A high-resolution rotation curve of NGC 6822

By D. Weldrake, E. D. Blok, Fabian Walter Mssso, Canberra, A. C. University, UK Nrao, Socorro, Usa. 2002

143 citations recorded by the source corpus.

We present high-resolution rotation curves of the Local Group dwarf irregular galaxy NGC 6822 obtained with the Australia Telescope Compact Array. Our best curves have an angular resolution of 8 arcsec or 20 pc and contain some 250 independent points. The stellar and gas components of NGC 6822 cannot explain the shape of the curve, except for the very inner regions, and NGC 6822 is consequently very dark-matter-dominated. There is no evidence for the presence of a steep density cusp down to scales of ∼20 pc, contrary to the predictions of cold dark matter.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7ed2783130b8a99b211a3eee82a56f81d9b30208

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In Astronomy and Astrophysics

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Citations in the corpus

• The universal rotation curve of spiral galaxies II: the dark matter distribution out to the virial radius (2007, background): “(3a): DM halos detected around spirals do not show the NFW central cusp in favor of a core-like structure (Gentile et 2005; van den Bosch & Swaters 2001; Swaters et al. 2003; Weldrake et al. 2003; Simon et al. 2005; Donato et al, 2004; Gentile et al. 2007).”
• The stellar mass-halo mass relation of isolated field dwarfs : a critical test of ΛCDM at the edge of galaxy formation (2016, methodology): “We compile HI data for 19 isolated dwarf irregular galaxies over the mass range 5×105 <∼M∗/M <∼ 108 from Weldrake et al. (2003) and Oh et al. (2015); and stellar mass and surface density data from Zhang et al. (2012).”
• HIGH-RESOLUTION DARK MATTER DENSITY PROFILES OF THINGS DWARF GALAXIES: CORRECTING FOR NONCIRCULAR MOTIONS (2008, methodology): “…of standard ΛCDM simulations to produce dark matter density profiles that match the observed profiles is now well known (Flores & Primack 1994; Moore 1994; de Blok et al. 2001; de Blok & Bosma 2002; Weldrake et al. 2003; Simon et al. 2003; Gentile et al. 2004; see also Swaters et al. 2003).”
• Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM (2016, background): “…along a central bar), and a gas sound speed of cs ∼ 60 km/s. NGC 6822, that has a comparable peak rotation velocity, has a measured dispersion of just σgas ∼ 6 km/s that is ∼ constant across the disc (Weldrake et al. 2003; and see §2.1.1 for a discussion of how σgas relates to σturb and cs).”
• The Core-Cusp Problem (2009, background): “Weldrake et al. (2003) present the HI velocity field of NGC 6822, a nearby Local Group dwarf galaxy.”
• BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, background): “…field galaxies (Persic et al. 1996; van den Bosch et al. 2000; de Blok et al. 2001; de Blok & Bosma 2002; Simon et al. 2003; Swaters et al. 2003; Weldrake et al. 2003; Kuzio de Naray et al. 2006; Salucci et al. 2007; Gentile et al. 2007; Spano et al. 2008; Trachternach et al. 2008; de Blok et…”
• HIGH-RESOLUTION ROTATION CURVES AND GALAXY MASS MODELS FROM THINGS (2008, background): “This core has a typical size of order a kpc (e.g., Moore 1994; de Blok et al. 1996; de Blok & McGaugh 1997; de Blok et al. 2001; de Blok & Bosma 2002; Marchesini et al. 2002; Weldrake et al. 2003; Gentile et al. 2005; Kuzio de Naray et al. 2006; Gentile et al. 2007).”
• DARK AND LUMINOUS MATTER IN THINGS DWARF GALAXIES (2010, background): “…density distribution at the centers of galaxies (Flores & Primack 1994; Moore 1994; de Blok et al. 2001; de Blok & Bosma 2002; Bolatto et al. 2002; Weldrake et al. 2003; Simon et al. 2003; Swaters et al. 2003; Gentile et al. 2004; Oh et al. 2008; Trachternach et al. 2008; de Blok et al. 2008, and…”
• The Dwarf Galaxy DDO 47 as a Dark Matter Laboratory: Testing Cusps Hiding in Triaxial Halos (2005, background): “…a large number of cases the inferred cores of dark matter halos are much shallower than expected from the NFW-fit (Flores & Primack 1994, Moore 1994, Burkert 1995, Salucci & Burkert 2000, de Blok, McGaugh & Rubin 2001, Salucci 2001, de Blok & Bosma 2002, Weldrake et al. 2003, Gentile et al. 2004).”
• NGC 3741: the dark halo profile from the most extended rotation curve (2006, background): “…from the observations; the velocity dispersion as a function of radius, which we kept at a fixed value of 6 km s−1, typical of dwarf irregulars (Weldrake et al. 2003); the surface density as a function of radius, which is derived from the total H I map; the scaleheight of the H I disc, which…”