PI: Haojing Yan, University of Missouri-Columbia, firstname.lastname@example.org
Address: Physics Department, University of Missouri, Columbia, MO 65201, USA
CoI: Mauro Stefanon, University of Missouri-Columbia
Title: DECam \boldmath z and \boldmath Y-band Imaging of the H-ATLAS SDP Field
Abstract: The very-wide-field \it Herschel surveys have resulted in hundreds of thousands of bright FIR/sub-mm sources awaiting further exploration. However many of them are still lacking optical identifications, which severely hampers the follow-up studies. Intertwined with the problem that lots of these FIR sources are intrinsically optical-faint due to their dusty nature, the source blending problem due to the large beam sizes of the \it Herschel instruments is a severe limitation. Nevertheless, the blended sources can be decomposed if the positions of the major components can be determined from the higher resolution optical data. For this purpose, optical images much deeper than the SDSS are in demand, and ideally they should cover the entire optical range in multiple bands for ease of studying their properties. We propose to do medium-deep DECam z and Y-band imaging of the H-ATLAS SDP field, which is \it currently the only wide, equatorial Herschel survey field that has \underline public data in both PACS and SPIRE passbands and can be accessed from both hemispheres. While it was designed primarily for science at z<1, the H-ATLAS is sensitive enough to detect non-lensed ULIRG to z>3 and beyond. In particular, its multiple FIR bands will enable direct measurement of the total IR luminosities without relying on extrapolation. Our DECam request in z and Y-bands is part of a larger program to acquire multi-wavelength data (optical to radio) in its SDP field to add to its legacy value. The counterpart program is to acquire imaging data in ugri-bands at the CFHT/Megacam, and the u- band component will be executed in the coming Nov-Jan season. Combining all these data with the WISE images after the similar source deblending procedures, we will construct reliable UV-to-FIR SEDs for future studies. In particular, we will be able to study the relation between the ULIRG phase and the underlying stellar populations, and the contribution of ULIRG to the global star formation rate density at z>1.
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