Suzuki, Tomoko L. and Kodama, Tadayuki and Onodera, Masato and Shimakawa, Rhythm and Hayashi, Masao and Tadaki, Ken-ichi and Koyama, Yusei and Tanaka, Ichi and Sobral, David and Smail, Ian and Best, Philip N. and Khostovan, Ali A. and Minowa, Yosuke and Yamamoto, Moegi (2017) 'The interstellar medium in [O iii]-selected star-forming galaxies at z ∼ 3.2.', Astrophysical journal., 849 (1). p. 39.
We present new results from near-infrared spectroscopy with Keck/MOSFIRE of [O III]-selected galaxies at z ~ 3.2. With our H and K band spectra, we investigate the interstellar medium (ISM) conditions, such as ionization states and gas metallicities. [O III] emitters at z ~ 3.2 show a typical gas metallicity of 12 log O H 8.07 0.07 + = ( ) at * log 9.0 9. () – M M ~ 2 and 12 log O H 8.31 0.04 + = ( ) at * log 9.7 10.2 () – M M ~ when using the empirical calibration method. We compare the [O III] emitters at z ~ 3.2 with UV-selected galaxies and Lyα emitters at the same epoch and find that the [O III]-based selection does not appear to show any systematic bias in the selection of star-forming galaxies. Moreover, comparing with star-forming galaxies at z ~ 2 from the literature, our samples show similar ionization parameters and gas metallicities as those obtained by the previous studies that used the same calibration method. We find no strong redshift evolution in the ISM conditions between z ~ 3.2 and z ~ 2. Considering that the star formation rates at a fixed stellar mass also do not significantly change between the two epochs, our results support the idea that the stellar mass is the primary quantity to describe the evolutionary stages of individual galaxies at z > 2.
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|Publisher Web site:||https://doi.org/10.3847/1538-4357/aa8df3|
|Publisher statement:||© 2017. The American Astronomical Society. All rights reserved.|
|Record Created:||14 Nov 2017 11:28|
|Last Modified:||14 Nov 2017 13:34|
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