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tokens: is listed in Table 1 , and plotted in Figure 2 together with LAE LFs at z ∼ 5.7–7.3 from the literature. The LF shows dramatic evolution not only in normalization, but also in the shape. Figure 2. Top: the Ly α LFs of LAE surveys at z ∼ [5.7, 6.6, 7, 7.3]. The red filled circles show our results at z ∼ 7 from the LAGER-COSMOS field. References: Ly α LFs at z = 5.7 from Ouchi et al. ( 2008 ; blue filled squares), Konno et al. ( 2017 ; blue filled stars), and Santos et al. ( 2016 ; light-blue filled hourglass), at z = 6.6 from Ouchi et al. ( 2010 ; green filled squares), Konno et al. ( 2017 ; green filled stars), and Santos et al. ( 2016 ; dark-green filled hourglass), at z ∼ 7 from this work (red filled circles) and Ota et al. ( 2010 ; pink empty circles with plus), and at z = 7.3 from Shibuya et al. ( 2012 ; purple empty circles), and Konno et al. ( 2014 ; purple empty circles with cross). The colored regions in blue and green show the best Schechter fit with ±1 σ error in L * at z ∼ 5.7 and 6.6, respectively, from Konno et al. ( 2017 ). The solid and dashed lines in red (gray) show the best Schechter fits at z ∼ 6.9 with L range 42.65 ≤ log 10 L ≤ 43.25 (42.65 ≤ log 10 L ≤ 43.65) (see Table 2 ). A truncated Schechter function is also plotted (red solid line, see the text for details) to measure the bright-end LF bump. The purple line shows the best Schechter fit at z ∼ 7.3 from Konno et al. ( 2014 ). All these Schechter fits have a fixed faint-end slope of α = −2.5. Bottom: the histogram of Ly α luminosities of LAGER LAEs. The average completeness fraction for our LAEs interpolated from Section 2.2 is also plotted as a red solid line with red triangles. Table 1 Ly α Luminosity Function at z ∼ 7 from LAGER-COSMOS Field Note. a 1 σ Poisson errors from Gehrels ( 1986 ). The relatively fainter end of our LF (42.65 ≤ log 10 L Ly α ≤ 43.25) at z ∼ 7 can be fitted with a a single Schechter function in the form ofBecause our survey does not go far below L *, we fix α = −2.5 in our fitting, which is suggested from recent studies on Ly α LFs at z = 5.7 and z = 6.6 by Konno et al. ( 2017 ). Konno et al. ( 2017 ) report the largest narrowband surveys to date for LAEs at z = 5.7 and z = 6.6 taken with Subaru HSC on the 14–21 deg 2 sky, and their best-fit Schechter function analyses also include the smaller but much deeper narrowband surveys taken with Subaru Suprime-Cam (Ouchi et al. 2008 , 2010 ) at the corresponding redshifts. Considering that the Ly α LFs by Konno et al. ( 2017 ) are derived from the largest LAE samples at z = 5.7 and z = 6.6 with the widest luminosity range, and we have used consistent selection and analysis methods, we choose their Ly α LFs for comparison in the following sections. At z > 7, we choose the Ly α LF at z = 7.3 by Konno et al. ( 2014 ) for comparison. The best-fit Schechter function parameters of these LFs are listed in Table 2 and plotted in the upper panel of Figure 3 . We find a large drop in Φ of Ly α LF, compared