When is the best time to observe 1 Camelopardalis?

1 Camelopardalis is best observed from October through December, with peak visibility during November when it transits around midnight in the Northern Hemisphere.

Where is 1 Camelopardalis located in the sky?

1 Camelopardalis lies in the constellation Camelopardalis at right ascension 04h 32m and declination +53° 55′.

What telescope do I need to split 1 Camelopardalis?

Splitting 1 Camelopardalis requires an aperture of roughly 60 mm or larger — the components are separated by about 10.4″ at magnitudes near 5.8. Larger apertures and steady seeing help resolve the pair cleanly.

1 Camelopardalis — Double Star in Camelopardalis

Observable Double Star Excellent (64/100)

Sep: 10.4", Companion: mag 6.8

Magnitude 5.8^m DoubleStar Camelopardalis (Cam) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 5.77

Spectral Type B0III giant

Star Color Yellow-white (B-V 0.18)

Distance 544 ly

2Position & Identifiers

RA 04h 32m 01.8s

Dec +53° 54' 39.0"

Constellation Camelopardalis (Cam)

HR 1417

HIP 21148

HD 28446

SAO 24672

Flamsteed 1 Cam

Variable ID Var?

Double Cat 3274

SIMBAD

3How easy to split?

Primary 5.8 mag Companion 6.8 mag Separation 10.4″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Easy	Easy	Easy
150 mm Newton 150mm Newt.	Easy	Easy	Easy
Celestron C8 (203 mm SCT) C8 203mm	Easy	Easy	Easy

Easy Medium Hard Very hard Impossible

Bortle 3 = rural · 4 = outer suburbs · 5 = suburbs

4Visibility

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Best season Oct – Dec (peak: Nov)

5Multiple Star System Triple

Components 3 (triple)

Component IDs AB

Separation 10.4″

Companion Mag 6.8

Position Angle 308°

Star Colors A: Yellow-white B: Yellow-white

Discoverer STF 550

Notes

AB binary. B, 6.94V, +0.16(B-V), -0.70(U-B), B1IV? vsini =<25k/s.

Separation over time

Measured 1800 → 2018 (218 y)

Separation drift 12.0" → 10.4" (-1.60")

Rate -0.0073" / y

PA drift 299° → 308° (+9°, +0.041°/y)

Slow change over generations — observable in lifetime comparisons.

Measured from the WDS observational archive. No orbital solution has been derived — most likely the period is too long to fit an orbit to the available measurement arc.