Object 17: Another cluster of emission-line stars near the galactic center

Tetsuya Nagata, Charles E. Woodward, Mark Shure, Naoto Kobayashi

Research output: Contribution to journalArticlepeer-review

106 Scopus citations

Abstract

Infrared imaging and spectroscopic studies suggest that regions of recent massive star formation exist in the central region of the Galaxy. Here, we present J(1.29 μm), H(1.67 μm), K(2.23 μm), and L′(3.82 μm) broadband images, as well as Brγ and Brα hydrogen recombination line images of the Object #17 detected in a near-infrared survey at a projected distance of 30 pc from the Galactic center. Our data show that this source is a cluster of luminous stars with emission lines. The line flux and width of these stars are similar to those of Of-type stars, Wolf-Rayet stars, and He I emission-line stars recently discovered in the central parsec of the Galaxy. However, although the He II line at 3.09 μm has been detected in Object #17, the He I line at 2.06 μm seems weak. The weakness contrasts with stars in the central parsec of the Galaxy. The broadband colors are consistent with the idea that the #17 cluster is near the Galactic center, and this consistency is further evidence for the recent occurrence of massive star formation near the Galactic center. It is possible that this cluster is responsible for the ionization of the thermal arched filaments observed in the radio.

Original languageEnglish (US)
Pages (from-to)1676-1681
Number of pages6
JournalAstronomical Journal
Volume109
Issue number4
DOIs
StatePublished - Apr 1995

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