When is the best time to observe HIP 16228?

HIP 16228 is best observed from October through December, with peak visibility during November when it transits around midnight in the Northern Hemisphere.

Where is HIP 16228 located in the sky?

HIP 16228 lies in the constellation Camelopardalis at right ascension 03h 29m and declination +59° 56′.

What telescope do I need to split HIP 16228?

Splitting HIP 16228 requires an aperture of roughly 100 mm or larger — the components are separated by about 2.3″ at magnitudes near 4.2. The companion is about 3.6 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 16228 — Double Star in Camelopardalis

Observable Double Star Good (49/100)

Sep: 2.3", Companion: mag 7.8

Magnitude 4.2^m DoubleStar Camelopardalis (Cam) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.21

Range 4.21 - 4.27

Period 26.8 days

Variable Type ACYG

Spectral Type B9Ia supergiant

Star Color Yellow-white (B-V 0.41)

2Position & Identifiers

RA 03h 29m 04.1s

Dec +59° 56' 25.0"

Constellation Camelopardalis (Cam)

HR 1035

HIP 16228

HD 21291

SAO 24054

Double Cat 2544

SIMBAD

3How easy to split?

Primary 4.2 mag Companion 7.8 mag Separation 2.3″

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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.	Hard+	Hard+	Hard+
Celestron C8 (203 mm SCT) C8 203mm	Medium	Medium	Medium

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)

5Light Curve

6Multiple Star System

Separation 2.3″

Companion Mag 7.8

Position Angle 162°

Star Colors A: Yellow-white B: Orange

Discoverer STF 385

Separation over time

Measured 1829 → 2021 (192 y)

Separation drift 2.4" → 2.3" (-0.10")

Rate -0.0005" / y

PA drift 161° → 162° (+1°, +0.005°/y)

Essentially fixed on human timescales — the same view your grandchildren will see.

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.