When is the best time to observe V774 Tauri?

V774 Tauri is best observed from October through December, with peak visibility during November when it transits around midnight in the Northern Hemisphere.

Where is V774 Tauri located in the sky?

V774 Tauri lies in the constellation Taurus at right ascension 04h 15m and declination +06° 11′.

What telescope do I need to split V774 Tauri?

Splitting V774 Tauri requires an aperture of roughly 60 mm or larger — the components are separated by about 64.6″ at magnitudes near 6.3. Larger apertures and steady seeing help resolve the pair cleanly.

V774 Tauri — Double Star in Taurus

Magnitude 6.3^m DoubleStar Taurus (Tau) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 6.31

Range 6.28 - 6.37

Variable Type BY:

Spectral Type G0IV subgiant

Star Color Yellow (B-V 0.59)

2Position & Identifiers

RA 04h 15m 29.2s

Dec +06° 11' 12.0"

Constellation Taurus (Tau)

HR 1322

HIP 19859

HD 26923

SAO 111698

Variable ID V774 Tau

Double Cat 3085

SIMBAD

3How easy to split?

Primary 6.3 mag Companion 7.0 mag Separation 64.6″

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 Quadruple C: optical

Components 4 (quadruple)

Component IDs AB

Separation 64.6″

Companion Mag 7.0

Companion Sp G3V

Position Angle 316°

Star Colors A: Yellow B: Yellow

Discoverer STTA 45

Notes

CPM with HR 1321.

Separation over time

Measured 1782 → 2021 (239 y)

Separation drift 62.6" → 64.6" (+2.00")

Rate +0.0084" / y

PA drift 314° → 316° (+2°, +0.008°/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.