Notas Técnicas
Permanent URI for this collection
Browse
Recent Submissions
Item Open Access OAUNI photometry of SN 2023mkt(R. E. Rutledge, 2023-09-07) Pereyra, Antonio; Tello, J.; Alvarado, D.; Torre, E.; Zevallos, M.; de Almeida, L.We report photometry of Type Ia SN 2023mkt gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging in R filter was performed on two consecutive nights under non-photometric conditions with an airmass lower than 1.7. The integration time was 90x20s=1800s in both nights. Our measurements are indicated below: Date (UT) | filter |seeing (") | mag, 2023-08-18.082 | R | 2.1 | 16.02 +/- 0.01, 2023-08-19.079 | R | 2.4 |16.05 +/- 0.01. UCAC4 field stars were used for the zero point calibration. Our observations are ~6 weeks after SN 2023mkt discovery date. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).Item Open Access OAUNI photometry of SN 2023fyq(R. E. Rutledge, 2023-09-02) Pereyra, Antonio; Tello, J.; Alvarado, D.; Torre, E.; Zevallos, M.; Espinoza, M.; de Almeida, L.Photometry of Type Ib-pec SN 2023fyq was gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging in R filter was performed on three consecutive nights under non-photometric conditions with the target at low altitude. Special care was taken to select the appropriate photometric aperture to minimize the contamination with the host galaxy. Our measurements are indicated below: Date (UT) | filter | IT | seeing (") | mag |, 2023-08-17.008 | R | 88x20s | 1.9 | 14.725 +/- 0.012, 2023-08-18.008 | R | 90x20s | 2.0 | 14.719 +/- 0.012, 2023-08-19.005 | R | 70x20s | 2.0 | 14.715 +/- 0.011. UCAC4 field stars were used for the zero point calibration. Our observations are ~3.8 weeks after K. Itagaki report showing the rapid brightening of the target. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).Item Open Access OAUNI photometry of SN 2023ijd(R. E. Rutledge, 2023-07-31) Pereyra, Antonio; Espinoza, M.; Tello, J.; Zevallos, M.; de Almeida, L.; Alvarado, D.Photometry of Type II SN 2023ijd (TNSTR-2023-1092, TNSCR-2023-1112) was gathered with the OAUNI 51cm telescope (arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging in R filter was performed on three consecutive nights under non-photometric conditions with airmasses lower than 1.8. The integration time was 70x20s=1400s in each observation. Our measurements yielded: Date (UT) / filter / seeing (") / mag ; 2023-07-15.072 / R / 2.1 / 15.52 +/- 0.01 ; 2023-07-16.057 / R / 1.8 / 15.61 +/- 0.01 ; 2023-07-17.053 / R / 2.2 / 15.56 +/- 0.01. UCAC4 field stars were used for the zero point calibration. Our observations are ~two months after the ASAS-SN detection (TNSTR-2023-1092). The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).Item Open Access OAUNI non-detection of AT 2023pow in R band(R. E. Rutledge, 2023-08-23) Pereyra, Antonio; Tello, J.; Alvarado, D.; Torre, E.; Zevallos, M.; Espinoza, M.; de Almeida, L.CCD imaging was performed of the NGC 1640 field using the OAUNI 51cm telescope at Huancayo Observatory, Peru, on 2023-08-19.310 (UT). No source is detected at the position of AT 2023pow (TNSTR-2023-1982) with limiting magnitude R ~ 18.5. This is consistent with the AT 2023pow report by T. Noguchi few hours after the detection alert. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio133-2020 Fondecyt).Item Open Access OAUNI photometry of SN 2023ixf(Instituto Geofísico del Perú, 2023-06-27) Pereyra, Antonio; Espinoza, M.; Tello, J.; Zevallos, M.; de Almeida, L.; Torre, E.We report photometry of Type II SN 2023ixf gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging in R filter was performed on two epochs under stable conditions (seeing ~1.7") and airmass lower than 2.5 (target with low altitude). Our integration times were 54x20s=1080s and 50x20s=1000s on 2023-06-20 and 2023-06-21, respectively. Our