When is the best time to observe 7 Camelopardalis?

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

Where is 7 Camelopardalis located in the sky?

7 Camelopardalis lies in the constellation Camelopardalis at right ascension 04h 57m and declination +53° 45′.

What telescope do I need to split 7 Camelopardalis?

Splitting 7 Camelopardalis requires an aperture of roughly 660 mm or larger — the components are separated by about 0.6″ at magnitudes near 4.5. The companion is about 3.4 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

7 Camelopardalis — Double Star in Camelopardalis

Magnitude 4.5^m DoubleStar Camelopardalis (Cam) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.47

Spectral Type A1V

Star Color White (B-V -0.02)

2Position & Identifiers

RA 04h 57m 17.2s

Dec +53° 45' 08.0"

Constellation Camelopardalis (Cam)

HR 1568

HIP 23040

HD 31278

SAO 24929

Flamsteed 7 Cam

Double Cat 3536

SIMBAD

3How easy to split?

Primary 4.5 mag Companion 7.9 mag Separation 0.6″

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

Easy Medium Hard Very hard Impossible

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

To reach "Medium" at Bortle 3, you'd need at least a 660 mm reflector.

4Visibility

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Best season Oct – Dec (peak: Nov)

5Multiple Star System Triple

Components 3 (triple)

Component IDs AB

Separation 0.6″

Companion Mag 7.9

Position Angle 200°

Star Colors A: White B: Yellow

Discoverer D 5

Notes

AB 4.5, 7.8, 284.0y, a = 0.78". C, 11v at 26" CPM, possibly physical.

Separation over time

Measured 1865 → 2013 (148 y)

Separation drift 1.2" → 0.60" (-0.60")

Rate -0.0041" / y

PA drift 309° → 200° (-109°, -0.736°/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.