{'fraction_non_alphanumeric': 0.03346613545816733, 'fraction_numerical': 0.05458167330677291, 'mean_word_length': 4.96437054631829, 'pattern_counts': {'":': 0, '<': 0, '<?xml version=': 0, '>': 0, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 0, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
COMMISSIONS G1 AND G4 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS

New photometry and radial velocities of the eclipsing binary GSC 3870–01172 are reported. Simultaneous analysis of the data using the Direct Distance Estimation method yields the absolute parameters, as well as the distance to the binary. A comparison of the distances and proper motions indicates that the nearby star GSC 3870-01361 may be a third component of the system. GSC 3890-01172 was identified as a candidate W Ursae Majoris (W UMa) eclipsing binary star by the Northern Sky Variability Survey (Hoffman et al., 2009). The observations reported herein confirm that the system is indeed a W UMa binary. Standardized photometric observations in 2013 and 2016 show that the system has partial eclipses and exhibits small night-to-night variations. Radial velocities measured for both components allow us to perform a simultaneous solution that includes the distance to the system as an adjustable parameter. The photometric observations were made at the Sonoita Research Observatory near Sonoita, AZ using a 0.5m folded Newtonian telescope and a Santa Barbara Instrument Group STL-6303 CCD camera with Johnson-Cousins BV filters. The images were calibrated in the usual way by bias/dark subtraction and then flatfielding using IRAF (Tody, 1993). Instrumental magnitudes were then measured using PSF fitting with SExtractor (Bertin & Arnouts, 1996) and PSFEx (Bertin, 2011). Using the method described in Terrell et al. (2016), the instrumental magnitudes were transformed onto the standard system using APASS standards (Henden et al., 2012) from Data Release 9 (APASS DR9). The standard BV magnitudes are available from the IBVS web site as file 6247-t2.txt. From 2016 to 2018, spectroscopic observations were made with the 1.85m Plaskett telescope at the Dominion Astrophysical Observatory in Victoria, British Columbia. The 21181 configuration of the spectrograph was employed with a grating of 1800 lines/mm, blazed at 5000 Å, giving a reciprocal linear dispersion of 10 Å/mm in the first order. The wavelengths ranged from 5000 to 5260 Å, approximately. Frame reduction was performed by the software RaVeRe (Nelson 2013). See Nelson (2010) and Nelson et al. (2014) for further details. Radial velocities were determined using the Rucinski broadening functions (Rucinski, 2004; Nelson, 2010) as implemented in the software Broad (Nelson, 2013; Nelson et al., 2014). Table 1 gives the details of the radial velocity observations.