HIGH-RESOLUTION ROTATION CURVES AND GALAXY MASS MODELS FROM THINGS

By W. D. de Blok, F. Walter, E. Brinks, C. Trachternach, S. Oh, R. C. K. J. U. O. C. T. MPIfA, Heidelberg University of Hertfordshire Ruhr-University Bochum Rsaa, M. Cambridge. 2008

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We present rotation curves of 19 galaxies from The H i Nearby Galaxy Survey (THINGS). The high spatial and velocity resolution of THINGS make these the highest quality H i rotation curves available to date for a large sample of nearby galaxies, spanning a wide range of H i masses and luminosities. The high quality of the data allows us to derive the geometric and dynamical parameters using H i data alone. We do not find any declining rotation curves unambiguously associated with a cut-off in the mass distribution out to the last measured point. The rotation curves are combined with 3.6 μm data from the Spitzer Infrared Nearby Galaxies Survey to construct mass models. Our best-fit dynamical disk masses, derived from the rotation curves, are in good agreement with photometric disk masses derived from the 3.6 μm images in combination with stellar population synthesis arguments and two different assumptions for the stellar initial mass function (IMF). We test the cold dark matter (CDM) motivated cusp model, and the observationally motivated central density core model and find that (independent of IMF) for massive, disk-dominated galaxies, all halo models fit apparently equally well; for low-mass galaxies, however, a core-dominated halo is clearly preferred over a cusp-like halo. The empirically derived densities of the dark matter halos of the late-type galaxies in our sample are half of what is predicted by CDM simulations, again independent of the assumed IMF.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

BARYONS MATTER: WHY LUMINOUS SATELLITE GALAXIES HAVE REDUCED CENTRAL MASSES (2012, background): “…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 observed in satellites (Kleyna et al. 2002, 2003; Mashchenko et al.…”
MOLECULAR GAS AND STAR FORMATION IN NEARBY DISK GALAXIES (2013, methodology): “We derive these from fits to the rotation curves of de Blok et al. (2008) wherever they are available.”
Forged in FIRE: cusps, cores and baryons in low-mass dwarf galaxies (2015, background): “…cored density profiles rather than the cuspy NFW-like profiles predicted in CDM simulations (Flores & Primack 1994; Kuzio de Naray et al. 2008; de Blok et al. 2008; Oh et al. 2008; Walker & Peñarrubia 2011; Salucci et al. 2012; Amorisco et al. 2014; Ogiya & Burkert 2015, but see Strigari et al.…”
The masses and density profiles of halos in a LCDM galaxy formation simulation (2014, neutral): “…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 galaxies; e.g. Adams et…”
The DiskMass Survey VII. The distribution of luminous and dark matter in spiral galaxies (2013, methodology): “When fitting a NFW-halo model, the median value of the concentration parameter in the 13 galaxies from de Blok et al. (2008) is similar to what we find (C = 9 and C = 11, respectively), but with a much larger scatter.”
Is there a "too big to fail" problem in the field? (2014, methodology): “For example, most of the spiral galaxies in the THINGS sample analyzed by de Blok et al. (2008) have RCs of exquisite reso- lution, and mass models constrained by multiwavelength data.”
Dwarf galaxies in CDM and SIDM with baryons: observational probes of the nature of dark matter (2014, background): “…that is inferred from low surface brightness galaxies (e.g. Kuzio de Naray, McGaugh & de Blok 2008), nearby field dwarf galaxies (e.g. de Blok et al. 2008; Oh et al. 2008) and Milky Way (MW) dwarf spheroidals (dSphs; e.g. Walker & Peñarrubia 2011; Amorisco, Zavala & de Boer 2014) seems…”
Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions (2011, background): “Figure 26: MOND rotation curve fits for representative galaxies from the THINGS survey [121, 166, 481].”
Non-linear evolution of cosmological structures in warm dark matter models (2011, background): “…2004; Springel et al. 2008; Stadel et al. 2009), whereas the density profiles inferred from galaxy rotation curves are significantly shallower (Moore et al. 1999) (and for recent studies see Swaters et al. 2003; Salucci et al. 2007; de Blok et al. 2008; Gentile et al. 2009 and references therein).”
The Core-Cusp Problem (2009, background): “Due to the cusp mass excess their average density is then also a factor of 2–3 too high (see also de Blok et al. 2008).”
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;…”
Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties (2012, result): “We have also avoided a strong cusp in the centre, in good agreement with observations (e.g. de Blok et al. 2001, 2008; de Blok & Bosma 2002; de Blok, Bosma & McGaugh 2003; Simon et al. 2003; Kuzio de Naray et al. 2006; Battaglia et al. 2008; Kuzio de Naray, McGaugh & de Blok 2008; Oh et al. 2008;…”
Galaxy Masses: A Review (2013, methodology): “Detailed mass models of spiral galaxies, including the equations for the density profiles and associated rotation curves for the bulge, disk and halo profiles can be found in, e.g., Dutton et al. (2005), de Blok et al. (2008), Tamm et al. (2012) and Section 11.1 of Mo et al. (2010).”
HERACLES: THE HERA CO LINE EXTRAGALACTIC SURVEY (2009, methodology): “The stellar masses are taken from Leroy et al. (2008), who estimate them from SINGS 3.6µm imaging assuming a Kroupa IMF (NGC 2903 comes from de Blok et al. 2008). de Blok et al. (2008) investigate possible variations in the 3.6µm mass-to-light ratio and find a factor of 2 plausible.”