UVUDF: ULTRAVIOLET IMAGING OF THE HUBBLE ULTRA DEEP FIELD WITH WIDE-FIELD CAMERA 3
UVUDF: ULTRAVIOLET IMAGING OF THE HUBBLE ULTRA DEEP FIELD WITH WIDE-FIELD CAMERA 3
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UVUDF：使用宽视场相机 3 对哈勃超深场进行紫外线成像
DOI：
10.1088/0004-6256/146/6/159
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
A. Wolfe
中科院分区：
文献类型：
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作者：
H. Teplitz;M. Rafelski;P. Kurczynski;N. Bond;N. Grogin;A. Koekemoer;H. Atek;T. Brown;D. Coe;J. Colbert;H. Ferguson;S. Finkelstein;J. Gardner;E. Gawiser;M. Giavalisco;C. Gronwall;D. Hanish;Kyoung;D. D. de Mello;S. Ravindranath;R. Ryan;B. Siana;C. Scarlata;E. Soto;E. Voyer;A. Wolfe
我们提出了一个90轨道哈勃太空望远镜国库计划的概述，以获得哈勃超深场的近紫外成像，使用宽视场相机3 UVIS探测器与F225 W，F275 W和F336 W过滤器。本调查旨在：（1）研究星系在1 < z < 2.5处的星星形成活动高峰期，（2）通过分辨亚星系单位（团块）来探索大质量星系的演化，（3）研究z <2-3处星系电离辐射的逃逸分数，（4）大大提高测光红移估计的可靠性，（5）研究星系的电离辐射逃逸分数，（6）研究星系的电离辐射逃逸分数，（7）研究星系的电离辐射逃逸分数，（8）研究星系的电离辐射逃逸分数，（9）研究星系的电离辐射逃逸分数，（10）研究星系（5）测量z = 1-3的中性原子占主导地位的氢气的星星形成率效率。在这篇概述性的论文中，我们描述了调查的细节和数据减少的挑战，包括专门校准的必要性和电荷转移效率低下的影响。我们提供了一个鲜明的证明电荷转移效率低的影响，所得的数据产品，当不校正，导致不确定的光度，伸长的形态在读出方向，和微弱的源远离读出的损失。我们同意STScI的建议，即未来需要非常敏感的测量的UVIS观测使用仪器的能力，通过“后闪光”添加背景光。本文给出了紫外选择星系的计数和z = 1时星系形态的初步结果。我们发现，在红移1.7，2.1，和2.7的UV辍学的数密度是在很大程度上与公布的光度函数预测的数量一致。我们还证实了图像拼接具有足够的灵敏度和分辨率来支持对恒星形成团块演化的分析，根据滤波器和观测时期，在0.″2半径孔径下，在5σ处达到28- 29等深度。
We present an overview of a 90 orbit Hubble Space Telescope treasury program to obtain near-ultraviolet imaging of the Hubble Ultra Deep Field using the Wide Field Camera 3 UVIS detector with the F225W, F275W, and F336W filters. This survey is designed to: (1) investigate the episode of peak star formation activity in galaxies at 1 < z < 2.5; (2) probe the evolution of massive galaxies by resolving sub-galactic units (clumps); (3) examine the escape fraction of ionizing radiation from galaxies at z ∼ 2–3; (4) greatly improve the reliability of photometric redshift estimates; and (5) measure the star formation rate efficiency of neutral atomic-dominated hydrogen gas at z ∼ 1–3. In this overview paper, we describe the survey details and data reduction challenges, including both the necessity of specialized calibrations and the effects of charge transfer inefficiency. We provide a stark demonstration of the effects of charge transfer inefficiency on resultant data products, which when uncorrected, result in uncertain photometry, elongation of morphology in the readout direction, and loss of faint sources far from the readout. We agree with the STScI recommendation that future UVIS observations that require very sensitive measurements use the instrument's capability to add background light through a “post-flash.” Preliminary results on number counts of UV-selected galaxies and morphology of galaxies at z ∼ 1 are presented. We find that the number density of UV dropouts at redshifts 1.7, 2.1, and 2.7 is largely consistent with the number predicted by published luminosity functions. We also confirm that the image mosaics have sufficient sensitivity and resolution to support the analysis of the evolution of star-forming clumps, reaching 28–29th magnitude depth at 5σ in a 0.″2 radius aperture depending on filter and observing epoch.