V1334 Cygni

A light curve for V1334 Cygni, plotted from TESS data.[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension 21h 19m 22.17915s[2]
Declination +38° 14′ 14.8688″[2]
Apparent magnitude (V) 5.77 - 5.96[3]
Characteristics
Spectral type F1II[4] + B7.0V[5]
B−V color index 0.50[6]
Variable type δ Cepheid[3]
Astrometry
Proper motion (μ) RA: 2.293±0.065[2] mas/yr
Dec.: 0.226±0.076[2] mas/yr
Parallax (π)1.0831 ± 0.0738 mas[2]
Distance720.35±7.84 pc
Absolute magnitude (MV)−3.06[7]
Orbit[8]
PrimaryAa
CompanionAb
Period (P)1932.8±1.8 d
Semi-major axis (a)8.54±0.04 mas"
(6.16±0.07 au)
Eccentricity (e)0.233±0.001
Inclination (i)124.94±0.09°
Longitude of the node (Ω)229.8±0.3°
Periastron epoch (T)2453316.75±4.1
Semi-amplitude (K1)
(primary)		14.168±0.014 km/s
Semi-amplitude (K2)
(secondary)		15.036±0.304 km/s
Details
Aa (Cepheid)
Mass4.288±0.133[8] M☉
Ab
Mass4.040±0.048[8] M☉
Other designations
HD 203156, ADS 14859 AB, BD+37 4271, HIP 105269, HR 8157, SAO 71203[9]
Database references
SIMBADdata

V1334 Cygni, also referred to as ADS 14859 and HR 8157 in astronomical literature, is a star about 2350±25 light years from the Earth in the constellation Cygnus.[8] It is a 5th magnitude star, which will be faintly visible to the naked eye of an observer located far from city lights. It is a classical Cepheid variable star, ranging in brightness from magnitude 5.77 to 5.96 over a period of 3.332816 days.[3] V1334 Cygni is an important calibrator for models of Cepheid variables, because its presence in triple star system with a close binary pair has allowed its distance to be measured geometrically with 1% accuracy.[8]

V1334 Cygni was discovered to be a double star in November of 1886, by George Hough using the 18.5 inch refractor at the old (Chicago) site of the Dearborn Observatory. It was given number 286 in his catalog.[10] In the fall of 1966, V1334 Cygni was discovered to be a variable star accidentally, when Robert Mills used it as a presumed constant-brightness comparison star in a search for Cepheid variables. Follow-up observations by Mills in 1968 at Lowell Observatory found that the star showed "cepheid-like" brightness changes with a period of 3.335 days.[11] It was given the variable star designation V1334 Cygni in 1970.[12] In 2000, Nancy Evans deduced from radial velocity measurements that the star is actually a triple star system, with a close binary pair (containing the Cepheid variable) forming one "star" (component A) of the double star that had been identified more than a century earlier.[13]