measurements yielded: on (UT) 2023-06-20.021, R = 11.28 +/- 0.02, and, on (UT) 2023-06-21.022, R = 11.30 +/- 0.02. UCAC4 field stars were used for the zero point calibration. Our observations are ~32-33 days after the earliest detection.Item Open Access OAUNI photometry of SN 2023gfo(R. E. Rutledge, 2023-06-10) Pereyra, Antonio; Espinoza, M.; Tello, J.; Zevallos, M.; Alvarado, D.; de Almeida, L.Multiband photometry of Type II SN 2023gfo on 2023-05-24 (UT) was gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging using VRI filters was performed under non-photometric conditions (seeing ~1.8") and airmass lower than 1.6. Total integration times of (45x20s=900s) for V, R and I filters yielded: V = 15.60 +/- 0.01 on 2023-05-24.228 (UT); R = 15.33 +/- 0.03 on 2023-05-24.197; I = 15.12 +/- 0.05 on 2023-05-24-212.Item Open Access Follow-up OAUNI photometry of SN2022hrs(R. E. Rutledge, 2022-08-03) Pereyra, Antonio; Tello, J.; Zevallos, M.; de Almeida, L.; Espinoza, M.; Alvarado, D.We report additional multiband photometry of Type Ia SN2022hrs (TNSTR-2022-994, TNSCR-2022-997, ATel #15378) on 2022-07-01 (UT) gathered with the OAUNI 51cm telescope (Pereyra et al. 2015; arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging using BVRI filters was performed under non-photometric conditions (seeing ~2.1") and airmass lower than 1.9. Total integration times of (60x20s=1200s) for V, R and I filters, and (90x20s=1800s) for B filter yielded: Date (UT) filter mag 2022-07-01.111 B 15.94 +/- 0.05 2022-07-01.042 V 15.04 +/- 0.01 2022-07-01.062 R 15.00 +/- 0.01 2022-07-01.086 I 15.16 +/- 0.02. UCAC4 field stars (508-055361 and 508-055359) were used for the zero point calibration. Following the GELATO classification (TNSCR-2022-997), our measurements are approximately two months after the maximum brightness. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).Item Open Access OAUNI photometry of SN2022jli(R. E. Rutledge, 2022-07-24) Pereyra, Antonio; Tello, J.; Zevallos, M.; de Almeida, L.; Espinoza, M.; Alvarado, D.Multiband photometry of Type Ic SN2022jli (TNSTR-2022-1198, TNSCR-2022-1261) on 2022-07-01 (UT) was gathered with the OAUNI 51cm telescope (arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging using VRI filters was performed under non-photometric conditions (seeing ~2.3") and airmass lower than 1.3. Total integration times of (60x20s=1200s) for V, R and I filters yielded: Date (UT) filter mag 2022-07-01.401 V 14.64 +/- 0.04 2022-07-01.359 R 14.52 +/- 0.05 2022-07-01.381 I 14.06 +/- 0.05. UCAC4 field stars were used for the zero point calibration. Caution must be taken in SN2022jli magnitudes for possible contamination with the host galaxy. Following GELATO and SNID classification (TNSCR-2022-1261), our measurements are aprox. 52 days after maximum brightness. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).Item Open Access OAUNI confirmation of optical flickering from RS Oph(R. E. Rutledge, 2022-05-20) Pereyra, Antonio; Tello, J.; Zevallos, M.; de Almeida, L.; Espinoza, M.; Alvarado, D.We report photometry post 2021 outburst of the recurrent nova RS Oph on 2022-05-02 (UT) gathered with the OAUNI 51cm telescope (Pereyra et al. 2015; arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging was performed in B filter under non-photometric conditions (seeing ~1.8") and airmass ~1.1. The observations span 1.7h with a total of 220 individual measurements of 20s each. UCAC4 field stars (417-071319 and 418-073342) were used for the zero point calibration. An average B magnitude of 12.43 +/- 0.04 (HJD middle = 2459701.772) is found with a clear detection of optical flickering on minute-to-hour time scale with peak-to-peak amplitude of 0.22 mag (see link below). This is supported by the standard deviation ratio of magnitudes between RS Oph and the comparison stars that is 2.8. Our observations confirm previous RS Oph optical flickering detections post last outburst (ATel #15330, ATel #15339). Following the onset of the 2021 outburst (Munari & Valisa 2021; arXiv:2109.01101), our measurements are 266.8 days old with an ongoing re-establishment of accretion. