研究目的
Investigating the physical properties of Hα emitters (HAEs) associated to the protocluster 4C23.56 at z ～ 2.5.
研究成果
The detected HAEs are all massive and the amount of dust extinction is Av > 1.3. For extreme cases, Av is > 3, suggesting extremely dusty. These galaxies are scattered near the main sequence defined at z ～ 2.5. At least one of them is above the main sequence and likely experiencing starburst-like phase.
研究不足
The detection rate and the sample size are limited and the resolution is yet large to look in details of the galaxy structure.
1：Experimental Design and Method Selection:
The study uses continuum observations at submm (270 GHz) and radio (3 GHz) frequencies with ALMA and JVLA to investigate the physical properties of HAEs.
2：Sample Selection and Data Sources:
Targets 19 and 24 HAEs in the FoV of each observation.
3：List of Experimental Equipment and Materials:
Atacama Large Mm/submm Array (ALMA) and K. Jansky Very Large Array (JVLA).
4：Experimental Procedures and Operational Workflow:
Deep and high resolution (～
5：6 - 7) observations with ALMA and JVLA that reach r.m.s. level of ～ 1 mJy at 1 mm and ～1-4 μJy at 10 cm (1σ). Data Analysis Methods:
Comparing the derived SFRs from submm, radio and Hα emission, and excluding HAEs having AGN signatures with a help of ancillary data sets.
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