Astronomy:2MASS J18450079–1409036
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Short description: Star system of two red dwarves in the constellation Scutum
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Scutum |
| Right ascension | 18h 45m 00.79s |
| Declination | –14° 09′ 03.6″ |
| Apparent magnitude (V) | 13.221 |
| Characteristics | |
| Spectral type | M5 / M5 |
| Astrometry | |
| Gaia EDR3 4105057482987021184 | |
| Proper motion (μ) | RA: 47.53±0.04[1] mas/yr Dec.: -85.95±0.03[1] mas/yr |
| Parallax (π) | 55.2002 ± 0.0422[1] mas |
| Distance | 59.09 ± 0.05 ly (18.12 ± 0.01 pc) |
| Gaia EDR3 4105057482994688384 | |
| Radial velocity (Rv) | -23.0±0.3[2] km/s |
| Proper motion (μ) | RA: 33.48±0.04 mas/yr Dec.: -91.47±0.03 mas/yr |
| Parallax (π) | 55.1253 ± 0.0443[3] mas |
| Distance | 59.17 ± 0.05 ly (18.14 ± 0.01 pc) |
| Orbit[4] | |
| Primary | 2MASS J18450097–1409053 A |
| Companion | 2MASS J18450097–1409053 B |
| Period (P) | 586 yr |
| Semi-major axis (a) | 3.224±0.016" (52 AU) |
| Details[4] | |
| 2MASS J18450079–1409036 | |
| Mass | 0.2 M☉ |
| 2MASS J18450097–1409053 | |
| Mass | 0.2 M☉ |
| Surface gravity (log g) | 4.50±0.05[5] cgs |
| Temperature | 3000±23[5] K |
| Metallicity [Fe/H] | -0.25±0.2[5] dex |
| Age | 40±10[2] Myr |
| Other designations | |
2MASS J18450097–1409053AB | |
| 2MASS J18450097–1409053A: UCAC3 152-2811762, UCAC4 380-128133, 2MASS J18450079–1409036 | |
| 2MASS J18450097–1409053B: UCAC3 152-281185, UCAC4 380-128136, 2MASS J18450097-1409053 | |
| Database references | |
| SIMBAD | 2MASS J18450079–1409036 |
| 2MASS J18450097–1409053 | |
2MASS J18450079–1409036 and 2MASS J18450097–1409053 is a system of two red dwarf stars both of which have spectral types of M5,[6] with projected separation of 3.2 seconds of arc.[7] The system is located in the constellation Scutum. The Gaia parallaxes place the system at 18.2 parsecs (59 light-years) from Earth.[1][3] Kinematically, it belongs to young (30-50 million years) Argus association.[2]
Proper motion
2MASS J18450079–1409036 and 2MASS J18450097-1409053 appear to be a common proper motion pair,[8] confirmed to be bound in 2016.[4]
References
- ↑ 1.0 1.1 1.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 Binks, A. S.; Jeffries, R. D. (2016), "A WISE-based search for debris discs amongst M dwarfs in nearby, young, moving groups", Monthly Notices of the Royal Astronomical Society 469: 579–593, doi:10.1093/mnras/stx838
- ↑ 3.0 3.1 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 4.0 4.1 4.2 Janson, Markus; Durkan, Stephen; Hippler, Stefan; Dai, Xiaolin; Brandner, Wolfgang; Schlieder, Joshua; Bonnefoy, Mickaël; Henning, Thomas (2016), "Binaries among low-mass stars in nearby young moving groups", Astronomy & Astrophysics 599: A70, doi:10.1051/0004-6361/201629945
- ↑ 5.0 5.1 5.2 "The PASTEL catalogue : B/pastel". https://cdsarc.unistra.fr/viz-bin/cat/B/pastel.
- ↑ Riaz, Basmah; Gizis, John E.; Harvin, James (2006). "Identification of New M Dwarfs in the Solar Neighborhood". The Astronomical Journal 132 (2): 866–872. doi:10.1086/505632. Bibcode: 2006AJ....132..866R. Table 1.
- ↑ [HAZMAT. III. The UV Evolution of Mid- to Late-M Stars with GALEX HAZMAT. III. The UV Evolution of Mid- to Late-M Stars with GALEX, Table: Target Sample GALEX Photometry]
- ↑ Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L. et al. (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal 753 (2): 156. doi:10.1088/0004-637X/753/2/156. Bibcode: 2012ApJ...753..156K.
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