Theta Reticuli

Theta Reticuli is double star in southern constellation of Reticulum, located just 50′ south of Alpha Reticuli.[9] The pair are visible to the naked eye as a dim, white-hued point of light with a combined apparent visual magnitude of 5.88.[2] They lie at roughly the same distance from the Sun based on parallax, with the primary being around 466 light years away. They also share a similar proper motion,[1][7] suggesting they may be gravitationally-bound.[10]

Theta Reticuli

Location of θ Reticuli (circled)
Observation data Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation	Reticulum
Right ascension	04h 17m 40.27169s[1]
Declination	−63° 15′ 19.4882″[1]
Apparent magnitude (V)	5.88[2] 6.05 + 7.65[3]
Characteristics
θ Ret A
Spectral type	B9IV[4]
B−V color index	−0.09[3]
Variable type	suspected[5]
θ Ret B
Spectral type	kA2hA5VmA7[4]
B−V color index	+0.14[3]
Astrometry
θ Ret A
Radial velocity (Rv)	3.0±7.4[2] km/s
Proper motion (μ)	RA: +6.273[1] mas/yr Dec.: +35.360[1] mas/yr
Parallax (π)	7.0053 ± 0.0401[1] mas
Distance	466 ± 3 ly (142.7 ± 0.8 pc)
Absolute magnitude (MV)	−0.04[6]
θ Ret B
Proper motion (μ)	RA: +8.512[7] mas/yr Dec.: +35.235[7] mas/yr
Parallax (π)	7.1837 ± 0.0540[7] mas
Distance	454 ± 3 ly (139 ± 1 pc)
Details
θ Ret A
Mass	3.363±0.117[6] M☉
Luminosity	179[6] L☉
Temperature	11,967[6] K
Age	166[6] Myr
θ Ret B
Mass	≥ 1.18[6] M☉
Temperature	9,132[7] K
Age	200[4] Myr
Other designations
θ2 Ret, CD−63°143, HD 27657, HIP 20020, HR 1372, WDS J04177-6315[8]
θ Ret A: NSV 1556, GC 5233, SAO 248986
θ Ret B: GC 5232, SAO 248985
Database references
SIMBAD	data
	A
	B

The magnitude 6.05[3] primary, designated component A, has a stellar classification of B9IV,[4] matching a B-type subgiant. It is 166 million years old with 3.4 times the mass of the Sun. The star is radiating 179 times the Sun's luminosity from its photosphere at an effective temperature of 11,967 K.[6]

As of 2015, the magnitude 7.65[3] secondary, component B, had an angular separation of 4.10″ from the primary along a position angle of 3°.[11] It is most likely a very young main sequence star,[6] and is an Am star with a stellar classification of kA2hA5VmA7.[4] This notation indicates the spectrum displays the K-line of an A2 type star, the hydrogen lines of a cooler A5 star, and the metal lines of an A7 star. This system is a source of X-ray emission, which may be coming from the companion.[6]