Class Instrument

Initializing an instance of Instrument.

Parameters:

• star_name (string) - The name of the star from Star.py
• instrument_name (string) - The name of the instrument (SPIRE or PACS)
• oversampling (int) - The instrumental oversampling, for correct convolution of the Sphinx output.
• code (string) - The radiative transfer code used to model the data

  (default: 'GASTRoNOoM')

• path (string) - Output folder in the code's home folder. Used to locate eg PACS database. If None, no model info required (eg for line measurement matching/identification)

  (default: None)

• intrinsic (bool) - Use the intrinsic Sphinx line profiles for convolving with the spectral resolution? Otherwise the beam convolved line profiles are used.

  (default: 1)

• path_linefit (string) - The folder name for linefit results from Hipe (created by Pierre, assuming his syntax). The folder is located in $path_pacs$/$star_name$/. If no folder is given, no linefits are processed.

  (default: '')

• blend_factor (float) - The relative factor with respect to the intrinsic instrumental FWHM that is compared with the fitted Gaussian FWHM to determine whether an emission line may be blended.

  (default: 1.2)

Overrides: object.__init__

Read the telescope properties from Telescope.dat.

This currently includes the telescope size in m, and the default absolute flux calibration uncertainty.

Return a list of all model id's in the star_grid.

Parameters:

• star_grid (list[Star()]) - The grid of parameter sets
• id_type (string) - the type of model id (MCMAX or GASTRONOOM or PACS)

Returns: list[string]

the model_ids

Retrieve the data filenames that you wish to be plotted.

Parameters:

• searchstring (string) - the searchstring conditional for selecting data files.

  (default: '')

Returns: list[string]

the data filenames found in the search

Read data from given filenames and remember them.

The data are saved as wavelength and flux lists in the object.

Parameters:

• data_filenames (list[string]) - The data filenames. If empty, auto-search is done

  (default: [])

• searchstring (string) - the searchstring conditional for the auto-search

  (default: '')

Read in data, taking special care of NaNs.

Four colums are taken as input! wave - contsub - original - continuum

Two columns still works, but may result in errors in other places in the code.

Data are always read in Jy versus micron, for both SPIRE and PACS.

Read the data from the line fit procedure.

Parameters:

• kwargs (dict) - Extra keywords for the readCols method.

  (default: dict())

Returns: list[array]

The line fit columns are returned.

Match the wavelengths of integrated intensities with transitions.

Checks if a blend might be present based on the data, as well as the available transitions.

Note that if a line is observed multiple times in the same band (eg in a line scan), it cannot at this moment be discerned. In other words, there is no point including a line fitted twice in two line scans, as it will not be taken into account for the int matching algorithm.

Parameters:

• trans_list (list[Transition()]) - The list of transitions for which the check is done.
• ifn (int) - The index of the filename in self.data_filenames. This is done per file!

Merge Sphinx output line profiles on a zero-continuum.

For now only done in wavelength units of micron for PACS/SPIRE spectra.

Parameters:

• star (Star()) - The Star object for which all lines are collected + merged

Returns: (list,list)

wave list in micron and flux list in Jy