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Seeing deconvolution of globular clusters in M31

Bendinelli, O. and Zavatti, F. and Parmeggiani, G. and Djorgovski, S. (1990) Seeing deconvolution of globular clusters in M31. Astronomical Journal, 99 (3). pp. 774-783. ISSN 0004-6256. doi:10.1086/115373.

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Seeing deconvolution of surface-brightness profiles using the regularized multi-Gaussian method is potentially a powerful method for extraction of morphological information from digital images. Here we illustrate this method by applying it to CCD images of six globular clusters in M31. We demonstrate that it is possible to make some judgments about the dynamical structure of M31 globulars, using good-seeing, deconvolved CCD images obtained from the ground; for example, whether they have post-core-collapse morphology or not. The effective resolution limit of the method is about 0.1-0.3 arcsec, for the CCD images obtained in FWHM ≃ 1 arcsec seeing, and sampling of 0.3 arcsec/pixel. We also demonstrate the robustness of the method, i.e., its insensivity to the exact choices of the functional representation of the point-spread function, details of the deconvolution technique, etc. The situation is equivalent in terms of angular resolution and sampling to observing globular clusters in the Virgo Cluster (e.g., around M87) with the Hubble Space Telescope, and the methods demonstrated here may be applied to HST data in the future. Dynamical structure of globular clusters, e.g., propensity for the post-core-collapse morphology as a function of position in the host galaxy, reflects the global dynamical evolution of a globular cluster system, as was already demonstrated for our galaxy. Similar studies of large samples of globulars in M31 and other Local Group galaxies from the ground, and out to Virgo with the HST, can provide valuable insights about the mass distribution in galaxies, and the formation and evolution of their globular cluster systems. This pilot study is a step in this direction.

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Djorgovski, S.0000-0002-0603-3087
Additional Information:© 1990 American Astronomical Society. Provided by the NASA Astrophysics Data System. Received 1 September 1989; revised 17 November 1989. We are indebted to many colleagues for stimulating and informative discussions. We also thank Dr. Hyron Spinrad and the staff of Kitt Peak National Observatory for their help in obtaining the data used here. S.D. acknowledges the hospitality and the stimulating atmosphere of Dipartimento di Astronomia, Università di Bologna, where this paper was prepared. This work was supported in part by the Ministero della Pubblica Istruzione (O.B., F.Z.), by the Osservatorio Astronomico di Bologna (G. P.), and by the Alfred P. Sloan Foundation and California Institute of Technology (S.D.).
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Ministero della Pubblica IstruzioneUNSPECIFIED
Osservatorio Astronomico di BolognaUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
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ID Code:98008
Deposited By: Tony Diaz
Deposited On:19 Aug 2019 22:30
Last Modified:16 Nov 2021 17:35

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