What’s New in the DAP¶
MPL-9 (2.4.1)¶
High-level changes¶
Extensions
SPX_ELLCOO
andBIN_LWELLCOO
have a new channel. The 4 channels are now radius in arcsec, radius in \(R_{\rm eff}\), radius in \(h^{-1}{\rm kpc}\), and azimuth; the third channel is the new one. So the channels are:C1 = 'Elliptical radius' / Data in channel 1 U1 = 'arcsec ' / Units of data in channel 1 C2 = 'R/Re ' / Data in channel 2 U2 = '' / Units of data in channel 2 C3 = 'R h/kpc ' / Data in channel 3 U3 = 'kpc/h ' / Units of data in channel 3 C4 = 'Elliptical azimuth' / Data in channel 4 U4 = 'degrees ' / Units of data in channel 4The following extensions were added to the MAPS files:
EMLINE_SEW_CNT
: Continuum used for summed-flux equivalent-width measurementEMLINE_GEW_CNT
: Continuum used for Gaussian-fit equivalent-width measurementSPECINDEX_BCEN
: Flux-weighted center of the blue sideband in the spectral-index measurementSPECINDEX_BCNT
: Continuum level in the blue sideband used in the spectral-index measurementSPECINDEX_RCEN
: Flux-weighted center of the red sideband in the spectral-index measurementSPECINDEX_RCNT
: Continuum level in the red sideband used in the spectral-index measurementSPECINDEX_MODEL
: Index measurement made using the best-fitting stellar continuum model.All emission-line extensions now contain 35 lines, and channel ordering of the line list has changed compared to MPL-8. Current ordering is:
C01 = 'OII-3727' / Data in channel 1 C02 = 'OII-3729' / Data in channel 2 C03 = 'H12-3751' / Data in channel 3 C04 = 'H11-3771' / Data in channel 4 C05 = 'Hthe-3798' / Data in channel 5 C06 = 'Heta-3836' / Data in channel 6 C07 = 'NeIII-3869' / Data in channel 7 C08 = 'HeI-3889' / Data in channel 8 C09 = 'Hzet-3890' / Data in channel 9 C10 = 'NeIII-3968' / Data in channel 10 C11 = 'Heps-3971' / Data in channel 11 C12 = 'Hdel-4102' / Data in channel 12 C13 = 'Hgam-4341' / Data in channel 13 C14 = 'HeII-4687' / Data in channel 14 C15 = 'Hb-4862 ' / Data in channel 15 C16 = 'OIII-4960' / Data in channel 16 C17 = 'OIII-5008' / Data in channel 17 C18 = 'NI-5199 ' / Data in channel 18 C19 = 'NI-5201 ' / Data in channel 19 C20 = 'HeI-5877' / Data in channel 20 C21 = 'OI-6302 ' / Data in channel 21 C22 = 'OI-6365 ' / Data in channel 22 C23 = 'NII-6549' / Data in channel 23 C24 = 'Ha-6564 ' / Data in channel 24 C25 = 'NII-6585' / Data in channel 25 C26 = 'SII-6718' / Data in channel 26 C27 = 'SII-6732' / Data in channel 27 C28 = 'HeI-7067' / Data in channel 28 C29 = 'ArIII-7137' / Data in channel 29 C30 = 'ArIII-7753' / Data in channel 30 C31 = 'Peta-9017' / Data in channel 31 C32 = 'SIII-9071' / Data in channel 32 C33 = 'Pzet-9231' / Data in channel 33 C34 = 'SIII-9533' / Data in channel 34 C35 = 'Peps-9548' / Data in channel 35Fixed flux ratios of doublets were improved using the following calculation: \(\lambda_2/\lambda_1\ \cdot\ (M1_1+E2_1)/(M1_2+E2_2)\), where \(M1\) and \(E2\) are the magnetic dipole and electric quadrapole Einstein \(A\) coefficients and \(\lambda\) is the line wavelength. The Einstein \(A\) coefficients are all taken from NIST. In all but the [O II] 7320,7330 complex (not included in MPL-9 fit), the magnetic dipole term dominates such that the electric quadrapole terms are effectively irrelevant. The fixed flux ratios are:
- NeIII-3968/NeIII-3968 = 0.3
- OIII-4960/OIII-5008 = 0.35
- OI-6365/OI-6302 = 0.32
- NII-6549/NII-6585 = 0.34
- SIII-9071/SIII-9533 = 0.41
Lines with tied velocity dispersions (some because their fluxes are also tied) are:
- OII-3727 + OII-3729
- HeI-3889 + Hzet-3890
- NeIII-3968 + NeIII-3968
- OIII-4960 + OIII-5008
- NI-5199 + NI-5201
- OI-6302 + OI-6365
- NII-6549 + NII-6585
- SIII-9071 + SIII-9533
User-level changes/bug fixes¶
- Allow emission-line moment, modeling, and spectral-index keys to be
None
, meaning that the DAP only fits the stellar kinematics but still produces the MAPS and LOGCUBE files.- Added beta version of hierarchically clustered MaStar templates
- Added a script that computes the weights used during the
ppxffit_qa
plot construction.
