Using the Modified Nearest Neighbor Method to Correct Fiber-collision
  Effects on Galaxy Clustering
  Fiber collision is a persistent problem faced by modern spectroscopic galaxy
surveys. In this work, we propose a new method to correct for this undesired
effect, focusing on the clustering from the fiber-collision scale up to
$\lesssim 10 \rm Mpc\,h^{-1}$. We assume that the fiber-collided galaxies are
in association with their nearest three angular neighbors. Compared with the
conventional nearest-neighbor method, we have properly accounted for the
foreground (background) galaxies that are associated with the foreground
(background) cosmic webs relative to the nearest neighbor. We have tested the
new method with mock catalogs of the Sloan Digital Sky Survey (SDSS) Data
Release 7 (DR7). The test demonstrates that our new method can recover the
projected two-point correlation functions at an accuracy better than 1\% on
small (below the fiber-collision scale) to intermediate (i.e., $10 \rm
Mpc\,h^{-1}$) scales, where the fiber collision takes effect and the SDSS main
sample can probe. The new method also gives a better recovery of the
redshift-space correlation functions almost on all scales that we are
interested in.
