tokens: its multiple imaging cross section at the redshift of the LAE in our sample will be comparable to or larger than the diameter of a BOSS fiber. As a result, the multiply imaged source search region associated with each CMASS galaxy is essentially the size of the fiber. This is very different from general studies of lens statistics (e.g.,Kochanek 1993a , 1993b , 1996 ; Maoz Rix 1993 ; Jaunsen et al. 1995 ; King Browne 1996 ; Möller et al. 2007 ) which must account for variations in the multiple imaging cross section with lens redshift, lens mass, and source redshift. Given this fact, our estimate of the magnification bias can be checked observationally by comparing the incidence of LAE detections in BOSS galaxy spectroscopic fibers to their incidence within the blank-sky fibers of the survey. To explore this, we rerun the full candidate selection procedure on BOSS sky fibers and obtain 9 candidates with - σ detection significance. This number can be compared to the 187 candidates found to this same significance threshold in the galaxy-fiber sample. Since there are approximately six times more galaxy fibers than sky fibers in the BOSS survey, we find that our high- z LAE detections occur with a frequency times higher in the galaxy fibers than in the sky fibers. This is consistent with the boost factor expected based on our simple magnification-bias calculation above: the higher relative incidence of LAE detections in the galaxy fibers thus suggests that the galaxy-fiber detections are highly magnified by strong lensing. We stress, however, that the close quantitative agreement between the predicted and observed detection-rate boost of galaxy fibers relative to sky fibers must be regarded as coincidental considering the rough approximations involved. 5. DISCUSSION We first emphasize that our spectroscopic selection technique is powerful and generic, and can be easily applied to a variety of scientific considerations with appropriate modifications. For instance, by changing the single-line detection strategy to detections for at least two of the lines [O ii ], [O iii ] 4959, 5007, H α , and H β at a common redshift, one can pick out lens candidates with star-forming galaxies as the background sources. That is exactly the approach adopted in the successful SLACS, BELLS, and S4TM surveys (Bolton et al. 2006a ; Brownstein et al. 2012 ; Shu et al. 2015 ). One can also specifically search for lensed quasars by tuning the selection criteria to the presence of more than one prominent quasar emission lines such as Ly α , C iv , C iii ], and Mg ii . Interested readers are encouraged to adopt the spectroscopic selection technique according to their own research interests. Although the size of the sample of galaxy–LAE lenses from our initial HST program seems to be relatively modest when compared to other galaxy-scale strong-lens samples, there are another 166 galaxy–LAE lens candidates remaining in the parent sample. We applied very stringent
ner_tags: O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O B-Citation I-Citation O B-Citation O B-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O B-Survey O O O O O O O O O O O O O O O O O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Survey I-Survey O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength B-Wavelength B-Wavelength I-Wavelength O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O B-Survey B-Survey O B-Survey O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O B-Telescope O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O