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Galaxies 2017, 5(3), 29; doi:10.3390/galaxies5030029

The Extended Baryonic Halo of NGC 3923

1
Gemini Observatory, Casilla 603, La Serena 1700000, Chile
2
Institute of Astrophysics, Pontificia Universidad Católica de Chile, Santiago 7820436, Chile
3
Physics and Astronomy Institute, Universidad de Valparaíso, Valparaíso 2360102, Chile
4
Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA
5
Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA
6
Optical Astronomy Division, Korea Astronomy and Space Science Institute, Daedeokdae-ro 776, Yuseong-gu, Daejeon 34055, Korea
7
Gemini Observatory, Hilo, HI 96720, USA
*
Author to whom correspondence should be addressed.
Academic Editors: Emilio Elizalde, Duncan A. Forbes and Ericson D. Lopez
Received: 1 July 2017 / Revised: 12 July 2017 / Accepted: 14 July 2017 / Published: 20 July 2017
(This article belongs to the Special Issue On the Origin (and Evolution) of Baryonic Galaxy Halos)
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Abstract

Galaxy halos and their globular cluster systems build up over time by the accretion of small satellites. We can learn about this process in detail by observing systems with ongoing accretion events and comparing the data with simulations. Elliptical shell galaxies are systems that are thought to be due to ongoing or recent minor mergers. We present preliminary results of an investigation of the baryonic halo—light profile, globular clusters, and shells/streams—of the shell galaxy NGC 3923 from deep Dark Energy Camera (DECam) g and i-band imaging. We present the 2D and radial distributions of the globular cluster candidates out to a projected radius of about 185 kpc, or 37 R e , making this one of the most extended cluster systems studied. The total number of clusters implies a halo mass of M h 3 × 10 13 M . Previous studies had identified between 22 and 42 shells, making NGC 3923 the system with the largest number of shells. We identify 23 strong shells and 11 that are uncertain. Future work will measure the halo mass and mass profile from the radial distributions of the shell, N-body models, and line-of-sight velocity distribution (LOSVD) measurements of the shells using the Multi Unit Spectroscopic Explorer (MUSE). View Full-Text
Keywords: galaxies: elliptical and lenticular, cD; galaxies: halos; galaxies: individual (NGC 3923); galaxies: structure; galaxies: star clusters: general galaxies: elliptical and lenticular, cD; galaxies: halos; galaxies: individual (NGC 3923); galaxies: structure; galaxies: star clusters: general
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Figure 1

This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. (CC BY 4.0).

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MDPI and ACS Style

Miller, B.W.; Ahumada, T.; Puzia, T.H.; Candlish, G.N.; McGaugh, S.S.; Mihos, J.C.; Sanderson, R.E.; Schirmer, M.; Smith, R.; Taylor, M.A. The Extended Baryonic Halo of NGC 3923. Galaxies 2017, 5, 29.

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