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Table 1

Overview of instruments and their involvement in photometric observations of the EE Cep eclipses since 1997.

Observatory Country Telescope type Diameter [m] Bands Epoch N Table
Altan, Mt Giant Czech Republic Reflector 0.2 m B,V,R,I 10 60 B.12
Athens Greece Cassegrain 0.4 m B,V,R,I 9, 10 176 B.2, B.24
Białków Poland Cassegrain 0.6 m B,V,R,I,HαW*, HαN* 9, 10 109 B.3, B.13
Green Island North Cyprus Ritchey-Chrétien 0.35 m B,V,R,I 10 35 B.14
Hankasalmi Finland RCOS 0.4 m B,V,R,I 10 28 B.25
Furzehill, Swansea United Kingdom Schmidt-Cassegrain 0.35 m B,V,R,I 10 68 B.15
Kraków Poland Cassegrain 0.5 m U,B,V,R,I 9, 10 336 B.4, B.27
Kryoneri Greece Cassegrain 1.2 m U,B,V,R,I 9, 10 42 B.5, B.21
GRAS, Mayhill USA (NM) Reflector 0.3 m B,V,I 10 127 B.31
Navas de Oro, Segovia Spain Reflector 0.35 m V 10 16 B.16
Ostrava Czech Republic Newton 0.2 m B,V,R,I 10 24 B.26
Ostrava Czech Republic Schmidt-Cassegrain 0.3 m B,V,R,I 10 4 B.17
Piszkéstetö Hungary Schmidt 0.6/0.9 m B,V,R,I 9 12 B.11
Piwnice** Poland Cassegrain 0.6 m U,B,V,R,I,c*, Hβ* 8, 9 612 B.1, B.6
Piwnice Poland Cassegrain 0.6 m U,B,V,R,I 10 470 B.6
Rolling Hills, Clermont USA (FL) Reflector 0.25 m B,V 10 80 B.32
Rozhen Bulgaria Ritchey-Chrétien 2 m U,B,V,R,I 9, 10 20 B.7, B.18
Rozhen Bulgaria Schmidt 0.5/0.7 m U,B,V,R,I 9, 10 33 B.8, B.19
Rozhen* Bulgaria Cassegrain 0.6 m U,B,V 9 18 B.9
Rozhen Bulgaria Cassegrain 0.6 m U,B,V,R,I 10 34 B.20
Skinakas Greece Ritchey-Chrétien 1.3 m U,B,V,R,I 9 44 B.10
Sonoita USA (AZ) Reflector 0.5 m B,V,R,I 10 349 B.22, B.23
Suhora Poland Cassegrain 0.6 m U,B,V,R,I 10 196 B.30
Tenagra-II USA (AZ) Ritchey-Chrétien 0.81 m U,B,V,R,I 10 20 B.28

Notes. N is the number of individual brightness determinations summed over all the photometric bands. The last column specifies the number of the table with the original data (available in the electronic version of this paper).

(*)

HαW and HαN are intermediate width (FWHM  ≈ 200 Å) and narrow (FWHM  ≈ 30 Å) photometric bands, both centred at the Hα spectroscopic line. c and Hβ are narrow (FWHM  ≈ 100 Å) photometric bands centred on λ = 4804 Å and at the Hβ spectroscopic line, respectively.

(**)

In these two cases, the photomultipliers were used as the light receiver (the vast majority of the data having been obtained using CCDs).

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