Our purpose is to provide photometric data and tools to compute magnitudes from images obtained by Unistellar telescopes and enhance their usefulness to the broader astronomical community. To do so, we provide relationships transforming Unistellar complementary metal oxide semiconductor sensor Bayer filter bands (blue B-e , green G(e) , and red R-e ) to the Johnson-Cousins photometric system. To enable this calibration, stars with known spectra were observed with Unistellar telescopes by citizen scientists in the Unistellar Network. We obtained the zero-point magnitudes of the telescopes for each band by combining those spectra with the telescope sensor responses. Using the observations of 794 stars with known Johnson-Cousins magnitudes, we established the relations to transform the Unistellar magnitudes. The zero-point magnitudes and their associated errors for the three bands were derived. Polynomial expressions for the relation between the Unistellar colour B-e - R-e and the Johnson-Cousins magnitudes were obtained for stars with Unistellar colour - 0.15 < B-e - R-e < 0.5 . The uncertainties on these transformations increase linearly with the R-e magnitude. These relations were applied to the observation of a type II supernova and an exoplanet transit, with the supernova example showing consistency with other published magnitudes but also demonstrating that narrow-line emission or absorption can bias the transformed magnitudes. Other limitations of the transformations were also identified, largely stemming from significant infrared contributions to all color channels and variability between individual telescope sensors. Nevertheless, the values and color relationships provided here can be used by professional and citizen astronomers alike to compute observed magnitudes and provide measurements in a standard system. This enhances the Unistellar Network's ability to contribute accurate photometry to the astronomical community that can be easily and faithfully combined with measurements from other instruments. (c) The Authors. Published by SPIE under a Creative Commons Attribution 4.0 International License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

We present highly sampled photometry of the supernova (SN) 2023ixf, a Type II SN in M101, beginning 2 days before its first known detection. To gather these data, we enlisted the global Unistellar Network of citizen scientists. These 252 observations from 115 telescopes show the SN’s rising brightness associated with shock emergence followed by gradual decay. We measure a peak M V  = − 18.18 ± 0.09 mag at 2023 May 25 21:37 UTC in agreement with previously published analyses.

More than 5,000 exoplanets have been confirmed and among them almost 4,000 were discovered by the transit method. However, few transiting exoplanets have an orbital period greater than 100 days. Here we report a transit detection of Kepler-167 e, a "Jupiter analog" exoplanet orbiting a K4 star with a period of 1,071 days, using the Unistellar ground-based telescope network. From 2021 November 18 to 20, citizen astronomers located in nine different countries gathered 43 observations, covering the 16 hour long transit. Using a nested sampling approach to combine and fit the observations, we detected the mid-transit time to be UTC 2021 November 19 17:20:51 with a 1σ uncertainty of 9.8 minutes, making it the longest-period planet to ever have its transit detected from the ground. This is the fourth transit detection of Kepler-167 e, but the first made from the ground. This timing measurement refines the orbit and keeps the ephemeris up to date without requiring space telescopes. Observations like this demonstrate the capabilities of coordinated networks of small telescopes to identify and characterize planets with long orbital periods.