HD 53680, HD 53705, and HD 53706

Last updated
HD 53705 / 53706 / 53680
Puppis constellation map.svg
Red circle.svg
Location of HD 53680, HD 53705, and HD 53706 (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Puppis [1]
HD 53705
Right ascension 07h 03m 57.315s [2]
Declination −43° 36′ 28.93″ [2]
Apparent magnitude  (V)5.559±0.003 [3]
HD 53706
Right ascension 07h 03m 58.921s [4]
Declination −43° 36′ 40.87″ [4]
Apparent magnitude  (V)6.859±0.003 [3]
HD 53680
Right ascension 07h 03m 50.214s [5]
Declination −43° 33′ 41.41″ [5]
Apparent magnitude  (V)8.686 [6]
Characteristics
HD 53705
Evolutionary stage main sequence [7]
Spectral type G1.5V [8]
B−V color index 0.624±0.009
HD 53706
Evolutionary stage main sequence [7]
Spectral type K0.5V [9]
B−V color index 0.779±0.020
HD 53680
Spectral type K6V [9]
B−V color index 1.180±0.012
Astrometry
HD 53705
Radial velocity (Rv)+88.81±0.12 [2] km/s
Proper motion (μ)RA: −105.047 mas/yr [2]
Dec.: +389.833 mas/yr [2]
Parallax (π)58.6192±0.0477  mas [2]
Distance 55.64 ± 0.05  ly
(17.06 ± 0.01  pc)
Absolute magnitude  (MV)+4.47 [10]
HD 53706
Radial velocity (Rv)+88.55±0.12 [4] km/s
Proper motion (μ)RA: −101.722 mas/yr [4]
Dec.: +382.507 mas/yr [4]
Parallax (π)58.6173±0.0126  mas [4]
Distance 55.64 ± 0.01  ly
(17.060 ± 0.004  pc)
Absolute magnitude  (MV)+5.99 [11]
HD 53680
Radial velocity (Rv)+89.065±0.005 [12] km/s
Proper motion (μ)RA: −91.391 mas/yr [5]
Dec.: +434.521 mas/yr [5]
Parallax (π)57.7938±0.3355  mas [5]
Distance 56.4 ± 0.3  ly
(17.3 ± 0.1  pc)
Absolute magnitude  (MV)7.81±0.03 [13]
Orbit [14]
PrimaryHD 53680 A
CompanionHD 53680 B
Period (P)1,685.2+0.37
−0.38 days
Semi-major axis (a)2.53±0.02  AU
Eccentricity (e)0.485±0.002
Inclination (i)163.6+1.4
−1.7 [12] °
Longitude of the node (Ω)147.86+0.06
−0.08°
Argument of periastron (ω)
(secondary)		226.17+0.13
−0.17°
Semi-amplitude (K1)
(primary)		1.252+0.001
−0.002 km/s
Details
HD 53705
Mass 0.99+0.02
−0.01 [15]   M☉
Radius 1.24±0.02 [16]   R☉
Luminosity 1.52+0.07
−0.08 [16]   L☉
Surface gravity (log g)4.29±0.02 [15]   cgs
Temperature 5,826±8 [15]   K
Metallicity [Fe/H]−0.230±0.006 [15]   dex
Rotational velocity (v sin i)1.6±0.5 [17]  km/s
Age 9.29+0.25
−0.26 [15]   Gyr
HD 53706
Mass 0.818±0.040 [4]   M☉
Radius 0.873±0.018 [4]   R☉
Luminosity 0.499±0.007 [4]   L☉
Surface gravity (log g)4.461+0.011
−0.020 [4]   cgs
Temperature 5192+9
−22 [4]   K
Metallicity [Fe/H]−0.28±0.03 [17]   dex
Rotational velocity (v sin i)0.3±0.5 [17]  km/s
Age 11.7+3.3
−9.6(weakly constrained) [17]   Gyr
HD 53680 A
Mass 0.71±0.04 [14]   M☉
Radius 0.68±0.03 [14]   R☉
Luminosity 0.17+0.04
−0.02 [14]   L☉
Surface gravity (log g)4.62±0.03 [14]   cgs
Temperature 4,460±100 [13]   K
Metallicity [Fe/H]−0.29±0.08 [12]   dex
Rotational velocity (v sin i)2.08±0.31 [12]  km/s
Age 0.7 - 9.4 (weakly constrained) [12]   Gyr
HD 53680 B
Mass 0.22±0.02 [12]   M☉
Other designations
WD J07040−4337, IRAS 07024−4332
HD 53705: GJ 264.1 A, GJ 9223 A, HD 53705, HIP 34065, HR 2667
HD 53706: GJ 264.1 B, GJ 9223 B, HD 53706, HIP 34069, HR 2668
HD 53680: GJ 264, HD 53680, HIP 34052
Database references
SIMBAD HD 53705
HD 53706
HD 53680

