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z-GAL -- A NOEMA spectroscopic redshift survey of bright Herschel galaxies: [III] Physical properties by Berta, S.; Stanley, F.; Ismail, D.; Cox, P.; Neri, R.; Yang, C.; Young, A. J.; Jin, S.; Dannerbauer, H.; Bakx, T. J.; Beelen, A.; Weiss, A.; Nanni, A.; Omont, A.; van der Werf, P.; Krips, M.; Baker, A. J.; Bendo, G.; Borsato, E.; Buat, V.; Butler, K. M.; Chartab, N.; Cooray, A.; Dye, S.; Eales, S.; Gavazzi, R.; Hughes, D.; Ivison, R. J.; Jones, B. M.; Lehnert, M.; Marchetti, L.; Messias, H.; Negrello, M.; Perez-Fournon, I.; Riechers, D. A.; Serjeant, S.; Urquhart, S.; Vlahakis, C. is a scholarly article available to read on EtoBox.

What is z-GAL -- A NOEMA spectroscopic redshift survey of bright Herschel galaxies: [III] Physical properties about?

The z-GAL survey observed 137 bright Herschel-selected targets with the IRAM NOrthern Extended Millimeter Array, with the aim to measure their redshift and study their properties. Several of them have been resolved into multiple sources. Consequently, robust spectroscopic redshifts have been measured for 165 individual galaxies in the range 0.8<z<6.5. In this paper we analyse the millimetre spectra of the z-GAL sources, using both their continuum and line emission to derive their physical properties. At least two spectral lines are detected for each source, including transitions of 12CO, [CI], and H2O. The observed 12CO line ratios and spectral line energy distributions of individual sources resemble those of local starbursts. In seven sources the para-H2O(2_11-2_02) transition is detected and follows the IR versus H2O luminosity relation of sub-millimetre galaxies. The molecular gas mass of the z-GAL sources is derived from their 12CO, [CI], and sub-millimetre dust continuum emission. The three tracers lead to consistent results, with the dust continuum showing the largest scatter when compared to 12CO. The gas-to-dust mass ratio of these sources was computed by combining the info

Author
Berta, S.; Stanley, F.; Ismail, D.; Cox, P.; Neri, R.; Yang, C.; Young, A. J.; Jin, S.; Dannerbauer, H.; Bakx, T. J.; Beelen, A.; Weiss, A.; Nanni, A.; Omont, A.; van der Werf, P.; Krips, M.; Baker, A. J.; Bendo, G.; Borsato, E.; Buat, V.; Butler, K. M.; Chartab, N.; Cooray, A.; Dye, S.; Eales, S.; Gavazzi, R.; Hughes, D.; Ivison, R. J.; Jones, B. M.; Lehnert, M.; Marchetti, L.; Messias, H.; Negrello, M.; Perez-Fournon, I.; Riechers, D. A.; Serjeant, S.; Urquhart, S.; Vlahakis, C.
Published
2023
Language
EN

More by Berta, S.; Stanley, F.; Ismail, D.; Cox, P.; Neri, R.; Yang, C.; Young, A. J.; Jin, S.; Dannerbauer, H.; Bakx, T. J.; Beelen, A.; Weiss, A.; Nanni, A.; Omont, A.; van der Werf, P.; Krips, M.; Baker, A. J.; Bendo, G.; Borsato, E.; Buat, V.; Butler, K. M.; Chartab, N.; Cooray, A.; Dye, S.; Eales, S.; Gavazzi, R.; Hughes, D.; Ivison, R. J.; Jones, B. M.; Lehnert, M.; Marchetti, L.; Messias, H.; Negrello, M.; Perez-Fournon, I.; Riechers, D. A.; Serjeant, S.; Urquhart, S.; Vlahakis, C.

Browse all works by Berta, S.; Stanley, F.; Ismail, D.; Cox, P.; Neri, R.; Yang, C.; Young, A. J.; Jin, S.; Dannerbauer, H.; Bakx, T. J.; Beelen, A.; Weiss, A.; Nanni, A.; Omont, A.; van der Werf, P.; Krips, M.; Baker, A. J.; Bendo, G.; Borsato, E.; Buat, V.; Butler, K. M.; Chartab, N.; Cooray, A.; Dye, S.; Eales, S.; Gavazzi, R.; Hughes, D.; Ivison, R. J.; Jones, B. M.; Lehnert, M.; Marchetti, L.; Messias, H.; Negrello, M.; Perez-Fournon, I.; Riechers, D. A.; Serjeant, S.; Urquhart, S.; Vlahakis, C.