NGC 4349

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NGC 4349
NGC 4349.png
NGC 4349
Observation data (J2000 epoch)
Right ascension 12h 24m 08s [1]
Declination −61° 52′ 18″ [1]
Distance 7,090 ly áááɢ
Apparent magnitude  (V)7.4 [1]
Apparent dimensions (V)12' [2]
Physical characteristics
Mass4,400 [3]   M☉
Estimated age250 million years [2]
Other designations Cr 255, Mel 110
Associations
See also: Open cluster, List of open clusters

NGC 4349 is an open cluster in the constellation Crux. It was discovered by James Dunlop in 1826. It is located approximately 7,000 light years away from Earth.

Contents

Characteristics

There are 390 probable member stars within the angular radius of the cluster and 129 within the central part of the cluster. The tidal radius of the cluster is 17.8 - 22.8 parsecs (58 - 75 light years) and represents the average outer limit of NGC 4349, beyond which a star is unlikely to remain gravitationally bound to the cluster core. [3] One blue straggler has been detected in the cluster. [4] There are four Cepheid variables in the direction of the cluster, among them R and T Crucis, which, however, are not members of the cluster. [5] R Crucis lies 16 arcminutes from the centre of the open cluster NGC 4349, which is beyond the outer limit of the cluster, and is estimated to be nearly 1 kpc closer to Earth than the cluster. [6] The cluster has subsolar metallicity (−0.12  ±  0.06). [7]

A brown dwarf with minimum mass 19.8 times that of Jupiter has been detected orbiting star no. 127 (vmag. 10.88 and with mass 3.9 M☉) every 678 days. At the time of discovery, star NGC 4349 No. 127 was the heaviest star with an accurate mass determination around which a substellar companion had been detected, and also one of the youngest systems known. [8] However, this star's radial velocity variations were later shown to result from stellar activity rather than a substellar companion. [9] [10]

Related Research Articles

NGC 2423-3 is a red giant star approximately 3,040 light-years away in the constellation of Puppis. The star is part of the NGC 2423 open cluster. The star has an apparent magnitude of 10 and an absolute magnitude of zero, with a mass of 2.4 times the Sun. In 2007, it was proposed that an exoplanet orbits the star, but this is now doubtful.

NGC 4349-127 is a probable red giant star approximately 6,100 light-years away in the constellation of Crux. It is a member of the open cluster NGC 4349. Its mass is estimated at 3.9 times Solar, and its age is about 200 million years.

<span class="mw-page-title-main">NGC 3293</span> Open cluster in the constellation Carina

NGC 3293 is an open cluster in the Carina constellation. It was discovered by Nicolas-Louis de Lacaille in 1751. It consists of more than 100 stars brighter than 14th magnitude in a 10 arc minute field, the brightest of which are blue supergiants of apparent magnitude 6.5 and 6.7. There is also a 7th magnitude pulsating red supergiant, V361 Carinae.

<span class="mw-page-title-main">Kappa Crucis (star)</span> Star in the constellation Crux

Kappa Crucis is a spectroscopic binary star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

NGC 6738 is an astronomical feature that is catalogued as an NGC object. Although listed as an open cluster in some astronomical databases, it may be merely an asterism; a 2003 paper in the journal Astronomy and Astrophysics describes it as being an "apparent concentration of a few bright stars on patchy background absorption".

<span class="mw-page-title-main">NGC 6281</span> Open cluster in the constellation of Scorpius

NGC 6281 is an open cluster of stars in the constellation Scorpius. It was not included in the Messier or Caldwell catalogues of nebulous objects, but it is the brightest such cluster in the constellation to be left out of both. It is readily observed with the naked eye; it is located about 2° to the east of Mu Scorpii. James Dunlop described the cluster as a "curiously curved line of pretty bright stars, with many stars mixt". John Herschel then described the cluster as both "pretty bright" and "pretty rich".

<span class="mw-page-title-main">NGC 2439</span> Open cluster in the constellation Puppis

NGC 2439 is a sparse open cluster of stars in the constellation Puppis. It has an apparent visual magnitude of 6.9, an angular size of 10 arcminutes, and is visible using a small telescope. This is a young cluster with age estimates in the range of 20–300 million years. It has a tidal radius of approximately 82 light years. No chemically peculiar stars have been found.

<span class="mw-page-title-main">HR 4887</span> Star in the constellation Crux

HR 4887 is a suspected variable star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">DS Crucis</span> Star in the constellation Crux

DS Crucis is a variable star near the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster. It is in the constellation Crux.

<span class="mw-page-title-main">BU Crucis</span> Star in the constellation Crux

BU Crucis is a variable star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">DU Crucis</span> Star in the constellation Crux

DU Crucis is a red supergiant and slow irregular variable star in the open cluster NGC 4755, which is also known as the Kappa (κ) Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">NGC 2539</span> Open cluster in the constellation Puppis

NGC 2539 is an open cluster in the constellation Puppis, located at the north edge of the constellation. It was discovered by William Herschel on January 31, 1785. It is a moderately rich cluster and with little central concentration, with Trumpler class II1m.

NGC 5662 is an open cluster in the constellation Centaurus. It was discovered by Nicolas Louis de Lacaille on May 17, 1752 from South Africa. James Dunlop observed it on July 10, 1826 from Parramatta, Australia and added it to his catalog as No. 342.

