2021/10/26 by J. Runge, James Runge, S. A. Walker +3
Physics and Astronomy · #Astrophysics #Dark matter #Dark matter halo #Dwarf galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy group #Galaxy rotation curve #Halo #Lambda #Local Group #Luminosity #Physics #Scientific Research and Discoveries #Stellar, planetary, and galactic studies #Surface brightness #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stab3139
published in Monthly Notices of the Royal Astronomical Society 509(2), 2647-2653 (Oxford University Press) · 7 pages, 5 figures. Accepted for publication in MNRAS
arxiv created 2021/10/26 · openalex publication_date 2021/10/28 · arxiv updated 2021/11/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT We investigate the properties of the dark matter (DM) halo surrounding the nearby galaxy group NGC 1600. Through the use of deep (252 ks) Chandra observations and 64.3 ks of XMM–Newton observations, we construct surface brightness profiles in multiple energy bands in order to perform hydrostatic equilibrium analysis of the hot plasma within NGC 1600. Regardless of the DM model profile assumed, we measure a halo concentration (c200) that is an extreme, positive outlier of the ΛCDM c200–M200 relation. For a typical NFW DM profile, we measure c200 = 26.7 ± 1.4 and M200 = (2.0 ± 0.2) × 1013 M⊙; assuming a similar halo mass, the average concentration expected is c200 = 6 − 7 for the theoretical ΛCDM c–M relation. Such a high concentration is similar to that of well-known fossil groups MRK 1216 and NGC 6482. While NGC 1600 exhibits some properties of a fossil group, it fails to meet the X-ray luminosity threshold of LX > 5 × 1041 erg s−1. Whether or not it is considered a fossil group, the high concentration value makes it part of a select group of galaxy groups.