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Many studies of void galaxies’ properties, including optical spectra and photometry, have been published (e.g., Popescu et al., 1997, 1999; Grogin & Geller, 2000; Hogg et al., 2004; Rojas et al., 2005; Collobert et al., 2006; Patiri et al., 2006; Wegner & Grogin, 2008; Hoyle et al., 2012). Combined with H I surveys (Szomoru et al., 1996; Huchtmeier et al., 1997; Kreckel et al., 2011a, 2012, 2015; Ricciardelli et al., 2014; Moorman et al., 2014, 2015, 2016; Douglas et al., 2018), this has resulted in a general consensus that the lower density environments within which the void galaxies reside has only a small effect on their properties. KPNO International Spectroscopic Survey (KISS; Salzer et al., 2000; Gronwall et al., 2004b), which consists of a narrow survey strip that crosses through the void. Several previous studies have considered the metallicities of void galaxies (e.g., Peimbert & Torres-Peimbert, 1992; Cruzen et al., 2002; Kreckel et al., 2015; Douglas et al., 2018), with the latter two studies focusing primarily on dwarf galaxies. Our primary result is that there are no significant differences in the metallicities or the star-formation rates between the KR2 galaxies located in higher density regions and those found in voids

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820 star-forming KR2 galaxies. We present a direct comparison of the properties of the KR2 Boötes Void galaxies against the KR2 galaxies located in higher-density environments in Table 2 and Figure 13. Figure 13 presents histograms of observed and derived properties for the galaxies in the two samples, while Table 2 presents the sample mean (and its formal error) and median values for the various properties for both the void and high-density environment galaxies, as well as their minimum and maximum values. Since both samples were selected by KISS with the same selection function (e.g., Salzer et al., 2000), and since they have very nearly identical redshift distributions, any differences in properties present between the two samples should be due to the dramatically different environments probed by the two samples. Our study appears to rule out any significant differences in the metallicities and SFRs of galaxies as a function of local environment. Metallicities are derived using the O3N2 abundance calibration presented in Hirschauer et al. Spectroscopic observations for the KISS ELGs are presented in (Wegner et al., 2003; Gronwall et al., 2004a; Jangren et al., 2005b; Salzer et al., 2005b). These spectra were necessary for determining accurate redshifts and for ascertaining the activity type of each galaxy (e.g., star forming versus AGN)