HD 53705/53706/53680 is a star system that lies 56 light-years away in the constellation of Puppis. The system consists of four stars in two binaries, making it one of the nearest quadruple star systems.

Contents

The four components are a main sequence star similar to the Sun, two smaller K-type main sequence stars, and a low-mass star.

Component discovery

A diagram of HD 53706 (GJ 264.1 B) and HD 53680 (GJ 264), relative to HD 53705 (GJ 264.1 A) Gliese264.1.png
A diagram of HD 53706 (GJ 264.1 B) and HD 53680 (GJ 264), relative to HD 53705 (GJ 264.1 A)

The earliest observation of the HD 53705/HD 53706 pair in the Washington Double Star Catalog (WDS) dates to 1826 and was made by James Dunlop, stating a position angle of 119 degrees and a separation of 21.5 arcseconds for the companion. [18] The two stars have moved very little relative to each other since, with the most recent measurement from 1999 stating a position angle of 126 degrees and a separation of 20.9 arcseconds. A separation of 21 arcseconds translates to a physical separation perpendicular to the line of sight of approximately 480 AU, [19] so the orbit of the stars lasts somewhere on the order of millennia.

The relationship of HD 53680 to the closer binary was recognised later, with the first measurement in the WDS dating to 1900. [18] With a position angle of 337 degrees and a separation of 185.7 arcseconds, HD 53680 lies on the opposite side of HD 53705 to HD 53706, and is about nine times more distant. This separation results in a physical separation perpendicular to the line of sight of 4390 AU, [19] which is atypically distant for a stellar companion but still close enough to be strongly gravitationally bound.

While all three components have similar proper motion, HD 53680's proper motion as measured by the Hipparcos satellite is sizeably discrepant from the proper motions of the other two components. A clue to the cause of this is that HD 53680's Tycho-2 proper motion is different from the Hipparcos values, which indicates that the star is being perturbed by a close companion. [20] A fit of the Hipparcos astrometric data found a weakly constrained fit found a period of 1500 days, an inclination of 180 degrees (a face-on orbit) and a semimajor axis of 30.6 milliarcseconds. [21] The fit is weakly constrained because Hipparcos observations do not span the full orbit of the companion, but the fit does adjust HD 53680's proper motion to be consistent with the proper motion of HD 53705/53706.

The low inclination of HD 53680 B's orbit reduces the amplitude of the radial velocity variation that it caused on HD 53680 A. In this case, the effect reduced the minimum mass of the companion into the brown dwarf regime as deduced from observations with the CORALIE spectrograph. [12] The spectroscopic orbit produces far stronger constraint compared to the astrometry-only orbit, and a mass of 0.22  M☉ is derived. [12]

Stellar properties

HD 53705, with a spectral type of G1.5V, is a G-type main-sequence star that is slightly hotter, larger and brighter than the Sun. HD 53706 and HD 53680 A are both K-type main-sequence stars, with spectral types of K0.5V and K6V, respectively. Both of these stars are substantially cooler, smaller and dimmer than the Sun.

