NOEMA3D: a Comprehensive Census of the Molecular Gas Distribution & Kinematics of Massive Main-Sequence Star Forming Galaxies at the Peak and Winding Down of Galaxy Formation Activity

 

PIs: Reinhard Genzel (DE), Roberto Neri (IRAMF), Linda Tacconi (DE)

CoIs:
Natascha Förster Schreiber (DE), Dieter Lutz (DE), Karl-Friedrich Schuster (IRAMF), Alessandra Contursi (DE), Melanie Krips (IRAMF), Stefano Berta (IRAMF), T. Naab (DE), Richard Davies (DE), Minju Lee (DE), Sedona Price (DE), Thomas Taro Shimizu (DE), Eckhard Sturm (DE), Hannah Uebler (DE), Francoise Combes (FR), David Elbaz (FR), Pierre Cox (FR), Santiago Garcia-Burillo (ES), Antonio Usero (ES), Alberto D. Bolatto (US), Monica Rubio (CL), Tadayuki Kodama (JP), Rodrigo Herrera-Camus (CL), Ken-Ichi Tadaki (DE) (wrong email), Alvio Renzini (IT), Andreas Burkert (DE), Avishai Dekel (IL), S. Wuyts (GB), Cinthya Herrera-Contreras (IRAMF)

 

Project ID: L19MD

 

Observing bands: 1mm & 2mm

Configurations: A,C

Observing type:Single field mappings

 

Abstract:

We propose spatially resolved interferometric imaging of the distribution and kinematics of the molecular ISM in a well-characterized sample of ~50-60 massive (M* ~ 10^10.7-11.5 Msol) star-forming galaxies (SFGs) near and after the peak of galaxy growth at z~0.5-2.0, and later in the program at very high redshifts. NOEMA3D will address a wide range of topics in baryon cycling, star formation, feedback and quenching that are linchpins in the cosmic evolution of SFGs.  NOEMA3D requests 1150 hours of 11-antenna equivalent time over a 5-year period  (2019-2024).  It will deliver high-quality data sets on SFGs that will be of high legacy value to the IRAM community. Key science goals are: 1) to measure inner and outer disk rotation curves and velocity dispersions; 2) establish few kpc scale gas scaling relations; 3) search for molecular outflows; 4) determine sizes and distributions of gas, dust and rest-optical emission; 5) investigate bulge formation through the presence of nuclear gas/dust concentrations, and look for non-circular motions in the disk; and 6) investigate dense gas properties through stacking of weaker tracers.
 

 

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