Spatial Binning
Analysis class: SpatiallyBinnedSpectra
Method definition: SpatiallyBinnedSpectraDef
Reference root: $MANGA_SPECTRO_ANALYSIS/$MANGADRP_VER/$MANGADAP_VER/common
Reference file: manga-[PLATE]-[IFUDESIGN]-[DRPQA_KEY]-[BIN_KEY].fits.gz
Config files: $MANGADAP_DIR/mangadap/config/spatial_binning
Example config: vor10.ini
[default]
key = VOR10
galactic_reddening = ODonnell
galactic_rv = 3.1
method = voronoi
minimum_snr = 1.0
operation = mean
velocity_register = False
stack_covariance_mode = channels
stack_covariance_par = 11
target_snr = 10
Important class dependencies:
GalacticExtinction
: Provides the Galactic extinction curves the can be selected and applied to the data.
mangadap.proc.spatialbinning
: Provides the classes that perform the binning (e.g.,VoronoiBinning
).
SpectralStack
: Provides the core functions that perform the spectral stacking
Algorithm:
Ignore any pixels that are either masked by the boolean mask or flagged with the flags returned by
do_not_use_flags()
.Calculate the Galactic extinction (
REDCORR
in the DAPLOGCUBE
file)Using
ReductionAssessment
object, find spaxels with >0.8 fractional spectral coverage and above theminimum_snr
in the configuration file. Only those spaxels satisfying both criteria are included in any bin.Determine which spaxels to put in each bin following the
method
specified in the config file:
none
(SPX
binning type): No binning performed. Every selected spaxels given a unique bin ID.
global
(ALL
binning type): Bin all valid spaxels into a single spectrum.
radial
(e.g.,NRE
binning type): Use the elliptical coordinates from theReductionAssessment
object to assign each spaxel to a unique radial bin. The binning annuli are defined using thecenter
,pa
,ell
,radius_scale
,radii
, andlog_step
config values; see$MANGADAP_DIR/mangadap/config/spatial_binning/nre.ini
for theNRE
binning case. Ifpa
,ell
, orradius_scale
are -1, they are replaced bypa
,ell
, andreff
, respectively, from The DAP Datacube Configuration File.
voronoi
(e.g.,VOR10
binning type): Use the Voronoi tessellation binning algorithm (written by M. Cappellari; see vorbin) to continually accrete adjacent spaxels to reach a minimum S/N (set bytarget_snr
in config), accounting for covariance if available, using the signal and noise measurements from theReductionAssessment
object.Stack all spectra assigned to a single bin:
Spectra are combined following the specified
operation
in config. Available options are set byoperation_options()
.Account for covariance according to
stack_covariance_mode
andstack_covariance_par
in config. Available options are set bycovariance_mode_options()
.Mask any wavelength channels in each spaxel with no unmasked pixels from the stack (maskbit set to
FLUXINVALID
in DAPLOGCUBE
file).Construct the map with the bin ID of each spaxel (
BINID
inMAPS
file)Calculate the mean signal (
BIN_MFLUX
inMAPS
file), variance (inverse ofBIN_MFLUX_IVAR
inMAPS
file) and S/N (BIN_SNR
inMAPS
file) of the stacked spectra. This is done over the same band/wavelength range as done for the individual spaxel data for theReductionAssessment
object.Using the mean signal from the
ReductionAssessment
object, calculate the luminosity-weighted on-sky (BIN_LWSKYCOO
inMAPS
file) and elliptical (BIN_LWELLCOO
inMAPS
file) coordinates. Also calculate the unweighted coordinates; the latter are not provided in the outputMAPS
file.Calculate the area of each bin (
BIN_AREA
inMAPS
file), and the ratio of that area to the expected area (BIN_FAREA
inMAPS
file) of the binning procedure. The latter is only relevant to the radial binning, where the expected area is the area of the bin annulus.Apply the Galactic reddening correction to the binned spectra, where the reddening law is defined by the
galactic_reddening
andgalactic_rv
parameters, and the E(B-V) value is taken from the DRP header keywordEBVGAL
; seeGalacticExtinction
. The valid reddening laws are:
ODonnell
: seereddening_vector_ccm()
.
CCM
: seereddening_vector_ccm()
.
FM
: seereddening_vector_fm()
.
Calzetti
: seereddening_vector_calzetti()
.
Note
Internally, the DAP performs all spectral fitting on the binned
spectra (termed as such even if a bin only contains a single spaxel)
after they have been corrected for Galactic extinction.
Therefore, the output emission-line fluxes have been corrected for
Galactic extinction. However, the models and binned spectra in the
output LOGCUBE
file are reverted to their reddened values for
direct comparison with the DRP LOGCUBE
file.