Attempts to identify component B (the companion star first seen by Hough in 1886) in the late 20th and early 21st centuries have been largely unsuccessful. This is surprising, because the speckle interferometry techniques employed by these later studies have far higher resolution than did Hough's refractor. But there are possible orbits for B which would be consistent with both a real 19th century detection and the non-detections a century later.[6] There are doubts over whether a third star exists at all.[14]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 24 January 2023.
  2. 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. 1 2 3 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  4. ↑ Kovtyukh, V.; Szabados, L.; Chekhonadskikh, F.; Lemasle, B.; Belik, S. (2015). "Discovery of blue companions to two southern Cepheids: WW Car and FN Vel". Monthly Notices of the Royal Astronomical Society. 448 (4): 3567–3571. arXiv:1503.04754. Bibcode:2015MNRAS.448.3567K. doi:10.1093/mnras/stv258.
  5. ↑ Cruzalèbes, P.; Petrov, R. G.; Robbe-Dubois, S.; Varga, J.; Burtscher, L.; Allouche, F.; Berio, P.; Hofmann, K. H.; Hron, J.; Jaffe, W.; Lagarde, S.; Lopez, B.; Matter, A.; Meilland, A.; Meisenheimer, K.; Millour, F.; Schertl, D. (December 2019). "A catalogue of stellar diameters and fluxes for mid-infrared interferometry". Monthly Notices of the Royal Astronomical Society. 490 (3): 3158–3176. arXiv:1910.00542. Bibcode:2019MNRAS.490.3158C. doi:10.1093/mnras/stz2803.
  6. 1 2 Evans, Nancy Remage; Franz, Otto; Massa, Derck; Mason, Brian; Walker, Richard L.; Karovska, Margarita (November 2006). "Cepheids in Multiple Systems: ADS 14859". The Publications of the Astronomical Society of the Pacific. 118 (849): 1545–1549. Bibcode:2006PASP..118.1545E. doi:10.1086/509791.
  7. ↑ Acharova, I. A.; et al. (2012). "Galactic restrictions on iron production by various types of supernovae". Monthly Notices of the Royal Astronomical Society. 420 (2): 1590. arXiv:1111.2152. Bibcode:2012MNRAS.420.1590A. doi:10.1111/j.1365-2966.2011.20161.x. S2CID 118404944.
  8. 1 2 3 4 5 Gallenne, A.; Kervella, P.; Evans, N. R.; Proffitt, C. R.; Monnier, J. D.; Mérand, A.; Nelan, E.; Winston, E.; Pietrzyński, G.; Schaefer, G.; Gieren, W.; Anderson, R. I.; Borgniet, S.; Kraus, S.; Roettenbacher, R. M.; Baron, F.; Pilecki, B.; Taormina, M.; Graczyk, D.; Mowlavi, N.; Eyer, L. (November 2018). "A Geometrical 1% Distance to the Short-period Binary Cepheid V1334 Cygni". The Astrophysical Journal. 867 (2): 121. arXiv:1809.07486. Bibcode:2018ApJ...867..121G. doi:10.3847/1538-4357/aae373.
  9. ↑ "V1334 Cyg -- Classical Cepheid Variable". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-01-24.
  10. ↑ Hough, G. W. (July 1890). "Catalogue of 94 New Double Stars and Measures of 107 Double Stars". Astronomische Nachrichten. 125 (1): 1. Bibcode:1890AN....125....1H. doi:10.1002/asna.18901250102.
  11. ↑ Mills, Robert L. (February 1969). "Photoelectric observations of HR 8157". Lowell Observatory Bulletin. 7 (148): 113–115. Bibcode:1969LowOB...7..113M.
  12. ↑ Kukarkin, B. V.; Kholopov, P. N.; Perova, N. B. (October 1970). "57th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 480 (1): 1. Bibcode:1970IBVS..480....1K. Retrieved 24 January 2023.
  13. ↑ Evans, Nancy Remage (June 2000). "V1334 Cygni: A Triple System Containing a Classical Cepheid". The Astronomical Journal. 119 (6): 3050–3059. Bibcode:2000AJ....119.3050E. doi:10.1086/301397.
  14. ↑ Gallenne, A.; Monnier, J. D.; Mérand, A.; Kervella, P.; Kraus, S.; Schaefer, G. H.; Gieren, W.; Pietrzyński, G.; Szabados, L.; Che, X.; Baron, F.; Pedretti, E.; McAlister, H.; ten Brummelaar, T.; Sturmann, J.; Sturmann, L.; Turner, N.; Farrington, C.; Vargas, N. (April 2013). "Multiplicity of Galactic Cepheids from long-baseline interferometry. I. CHARA/MIRC detection of the companion of V1334 Cygni". Astronomy and Astrophysics. 552: A21. arXiv:1302.1817. Bibcode:2013A&A...552A..21G. doi:10.1051/0004-6361/201321091.
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