indices.rst

Spectral-Index Measurements

Analysis class: :class:`~mangadap.proc.spectralindices.SpectralIndices`

Reference root: see :class:`~mangadap.config.analysisplan.AnalysisPlan.method_path`; $MANGA_SPECTRO_ANALYSIS/$MANGADRP_VER/$MANGADAP_VER/[METHOD]/[PLATE]/[IFUDESIGN]/ref for MaNGA

Reference file: see :class:`~mangadap.proc.spectralindices.SpectralIndices.default_paths`; manga-[PLATE]-[IFUDESIGN]-[RDXQA]-[BINNING]-[CONTINUUM]-[ELFIT]-[INDICES].fits.gz for MaNGA

Optional Parameters: see :ref:`plan`. The table below lists the parameters defined by :class:`~mangadap.proc.spectralindices.SpectralIndicesDef`

Important class dependencies:

• :class:`~mangadap.par.absorptionindexdb.AbsorptionIndexDB`: Generalized class that provides the detailed parameters for a set of absorption-line spectral indices.
• :class:`~mangadap.par.bandheadindexdb.BandheadIndexDB`: Generalized class that provides the detailed parameters for a set of bandhead (or "color") spectral indices.
• :mod:`mangadap.proc.bandpassfilter`: Provides the core functions that perform the bandpass integrals.

Algorithm:

• Read the artifact database to setup the :class:`~mangadap.util.pixelmask.SpectralPixelMask` object based on the artifact_mask config.

• Setup the :class:`~mangadap.par.absorptionindexdb.AbsorptionIndexDB` (using absorption_indices config) and :class:`~mangadap.par.bandheadindexdb.BandheadIndexDB` (using bandhead_indices config) databases with the indices to measure.

• Determine the binned spectra above the S/N limit set by the minimum_snr config.

• Mask binned spectra, ignoring pixels masked as DONOTUSE, IGNORED, FLUXINVALID, or FORESTAR in DAP LOGCUBE file.

• Get the best-fitting emission-line models from the :class:`~mangadap.proc.emissionlinemodel.EmissionLineModel` object and subtract it from them from the data; keep track of where an emission-line model is and is not defined.

• Measure the indices using :func:`~mangadap.proc.spectralindices.SpectralIndices.measure_indices`:

  • Compute flux per frequency, needed for some indices; i.e., convert spectra from F_\lambda to F_\nu.

  • Isolate which indices use each definition (F_\lambda vs. F_\nu)

  • Mask any "dummy" indices.

  • For each spectrum, redshift the band definition, measure the absorption-line indices using :class:`~mangadap.proc.spectralindices.AbsorptionLineIndices`, and the bandhead indices using :class:`~mangadap.proc.spectralindices.BandheadIndices`, and save the results using :func:`~mangadap.proc.spectralindices.SpectralIndices.save_results`.

    • Part of saving the results is to determine which indices were successfully measured. Only bands that are completely masked (or empty) are flagged as NOVALUE in the output maps. I also keep track of which bands are incomplete (only partially masked).

• Compute the velocity-dispersion corrections:

  • Get the best-fitting continuum model from the :class:`~mangadap.proc.stellarcontinuummodel.StellarContinuumModel`, both with (continuum) and without (continuum_dcnvlv) the convolution with the best-fitting line-of-sight velocity distribution function (LOSVD) using :func:`~mangadap.proc.stellarcontinuummodel.StellarContinuumModel.fill_to_match`.

  • Remeasure the indices on these two models (indx and dcnvlv_indx, respectively) and the correction based on the result using :func:`~mangadap.proc.spectralindices.SpectralIndices.calculate_dispersion_corrections`

    • For mag unit indices, the correction is dcnvlv_indx-indx
    • For ang unit indices, the correction is dcnvlv_indx/indx

  • Any index with a bad correction is flagged as NOCORRECTION.

• Construct spectral-index BINID map. Bin IDs are the same as for the binned spectra except that any bin that does not meet the S/N limit are given a spectral-index bin ID of -1.