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).Item Open Access OAUNI multiband photometry of SN2022hrs(R. E. Rutledge, 2022-05-13) Pereyra, Antonio; Tello, J.; Zeballos, M.; de Almeida, L.; Espinoza, M.; Alvarado, D.We report multiband photometry of Type Ia SN2022hrs (TNSTR-2022-994, TNSCR-2022- 997) on 2022-05-02 (UT) gathered with the OAUNI 51cm telescope (Pereyra et al. 2015; arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging using BVRI filters was performed under non-photometric conditions (seeing ~1.8") and airmass lower than 1.2. Total integration times of (45x20s=900s) for V, R and I filters, and (60x20s=1200s) for B filter yielded: Date (UT) filter mag 2022-05-02.208 B 12.54 +/- 0.22 2022-05-02.087 V 12.38 +/- 0.14 2022-05-02.104 R 12.52 +/- 0.10 2022-05-02.190 I 13.21 +/- 0.13. UCAC4 field stars were used for the zero point calibration. Following the GELATO classification (TNSCR-2022-997), our measurements are very close to the maximum brightness. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).Item Open Access Astrometric observations of the Potentially Hazardous Asteroid (52768) 1998 OR2 near its maximum approach to earth(The Astronomer's Telegram, 2020-05-13) Villanueva, R.; Ricra, J.; Zegarra-Valles, M.; Baella, Nobar; Santivanez, J.Our team presents astrometric measurements of the PHA (52768) 1998 OR2 obtained close to its maximum approach to Earth. The observations were made from Observatorio Planetario Moche, located in Trujillo, Peru (Long. 79 00 39.2 W, Lat. 08 06 47.9 S, Alt. 48 m), on April 23, 24, 25 and 29, 2020. It is important to note that April 29's measurements were obtained approximately 5 hours before the asteroid's closest approach to Earth. A Celestron NexStar 11 GPS telescope and a ZWO ASI 071MC camera (without filter) were used. In addition, Dimension 4 software was employed to synchronize our time with special purpose Internet Time Servers. A total of 240 images were obtained, of which 19 were selected for presenting better ellipticity and FWHM values. The astrometric measurements were made with the Astrometrica software, using between 13 and 31 field stars identified by means of the Gaia DR1 catalog.Item Open Access Astrometric observations near the maximun approach of the Potencially Hazardous Asteroid (66391) 1999 KW4(The Astronomer's Telegram, 2019-08-08) Ricra, J.; Zegarra-Valles, M.; Baella, Nobar; Villanueva, R.Our team decided to collaborate with the campaign to observe the maximum approach of the PHA (66391) 1999 KW4, organized by the International Asteroid Warning Network (IAWN). The observations were made from CIEASEST, in the Universidad Nacional San Luis Gonzaga de Ica, Peru (Long. 75 44 12.5 W, Lat. 14 05 21.1 S, Alt. 401 m). A 60 cm Nishimura telescope (f10) and a ZWO ASI 071MC camera were used. The night of the maximum approach (May 25, 2019) we had cloudy skies; however, the night of May 26-27 we had clear skies and we were able to take 147 images with a exposure time of 4 seconds. Dimension 4 software was used to synchronize our time with special purpose Internet Time Servers, ensuring less than one second accuracy. The astrometric measurements were made with the Astrometrica software, using between 15 and 25 stars in the field identified by means of the Gaia DR2 catalog.Item Open Access 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.Item Open Access 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.Item Open Access OAUNI photometry of