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Kyba, C.C.M.; Bouroussis, C.; Canal-Domingo, R.; Falchi, F.; Giacomelli, A.; Hänel, A.; Kolláth, Z.; Massetti, L.; Ribas, S.J.; Spoelstra, H.; Tong, K.P.; Wuchterl, G. |
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Title |
Report of the 2015 LoNNe Intercomparison Campaign |
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2015 |
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skyglow; instrumentation |
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LoNNe @ kyba @; IDA @ john @; GFZ @ kyba @ |
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1255 |
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Ribas, S. J.; Aubé, M.; Bará, S.; Bouroussis, C.; Canal-Domingo, R.; Espey, B.; Hänel, A.; Jechow, A.; Kolláth, Z.; Marti, G.; Massana, P.; Schmidt, W.; Spoelstra, H.; Wuchterl, G.; Zamorano, J.; Kyba, C. |
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Title |
Report of the 2016 STARS4ALL/LoNNe Intercomparison Campaign |
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Report |
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2017 |
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Skyglow; Instrumentation |
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The 2016 LoNNe (Loss of the Night Network) intercomparison campaign is the fourth of four campaigns planned during EU COST Action ES1204. The first campaign took place in 2013 in Lastovo, Croatia, the second in Madrid, Spain (Bará et al 2015), the third in Torniella and Florence, Italy (Kyba et al 2015a). The 2016 campaign took place at the Parc Astronòmic Montsec (PAM). The campaign continued the strategy of taking measurements at multiple sites, this year with a main fixed site and then excursions to other sites. The goals of the campaigns included:
● Understanding the difference between extinction measurements made by DSLR photometry and classical astronomical (telescope) photometry, and also understanding the relation between extinction and sky brightness at these two sites.
● Examining the difference in radiance measured with the mosaic technique of the US National Parks Service camera compared to all-sky fisheye imagery
● Examining the relationships between all-sky and zenith radiance reported by different instruments
● Quantifying the sky brightnes at the sites, including full zenith spectral radiance at selected locations
● Measuring the systematic uncertainty on handheld SQM observations due to unit-to-unit differences |
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GFZ Data Services |
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GFZ @ kyba @ |
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3057 |
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Walczak, K.; Crim, G.; Gesite, T.; Habtemichael, S.; Morgan, J.; Tarr, C.; Turkic, L.; Wiedemann, J. |
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Title |
The GONet (Ground Observing Network) Camera: An Inexpensive Light Pollution Monitoring System |
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Report |
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2020 |
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preprint |
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Instrumentation; GONet; Light pollution; All-sky imaging; Sky brightness; Monitoring |
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Instrumentation developed to monitor and characterize light pollution from the ground has helped frame our understanding of the impacts of artificial light at night (ALAN) [Bará, Lima, & Zamorano, 2019; Hänel et al., 2018; Zamorano et al., 2017]. All-sky imaging has been used to quantify and characterize ALAN in a variety of environments [D. M. Duriscoe, 2016; Jechow, Kyba, & Hölker, 2019]. Over the past decade growth in access to DIY electronics has afforded the opportunity for the development of new and affordable instrumentation for ALAN research. The
GONet (Ground Observing Network) camera is an inexpensive (~USD 100), simple to use, all-sky imaging system designed to allow measurements of sky quality at night. Due to their ease of use and low price, GONet cameras allow observations by users with little technical expertise, large inter-comparison campaigns and deployments of opportunity. Developed as a student engineering project at the Adler Planetarium, initial field tests of the GONet system have demonstrated its utility as a tool that can benefit ALAN research. Here we present an overview of the
design and use of the GONet device, methods of calibration, initial results from observations, potential use cases, and limitations of the system. What we describe here is the version 1 GONet camera. We conclude with a brief description
of the version 2 unit already under development. |
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Adler Planetarium, Chicago, Illinois 60605, USA; kwalczak ( at ) adlerplanetarium.org |
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English |
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IDA @ john @ |
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3305 |
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Hampf, D.; Rowell, G.; Wild, N.; Sudholz, T.; Horns, D.; Tluczykont, M. |
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Title |
Measurement of night sky brightness in southern Australia |
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2011 |
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Advances in Space Research |
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Advances in Space Research |
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48 |
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6 |
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1017-1025 |
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Observatories and site testing; Airglow and aurorae; Photometric, polarimetric, and spectroscopic instrumentation |
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Night sky brightness is a major source of noise both for Cherenkov telescopes as well as for wide-angle Cherenkov detectors. Therefore, it is important to know the level of night sky brightness at potential sites for future experiments.
The measurements of night sky brightness presented here were carried out at Fowler’s Gap, a research station in New South Wales, Australia, which is a potential site for the proposed TenTen Cherenkov telescope system and the planned wide-angle Cherenkov detector system HiSCORE.
A portable instrument was developed and measurements of the night sky brightness were taken in February and August 2010. Brightness levels were measured for a range of different sky regions and in various spectral bands.
The night sky brightness in the relevant wavelength regime for photomultipliers was found to be at the same level as measured in similar campaigns at the established Cherenkov telescope sites of Khomas, Namibia, and at La Palma. The brightness of dark regions in the sky is about 2 × 1012 photons/(s sr m2) between 300 nm and 650 nm, and up to four times brighter in bright regions of the sky towards the galactic plane. The brightness in V band is 21.6 magnitudes per arcsec2 in the dark regions. All brightness levels are averaged over the field of view of the instrument of about 1.3 × 10−3 sr.
The spectrum of the night sky brightness was found to be dominated by longer wavelengths, which allows to apply filters to separate the night sky brightness from the blue Cherenkov light. The possible gain in the signal to noise ratio was found to be up to 1.2, assuming an ideal low-pass filter. |
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Department of Physics, University of Hamburg, Luruper Chaussee 149, 22761 Hamburg, Germany |
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0273-1177 |
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IDA @ john @ |
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189 |
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Downey, J.W. |
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Title |
Determination of minimum light sense and retinal dark adaptation with presentation of a new type of photometer |
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1919 |
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American Journal of Ophthalmology |
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2 |
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1 |
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13-20 |
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Vision; Instrumentation |
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This paper reviews the principal hypotheses with reference to light and dark adaptation, and suggests a practical photometer, using a radioactive substance as a standard of comparison. With three illustrations, and experimental findings with this instrument. |
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GFZ @ kyba @ |
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2418 |
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