LOGIN TO YOUR ACCOUNT

Username
Password
Remember Me
Or use your Academic/Social account:

CREATE AN ACCOUNT

Or use your Academic/Social account:

Congratulations!

You have just completed your registration at OpenAire.

Before you can login to the site, you will need to activate your account. An e-mail will be sent to you with the proper instructions.

Important!

Please note that this site is currently undergoing Beta testing.
Any new content you create is not guaranteed to be present to the final version of the site upon release.

Thank you for your patience,
OpenAire Dev Team.

Close This Message

CREATE AN ACCOUNT

Name:
Username:
Password:
Verify Password:
E-mail:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:
fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Longmore, A.J.; Kurtev, R.; Lucas, P.W.; Froebrich, D.; de Grijs, R.; Ivanov, V.D.; Maccarone, T.J.; Borissova, J.; Ker, L.M. (2011)
Languages: English
Types: Article
Subjects: QB460

Classified by OpenAIRE into

arxiv: Astrophysics::Galaxy Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
We present a detailed study of a dust-obscured Galactic star cluster Mercer 5 ([MCM2005b] 5) in an extremely crowded field in the Milky Way. Near-infrared (near-IR) photometry from United Kingdom Infrared Digital Sky Surveys (UKIDSS) and the Son of ISAAC on the New Technology Telescope (SofI/NTT), combined with near-IR spectroscopy also from SofI, indicates that it is almost certainly a Galactic globular cluster, located at the edge of the Galactic bulge. The cluster suffers ~9 mag of visual extinction, with strong evidence for an extinction gradient across the cluster. A simulation of the differential reddening in the cluster using empirical data from NGC 6539 (chosen because it had high signal-to-noise ratio data and low field star contamination) as a template mimics the observations extremely well. This simulation and other arguments are used to indicate that the most prominent clump of stars in the colour-magnitude diagrams is a horizontal branch clump. On this basis we conclude that the cluster is at a distance of ~5.5kpc and suffers from visual extinction ranging from ~8.5 to ~12.5 mag. Alternative explanations for its nature, such as a young cluster or an old open cluster, are much less likely, on the grounds of no visible main sequence or stars with IR excesses for the former and location versus lifetime arguments for the latter. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • The K-band spectra of five likely cluster giants are consistent with those of RGB stars, although they tend to indicate lower metallicity than implied by the existence of a dominant red HB clump. Aguirre J. E. et al., 2011, ApJS, 192, 4 Barbuy B., Bica E., Ortolani S., 1998, A&A, 333, 117 Bastian N., Konstantopoulos I., Smith L. J., Trancho G., Westmoquette M.
    • Cambridge Univ. Press, Cambridge, p. 97 Ostriker J. P., Spitzer L., Chevalier R. A., 1972, ApJ, 176, L51 Pfleiderer J., Weinberger R., Mross R., 1977, Star Cluster Symp. Vol. 5.
    • Eotvos University, Budapest, p. 39 Robin A. C., Reyle´ C., Derrie`re S., Picaud S., 2003, A&A, 409, 523 Rieke G. H., Lebofsky M., 1985, ApJ, 288, 618 Spitzer L., 1958, ApJ, 127, 17 Stead J. J., Hoare M. G., 2009, MNRAS, 400, 731 Stephens A. W., Frogel J. A., 2004, AJ, 127, 925 Stetson P., Davis L. E., Crabtree D. R., 1990, in Jocoby G. H., ed., ASP Conf. Ser. Vol. 8, CCDs in Astronomy. Astron. Soc. Pac., San Francisco, p. 289 Stetson P., 1996, User's Manual for DAOPHOT II. Dominion Astrophysical Observatory, Victoria Strader J., Kobulnicky H. A., 2008, AJ, 136, 2102 Valenti E., Ferraro F. R., Origlia L., 2004, MNRAS, 354, 815 Valenti E., Origlia L., Ferraro F. R., 2005, MNRAS, 361, 272 Valenti E., Ferraro F. R., Origlia L., 2007, AJ, 133, 287 Valenti E., Ferraro F. R., Origlia L., 2010, MNRAS, 402, 1729 Watson M. G. et al., 2009, A&A, 493, 339
  • No related research data.
  • No similar publications.

Share - Bookmark

Download from

Cite this article