Minor changes/bug fixes¶
- Hotfix to accommodate change in padding computation in
ppxf>=6.7.15
- Fixed units bug in
mangadap.proc.util.flux_to_fnu()
.- Fixed bug in templates when using
iteration_mode = 'global_template'
- Change from
time.clock()
totime.perf_counter()
- Bug fix in record array dimensionality when writing to binary table
- Minor plotting changes for Overview paper plots
- Fixed masking of emission-line chi-square measurements
- Remove
MASKNAME
header keyword inherited from DRP files
MPL-8 (2.3.0)¶
High-level changes¶
- Change to
DAPTYPE
construction.DAPTYPE
is nowbinning
-stellar templates
-emission-line templates
. This was done because in future releases we plan to switch the templates used for the stellar kinematics (likely to remainMILESHC
) to a different template set for the emission-line modeling with a longer spectral range to fit the full MaNGA spectral range.- Three additional emission-lines are fit: He I at 3889 angstroms, and the [N I] doublet at 5200 angstroms. The He I line has its dispersion tied to H:math:zeta at 3890, and the dispersions of the [N I] doublet are tied.
- The
MAPS
file extensions were modified:
STELLAR_SIGMACORR
now has two channels. The first provides the correction constructed using the same methodology as in MPL-7/DR15; the second provides a correction that we are currently testing for robustness as a replacement correction.- The data in the
STELLAR_CONT_FRESID
andSTELLAR_CONT_RCHI2
extensions has been consolidated into a new single extension,STELLAR_FOM
(FOM=figure-of-merit). Channel 3 ofSTELLAR_FOM
is the same asSTELLAR_CONT_RCHI2
, and channels 4 and 5 are the same as the two channels inSTELLAR_CONT_FRESID
. See the data model for the full description of the additional channels in this extension.- 4 additional channels are provided related to the emission lines:
EMLINE_GA
: The amplitude of the fitted GaussiansEMLINE_GANR
: The amplitude over noise of the fitted GaussiansEMLINE_FOM
: Full-spectrum figures-of-merit for the emission-line module; this now has exactly the same format as the STELLAR_FOM extensionEMLINE_LFOM
: The reduced chi-square in 15 pixel windows around each fitted emission line.- To make the files easier to use, the
LOGCUBE
extensions were modified:
- The
EMLINE_BASE
andEMLINE_MASK
extensions have been removed.- The following extensions have been added:
MODEL_MASK
is the mask to use with theMODEL
extension (the result of the emission-line+continuum fit)STELLAR
is best-fitting stellar continuum from the stellar continuum fitSTELLAR_MASK
is the mask for the stellar-continuum fit.- Numerous QA plots have been added; see the data model description.
Under-the-hood algorithmic changes¶
- Allow the emission-line fitter to use the bin ID numbers directly instead of matching the spaxels to bins by coordinate proximity
- Construction of the parameter tying object in the emission-line fitter is now done just before each spectrum is fit by ppxf (not globally in Sasuke) to better handle when components are omitted.
- When deconstructing bins into spaxels for the emission-line modeling (hybrid binning scheme), the second fit iteration only fits spaxels that are components of binned spectra and does not refit spectra that constitute an entire bin themselves. I.e. this removes some largely redundant fitting.
mangadap.proc.ppxffit.PPXFFit
andmangadap.proc.sasuke.Sasuke
include calculations of the chi-square growth; and changed the names of the growth columns in the reference files.- Changed definitions of \(A\) to be the model amplitude; \(A/N\) is the model amplitude divided by the median noise in the two sidebands defined for the emission-line EW calculation.
- Major changes to survey-level execution of the DAP, including that the input data is now pulled from the
DRPall
file instead of theplateTargets
files.- Ignore minimum \(S/N\) limitation in emission-line moments and spectral indices for hybrid scheme as a stop-gap to minimize differences in moments, models, and indices
BINID
.
User-level changes/bug fixes¶
- Fixed an error in setting up the tying structure passed to pPXF that led to the [O II] dispersion maps being fully masked.
- Fixed an error in the propagation of the error in the passband integral calculation, which affects the non-parameteric emission-line measurement errors (summed data) and the spectral index errors. The calculation is now formally correct, but these propagated errors are still underestimated with respect to more robust calculations via an MC.
- Fixed a bug that omitted the
FORESTAR
flag from getting propagated in the hybrid binning case.- Fixed \(\chi^2\) calculations reported in
MAPS
files (does not affect chi-square used during fit optimization) for both the stellar-continuum fit and the emission-line modeling.- Velocity-dispersion corrections are now applied to the spectral indices summary data provided in the
DAPall
file.- Fixed minor issue in propagating masks from the reference files to the maps files; primarily an issue for the hybrid binning scheme.
Minor changes/bug fixes¶
- Fixed the bug that led to the error in the sigma corrections for MPL-7, what were replaced before distributing these data via DR15.
- Fixed bug that was causing multiple instances of “Warning: converting a masked element to nan” during the emission-line moment measurements.
- Significant changes to the pixel resampling code, but has a minor effect on the results.