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Surprisingly parallel discrepancies between observations I discovered that there are surprisingly parallel discrepancies between observations of V Gem. YYYYMMDD(UT) mag observer 20030220.831 121 (Alfons Diepvens) 20030220.940 120 (Erwin van Ballegoij) 20030222.800 127 (Balogh Istvan) 20030222.819 123 (Georg Comello) 20030222.847 113 (Thorsten Lange) -- B 20030224.851 110 (Thorsten Lange) -- B 20030226.778 86 (Adrian Sonka Bruno) -- A 20030226.867 112 (Thorsten Lange) -- B 20030227.067 125 (Mike Simonsen) 20030301.800 127 (Georg Comello) 20030306.819 129 (Georg Comello) 20030306.960 132 (Erwin van Ballegoij) 20030309.775 90 (Adrian Sonka Bruno) -- A 20030313.835 <116 (Thorsten Lange) -- B 20030313.940 130 (Erwin van Ballegoij) 20030315.790 134 (Georg Comello) 20030321.826 <122 (Thorsten Lange) -- B 20030321.847 <142 (Alfons Diepvens) 20030323.812 135 (Guenther Krisch) 20030323.817 124 (Thorsten Lange) -- B 20030323.910 133 (Erwin van Ballegoij) 20030324.783 96 (Adrian Sonka Bruno) -- A 20030330.815 <122 (Thorsten Lange) 20030404.765 99 (Adrian Sonka Bruno) -- A There are three groups of observations. (1) observations with no marks, (2) group A, and (3) group B. Surprisingly enough, all observations have a common fading rate in spite of discrepancies up to several magnitudes!! Even if the group B observations can be interpreted as a result of different sequence or observer's response, the group A observations are a mystery. There are confusing stars in the field of V Gem, but it would be difficult to think any variation of a much fainter Mira star could have affected a much brighter field star. Regards, Taichi Kato
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