When is the best time to observe HIP 16587?

HIP 16587 is best observed from October through December, with peak visibility during November when it transits around midnight in the Northern Hemisphere.

Where is HIP 16587 located in the sky?

HIP 16587 lies in the constellation Camelopardalis at right ascension 03h 34m and declination +58° 46′.

What telescope do I need to split HIP 16587?

Splitting HIP 16587 requires an aperture of roughly 60 mm or larger — the components are separated by about 20.5″ at magnitudes near 6.4. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 16587 — Double Star in Camelopardalis

Magnitude 6.4^m DoubleStar Camelopardalis (Cam) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 6.40

Spectral Type A4III giant

Star Color White (B-V 0.14)

Distance 362 ly

2Position & Identifiers

RA 03h 33m 32.1s

Dec +58° 45' 54.0"

Constellation Camelopardalis (Cam)

HR 1068

HIP 16587

HD 21769

SAO 24093

Double Cat 2592

SIMBAD

3How easy to split?

Primary 6.4 mag Companion 7.7 mag Separation 20.5″

Sign in and configure your equipment and default location to see a personalized row.

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

Set a location in User Settings to see visibility data.

Best season Oct – Dec (peak: Nov)

5Multiple Star System Triple C: optical

Components 3 (triple)

Component IDs AB

Separation 20.5″

Companion Mag 7.7

Position Angle 245°

Star Colors A: White B: Yellow-white

Discoverer STF 396

Notes

AB CPM. B, spectral class F2V. Component C, 10.5v at 164".

Separation over time

Measured 1829 → 2019 (190 y)

Separation drift 20.4" → 20.5" (+0.10")

Rate +0.0005" / y

PA drift 242° → 245° (+3°, +0.016°/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.