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 report photometric observations of Comet 103P/Hartley 2 during its 2023 apparition. Our campaign, conducted from August through 2023 December, combined data from a global network of citizen astronomers coordinated by Unistellar and the Association Fran & ccedil;aise d'Astronomie. Photometry was derived using an automated pipeline for eVscope observations in partnership with the SETI Institute and aperture photometry via AstroLab Stellar. We find that the comet's peak reduced brightness, measured at Gmin=10.24 +/- 0.47 , continues a long-term fading trend since 1991. The decline in activity follows a per-apparition minimum magnitude increase of Delta Gmin=0.59 +/- 0.11 mag, corresponding to a similar to 42% reduction in brightness each return. This trend implies that the comet's active fraction has declined by approximately an order of magnitude since 1991 and may indicate that Hartley 2 is no longer hyperactive by definition. The fading is consistent with progressive volatile depletion rather than orbital effects. These results offer insight into the evolutionary processes shaping Jupiter-family comets.

NASA's Transiting Exoplanet Survey Satellite (TESS) has identified over 7,000 candidate exoplanets via the transit method, with gas giants among the most readily detected due to their large radii. Even so, long intervals between TESS observations for much of the sky lead to candidates for which only a single transit is detected in one TESS sector, leaving those candidate exoplanets with unconstrained orbital periods. Here, we confirm the planetary nature of TIC 393818343 b, originally identified via a single TESS transit, using radial velocity data and ground-based photometric observations from citizen scientists with the Unistellar Network and Exoplanet Watch. We determine a period of $P$ = 16.24921 $\substack{+0.00010 \\ -0.00011}$ days, a mass $M_{P}$ = 4.34 $\pm$ 0.15 $M_{J}$, and semi-major axis $a$ = 0.1291 $\substack{+0.0021 \\ -0.0022}$ au, placing TIC 393818343 b in the "warm Jupiter" population of exoplanets. With an eccentricity $e$ = 0.6058 $\pm$ 0.0023, TIC 393818343 b is the most eccentric warm Jupiter to be discovered by TESS orbiting less than 0.15 au from its host star and therefore an excellent candidate for follow-up, as it may inform our future understanding of how hot and warm Jupiter populations are linked.

Abstract First detected on 2023 November 4 by the Gravitational-wave Optical Transient Observer, SN 2023wrk is a Type Ia Supernova at 40 Mpc, with significant unburned carbon in the outer ejecta. In this note, we present photometric and spectroscopic observations and analysis conducted by the Global Rapid Advanced Network Devoted to the Multi-messenger Addict over a 115 days period, which includes 78 days of measurements. The observations were contributed by both amateur and professional astronomers. J. Liu et al. analyzed the physical processes involved, and compared the evolution of color and spectral lines. We conclude that SN 2023wrk is the second 1999aa-like object with strong carbon absorption lines that has ever been found, which enriches our understanding of the subclass of 1999aa-like SNe.

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.

In this paper we present pCellTM technology, the first commercial-grade wireless system that employs cooperation between distributed transceiver stations to create concurrent data links to multiple users in the same spectrum. First we analyze the per-user signal-to-interference-plus-noise ratio (SINR) employing a geometrical spatial channel model to define volumes in space of coherent signal around user antennas (or personal cells, i.e., pCells). Then we describe the system architecture consisting of a general-purpose-processor (GPP) based software-defined radio (SDR) wireless platform implementing a real-time LTE protocol stack to communicate with off-the-shelf LTE devices. Finally we present experimental results demonstrating up to 16 concurrent spatial channels for an aggregate average spectral efficiency of 59.3 bps/Hz in the downlink and 27.5 bps/Hz in the uplink, providing data rates of 200 Mbps downlink and 25 Mbps uplink in 5 MHz of TDD spectrum.

In this letter, the feasibility of a 40‐Gb/s subcarrier multiplexed optical transmission system using low‐cost optical electronic components and CMOIS IC technology is studied. A test chip and its measurement results are reported. © 2007 Wiley Periodicals, Inc. Microwave Opt Technol Lett 49: 1272–1274, 2007; Published online in Wiley InterScience (www.interscience.wiley.com). DOI 10.1002/mop.22433

In this paper, we present a low-power small-area electrical backplane equalizer using programmable analog zeros and folded active inductors. We also present a dc-offset cancellation circuit, which occupies less chip area than the traditional offset cancellation schemes. The equalizer circuit was fabricated in a 10-V 90-nm CMOS process. With one zero stage, the equalizer occupies 0.015-mm(2) chip area and dissipates 12 mW of power. At 4.25-Gb/s data rate, the equalizer provides 7.8-dB gain boost at the Nyquist frequency. Without the use of any transmitter equalization, the analog zero equalizer demonstrated error-free transmission for pseudorandom-bit-sequence-31 data patterns over 34-in lossy FR4 backplanes.

The feasibility of a 40 Gb/s subcarrier modulated optical transmission system using low-cost optoelectronic components and CMOS IC technology is presented. The optical channel impairments are studied. A complete DSP framework is developed to cancel out the optical channel impairments as well as analog circuit imperfections. To validate that the 40 Gb/s system can be implemented in CMOS, an integrated QAM-16 transceiver with a carrier frequency of 13.32 GHz was designed and fabricated in a 0.14 mum, 1.5 V CMOS technology. The test chip occupies 3.6 mm2 of area and consumes 340 mW of power. Measurement results for a transmission link consisting of the CMOS QAM-16 modulator/demodulator, a directly modulated laser (DML), a 30 km single mode fiber and a p-i-n photo-detector are reported

This paper proposes sub-carrier multiplexing (SCM) modulation in the electrical domain as a bandwidth efficient modulation with advantages over on-off keying in the design and implementation of a low-cost short-haul high-speed optical communication system. With SCM the signaling rate can be lowered to a level where current cost-effective mixed-signal and digital circuit technology can operate and be effectively implemented. Novel digital signal processing techniques and architectures are presented that reduce overall system SCM design specification constraints and alleviate linear channel impairments.

In this paper we study a 40Gb/s electrical transmission scheme used in an optical system based on sub-carrier multiplexing (SCM). The proposed bandwidth efficient modulation reduces the signal bandwidth to 14GHz. This enables implementation in lower cost silicon technology and allows the use of optical components developed for 10Gbps digital transmission. We present digital signal processing techniques and architectures that relax analog specifications and alleviate linear channel impairments. We also present the implementation of a test-chip in standard 0.14/spl mu/m CMOS process, validating the most challenging circuits.