When is the best time to observe Revati?

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

Where is Revati located in the sky?

Revati lies in the constellation Pisces at right ascension 01h 14m and declination +07° 35′.

What telescope do I need to split Revati?

Splitting Revati requires an aperture of roughly 60 mm or larger — the components are separated by about 22.8″ at magnitudes near 5.2. Larger apertures and steady seeing help resolve the pair cleanly.

Revati — Double Star in Pisces

HIP 5737; Zeta Piscium; 86 Piscium

Observable Double Star Excellent (66/100)

Sep: 22.8", Companion: mag 6.3

Magnitude 5.2^m DoubleStar Pisces (Psc) Visible

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Observe

1Physical Properties

Magnitude 5.24

Spectral Type A7IV subgiant

Star Color Yellow-white (B-V 0.32)

Distance 125 ly

2Position & Identifiers

RA 01h 13m 43.9s

Dec +07° 34' 31.0"

Constellation Pisces (Psc)

HR 361

HIP 5737

HD 7344

SAO 109739

Bayer Zeta

Flamsteed 86 Psc

Double Cat 996

SIMBAD Wikipedia

3How easy to split?

Primary 5.2 mag Companion 6.3 mag Separation 22.8″

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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

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Best season Sep – Nov (peak: Oct)

5Multiple Star System Quintuple

Components 5 (quintuple)

Component IDs O

Separation 22.8″

Companion Mag 6.3

Companion Sp F7V

Position Angle 63°

Star Colors A: Yellow-white B: Yellow

Discoverer STF 100

Notes

CPM with HR 362 at 24". ADS 996A is close occultation double, 6.3, 6.3v, 0.05":. Component B, HR 362 is SB; C, 12.2 is | 1" from B.

Separation over time

Measured 1755 → 2021 (266 y)

Separation drift 25.2" → 22.8" (-2.40")

Rate -0.0090" / y

PA drift 67° → 63° (-4°, -0.015°/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.