When is the best time to observe HIP 18488?

HIP 18488 is best observed from October through December, with peak visibility during November when it transits around midnight in the Northern Hemisphere.

Where is HIP 18488 located in the sky?

HIP 18488 lies in the constellation Camelopardalis at right ascension 03h 57m and declination +61° 07′.

What telescope do I need to split HIP 18488?

Splitting HIP 18488 requires an aperture of roughly 200 mm or larger — the components are separated by about 1.7″ at magnitudes near 5.0. The companion is about 3.1 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 18488 — Double Star in Camelopardalis

Observable Double Star Fair (26/100)

Sep: 1.7", Companion: mag 8.1

Magnitude 5.0^m DoubleStar Camelopardalis (Cam) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 5.00

Spectral Type K3I-II+A3V: supergiant

Star Color Red (B-V 1.45)

Distance 217 ly

2Position & Identifiers

RA 03h 57m 08.3s

Dec +61° 06' 32.0"

Constellation Camelopardalis (Cam)

HR 1205

HIP 18488

HD 24481

Double Cat 2867

SIMBAD

3How easy to split?

Primary 5.0 mag Companion 8.1 mag Separation 1.7″

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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	Hard+	Hard+	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 200 mm reflector.

4Visibility

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Best season Oct – Dec (peak: Nov)

5Multiple Star System

Separation 1.7″

Companion Mag 8.1

Position Angle 49°

Star Colors A: Red

Discoverer STT 67

Notes

Companion A0, CPM.

Separation over time

Measured 1843 → 2016 (173 y)

Separation drift 1.7" → 1.7" (+0.00")

Rate +0.0000" / y

PA drift 44° → 49° (+5°, +0.029°/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.