When is the best time to observe 26 Andromedae?

26 Andromedae is best observed from August through October, with peak visibility during September when it transits around midnight in the Northern Hemisphere.

Where is 26 Andromedae located in the sky?

26 Andromedae lies in the constellation Andromeda at right ascension 00h 19m and declination +43° 47′.

What telescope do I need to split 26 Andromedae?

Splitting 26 Andromedae requires an aperture of roughly 80 mm or larger — the components are separated by about 6.1″ at magnitudes near 6.1. The companion is about 4.0 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

26 Andromedae — Double Star in Andromeda

Magnitude 6.1^m DoubleStar Andromeda (And) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 6.11

Spectral Type B8V

Star Color Blue-white (B-V -0.08)

2Position & Identifiers

RA 00h 18m 42.1s

Dec +43° 47' 28.0"

Constellation Andromeda (And)

HR 70

HIP 1501

HD 1438

SAO 36256

Flamsteed 26 And

Double Cat 254

SIMBAD

3How easy to split?

Primary 6.1 mag Companion 10.1 mag Separation 6.1″

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.	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

Set a location in User Settings to see visibility data.

Best season Aug – Oct (peak: Sep)

5Multiple Star System

Separation 6.1″

Companion Mag 10.1

Position Angle 240°

Star Colors A: Blue-white B: Yellow

Discoverer STT 5

Notes

CPM. Companion F3V.

Separation over time

Measured 1846 → 2016 (170 y)

Separation drift 7.1" → 6.1" (-1.00")

Rate -0.0059" / y

PA drift 235° → 240° (+5°, +0.029°/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.