NGC 7142

NGC 7142
Observation data
Constellation Cepheus
Right ascension 21h 45m 9s[1]
Declination +65° 46′ 30″[1]
Distance ~6,200 (~1,900)
Apparent magnitude (V) 9.3[1]
Apparent dimensions (V) (Unknown)
Physical characteristics
Mass (Unknown) M☉
Radius (Unknown)
Estimated age Between 3 x 109 yr and 6 x 109 yr
Other designations C 2144+655 and
Cl Collinder 442

NGC 7142 is an open cluster about 6,200 light-years away in the constellation Cepheus.

Observational Difficulties

NGC 7142 is located near the reflection nebula NGC 7129, which is a first indication that the cluster may be obscured by an interstellar cloud. Many studies have demonstrated this to be true dating back to the earliest investigations of this cluster. A thorough study of the Cepheus region concluded "that no part of the field may be considered unobscured." [2]

Other astronomers have noted that the reddening across the face of this cluster is likely to be uneven.[3][4][5] The visibility of several background galaxies in the NW corner of the cluster indicate that the obscuring medium may be lowest here.[6]

Estimates of the amount of reddening range from 0.18 magnitudes,[7] to as high as 0.41 magnitudes.[4]

Age

Due to the uncertain amount of interstellar reddening, precise determination of age for this cluster has been especially difficult. Based on NGC 7142's Color-magnitude diagram, it is believed that this cluster is close in age to the old open clusters M 67 and NGC 188 (although age determinations for these two clusters varies wildly in the literature). This makes it one of the oldest open clusters currently known.

Distance

The distance to this cluster has also been difficult to determine, again, owing to the absorption. Estimates for the Distance modulus range from 12.5[4] to 14.5.[6]

Variable Stars

Due to the similarities between NGC 7142 and NGC 188 in both age and density, some astronomers have speculated that NGC 7142 should be home to a high number of a rare type of variable star known as W UMa since NGC 188 has a high number. Crinklaw & Talbert conducted a search for such stars in 1991, but their study only revealed one variable star. However, their investigation only spanned two days, which did not afford enough data points to determine the type of variable. Roughly two more nights of data were appended to the beginning of the Crinklaw & Talbert study but have still not given enough information to classify the variable star.[8]

Other Oddities

Although thought to be an old cluster, NGC 7142 contains a surprisingly high number of blue stars.[3] This runs contrary to the standard model of cluster evolution which predicts that old clusters should be devoid of such stars since bluer stars are more massive and thus evolve and die off faster, which should prevent them from still being present. Such stars are said to be blue stragglers.

Ongoing research

Due to the observational difficulties NGC 7142 presents, it has been an infrequent topic of research. Current known studies include only work being done at the University of Kansas.

See also

References

  1. 1 2 3 "SIMBAD Astronomical Database". Results for NGC 7142. Retrieved 2007-05-02.
  2. ↑ Risley, Marguerite (May 1943). "The Milky way in Cepheus". The Astrophysical Journal. 97: 277. Bibcode:1943ApJ....97..277R. doi:10.1086/144523.
  3. 1 2 Sharov, A. S. (May 1965). "The Apparent Structure of Galactic Cluster NGC 7142". Soviet Astronomy. Soviet Astronomy. 8: 780. Bibcode:1965SvA.....8..780S.
  4. 1 2 3 S. van den Bergh, & R. Heeringa; Heeringa, R. (1970-07-28). "The Old Open Cluster NGC 7142". Astronomy & Astrophysics. 9: 209. Bibcode:1970A&A.....9..209V.
  5. ↑ Crinklaw, G, & Talbert, F. D.; Talbert, F. D. (1991-03-18). "CCD Photometry of the Old Open Cluster NGC 7142". Publications of the Astronomical Society of the Pacific. Pulblications of the Astronomical Society of the Pacific. 103: 536. Bibcode:1991PASP..103..536C. doi:10.1086/132850.
  6. 1 2 Crinklaw, G, & Talbert, F. D.; Talbert, F. D. (1991-03-18). "CCD Photometry of the Old Open Cluster NGC 7142". Publications of the Astronomical Society of the Pacific. Pulblications of the Astronomical Society of the Pacific. 103: 536. Bibcode:1991PASP..103..536C. doi:10.1086/132850.
  7. ↑ Johnson, H. L. (1961). "Galactic clusters as indicators of stellar evolution and galactic structure". Bulletin / Lowell Observatory. Lowell Observatory Bulletain. 5 (113): 133. Bibcode:1961LowOB...5..133J.
  8. ↑ Seeberger, R.; Weinberger, R.; Ziener, R. (1991-09-09). "Some Additional Data on the New Short-Period Variable In NGC 7142". Information Bulletin on Variable Stars. Commission 27 of the I.A.U., Information Bulletin on Variable Stars. 3657 (3657): 1. Bibcode:1991IBVS.3657....1S.

Coordinates: 21h 45m 09s, +65° 46′ 30″

This article is issued from Wikipedia - version of the 5/10/2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.