研究目的
To provide deep rest-frame optical/near-IR imaging over a large area of the sky with deep ground-based imaging available, specifically for studying galaxy evolution at high redshifts (z > 3) by mapping the rest-frame near-IR light from distant galaxies and identifying active galactic nuclei.
研究成果
SMUVS provides deep IRAC imaging and catalogs with high sensitivity and uniform coverage, enabling studies of galaxy evolution at high redshifts. The catalogs contain about 350,000 sources and are publicly available. The survey improves upon previous efforts in depth and area, facilitating cosmological investigations, though limitations exist for extended and very bright sources.
研究不足
The catalogs are not optimal for extended sources, which may be shredded into multiple objects. Photometry for very bright sources (brighter than ～13 AB mag) may be underestimated. Source confusion is significant at faint magnitudes, affecting photometric uncertainties. Incompleteness begins around 25 AB mag at 3.6 μm and 24.5 AB mag at 4.5 μm.
1：Experimental Design and Method Selection:
The survey used Spitzer's IRAC for deep imaging in the 3.6 and 4.5 μm bands over three UltraVISTA stripes in the COSMOS field. Data reduction involved custom techniques including sky background subtraction, artifact correction, and mosaicking with IRACproc. PSF-fitting photometry was performed using StarFinder.
2：6 and 5 μm bands over three UltraVISTA stripes in the COSMOS field. Data reduction involved custom techniques including sky background subtraction, artifact correction, and mosaicking with IRACproc. PSF-fitting photometry was performed using StarFinder.
Sample Selection and Data Sources:
2. Sample Selection and Data Sources: The data sources are the three easternmost UltraVISTA survey stripes in the COSMOS field, covering about 0.66 deg2. Ancillary data from previous surveys like S-COSMOS, SEDS, and SPLASH were incorporated.
3：66 degAncillary data from previous surveys like S-COSMOS, SEDS, and SPLASH were incorporated.
List of Experimental Equipment and Materials:
3. List of Experimental Equipment and Materials: Spitzer Space Telescope with the Infrared Array Camera (IRAC), VISTA telescope with VIRCAM for UltraVISTA data, and computational tools for data processing.
4：Experimental Procedures and Operational Workflow:
Observations were conducted over multiple epochs from 2005 to 2017, using raster mapping patterns with dithering. Data reduction included background subtraction, artifact correction, mosaicking, and source extraction with iterative PSF fitting.
5：Data Analysis Methods:
Photometry was performed using StarFinder for PSF fitting, with aperture corrections and uncertainty estimates. Catalogs were validated through comparisons with existing surveys and astrometric checks.
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