Near-Infrared Spectroscopy of Galaxies During Reionization: Measuring CIII] in a Galaxy at
arXiv:1905.08812 · doi:10.3847/1538-4357/ab22a2
Abstract
We present Keck/MOSFIRE -band spectroscopy targeting CIII] 1907,1909 in a galaxy previously identified via Ly emission. We detect strong line emission at m with a line flux of () erg s cm. We tentatively identify this line as [CIII] 1907, but we are unable to detect CIII] 1909 owing to sky emission at the expected location. This gives a galaxy systemic redshift, , with a velocity offset to Ly of v = km s. The ratio of combined CIII]/Ly is 0.30-0.45, one of the highest values measured for any galaxy. We do not detect SiIII] 1883, 1892, and place an upper limit on SiIII]/CIII] 0.35 (). Comparing our results to photoionization models, the CIII] equivalent width (WÅ), low SiIII]/CIII] ratio, and high implied [OIII] equivalent width (from the /IRAC [3.6][4.5]0.8 mag color) require sub-Solar metallicities () and a high ionization parameter, logU . These results favor models that produce higher ionization, such as the BPASS models for the photospheres of high-mass stars, and that include both binary stellar populations and/or an IMF that extends to 300 M. The combined CIII] equivalent width and [3.6][4.5] color are more consistent with ionization from young stars than AGN, however we cannot rule out ionization from a combination of an AGN and young stars. We make predictions for spectroscopy using these different models, which will ultimately test the nature of the ionizing radiation in this source.
arXiv comment19 pages, 12 figures, accepted for publication in ApJ
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