument-specific header cards using meta.

name = 'vlt_uves_blue': The name of the spectrograph. See Spectrographs for the currently supported spectrographs.

ndet = 1: Number of detectors for this instrument.

class pypeit.spectrographs.vlt_uves.VLTUVESRedSpectrograph[source]

Bases: VLTUVESSpectrograph

property allowed_mosaics

Return the list of allowed detector mosaics.

Only red arm on VLT/UVES requires mosaicing.

Returns:: List of tuples, where each tuple provides the 1-indexed detector numbers that can be combined into a mosaic and processed by PypeIt.
Return type:: list

camera = 'VLT_UVES_red': Name of the spectrograph camera or arm. This is used by specdb, so use that naming convention

config_specific_par(inp, inp_par=None)[source]

Modify the PypeIt parameters to hard-wired values used for specific instrument configurations.

Parameters:

inp (str, list, Path, astropy.io.fits.Header, astropy.table.Table) – Input filename, an astropy.io.fits.Header object, or a list of astropy.io.fits.Header objects. Or a row from the metadata table.
inp_par (ParSet, optional) – Parameter set used for the full run of PypeIt. If None, use default_pypeit_par().

Returns:

The PypeIt parameter set adjusted for configuration specific parameter values.

Return type:

ParSet

property default_mosaic

Return the default detector mosaic.

For instruments with no allowed detector mosaics, this must be returned as None.

classmethod default_pypeit_par()[source]

Return the default parameters to use for this instrument.

Returns:: Parameters required by all of PypeIt methods.
Return type:: PypeItPar

get_detector_par(det, hdu=None)[source]

Return metadata for the selected detector.

Parameters:

det (int) – 1-indexed detector number.
hdu (astropy.io.fits.HDUList, optional) – The open fits file with the raw image of interest. If not provided, frame-dependent parameters are set to a default.

Returns:

Object with the detector metadata.

Return type:

DetectorContainer

get_echelle_angle_files()[source]

Pass back the files required to run the echelle method of wavecalib

Returns:: List of files
Return type:: list

get_mosaic_par(mosaic, hdu=None, msc_ord=0)[source]

Return the hard-coded parameters needed to construct detector mosaics from unbinned images.

The parameters expect the images to be trimmed and oriented to follow the PypeIt shape convention of (nspec,nspat). For returned lists, the length of the list is the same as the number of detectors in the mosaic, and they are ordered by the detector number.

Parameters:

mosaic (tuple) – Tuple of detector numbers used to construct the mosaic. Must be one among the list of possible mosaics as hard-coded by the allowed_mosaics() function.
hdu (astropy.io.fits.HDUList, optional) – The open fits file with the raw image of interest. If not provided, frame-dependent detector parameters are set to a default. BEWARE: If hdu is not provided, the binning is assumed to be 1,1, which will cause faults if applied to binned images!
msc_ord (int, optional) – Order of the interpolation used to construct the mosaic.

Returns:

Object with the mosaic and detector parameters.

Return type:

Mosaic

init_meta()[source]

Define how metadata are derived from the spectrograph files.

That is, this associates the PypeIt-specific metadata keywords with the instrument-specific header cards using meta.

name = 'vlt_uves_red': The name of the spectrograph. See Spectrographs for the currently supported spectrographs.

ndet = 2: Number of detectors for this instrument.

class pypeit.spectrographs.vlt_uves.VLTUVESSpectrograph[source]

Bases: Spectrograph

Child to handle VLT/UVES specific code.

This spectrograph is not yet supported.

check_frame_type(ftype, fitstbl, exprng=None)[source]

Check for frames of the provided type.

Parameters:

ftype (str) – Type of frame to check. Must be a valid frame type; see frame-type Definitions.
fitstbl (astropy.table.Table) – The table with the metadata for one or more frames to check.
exprng (list, optional) – Range in the allowed exposure time for a frame of type ftype. See pypeit.core.framematch.check_frame_exptime().

Returns:

Boolean array with the flags selecting the exposures in fitstbl that are ftype type frames.

Return type:

numpy.ndarray

compound_meta(headarr, meta_key)[source]

Methods to generate metadata requiring interpretation of the header data, instead of simply reading the value of a header card.

Parameters:

headarr (list) – List of astropy.io.fits.Header objects.
meta_key (str) – Metadata keyword to construct.

Returns:

Metadata value read from the header(s).

Return type:

object

config_independent_frames()[source]

Define frame types that are independent of the fully defined instrument configuration.

Bias and dark frames are considered independent of a configuration, but the DATE-OBS keyword is used to assign each to the most-relevant configuration frame group. See set_configurations().

Returns:: Dictionary where the keys are the frame types that are configuration independent and the values are the metadata keywords that can be used to assign the frames to a configuration group.
Return type:: dict

configuration_keys()[source]

Return the metadata keys that define a unique instrument configuration.

This list is used by PypeItMetaData to identify the unique configurations among the list of frames read for a given reduction.

Returns:: List of keywords of data pulled from file headers and used to construct the PypeItMetaData object.
Return type:: list

classmethod default_pypeit_par()[source]

Return the default parameters to use for this instrument.

Returns:: Parameters required by all of PypeIt methods.
Return type:: PypeItPar

ech_fixed_format = False: If an echelle spectrograph, this will be set to a boolean indicating whether it is a fixed format or tiltable echelle.

header_name = 'UVES': Name of the spectrograph camera or arm from the Header. Usually the INSTRUME card.

init_meta()[source]

Define how metadata are derived from the spectrograph files.

That is, this associates the PypeIt-specific metadata keywords with the instrument-specific header cards using meta.

order_platescale(order_vec, binning=None)[source]

Return the platescale for each echelle order.

This routine is only defined for echelle spectrographs, and it is undefined in the base class.

Parameters:

order_vec (numpy.ndarray) – The vector providing the order numbers.
binning (str, optional) – The string defining the spectral and spatial binning.

Returns:

An array with the platescale for each order provided by order.

Return type:

numpy.ndarray

pypeline = 'Echelle': String used to select the general pipeline approach for this spectrograph.

raw_header_cards()[source]

Return additional raw header cards to be propagated in downstream output files for configuration identification.

The list of raw data FITS keywords should be those used to populate the configuration_keys() or are used in config_specific_par() for a particular spectrograph, if different from the name of the PypeIt metadata keyword.

This list is used by subheader_for_spec() to include additional FITS keywords in downstream output files.

Returns:: List of keywords from the raw data files that should be propagated in output files.
Return type:: list

supported = True: Flag that PypeIt code base has been sufficiently tested with data from this spectrograph that it is officially supported by the development team.

telescope = Parameter Value Default Type Callable ---------------------------------------------------------------- name VLT KECK str False longitude -70.40498688000002 None int, float False latitude -24.627439409999997 None int, float False elevation 2668.999999999649 None int, float False fratio None None int, float False diameter 8.2 None int, float False eff_aperture 51.2 None int, float False : Instance of TelescopePar providing telescope-specific metadata.

url = 'https://www.eso.org/sci/facilities/paranal/instruments/uves.html': Reference url