<span class="mw-page-title-main">NGC 5460</span> Open cluster in the constellation Centaurus

NGC 5460 is an open cluster in the constellation Centaurus. It is a bright but loose cluster of intermediate age located approximately 2,300 light years away from Earth. It is located nearly 2 degrees east-southeast of Zeta Centauri.

<span class="mw-page-title-main">NGC 5316</span> Open cluster in the constellation Centaurus

NGC 5316 is an open cluster in the constellation Centaurus. It was discovered by James Dunlop in 1826. Located approximately 4,000 light years away from Earth, it is located in the Carina-Sagittarius arm.

<span class="mw-page-title-main">NGC 4103</span> Open cluster in the constellation Crux

NGC 4103 is an open cluster in the constellation Crux. It was discovered by James Dunlop in 1826. It is located approximately 5,000 light years away from Earth, in the Carina-Sagittarius arm.

<span class="mw-page-title-main">IC 2714</span> Open cluster in the constellation of Carina

IC 2714 is an open cluster in the constellation Carina. It was discovered by James Dunlop in 1826. It is located approximately 4,000 light years away from Earth, in the Carina–Sagittarius Arm.

<span class="mw-page-title-main">NGC 2527</span> Open cluster in the constellation Puppis

NGC 2527 is an open cluster in the constellation Puppis. It was discovered by William Herschel on December 9, 1784. The cluster was also observed by John Herschel on January 7, 1831. He also observed it on February 5, 1837, identifying it as a different object, which was catalogued as NGC 2520. It is a poor cluster and with no central concentration, with Trumpler class III1p.

<span class="mw-page-title-main">NGC 7160</span> Open cluster in the constellation Cepheus

NGC 7160 is an open cluster in the constellation Cepheus. It was discovered by William Herschel on November 9, 1789. The cluster was also observed by John Herschel on October 7, 1829. It is a poor cluster and with little central concentration, with Trumpler class II3p. It is part of the stellar association Cepheus OB2, located one degree south-southwest of VV Cephei.

References

  1. 1 2 3 "NGC 4349". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2017-08-19.
  2. 1 2 Kharchenko, N. V.; Piskunov, A. E.; Schilbach, E.; Röser, S.; Scholz, R.-D. (3 October 2013). "Global survey of star clusters in the Milky Way". Astronomy & Astrophysics. 558: A53. arXiv: 1308.5822 . Bibcode:2013A&A...558A..53K. doi:10.1051/0004-6361/201322302. S2CID   118548517.
  3. 1 2 Piskunov, A. E.; Schilbach, E.; Kharchenko, N. V.; Röser, S.; Scholz, R.-D. (6 November 2007). "Tidal radii and masses of open clusters". Astronomy & Astrophysics. 477 (1): 165–172. Bibcode:2008A&A...477..165P. doi: 10.1051/0004-6361:20078525 .
  4. ↑ Ahumada, J. A.; Lapasset, E. (20 November 2006). "New catalogue of blue stragglers in open clusters". Astronomy & Astrophysics. 463 (2): 789–797. Bibcode:2007A&A...463..789A. doi: 10.1051/0004-6361:20054590 .
  5. ↑ Anderson, Richard I.; Eyer, Laurent; Mowlavi, Nami (July 2013). "Cepheids in open clusters: an 8D all-sky census". Monthly Notices of the Royal Astronomical Society. 434 (3): 2238–2261. arXiv: 1212.5119 . Bibcode:2013MNRAS.434.2238A. doi: 10.1093/mnras/stt1160 .
  6. ↑ Chen, X.; de Grijs, R.; Deng, L. (19 November 2014). "A search for open cluster Cepheids in the Galactic plane". Monthly Notices of the Royal Astronomical Society. 446 (2): 1268–1282. arXiv: 1410.4489 . Bibcode:2015MNRAS.446.1268C. doi: 10.1093/mnras/stu2165 .
  7. ↑ Santos, N. C.; Lovis, C.; Melendez, J.; Montalto, M.; Naef, D.; Pace, G. (17 February 2012). "Metallicities for six nearby open clusters from high-resolution spectra of giant stars". Astronomy & Astrophysics. 538: A151. arXiv: 1201.1108 . Bibcode:2012A&A...538A.151S. doi:10.1051/0004-6361/201118276. S2CID   119297455.
  8. ↑ Lovis, C.; Mayor, M. (26 June 2007). "Planets around evolved intermediate-mass stars". Astronomy & Astrophysics. 472 (2): 657–664. arXiv: 0706.2174 . Bibcode:2007A&A...472..657L. doi:10.1051/0004-6361:20077375. S2CID   15173677.
  9. ↑ Delgado Mena, E.; Lovis, C.; et al. (November 2018). "Planets around evolved intermediate-mass stars. II. Are there really planets around IC 4651 No. 9122, NGC 2423 No. 3, and NGC 4349 No. 127?". Astronomy & Astrophysics . 619: A2. arXiv: 1807.09608 . Bibcode:2018A&A...619A...2D. doi:10.1051/0004-6361/201833152. S2CID   119483881.
  10. ↑ Delgado Mena, E.; Gomes da Silva, J.; et al. (November 2023). "Planets around evolved intermediate-mass stars. III. Planet candidates and long-term activity signals in six open clusters". Astronomy & Astrophysics . 679: A94. arXiv: 2309.13589 . Bibcode:2023A&A...679A..94D. doi:10.1051/0004-6361/202346890.
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