NOAO >   Observing Info >   Approved Programs >   2018A-0222

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Program Information for 2018A-0222


PI: Joaquin Vieira, U. of Illinois Urbana-Champaign, jvieira@illinois.edu
Address: Department of Astronomy, 103 Astronomy Building, 1002 West Green Street, Urbana, IL, 61801 USA

CoI: Scott Chapman, Dalhousie University
CoI: Emily Pass, Dalhousie University
CoI: Tim Miller, Dalhousie University
CoI: Kaja Rotermund, Dalhousie University
CoI: Ryan Perry, Dalhousie University
CoI: Alexey Tikhomirov, Dalhousie University
CoI: Arif Babul, University of Victoria
CoI: Daniel Cunningham, Saint Mary's University
CoI: Kevin Lacaille, McMaster U.
CoI: Gil Holder, McGill University
CoI: Yashar Hezaveh, Stanford U.
CoI: Thomas Greve, University College London
CoI: Daniel Marrone, U. of Arizona
CoI: Manuel Aravena, ESO Chile
CoI: John Carlstrom, U. of Chicago
CoI: Justin Spilker, U. of Arizona
CoI: Brian Stalder, Harvard-Smithsonian Center for Astrophysics
CoI: Matthew Ashby, Harvard-Smithsonian Center for Astrophysics
CoI: Carlos De Breuck, ESO

Title: Optical followup of the SPT2052-55 protocluster at z=4.3

Abstract: We propose to obtain deep GMOS spectroscopy and imaging and Flamingos2 imaging towards SPT2052-55 at z=4.3. This system shares many similarities with SPT2349-56, the densest protocluster system discovered so far, which we have recently characterized using similar optical spectroscopy. While comparable to SPT2349-56 in many ways, SPT2052-55 also possesses distinct propeties: its activity is extended over a larger area, but it features two objects at its centre that are far more extreme than any present in the SPT2349-56 protocluster. Using ALMA, we have identified five SMGs in SPT2052-55 through their CO emission, with additional faint C+ emitters, and further sources expected in followup ALMA cy5 data. SPT2349-56 and SPT2052-55 illustrate the South Pole Telescope's remarkable potential as a protocluster-detecting device. With our analysis of SPT2052-55, along with SPT2349-56, we mark the beginning of a systematic characterization of structure formation in the universe. The proposed observations are essential to this goal, allowing us to obtain a census of the fainter UV-emitting galaxy population in this protocluster field. Our main goals with these observations are to (i) characterize the environment by identifying Lyman-break galaxies. The rich complimentary data will enable a full characterization of their properties; and (ii) probe the stellar masses of both the ULIRGs and the LBGs in the protocluster through deep Ks-band imaging (rest G-band).

Program Type: Standard/Extragalactic

Scheduled Nights:
Run 1 (2018A):  GEM-SQ/Flamingos2 -- 10.5hrs band 3 (GS-2018A-Q-303 )


National Optical Astronomy Observatory, 950 North Cherry Avenue, P.O. Box 26732, Tucson, Arizona 85726, Phone: (520) 318-8000, Fax: (520) 318-8360



NOAO >   Observing Info >   Approved Programs >   2018A-0222

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