Volume 575, March 2015
|Number of page(s)||32|
|Section||Cosmology (including clusters of galaxies)|
|Published online||26 February 2015|
Table A.1 lists the basic properties of the galaxies studied in the paper. All the sources from the Casertano et al. (2000) catalogue that fall within the field of view of the final MUSE data cube are included as well as sources without an entry in the Casertano et al. catalogue. Note that F814W magnitudes have been manually computed for a few objects that were missing in the Casertano et al. (2000) catalogue but were clearly present in the HST image. The table is sorted by increasing apparent F814W magnitude from the catalogue with no particular ordering of the sources without a catalogue magnitude.
The first column gives a running number which is the one used for ID#XX entries in the text. The subsequent two columns give the right ascenscion and declination from the MUSE observations, then follows the F814 SExtractor BEST magnitude from the Casertano et al. catalogue and the F606W − F814W colour from the BEST magnitudes. The redshift and its confidence follows thereafter, with the subsequent column indicating features identified in the spectrum. The final column gives the running number of the object in the Casertano et al. catalogue.
The second-to-last column, Nexp, gives the median number of exposures going into the reduction of the region where the spectrum was extracted. Recall that the exposures are 30 min in duration, so a value of 40 corresponds to an exposure time of 20 h. Our redshift catalogue is naturally less complete where Nexp < 30.
Table A.2 gives the emission line fluxes measures off the 1D spectra produced by straight summation. In this table only the 181 sources with redshift >0 with redshift confidence ≥1 are included. The procedure adopted for emission line flux measurements is given in Sect. 4.3. Note that the fluxes have been corrected for Galactic reddening using the Schlegel et al. (1998) dust maps using the reddening curve from O’Donnell (1994) for consistency with that work.
We emphasise that there has been no attempt to correct these fluxes to true total fluxes. In particular these fluxes are generally lower than those used in Sect. 6.3 which are aperture corrected. However the technique used in Sect. 6.3 is not suitable for all galaxies so we use the simpler approach here. Note also that the Lyα fluxes have been measured by fitting a Gaussian to an asymmetric line so are likely to give suboptimal flux measurements. Finally observe also that flux measurements are provided for all lines within the wavelength range of the spectrum, regardless of whether they were reliably detected or not.
Table A.3 gives the list of the redshift comparison between MUSE and published spectroscopic redshifts discussed in Sect. 4.4.
Basic data and redshifts on sources with spectra in the HDF-S.
Line fluxes for galaxies with secure redshifts in units of 10-18 erg s-1 cm-2 Å-1.
In addition to the source catalogue, we release the reduced data cube and associated files. We also deliver spectra and reconstructed images in the main emission lines for all the catalogue sources4.
© ESO, 2015
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