VizieR Online Data Catalog: High-z H-II star-forming galaxies (Gonzalez-Moran+, 2021)

We use a new set of high resolution spectrophotometric observations of high redshift HIIG obtained with KMOS at the ESO VLT to improve the constraints in the parameters space of the DE EoS and Ωm on the crucial range of intermediate redshift 1.2 < z < 2.6.

The sample of 96 star-forming galaxies was selected from references list (see note (1) in tablea1.dat description) and following the criteria described in detail in Gonzalez-Moran et al. 2019MNRAS.487.4669G. The candidates have high rest-frame equivalent width (EW) in their emission lines in a range of 1.2 < z <1.7 and 1.9 < z < 2.6 in order to observe either Halpha or Hbeta and O III lines in the H band and K-band.

The data were obtained in service mode from 2016 June to 2017 July for period 97A with a total of 16 Observing Blocks (OBs) distributed in two fields on the cosmological field Q2343 (Steidel et al. 2004ApJ...604..534S; Erb et al. 2006ApJ...646..107E, 2006ApJ...647..128E, Cat. J/ApJ/647/128) and from 2016 December to 2017 October for the 98A period, distributed in five FoV on three cosmological fields: the Ultra Deep Survey (UDS; Cirasuolo et al. 2007MNRAS.380..585C; Lawrence et al. 2007MNRAS.379.1599L, Cat. II/314 and II/319), GOODS-South Deep (GSD; Giavalisco et al. 2004ApJ...600L..93G, Cat. II/261), and the Cosmic Evolution Survey (COSMOS; Koekemoer et al. 2007ApJS..172..196K; Scoville et al. 2007ApJS..172....1S), each OB with ~40 min exposure time.

The observed sample is presented in Table A1. The target name is given in the first column, the coordinates in the second and third columns, the cosmological field that each object belongs to in column 4, the seeing in arcseconds corrected by airmass during the field observations in column 5, the total exposure time per target in seconds in column 6, and the reference from where the candidates were selected in column 7.

After data reduction permetting to do a selective sort on candidates having or not emission lines dectection and a signal to noise ratio S/N sufficient to determine the line width with the needed accuracy. It remains 54 objects which form the sample showed in tablea2.dat.

Next, we have selected only those HIIG that have a logarithmic velocity dispersion (logσ - {epsilon}_logσ<= 1.83) that minimizes the probability of including rotationally supported systems, leaving 41 objects (29 news HIIG + 15 HIIG already studied with MOSFIRE). Finally, joining KMOS data with previous ones (e.g see note (2) in tablea3.dat description), giving the total sample of 181 HIIGs for the cosmological analysis exhibited in tablea3.dat.

(3 data files).