When is the best time to observe HIP 16292?

HIP 16292 is best observed from October through December, with peak visibility during November when it transits around midnight in the Northern Hemisphere.

Where is HIP 16292 located in the sky?

HIP 16292 lies in the constellation Camelopardalis at right ascension 03h 30m and declination +55° 27′.

What telescope do I need to split HIP 16292?

Splitting HIP 16292 requires an aperture of roughly 60 mm or larger — the components are separated by about 14.6″ at magnitudes near 5.1. The companion is about 4.9 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 16292 — Double Star in Camelopardalis

Magnitude 5.1^m DoubleStar Camelopardalis (Cam) Visible

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Observe

1Physical Properties

Magnitude 5.09

Variable Type Delta Scuti (Pulsating)

Spectral Type A1V

Star Color White (B-V 0.05)

Distance 130 ly

2Position & Identifiers

RA 03h 30m 00.2s

Dec +55° 27' 07.0"

Constellation Camelopardalis (Cam)

HR 1046

HIP 16292

HD 21447

SAO 24064

Double Cat 2565

SIMBAD

3How easy to split?

Primary 5.1 mag Companion 10.0 mag Separation 14.6″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Medium+	Medium	Hard+
150 mm Newton 150mm Newt.	Easy	Easy	Medium+
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 C: optical

Components 3 (triple)

Component IDs AB

Separation 14.6″

Companion Mag 10.0

Position Angle 159°

Star Colors A: White B: Orange

Discoverer STF 390

Notes

AB CPM.

Separation over time

Measured 1831 → 2015 (184 y)

Separation drift 13.5" → 14.6" (+1.10")

Rate +0.0060" / y

PA drift 162° → 159° (-3°, -0.016°/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.