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Proceedings

Cold Gas in High-z Galaxies: CO as Redshift Beacon

MPS-Authors

Decarli,  R.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Carilli,  C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Casey,  C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Emonts,  B.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Hodge,  J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kohno,  K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Narayanan,  D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Riechers,  D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Sargent,  M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Walter,  F.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018ASPC..517..581D
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Citation

Decarli, R., Carilli, C., Casey, C., Emonts, B., Hodge, J., Kohno, K., et al. (2018). Cold Gas in High-z Galaxies: CO as Redshift Beacon.


Cite as: https://hdl.handle.net/21.11116/0000-0005-CE0E-5
Abstract
The goal of this chapter is to address the use of the ngVLA as a CO redshift machine for dust-obscured high-redshift galaxies which lack of clear counterparts at other wavelengths. Thanks to its unprecedented large simultaneous bandwidth and sensitivity, the ngVLA will be able to detect multiple low-J CO transitions at all redshifts > 1. In particular, at z ≥ 4.76 two CO transitions will be covered in a single frequency setting, thus ensuring unambiguous line identification. The ngVLA capabilities fill in a redshift range where other approaches (e.g., photometric redshifts, search for optical/radio counterparts, etc.) typically fail due to the combination of intrinsically faint emission and increasing luminosity distance. This will allow us to explore the formation of massive galaxies in the early cosmic times.