Differential photometry was applied on V893 Sco star, observed from the Astronomical Observatory of the Universidad Nacional de Ingeniería in Peru. From its light curve it was measured an orbital period of 0.076 days approximately. Moreover, spectroscopic analysis was performed on the HS 0220 + 0603 star, which data was acquired from a database. A fitting program was written in Python to find, out of several synthetic spectra of white dwarf and templates of red dwarf, the combination of a white dwarf and a red dwarf spectrum that fits best the HS 0220 + 0603 spectrum, thus we found that this spectrum is a composition of a white dwarf spectrum of 30000 K and surface gravity (log g) = 8.0, and a M5.5 type red dwarf star.

This work was supported by Convenio 102-2015 Fondecyt - Cienciactiva (OAUNI project, P.I. Antonio Pereyra) and Convenio 168-2015 UNI-MINEDU-CONCYTEC (doctorate scholarship for W.C. at Universidad Nacional de Ingenier´ıa). We thank Instituto Geof´ısico del Per´u for lodging at Observatorio de Huancayo during photometric observations at OAUNI and Grupo Astronom´ıa members for their help on these observations. Spectroscopic part of this work was based on observations made with ESO Telescopes at the La Silla Paranal Observatory under program ID 074.D-0657(A). This research has made use of the Spanish Virtual Observatory (http://svo.cab.inta-csic.es) supported from the Spanish MINECO/FEDER through grant AyA2014-55216. We also thank to the editors, Ener Salinas, Harold Blas and Rosendo Ochoa, for their useful suggestions and corrections.

We report multiband photometry of Type Ib SN PSNJ14102342-4318437 (ATel #8415, ATel #8434, ATel #8437, ATel #8504) on 2016-01-10 (UT) gathered with the OAUNI 51cm telescope (Pereyra et al. 2015; arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging using VRI filters was performed under non-photometric conditions (seeing ~1.9") and airmass = 1.4. Total integration times of (30x20s=600s) for V and R filters, and (24x20s=480s) for I filter yielded: Date (UT) | filter | mag 2016-01-10.385 | V | 16.79 +/- 0.06 2016-01-10.395 | R | 15.93 +/- 0.12 2016-01-10.409 | I | 15.68 +/- 0.10 USNO-B1 field stars were used for the zero point calibration. The measurements presented here are ~25d after the MASTER discovery (ATel #8415) and ~32d after the maximum (ATel #8434). Consistent with this, and considering the NED extinction toward the host galaxy (NGC5483, z=0.006), the color indices (V-R) an...

During the commissioning runs of the National University of Engineering's Astronomical Observatory (OAUNI) project, we report optical imaging of the Type Ia SN ASASSN-15lp (ATel #7691, ATel #7692) on 2015-07-17.352 (UT). The measurement was gathered using the OAUNI 51cm telescope at the Huancayo Observatory, Peru (3300 masl at the central peruvian Andes). The observation was made under non-photometric clear skies and through an airmass of 1.4. A 180-second exposure in V filter yielded V = (15.86 +/- 0.05) mag. The zero point calibration was obtained using comparison stars in the neighborhood of the field. Our measurement is 28 days after the discovery (ATel #7691) and caution must be taken for contamination with the host galaxy. The OAUNI project is supported by UNI, The World Academy of Sciences (TWAS) and IGP.