Browsing by Author "Cori, W."

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    Multiband photometry of PSNJ14102342-4318437 with OAUNI
    (The Astronomer's Telegram, 2016-01-21) Pereyra, Antonio; Cori, W.; Ricra, J.; Tello, J.
    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) and (R-I) are in reasonable agreement with the zero-redshift color-color diagrams for Type Ib SNe about 20-30d past the maximum (Poznanski et al., 2002, PASP, 114, 833). The OAUNI project is supported by UNI, TWAS and IGP.
    Palabras clave:OpticalSupernovaeStars
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    OAUNI optical observation of the supernova ASASSN-15lp
    (The Astronomer's Telegram, 2015-08-26) Pereyra, Antonio; Cori, W.; Meza, E.; Ricra, J.; Zevallos, M.
    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.
    Palabras clave:OpticalSupernovaeStars