Gaze mechanisms enabling the detection of faint stars in the night sky.
Gaze mechanisms enabling the detection of faint stars in the night sky.
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DOI：
10.1111/ejn.15335
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发表时间：
2021-08
期刊：
影响因子：
--
通讯作者：
Martinez-Conde S
中科院分区：
文献类型：
--
作者：
Alexander RG;Mintz RJ;Custodio PJ;Macknik SL;Vaziri A;Venkatakrishnan A;Gindina S;Martinez-Conde S
几千年来，人们一直使用“回避视觉”来改善他们对微弱天体的探测，这一技术最早记录于公元前325年左右。然而，没有研究评估视线转移时的位置，以确定什么样的模式最有利于感知。在这里，我们第一次记录了适应黑暗的人类参与者的眼睛位置，同时描述了回避视觉的特征。我们模拟了视星等为3.3和3.5的恒星，将它们的亮度与Megrez（北斗七星中最暗的星星）和Tau Ceti相匹配。参与者指出是否每个星星是可见的，从一系列的固定位置，提供了一个全面的地图，在所有方向的检测性能。与先前的预测相反，最大的检测首先在距离星星约8°处实现，比单独从棒锥分布预期的更接近中央凹。这些发现挑战了在视杆密度峰值处进行最佳检测的假设，并首次对人类视觉的古老方面进行了系统评估。2,000多年来，天文学家一直使用“转移视觉”来改善他们对天体的探测。我们跟踪眼睛的位置，在转移视力，以确定凝视模式，产生最佳的星星检测，为第一次。与先前的预测相反，在距星星约8-14°处，可探测性最高，该预测认为峰值星星探测应该与视网膜杆密度的峰值重叠。
For millennia, people have used “averted vision” to improve their detection of faint celestial objects, a technique first documented around 325 BCE. Yet, no studies have assessed gaze location during averted vision to determine what pattern best facilitates perception. Here, we characterized averted vision while recording eye-positions of dark-adapted human participants, for the first time. We simulated stars of apparent magnitudes 3.3 and 3.5, matching their brightness to Megrez (the dimmest star in the Big Dipper) and Tau Ceti. Participants indicated whether each star was visible from a series of fixation locations, providing a comprehensive map of detection performance in all directions. Contrary to prior predictions, maximum detection was first achieved at ~8° from the star, much closer to the fovea than expected from rod-cone distributions alone. These findings challenge the assumption of optimal detection at the rod density peak and provide the first systematic assessment of an age-old facet of human vision. For over 2,000 years, stargazers have used “averted vision” to improve their detection of celestial objects. We tracked eye position during averted vision to determine the gaze patterns that produce optimal star detection, for the first time. Detectability was highest at ~8–14° from the star, contrary to prior predictions that peak star detection should overlap with the peak of retinal rod density.
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影响因子：
3.4
作者：
Alexander RG;Macknik SL;Martinez-Conde S
通讯作者：
Martinez-Conde S
影响因子：
2.3
作者：
BRIDGEMAN, B;MACKNIK, SL
通讯作者：
MACKNIK, SL
影响因子：
1.8
作者：
BALL, K;SEKULER, R
通讯作者：
SEKULER, R
影响因子：
2
作者：
Alexander, Robert G.;Schmidt, Joseph;Zelinsky, Gregory J.
通讯作者：
Zelinsky, Gregory J.
DOI：
10.1073/pnas.88.11.4966
发表时间：
1991-06-01
影响因子：
11.1
作者：
KARNI, A;SAGI, D
通讯作者：
SAGI, D