Mass Models for Low Surface Brightness Galaxies with High-Resolution Optical Velocity Fields

By R. K. D. Naray, S. McGaugh, W. D. de Blok. 2007

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We present high-resolution optical velocity fields from DensePak integral field spectroscopy, along with derived rotation curves, for a sample of low surface brightness galaxies. In the limit of no baryons, we fit the NFW and pseudoisothermal halo models to the data and find the rotation curve shapes and halo central densities to be better described by the isothermal halo. For those galaxies with photometry, we present halo fits for three assumptions of the stellar mass-to-light ratio, Υ*. We find that the velocity contribution from the baryons is significant enough in the maximum disk case that maximum disk and the NFW halo are mutually exclusive. We find a substantial cusp mass excess at the centers of the galaxies, with at least 2 times more mass expected in the cuspy CDM halo than is allowed by the data. We also find that to reconcile the data with ΛCDM, ~20 km s−1 noncircular motions are needed and/or the power spectrum has a lower amplitude on the scales that we probe.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/23c83c5236c0086d284dd665b9e9e8fe44f4db3c

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Too big to fail? The puzzling darkness of massive Milky Way subhaloes (2011, background): “…is unlikely to have an influence, as 3 Lower concentrations of dark matter are also favored by many observations of low-mass field galaxies (e.g., Kuzio de Naray et al. 2008), although these tend to be gas-rich, disk-dominated systems with higher luminosities than the bright MW dwarf spheroidals.”
Concentration, spin and shape of dark matter haloes as a function of the cosmological model: WMAP1, WMAP3 and WMAP5 results (2008, background): “…between the inner density slopes of dwarf and LSB galaxies and those predicted by CDM (e.g., Moore 1994; Flores & Primack 1994; van den Bosch & Swaters 2001; de Blok et al. 2001, 2002; Swaters et al. 2003, Dutton et al. 2005; Gentile et al. 2005; Simon et al. 2005; Kuzio de Naray et al. 2008).”
A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “Furthermore, there is considerable observational evidence for the existence of dark matter cores in the centers of low surface brightness galaxies (Kuzio de Naray et al. 2008; de Blok 2010; Oh et al. 2011) and in at least two MW dwarf spheroidal satellites (Walker & Peñarrubia 2011).”
On the frequency, intensity, and duration of starburst episodes triggered by galaxy interactions and mergers (2008, background): “This has been shown to be valid either for dwarf galaxies (Flores & Primack 1994; Marchesini et al. 2002; Gentile et al. 2005), or for Low Surface Brightness (LSB) galaxies (de Blok et al. 2001; McGaugh et al. 2001; Marchesini et al. 2002; Kuzio de Naray et al. 2006, 2008).”
Constraining self-interacting dark matter with the Milky Way’s dwarf spheroidals (2012, background): “It is now clear that observations of dark matter dominated systems such as low-mass (dwarf) and low surface brightness (LSB) galaxies favour the presence of dark matter cores ofO(1 kpc) (e.g. Moore 1994, Kuzio de Naray et al. 2008, de Blok 2010, Walker & Peñarrubia 2011, Amorisco & Evans 2012).”
Can feedback solve the too-big-to-fail problem? (2013, background): “…and low surface brightness (LSB) galaxies appear to favor corelike density distributions rather than the cuspy distributions seen in dissipationless simulations (Flores & Primack 1994; Moore 1994; Kuzio de Naray et al. 2008; Trachternach et al. 2008; de Blok 2010; Kuzio de Naray & Kaufmann 2011).”
The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores (2013, background): “We note that, in agreement with our findings, the most clear observational measurements of flattened “core” profiles of disc galaxies (de Blok et al. 2008; Kuzio de Naray et al. 2008, 2009; Oh et al. 2011) are found in low surface brightness (LSB) galaxies withVrot < 100 kms−1.”
HIGH-RESOLUTION MASS MODELS OF DWARF GALAXIES FROM LITTLE THINGS (2015, background): “L. Verdes-Montenegro, A. Del Olmo, & J. Sulentic, 137 Kregel, M., van der Kruit, P. C., & de Grijs, R. 2002, MNRAS, 334, 646 Kuzio de Naray, R., McGaugh, S. S., & de Blok, W. J. G. 2008, ApJ, 676, 920 Kuzio de Naray, R., McGaugh, S. S., de Blok, W. J. G., & Bosma, A. 2006, ApJS, 165, 461 Larson, R. ”
Numerical simulations of the dark universe: State of the art and the next decade (2012, background): “Two-dimensional stellar and gaseous kinematic measurements in low surface brightness field galaxies [64, 273–275], as well as chemo-”
Small scale problems of the $\Lambda$CDM model: a short review (2016, result): “ Ha observations a slit misplacement may lead to missing the dynamic centre of the galaxy, with the result of having ﬂatter proﬁles. The problem can be solved in different ways (e.g., 3d spectroscopy [180,188]). The gas is usually assumed to move on circular orbits, so non-circular motions produce a”
The Core-Cusp Problem (2009, methodology): “[88, 89] present DensePak velocity fields of LSB galaxies, many of them taken from the de Blok and McGaugh [62] sample.”