NGC 3741: the dark halo profile from the most extended rotation curve

By G. Gentile, P. Salucci, U. Klein, G. Granato. 2006

182 citations recorded by the source corpus.

We present new H i observations of the nearby dwarf galaxy NGC 3741. This galaxy has an extremely extended H i disc, which allows us to trace the rotation curve out to unprecedented distances in terms of the optical disc: we reach 42 B-band exponential scalelengths or about 7 kpc. The H i disc is strongly warped, but the warp is very symmetric. The distribution and kinematics are accurately derived by building model data cubes, which closely reproduce the observations. In order to account for the observed features in the data cube, radial motions of the order of 5–13 km s−1 are needed. They are consistent with an inner bar of several hundreds of pc and accretion of material in the outer regions. The observed rotation curve was decomposed into its stellar, gaseous and dark components. The Burkert dark halo (with a central constant density core) provides very good fits. The dark halo density distribution predicted by the Λ cold dark matter (CDM) theory fails to fit the data, unless NGC 3741 is a 2.5σ exception to the predicted relation between concentration parameter and virial mass and at the same time a high value of the virial mass (though poorly constrained) of 1011 M⊙. Noticeably, modified Newtonian dynamics (MOND) seems to be consistent with the observed rotation curve. Scaling up the contribution of the gaseous disc also gives a good fit.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d2a39f6bd18f3fcd00b925ead464da7dfc6490ce

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A wide-field H I mosaic of Messier 31 - II. The disk warp, rotation, and the dark matter halo (2009, methodology): “We consider also the Burkert dark matter density profile (Burkert 1995) since this successfully fitted the rotation curve of dark matter dominated dwarf galaxies (e.g. Gentile et al. 2007, and references therein).”
The Core-Cusp Problem (2009, methodology): “Gentile et al. (2007b) take a different approach and identify halos that have the same enclosed mass as observed galaxies.”
A constant dark matter halo surface density in galaxies (2009, background): “In addition, this galaxy has an extremely extended HI disk, which allowed Gentile et al. (2007b) to carefully trace the RC and therefore its gravitational potential out to unprecedented distances, relative to the extent of the optical disk.”
Cosmological simulations with self-interacting dark matter – II. Halo shapes versus observations (2012, background): “In fact, there are hints of tension with the neutralino paradigm on subgalactic scales (Dobler & Keeton 2006; Gentile et al. 2007; de Blok et al. 2008; Kuzio de Naray, McGaugh & de Blok 2008; Kuzio de Naray et al. 2010; Zwaan, Meyer & Staveley-Smith 2010; BoylanKolchin, Bullock & Kaplinghat 2011;…”
BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, background): “…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 al. 2008; Donato et al. 2009; Oh et al. 2011; Del Popolo 2012), and…”
The masses and density profiles of halos in a LCDM galaxy formation simulation (2014, result): “…galaxies is still a matter of lively debate, with some authors reporting cores (e.g. Salucci & Burkert 2000; Swaters et al. 2003; Simon et al. 2005; Gentile et al. 2007; de Blok et al. 2008; Kuzio de Naray, McGaugh & de Blok 2008; Oh et al. 2011), others reporting cusps (even for some of the same…”
THE BARYONIC TULLY–FISHER RELATION OF GAS-RICH GALAXIES AS A TEST OF ΛCDM AND MOND (2011, background): “It is not uncommon for the optical portions of gas rich galaxies to be much smaller than their dominant HI disks (e.g., Meurer et al. 1996; Gentile et al. 2007) and for the outer HI isophotes to have a different shape than the optical isophotes (Oh et al. 2008; Trachternach et al. 2009).”
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).”
HALO EXPANSION IN COSMOLOGICAL HYDRO SIMULATIONS: TOWARD A BARYONIC SOLUTION OF THE CUSP/CORE PROBLEM IN MASSIVE SPIRALS (2011, background): “(1) This profile, when combined with appropriate baryonic gaseou and stellar components, is found to reproduce very well the oserved kinematics of disc systems (e.g. Salucci & Burkert 2000; Gentile et al. 2007).”
Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, background): “2) and to the stellar mass-to-light ratio [168, 324].”