The Peruvian Andean Plateau, one of the main production areas of native varieties of Chenopodium quinoa, is exposed to abrupt decreases in environmental temperature, affecting crop production. Plant-growth-promoting rhizobacteria that tolerate low temperatures could be used as organic biofertilizers in this region. We aimed to bioprospect the native psychrotolerant bacteria of the quinoa rhizosphere in this region that show plant-growth-promoting traits. Fifty-one strains belonging to the quinoa rhizosphere were characterised; 73% of the total could grow at low temperatures (4, 6, and 15 °C), whose genetic diversity based on DNA amplification of interspersed repetitive elements (BOX) showed 12 different profiles. According to the 16S rRNA sequence, bacterial species belonging to the classes Beta-and Gammaproteobacteria were identified. Only three (6%) isolates identified as nonpathogeni...

Thirty strains of V. cholerae O1 Ogawa and 2 Inaba, isolated during the outbreak of 1998, were studied in relation to thier sensibility in front of 10 antibiotics of clinical use. Nine strains were determined (28.1%) resistant to 1 up to 6 antibiotics. The SIDS-PAGE of the studied strains exhibited similar pattern of bands.

Treinta cepas de V. cholerae O1 Ogawa y 2 Inaba, aisladas durante el brote de 1998, fueron estudiados en relación a su sensibilidad frente a 10 antibióticos de uso clínico. Nueve cepas (28.1%) fueron resistentes de 1 hasta 6 antibióticos. El SIDS-PAGE de las cepas estudiadas exhibieron un patrón similar de bandas.

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).

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).

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-Co...

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 #153...

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).

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).

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.

We report photometry of Type II SN 2024ggi gathered with the OAUNI 51cm telescope (arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging in R filter was performed on five consecutive nights under nonˇphotometric conditions with airmasses lower than 1.6. The integration time was 50x20s=1000s in the first observation and 60x20s=1200s for the rest. Our measurements yielded: Date (UT) | filter | seeing (") | mag, 2024-06-05.108 | R | 3.2 | 12.27 +/- 0.06, 2024-06-06.080 | R | 2.6 | 12.25 +/- 0.06, 2024-06-07.064 | R | 2.8 | 12.27 +/- 0.06, 2024-06-08.061 | R | 2.7 | 12.27 +/- 0.06, 2024-06-09.062 | R | 2.9 | 12.28 +/- 0.06. UCAC4 field stars were used for the zero point calibration. Our observations are ~7.9 weeks after ATLAS discovery (TNSAN-2024-100). The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).

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).

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).

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).

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).

We report photometry of Type II SN 2024jlf gathered with the OAUNI 51cm telescope (arXiv:1512.03104) at Huancayo Observatory, Peru. CCD imaging in R filter was performed on five consecutive nights under non-photometric conditions with airmasses lower than 1.3. The integration time was 40x20s=800s for all observations. Our measurements yielded: Date (UT) | filter | seeing (") | mag, 2024-06-05.056 | R | 2.5 | 14.71 +/- 0.01, 2024-06-06.024 | R | 2.7 | 14.57 +/- 0.03, 2024-06-07.013 | R | 2.9 | 14.45 +/- 0.03, 2024-06-08.010 | R | 2.7 | 14.54 +/- 0.02, 2024-06-09.005 | R | 2.5 | 14.66 +/- 0.02. UCAC4 field stars were used for the zero point calibration. Our first observation is ~8 days after ZTF discovery. The OAUNI project is supported by UNI, TWAS, IGP and ProCiencia-Concytec (Convenio 133-2020 Fondecyt).

This work was partially funded by the AECID (Agencia Española de Cooperación Internacional para el Desarrollo) grant numbers A/3795/05, A/4892/06, A/9727/07 A/4817/06; ACCD (Agència Catalana de Cooperació al Desenvolupament, Generalitat de Catalunya) grant U2006; CCD-UPC (Centre de Cooperació per al Desenvolupament, Universitat Politècnica de Catalunya) to LJdV; and by the CONCYTEC (Consejo Nacional de Ciencia, Tecnología e Innovación Tecnológica, Perú) grant 189-2005-CONCYTEC-OAJ. JR's research is supported by grant CP05/0130 of the FIS (Fondo de Investigaciones Sanitarias). The authors thank M.J. Pons and Donna Pringle for assistance in the preparation of the final version of the manuscript. Conflict of interest: No conflict of interest to declare.