A feature of stellar density distribution within the tidal radius of globular cluster NGC 6626 (m28) in the galactic bulge

Sang Hyun Chun, Jae Woo Kim, Myo Jin Kim, Ho Il Kim, Jang Hyun Park, Young-Jong Sohn

Research output: Contribution to journalArticle

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Abstract

Using wide-field J, H, and K s images obtained with the WIRCam near-infrared camera on the Canada-France-Hawaii Telescope, we investigated the spatial density configuration of stars within the tidal radius of metal-poor globular cluster NGC 6626, which is known to be located near the bulge region and have a thick-disk orbit motion. In order to trace the stellar density around a target cluster, we sorted the cluster's member stars using a mask-filtering algorithm and weighted the stars on the color-magnitude diagram. From the weight-summed surface density map, we found that the spatial density distribution of stars within the tidal radius is asymmetric with distorted overdensity features. The extending overdensity features are likely associated with the effects of the dynamic interaction with the Galaxy and the cluster's space motion. An interesting finding is that the prominent overdensity features extend toward the direction of the Galactic plane. This orientation of stellar density distribution can be interpreted with the result of the disk-shock effect of the Galaxy, previously experienced by the cluster. Indeed, the radial surface density profile accurately describes this overdensity feature with a break in the slope inside the tidal radius. Thus, the observed results indicate that NGC 6626 experienced a strong dynamical interaction with the Galaxy. Based on the result of strong tidal interaction with the Galaxy and previously published results, we discussed possible origins and evolutions of the cluster: (1) the cluster might have formed in satellite galaxies that were merged and created the Galactic bulge region in the early universe, after which time its dynamical properties were modified by dynamical friction, or (2) the cluster might have formed in primordial and rotationally supported massive clumps in the thick disk of the Galaxy.

Original languageEnglish
Article number26
JournalAstronomical Journal
Volume144
Issue number1
DOIs
Publication statusPublished - 2012 Jul 1

Fingerprint

galactic bulge
globular clusters
density distribution
radii
galaxies
stars
color-magnitude diagram
interactions
clumps
distribution
France
Canada
near infrared
friction
diagram
masks
universe
shock
cameras
telescopes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Chun, Sang Hyun ; Kim, Jae Woo ; Kim, Myo Jin ; Kim, Ho Il ; Park, Jang Hyun ; Sohn, Young-Jong. / A feature of stellar density distribution within the tidal radius of globular cluster NGC 6626 (m28) in the galactic bulge. In: Astronomical Journal. 2012 ; Vol. 144, No. 1.
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abstract = "Using wide-field J, H, and K s images obtained with the WIRCam near-infrared camera on the Canada-France-Hawaii Telescope, we investigated the spatial density configuration of stars within the tidal radius of metal-poor globular cluster NGC 6626, which is known to be located near the bulge region and have a thick-disk orbit motion. In order to trace the stellar density around a target cluster, we sorted the cluster's member stars using a mask-filtering algorithm and weighted the stars on the color-magnitude diagram. From the weight-summed surface density map, we found that the spatial density distribution of stars within the tidal radius is asymmetric with distorted overdensity features. The extending overdensity features are likely associated with the effects of the dynamic interaction with the Galaxy and the cluster's space motion. An interesting finding is that the prominent overdensity features extend toward the direction of the Galactic plane. This orientation of stellar density distribution can be interpreted with the result of the disk-shock effect of the Galaxy, previously experienced by the cluster. Indeed, the radial surface density profile accurately describes this overdensity feature with a break in the slope inside the tidal radius. Thus, the observed results indicate that NGC 6626 experienced a strong dynamical interaction with the Galaxy. Based on the result of strong tidal interaction with the Galaxy and previously published results, we discussed possible origins and evolutions of the cluster: (1) the cluster might have formed in satellite galaxies that were merged and created the Galactic bulge region in the early universe, after which time its dynamical properties were modified by dynamical friction, or (2) the cluster might have formed in primordial and rotationally supported massive clumps in the thick disk of the Galaxy.",
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A feature of stellar density distribution within the tidal radius of globular cluster NGC 6626 (m28) in the galactic bulge. / Chun, Sang Hyun; Kim, Jae Woo; Kim, Myo Jin; Kim, Ho Il; Park, Jang Hyun; Sohn, Young-Jong.

In: Astronomical Journal, Vol. 144, No. 1, 26, 01.07.2012.

Research output: Contribution to journalArticle

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