The three stars with observed spectra in the system have similar metallicity values: [Fe/H] = −0.21±0.03 and −0.28±0.03 for HD 53705 and B, [17] and [Fe/H] = −0.29±0.08 for HD 53680 A. [12]

The sub-solar metallicity of the stars has the effect of heating up their chromospheres; Though HD 53705 has a mass that is approximately solar, its effective temperature is about fifty degrees hotter. [7]

The kinematics of the stars, with large proper motion and radial velocity, suggests that the system is a member of the thick disk, [19] [21] the population of stars that comprise most of the older members of the Milky Way's spiral arms. This is supported by the parameters of HD 53705; the surface gravity of 4.34 is somewhat low for a G0V star, indicating that it is relatively old and moving towards the end of its main sequence lifetime [7] - which, when coupled with the solar mass, mean that estimates for the star's age are approximately 9 billion years old, approximately twice the solar age. With a peculiar velocity of 75.7 km/s, The orbit of the system about the galaxy has an eccentricity of 0.31 and brings the system up to 151 parsecs away from the galactic plane - again indicative of a thick disk system. [19]

Planet searches

Being bright, solar-type and nearby, HD 53705 and B are targets for radial velocity (RV)-based planet searches.

HD 53705 was one of the 37 targets of the first RV-based planet search in the southern hemisphere, the ESO CES survey. [22] This survey did not detect any companion with several Jovian masses out to a few AU. An extension of this survey to the HARPS spectrograph provides further constraint, suggesting that there are no Jupiter-mass companions out to about 5 AU. [23]

HD 53705 can be presumed to be on the CORALIE sample, as it satisfies the criteria of parallax = ≥20 mas with error ≤5 mas, and spectral type between F8 and M1. [24] HD 53706 fails the criteria due to the large error on its parallax, while HD 53680 satisfies them. [12]

The two stars are also on the Anglo-Australian Telescope sample, [25] which has found that they are stable to 4.5 and 2.9 m/s, respectively. This excludes the presence of giant planets at separations of a few AU around either star. [26]

