Double star system in the constellation Camelopardalis
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! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000      Equinox J2000
! style="text-align:left" | Apparent magnitude (V)
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:center" colspan="2" | 1 Cam A
! style="text-align:left" | Spectral type
! style="text-align:left" | U−B 
! style="text-align:left" | B−V 
! style="text-align:left" | Variable type
! style="text-align:center" colspan="2" | 1 Cam B
! style="text-align:left" | Spectral type
! style="text-align:left" | U−B 
! style="text-align:left" | B−V 
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1 Camelopardalis (1 Cam) is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately away. It is faintly visible to the naked eye under good observing conditions.
The 1 Camelopardalis system is part of the Camelopardalis OB1 stellar association, which is 820 pc away. 1 Camelopardalis A is a hot massive star which has evolved away from the main sequence to become a giant. 1 Camelopardalis B is 10" away and is probably an early B class subgiant.
There is an 11th magnitude star 150" away. It has been considered to be a member of a triple system, but Gaia observations show it to be an unrelated background object.
In 1982, Mikołaj Jerzykiewicz and Christiaan L. Sterken reported that 1 Camelopardalis might be a variable star, but some subsequent studies failed to confirm that. Its brightness was convincingly shown to be variable when the "Hipparcos" data was analyzed. It was given its variable star designation, DL Camelopardalis, in 1999. 1 Camelopardalis A is a variable star with a small amplitude. It has a likely period of 0.22132 days and is thought to be a β Cephei variable or slowly pulsating B-type star. "Hipparcos" photometry shows an amplitude of 0.035 magnitudes. It has a rotational velocity of , one of the highest known.
References.
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