HD 174474
High proper motion star; Telescopium
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HD 174474, also designated as HR 7095 or rarely 35 G. Telescopii, is a solitary white-hued star located in the southern constellation Telescopium. It has an apparent magnitude of 6.17,[2] placing it near the limit for naked eye visibility. The object is located relatively close at a distance of 244 light years based on Gaia DR3 parallax measurements[1] but is drifting closer with a heliocentric radial velocity of −44 km/s.[5] At its current distance, HD 174474's brightness is diminished by 0.26 magnitudes due to interstellar dust.[15] It has an absolute magnitude of +1.61.[6]
 | |
| Observation data Epoch J2000.0 Equinox ICRS | |
|---|---|
| Constellation | Telescopium |
| Right ascension | 18h 53m 02.34680s[1] |
| Declination | −48° 21′ 39.2965″[1] |
| Apparent magnitude (V) | 6.17±0.01[2] |
| Characteristics | |
| Spectral type | A2 V[3] |
| U−B color index | +0.08[4] |
| B−V color index | +0.14[4] |
| Astrometry | |
| Radial velocity (Rv) | −44±4[5] km/s |
| Proper motion (μ) | RA: −17.178 mas/yr[1] Dec.: −77.772 mas/yr[1] |
| Parallax (π) | 13.3771±0.0444 mas[1] |
| Distance | 243.8 ± 0.8 ly (74.8 ± 0.2 pc) |
| Absolute magnitude (MV) | +1.61[6] |
| Details | |
| Mass | 2.05±0.04[7] M☉ |
| Radius | 1.89±0.10[8] R☉ |
| Luminosity | 18.14[9] L☉ |
| Surface gravity (log g) | 4.21+0.09 −0.06[10] cgs |
| Temperature | 8664±295[11] K |
| Metallicity [Fe/H] | −0.11[12] dex |
| Age | 630[11] Myr |
| Other designations | |
| 35 G. Telescopii[13], CD−48°12769, CPD−48°9971, GC 25872, HD 174474, HIP 92676, HR 7095, SAO 229342[14] | |
| Database references | |
| SIMBAD | data |
This is an ordinary A-type main-sequence star with a stellar classification of A2 V.[3] It has double the mass of the Sun and 1.89 times the Sun's radius.[8] It radiates 18.1 times the luminosity of the Sun from its photosphere at an effective temperature of 8,664 K.[11] HD 174474 is slightly metal deficient with an iron abundance 22% below solar levels ([Fe/H] = −0.11). It is estimated to be 630 million years old based on stellar evolution models from David & Hillenbrand (2015).[11]