Spectra of Two Luminous Young Globular Clusters in the Merger Remnant NGC 7252

Details Spectra of Two Luminous Young Globular Clusters in the Merger Remnant NGC 7252 Spectra of Two Luminous Young Globular Clusters in the Merger Remnant NGC 7252

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...417l..29s&link_type=abstract

Astrophysical Journal Letters v.417, p.L29

Astronomy and Astrophysics

Astronomy

69

Galaxies: Formation, Galaxies: Individual Ngc Number: Ngc 7252, Galaxies: Interactions, Galaxies: Star Clusters

Scientific paper

Spectra of the two brightest "bluish knots" surrounding the nucleus of the merger remnant NGC 7252 are presented. These knots were among a half dozen discovered from the ground and belong to a population of 40 similar blue objects found and resolved by Whitmore et al. with the Hubble Space Telescope. The spectra, obtained with the Hale 5 m telescope, show Hα, Hβ, Mg I, and Fe I absorption lines characteristic of late A-type to mid-F-type stars at the redshift of NGC 7252 (within +/- 150 km s^-1^), but no emission lines. These spectra demonstrate that the two knots are relatively young (~10-500 Myr), populous star clusters of exceptional luminosity (M_V_ = - 17.1 and - 15.6 for H_0_ = 50). Because of their age and small effective radii (~10 pc), these clusters must be gravitationally bound and are most likely young globular clusters. They formed during the merger of two gas-rich spirals and will fade by 3 1/2-7 mag during the next 15 Gyr. We discuss the implications of finding young globular clusters in a merger remnant likely to evolve into an elliptical galaxy.

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