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific . 99 (617): 695. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Constellation record for this object at VizieR.
  2. 1 2 3 4 5 6 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 Paunzen, E. (2015-08-01). "A new catalogue of Strömgren-Crawford uvbyβ photometry". Astronomy and Astrophysics. 580: A23. arXiv: 1506.04568 . Bibcode:2015A&A...580A..23P. doi:10.1051/0004-6361/201526413. ISSN   0004-6361.
  4. 1 2 3 4 5 6 7 8 9 10 11 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.
  5. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  6. ↑ Koen, C.; Kilkenny, D.; van Wyk, F.; Marang, F. (2010-04-21). "UBV ( RI ) C JHK observations of Hipparcos -selected nearby stars". Monthly Notices of the Royal Astronomical Society. 403 (4): 1949–1968. doi: 10.1111/j.1365-2966.2009.16182.x .
  7. 1 2 3 4 Chmielewski, Y.; Cayrel De Strobel, G.; Lebreton, Y.; Bentolila, C. (1991). "Spectroscopic study of the visual binary HD 53705 and HD 53706". Astronomy and Astrophysics. 247: 368. Bibcode:1991A&A...247..368C.
  8. ↑ Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins Catalog of Revised MK Types for the Cooler Stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  9. 1 2 Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161. arXiv: astro-ph/0603770 . Bibcode:2006AJ....132..161G. doi:10.1086/504637.
  10. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters . 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  11. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters . 38 (5): 331. arXiv: 1108.4971 . Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  12. 1 2 3 4 5 6 7 8 9 10 Sahlmann, J.; et al. (2010). "Search for brown-dwarf companions of stars". Astronomy & Astrophysics. 525: A95. arXiv: 1009.5991 . Bibcode:2011A&A...525A..95S. doi:10.1051/0004-6361/201015427. S2CID   119276951.
  13. 1 2 Houdebine, E. R. (September 2011). "Observation and modelling of main-sequence star chromospheres - XVI. Rotation of dK5 stars". Monthly Notices of the Royal Astronomical Society . 407 (3): 1657–1673. Bibcode:2011MNRAS.416.2233H. doi: 10.1111/j.1365-2966.2011.19199.x .
  14. 1 2 3 4 5 Barbato, D.; Ségransan, D.; Udry, S.; Unger, N.; Bouchy, F.; Lovis, C.; Mayor, M.; Pepe, F.; Queloz, D.; Santos, N. C.; Delisle, J. B.; Figueira, P.; Marmier, M.; Matthews, E. C.; Curto, G. Lo (2023-06-01). "The CORALIE survey for southern extrasolar planets - XIX. Brown dwarfs and stellar companions unveiled by radial velocity and astrometry". Astronomy & Astrophysics. 674: A114. arXiv: 2303.16717 . Bibcode:2023A&A...674A.114B. doi:10.1051/0004-6361/202345874. ISSN   0004-6361. HD 53680's database entry at VizieR.
  15. 1 2 3 4 5 Martos, Giulia; Meléndez, Jorge; Rathsam, Anne; Carvalho-Silva, Gabriela (2023-04-21). "Metallicity and age effects on lithium depletion in solar analogues". Monthly Notices of the Royal Astronomical Society. 522 (3): 3217–3226. arXiv: 2305.01861 . Bibcode:2023MNRAS.522.3217M. doi: 10.1093/mnras/stad1177 . ISSN   0035-8711.
  16. 1 2 Harada, Caleb K.; et al. (June 2024). "Setting the Stage for the Search for Life with the Habitable Worlds Observatory: Properties of 164 Promising Planet-survey Targets". The Astrophysical Journal Supplement Series. 272 (2). id. 30. arXiv: 2401.03047 . Bibcode:2024ApJS..272...30H. doi: 10.3847/1538-4365/ad3e81 . HD 53705's database entry at VizieR.
  17. 1 2 3 4 5 Valenti, J. A.; Fischer, D. A. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi: 10.1086/430500 .
  18. 1 2 "VizieR".
  19. 1 2 3 4 Allen, C.; et al. (2000). "Wide binaries among high-velocity and metal-poor stars". Astronomy and Astrophysics. 356: 529. Bibcode:2000A&A...356..529A.
  20. ↑ Makarov, V. V.; et al. (2005). "Statistical Constraints for Astrometric Binaries with Nonlinear Motion". The Astronomical Journal. 129 (5): 2420–2427. Bibcode:2005AJ....129.2420M. doi: 10.1086/429590 .
  21. 1 2 Makarov, V. V.; et al. (2008). "Common Proper Motion Companions to Nearby Stars: Ages and Evolution". The Astrophysical Journal. 687 (1): 566–578. arXiv: 0808.3414 . Bibcode:2008ApJ...687..566M. doi:10.1086/591638. S2CID   17811620.
  22. ↑ Endl, M.; et al. (2002). "The planet search program at the ESO Coudé Echelle spectrometer. III. The complete Long Camera survey results". Astronomy & Astrophysics. 392 (2): 671–690. arXiv: astro-ph/0207512 . Bibcode:2002A&A...392..671E. doi:10.1051/0004-6361:20020937. S2CID   17393347.
  23. ↑ Zechmeister, M.; et al. (2013). "The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars". Astronomy & Astrophysics. 552: A78. arXiv: 1211.7263 . Bibcode:2012yCat..35520078Z. doi:10.1051/0004-6361/201116551. S2CID   53694238.
  24. ↑ Udry, S. (2000). "The CORALIE Planet-Search Sample". From Extrasolar Planets to Cosmology: The VLT Opening Symposium. Eso Astrophysics Symposia. p. 571. Bibcode:2000fepc.conf..571U. doi:10.1007/10720961_83. ISBN   978-3-540-67163-3.
  25. ↑ Jones, Hugh R. A.; et al. (2002). "Extrasolar planets around HD 196050, HD 216437 and HD 160691". Monthly Notices of the Royal Astronomical Society. 337 (4): 1170–1178. arXiv: astro-ph/0206216 . Bibcode:2002MNRAS.337.1170J. doi: 10.1046/j.1365-8711.2002.05787.x . S2CID   119520409.
  26. ↑ Wittenmyer, Robert A.; et al. (2011). "On the Frequency of Jupiter Analogs". The Astrophysical Journal. 727 (2): 102. arXiv: 1011.4720 . Bibcode:2011ApJ...727..102W. doi:10.1088/0004-637X/727/2/102. S2CID   56204861.
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