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[vsnet-obs 19017] NAS.VSS 1999 Jan 25-29 UT (GRL); Cepheid Observations

Norwegian Astronomical Society - Variable Star Section

Visual observations by observers of NAS.VSS (Report 1999v-004):

Object       YYMMDD(UT)   Mag   Obs  Instrum    Observation  Cl Notes
AQLV         990129.26    7.9   GRL  C203;123x  785-2; 816+3  2 Tycho
AURRT        990125.05    5.9   GRL  B10x50    576-1.5;602+0.5 2 HIP
CEPT         990125.04    8.9   GRL  C203;123x   88-1;  92+3  1 AAVSO
CRBR         990125.04    9.7   GRL  C203;123x  925-4; 994+1  1 Tycho
CRBR         990129.26    9.6   GRL  C203;123x  924-2; 994+2  2 Tycho
CRBS         990125.04    9.0   GRL  C203;123x   90=V;  93+3  1 AAVSO
CRBT         990125.04   10.3   GRL  C203;123x   98-4; 107+4  1 Tycho
CRBT         990129.26   10.2   GRL  C203;123x   98-4; 107+5  2 AAVSO
CYGCH        990125.04    7.6   GRL  C203;123x  740-2; 847+8  1 Tycho
CYGCH        990129.27    7.8   GRL  C203;123x  740-3; 847+6  2 Tycho
CYGSS        990125.04   11.7   GRL  C203;123x  119-6; 118=V  2 AAVSO
CYGZ         990129.27    8.8   GRL  C203;123x  894=V; 963+7  2 Tycho
CYGchi       990129.27    8.6   GRL  C203;123x  822-4; 882+2  2 Tycho
LYRW         990125.04    8.1   GRL  C203;123x   78-3;  83+2  1 AAVSO
MONU         990125.05    6.4   GRL  B10x50     575-6; 660+2  2 HIP
PERTX        990125.05   10.6   GRL  C203;123x  101-5; 106=V  1 SUAA
SCTR         990129.27    5.1   GRL  C203;123x  423-8; 598+8  2 Tycho
TRIR         990125.05   10.6   GRL  C203;123x  102-3; 110+3  2 AAVSO

Observer:
GRL = Bjorn H. Granslo (Fjellhamar, Norway). Instrument: 20.3-cm SCT,
  10x50 binoculars (B10x50). Sequences are Hipparcos (HIP, V-mag),
  Tycho (V-mag), SUAA.VSS and AAVSO. Observations from Jan 29 UT were
  made in morning twilight.

Note: NAS.VSS has started to follow some bright cepheids (RT Aur,
  X Cyg, Zeta Gem etc.), both for educational and scientific purposes.
  Cepheids should be suitable targets in learning how to make
  brightness observations due to their rather regular behaviour.
  Observers are asked to collect observations (step estimates) over an
  extended time interval (e.g. 1-2 years) and use these to construct
  individual light curves, where the brightness of the variable
  (expressed in grades) are plotted as a function of phase by using
  the elements from GCVS or other sources. An important goal is to
  show that it is possible derive good results without using
  magnitudes of the comparison stars. These light curves can hopefully
  be used to improve our knowledge of the periods of these stars.

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