VizieR Online Data Catalog: NIR lines for AGN up to z~3 (Calabro+, 2023)

Measurements of emission lines from fully calibrated spectra observed with JWST/NIRSpec in M-grating mode (R=1000) for 90 emission line galaxies in CEERS in the redshift range 1<z<3. The emission lines are modeled as Gaussians and fitted with MPFIT (Markwardt et al., 2009, Astronomical Data Analysis Software and Systems XVIII, 411, 251 doi:10.48550/arXiv.0902.2850) following the procedure explained in Section 2.2 of the paper. The spectroscopic redshift zspec and the velocity width sigma of the lines are first determined from the highest S/N emission line (typically Hα or [SIII] 9530.65Å). and then fixed when fitting the remaining lines, with a tolerance of 500km/s and 100km/s, respectively. The Hβ+[OIII] line complex in the optical is fitted simultaneously, that is, assuming a single redshift, line velocity width, and underlying continuum in the form of first order polynomial. The same approach is followed when fitting the H-alpha + [NII] complex, the [SII] doublet, the HeI+Paγ complex, and the [FeII]+Paβ complex. In this table we report the results (including redshift, flux, flux uncertainty, underlying continuum, and line width) for the emission lines ranging from Hβ to Paα.

When upper limit flag (f in f_Flux) the flux of the corresponding emission line should be treated as an upper limit at 1sigma. For the broad line AGNs selected in the paper, the flux, redshift, and velocity width of permitted lines always refer to the narrow component.

(1 data file).