Available Data files

Reduced IFU data cubes

The reduced IFU data have been processed with the official MUSE pipeline and with Py3D for VIMOS and PMAS. They are fully calibrated, sky-subtracted and combined data cubes for each target. Given the difference in the used pipeline the data formation for the IFUs is a little different.

MUSE data

Extension	Header	Data
Primary HDU	Observational and Pipeline info	None
First HDU (DATA)	Basic header including WCS and wavelength parameters	Calibrated fluxes
Second HDU (ERROR)	Basic header	Statistical error on the fluxes

VIMOS and PMAS data

Extension	Header	Data
Primary HDU	Observational and pipeline info with WCS and wavelength parameters	Calibrated fluxes
First HDU (ERROR)	Basic header	Statistical error on the fluxes
Second HDU (ERRWEIGHT)	Basic header	Weighting for correlated errors (not important for these data)
Third HDU (BADPIX)	Basic header	Bad pixel flags, bad pixels may be unreliable

AGN data cubes

The AGN data cubes represent the AGN contribution to the reduced data cubes after the 3D AGN-host galaxy decomposition. The data format is the following:

Extension	Header	Data
PrimaryHDU	Observational and pipeline info with WCS and wavelength parameters	Calibrated fluxes of the AGN contribution

Host data cubes and binned host data cubes

The host data cubes represent the host contribution to the reduced data cubes after the 3D AGN-host galaxy decomposition The binned data are constructed from those data by doing a 8×8, 3×3, and 2×2 spaxel binning of the MUSE, VIMOS and PMAS data respectively. The data format is the following:

Extension	Header	Data
PrimaryHDU	Observational and pipeline info with WCS and wavelength parameters	Calibrated fluxes of the AGN contribution

Host continuum cubes

The Host data continuum cube contain the stellar continuum model based on PyParadise fits to the Host data cubes after AGN point-source subraction. The emission-line data cube can be re-constructed by subtraction the Host continuum model cubes from the Host data cubes. The data format is the following:

Extension	Header	Data
PrimaryHDU	Observational and pipeline info with WCS and wavelength parameters	Calibrated fluxes of the stellar continuum model

Full maps and binned maps

The map files contain the stellar/gas kinematics and the line fluxes as FITS images in a multi-Extension FITS file. The available Extensions are described below.

Extension	Header	Data
PrimaryHDU	Observational and pipeline info	None
STAR_VEL	WCS parameters and units	stellar radial velocity
STAR_VEL_ERR	WCS parameters and units	stellar radial velocity error
STAR_DISP	WCS parameters and units	stellar velocity dispersion
STAR_DISP_ERR	WCS parameters and units	stellar velocity dispersion error
ELINE_VEL	WCS parameters and units	radial velocity of emission lines
ELINE_VEL_ERR	WCS parameters and units	radial velocity error of emission lines
ELINE_DISP	WCS parameters and units	velocity dispersion of emission lines
ELINE_DISP_ERR	WCS parameters and units	velocity dispersion error of emission lines
ELINE_DISP	WCS parameters and units	velocity dispersion of emission lines
LINE	WCS parameters and units	emission line flux
LINE_ERR	WCS parameters and units	emission line flux error

Where LINE can be HEII4685, HBETA, OIII5007, NI5197, OI6300, OI6363, HALPHA, NII6583, SII6717, SII6730, ARIII7135, SIII9068

Spectroastrometry maps

The spectroastrometry files contain the line flux maps of the broad Hbeta, the core and wing [OIII] components in the central region of the IFU used to estimate their relative positions and shape. The flux scaling is in arbitrary units. Spatial pixel sampling is consistent with the reduced data cubes of the respective object. Only the distribution of light is considered important for the spectroastrometric analysis. The available Extensions are described below.

Extension	Header	Data
PrimaryHDU	Basic	None
HB_BLR_BR_DATA	Basic	Flux map of the broad Hbeta line component
OIII_BR_DATA	Basic	Flux map of the wing [OIII] line component
OIII_NR_DATA	Basic	Flux map of the core [OIII] line component
HB_BLR_BR_MODEL	Basic	Moffat PSF model to the broad Hbeta light distribution
OIII_BR_MODEL	Basic	scaled and shifted Moffat PSF model to the wing OIII light distribution
OIII_NR_MODEL	Basic	scaled and shifted Moffat PSF model to the core OIII light distribution
HB_BLR_BR_RES	Basic	Residual light of the best-fit Moffat PSF
OIII_BR_MODEL_RES	Basic	Residual light of the scaled and shifted Moffat PSF
OIII_NR_MODEL_RES	Basic	Residual light of the scaled and shifted Moffat PSF