Browsing by Author "Zevallos, M."
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Item Open Access Follow-up OAUNI photometry of SN 2024iss(R. E. Rutledge, 2024-07-16) Pereyra, Antonio; Zevallos, M.; Alvarado, D.; Delgado, J.; Torre, E.; Tello, J.; de Almeida, L.We report new photometry of Type II SN 2024iss gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging in R filter was performed on four consecutive nights under non-photometric conditions with the target on higher airmasses. The integration time was 80x20s=1600s in each observation. Our measurements yielded: Date (UT) | filter | seeing (") | mag, 2024-07-03.124 | R | 14.70 +/- 0.02, 2024-07-04.129 | R | 14.72 +/- 0.02, 2024-07-05.112 | R | 14.76 +/- 0.01, 2024-07-06.097 | R | 14.77 +/- 0.01. UCAC4 field stars were used for the zero point calibration. Our observations are ~7.3 weeks after the GOTO detection. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).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 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 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 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 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 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 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 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 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 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 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 2024iss(R. E. Rutledge, 2024-06-18) Pereyra, Antonio; Zevallos, M.; Alvarado, D.; Delgado, J.; Tello, J.; de Almeida, L.; Torre, E.We report photometry of Type II SN 2024iss 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 airmasses lower than 1.5. The integration time was 70x20s=1400s in each observation. Our measurements yielded: Date (UT) | filter | seeing (") |mag, 2024-06-07.102 | R | 2.6 |13.40 +/- 0.02, 2024-06-08.093 | R | 2.6 | 13.49 +/- 0.02, 2024-06-09.094 | R | 2.8 | 13.59 +/- 0.02. UCAC4 field stars were used for the zero point calibration. Our observations are ~3.7 weeks after the GOTO detection. 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 Seeing measurements at OAUNI on 2016 and 2017 campaigns(IOP Publishing, 2022) Pereyra, Antonio; Tello, J.; Zevallos, M.We present seeing measurements at OAUNI site gathered on 2016 and 2017 campaigns using V and R broadband filters. In order to quantify the seeing we used the full-width-at-half-maximum from stellar profiles on photometric sequences during the observational windows of our supernovae program. A typical median seeing of 1” .8 was found on 2016 and a worst value of 2” .0 on 2017. The last one was probably affected by anomalous conditions related to the 2017 extreme climatic event. The monthly first quartile analysis indicates that best seeing conditions can be achieved at a level of 1” .5. In general, our results indicate a reasonable sky quality for the OAUNI site.