ASASSN-16hw(The Astronomer's Telegram, 2016-09-30) Pereyra, Antonio; Ricra, J.; Zevallos, M.We report optical photometry of Type Ia SN ASASSN-16hw (=SN 2016ekt, ATel #9278, ATel #9289, ATel #9300) on 2016-08-06 (UT) gathered with the OAUNI 51cm telescope (Pereyra et al. 2015;arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging measurements using V and R broadband filters were acquired with seeing ~1.9" and airmass = 1.5. A total integration time of 42x20s=840s in each filter yielded: Date (UT) filter mag 2016-08-06.119 R 14.656 +/- 0.003 2016-08-06.120 V 14.497 +/- 0.004 Field stars were used for the zero point calibration. Following PESSTO and Du Pont classifications (ATel #9289, ATel #9300), our measurements are very close to maximum. The OAUNI project is supported by UNI, TWAS, IGP and Cienciactiva (Convenio 102-2015 Fondecyt).Item Open Access OAUNI photometry of ASASSN-16hz(The Astronomer's Telegram, 2016-12-07) Pereyra, Antonio; Ricra, J.; Zevallos, M.We report optical photometry of Type Ia SN ASASSN-16hz (=SN 2016eqb, ATel #9332, ATel #9333) on 2016-08-09 (UT) gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging was performed with seeing ~1.8" and airmass = 1.3. A total integration time of 900s (45x20s) and 880s (44x20s) in R and V filter, respectively, yielded: Date (UT) | filter | mag 2016-08-09.397 | R | 15.84 +/- 0.04 2016-08-09.412 | V | 15.82 +/- 0.05 UCAC4 field stars were used for the zero point calibration. Following Mayall/KOSMOS classification (ATel #9333), our measurements are ~2 days after maximum. The OAUNI project is supported by UNI, TWAS, IGP and Cienciactiva (Convenio 102-2015 Fondecyt)."Item Open Access OAUNI photometry of ASASSN-16gq/AT2016cym(The Astronomer's Telegram, 2017-04-21) Pereyra, Antonio; Ricra, J.; Zevallos, M.We report optical photometry of Type Ia SN ASASSN-16gq/AT2016cym (ATel #9199, ATel #9219) on 2016-07-11 (UT) gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging was performed with seeing ~1.7" and airmass = 1.3. Our measurements yielded: Date (UT) | filter | IT | mag 2016-07-11.085 | V | 1200s (60x20s) | 17.94 +/- 0.06 2016-07-11.106 | R | 0760s (38x20s) | 17.84 +/- 0.04 Field stars were used for the zero point calibration. Caution must be taken for contamination of edge-on Sc host galaxy (ESO 446-G023). Following FLWO/FAST classification (ATel #9219), our measurements are ~17 days after maximum. The OAUNI project is supported by UNI, TWAS, IGP and Cienciactiva (Convenio 102-2015 Fondecyt)."Item Open Access OAUNI photometry of SN2017glq/Gaia17cfi(The Astronomer's Telegram, 2017-12-08) Pereyra, Antonio; Ricra, J.We report optical photometry of Type Ia SN2017glq/Gaia17cfi (TNSDR 2017-13365, TNSCR 2017-1194) on 2017-09-19.182 (UT) gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging was performed using R band with seeing ~1.6" and airmass = 1.5. A total integration time of 59x20s=1180s yielded R = (14.16 +/- 0.05) mag. NOMAD field stars were used for the zero point calibration. Following OSC (Guillochon et al. 2016, arXiv:1605.01054) light curve, our measurements are very close to the maximum. The OAUNI project is supported by UNI, TWAS, IGP and Cienciactiva (Convenio 102-2015 Fondecyt)."Item Open Access OAUNI photometry of SN2017gmr/DLT17cq(The Astronomer's Telegram, 2017-12-22) Pereyra, Antonio; Ricra, J.Optical photometry of Type II SN2017gmr/DLT17cq (ATel #10706, ATel #10717, TNSCR 2017-1220) on 2017-09-19.207 (UT) was gathered using the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging was performed in R band with seeing ~1.5" and airmass = 1.3. A total integration time of 55x20s=1100s yielded R = (14.05 +/- 0.04) mag. NOMAD field stars were used for the zero point calibration. The OAUNI project is supported by UNI, TWAS, IGP and Cienciactiva (Convenio 102-2015 Fondecyt).