tokens: be the H ii regions misidentified as galaxies. Thus, follow-up may be needed to confirm this parallel sequence. Figure 13. Zoom-in regions of the M r / and M * / diagrams. The dashed–dotted lines indicate the separation between the fainter paralleled sequence and the main population of galaxies. 127 common galaxies from both panels are color coded by redshift, while the distinct ones are shown by the gray color. Four outliers on the left side of each panel are actually three galaxies, for which two outliers with are two H ii regions in the same galaxy. Alternatively, the distribution of the individual field for each panel in Figure 12 also has been shown in Figure 14 . Figure 14. Same as Figure 12 but for individual fields. Each galaxy has been color coded by redshift. The histograms of each unique color index are shown on the right side of the panel. 6. Summary We present here a spectroscopic redshift catalog from the LAMOST Key Project, LaCoSSPAr, which is designed to observe all sources (Galactic and extragalactic) by using repeating observations with a limiting magnitude of in two FOVs in the SGC. The project is mainly focusing on the completeness of LEGAS in the SGC, the deficiencies of source selection methods and the basic performance parameters of the LAMOST telescope. Two chosen FOVs represent the relatively lower (Field A) and higher (Field B) density of galaxies. Targets in the FOV are mainly consisted of stars, galaxies, quasars, and u -band variables, as well as complementary H ii regions. We conduct the observation from 2012 September to 2014 January. Field A contains 2519 galaxies and 13,930 stars in which 2447 () and 13,278 () of them have been observed (97%) with 5 B () and 12 F plates (), respectively. Field B contains 3104 galaxies and 11,381 stars in which 2995 () and 10,224 () of them have been observed with 6 B and 5 F plates, respectively. The raw data have been reduced with LAMOST 2D and 1D pipelines. An additional post-processing has been applied to the LAMOST 1D spectrum to remove the majority of remaining sky background residuals. More than 10,000 spectra have been visually inspected to measure redshift by using combinations of different emission/absorption features with a uncertainty of . All galaxies have been divided into two categories as emission and absorption line galaxies, depending on whether there are obvious emission lines appeared or not. In total, 1528 redshifts ( of observed galaxies; including 623 absorption and 905 emission line galaxies) have been measured in Field A with a median value of z = 0.125 and a range from 0.001 to 1.598 (99% at ). For Field B, 1570 redshifts ( of observed galaxies; including 569 absorption and 1001 emission line galaxies) have been measured with a median value of z = 0.0952 and a range from 0.006 to 3.148 (99% at ). The results show that it is possible to derive redshift from low S/N galaxies with our post-processing and visual inspection, since the S/N r is less than
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