We present rotation curves of 19 galaxies from THINGS, The H I Nearby Galaxy Survey. 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 geometrical 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 SINGS (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-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 cuspy 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. Stellar mass-to-light ratio trendsAn overview of the derived Υ 3.6 ⋆ values of the main disk components of our sample galaxies is given in Fig. 59. Here we plot the photometric (fixed) and dynamical (free) values for Υ 3.6 ⋆ against the colors and luminosities of the galaxies. The left-hand panels show the fixed and free Υ 3.6 ⋆ values of the disks for both the ISO and NFW model plotted against (J − K) color. We also distinghuish between our two choices for the IMF. Also shown is the predicted relation between Υ 3.6 ⋆ and color (Eqs. 4 and 5), again for both the diet-Salpeter and the Kroupa IMFs. By definition, the photometric Υ 3.6 ⋆ values follow their respective relations. The small scatter is caused by the color gradients present in these galaxies which make the photometric Υ 3.6 ⋆ differ slightly from those with a constant Υ 3.6 ⋆ as a function of radius.In general, we see that the diet-Salpeter curve defines an approximate upper limit to the distribution of the majority of the best fit values (apart from a few obviously discrepant cases). Accepting the best fit (free) Υ 3.6 ⋆ values at face value, this would suggest that a diet-Salpeter Υ 3.6 ⋆ analysis overestimates the disk masses slightly. Indeed, the Kroupa fixed Υ 3.6 ⋆ values seem to be a better match to the free Υ 3.6 ⋆ values. Alternative explanations could be effects of star formation history, or unexpectedly large contamination by PAHs, AGBs or hot dust in the 3.6 µm maps, though it is likely that the IMF plays the dominant role. Future rigorous population synthesis modeling should shed light on s...

We present harmonic decompositions of the velocity fields of 19 galaxies from THINGS (The H I Nearby Galaxy Survey) which quantify the magnitude of the non-circular motions in these galaxies and yield observational estimates of the elongations of the dark matter halo potentials. Additionally, we present accurate dynamical center positions for these galaxies. We show that the positions of the kinematic and photometric centers of the large majority of the galaxies in our sample are in good agreement. The median absolute amplitude of the non-circular motions, averaged over our sample, is 6.7 km s −1 , with ∼ 90 percent of the galaxies having median non-circular motions of less than ∼ 9 km s −1 . As a fraction of the total rotation velocity this translates into 4.5 percent on average. The mean elongation of the gravitational potential, after a statistical correction for an unknown viewing angle, is 0.017 ± 0.020, i.e., consistent with a round potential. Our derived non-circular motions and elongations are smaller than what is needed to bring Cold Dark Matter (CDM) simulations in agreement with the observations. In particular, the amplitudes of the non-circular motions are not high enough to hide the steep central mass-density profiles predicted by CDM simulations. We show that the amplitudes of the non-circular motions decrease towards lower luminosities and later Hubble types.

Context. The baryonic Tully-Fisher relation (BTF) is a fundamental relation between baryonic mass and maximum rotation velocity. It can be used to estimate distances, as well as to constrain the properties of dark matter and its relation with the visible matter. Aims. In this paper, we explore if extremely low-mass dwarf galaxies follow the same BTF relation as high-mass galaxies. We quantify the scatter in the BTF relation and use this to constrain the allowed elongations of dark matter halo potentials. Methods.We obtained H i synthesis data of 11 dwarf galaxies and derive several independent estimates for the maximum rotation velocity. Results. Constructing a BTF relation using data from the literature for the high-mass end, and galaxies with detected rotation from our sample for the low-mass end results in a BTF with a scatter of 0.33 mag. Conclusions. This scatter constrains the ellipticities of the potentials in the plane of the disks of the galaxies to an upper limit of 0−0.06, indicating that dwarf galaxies are at most only mildly tri-axial. Our results indicate that the BTF relation is a fundamental relation which all rotationally dominated galaxies seem to follow.

Aims. In this paper the optical data of the ESO Deep-Public-Survey observed with the Wide Field Imager and reduced with the THELI pipeline are described. Methods. Here we present 63 fully reduced and stacked images. The astrometric and photometric calibrations are discussed and the properties of the images are compared to images released by the ESO Imaging Survey team covering a subset of our data. Results. These images are publicly released to the community. Our main scientific goals with this survey are to study the high-redshift universe by optically pre-selecting high-redshift objects from imaging data and to use VLT instruments for follow-up spectroscopy as well as weak lensing applications.

Context. The cusp-core discrepancy is one of the major problems in astrophysics. It results from comparing the observed mass distribution of galaxies with the predictions of cold dark matter simulations. The latter predict a cuspy density profile in the inner parts of galaxies, whereas observations of dwarf and low surface brightness galaxies show a constant-density core. Aims. We want to determine the shape of the dark matter potential in the nuclear regions of a sample of six nearby irregular dwarf galaxies. Methods. In order to quantify the amount of non-circular motions that could potentially affect a mass decomposition, we first perform a harmonic decomposition of the H i Hermite velocity fields of all sample galaxies. We then decompose the H i rotation curves into different mass components by fitting NFW and pseudo-isothermal halo models to the H i rotation curves using a χ 2 minimisation. We model the minimum-disc, the minimum-disc + gas, and the maximum-disc cases.Results. The non-circular motions are in all cases studied here of the order of only a few km s −1 (generally corresponding to less than 25% of the local rotation velocity), which means that they do not significantly affect the rotation curves. The observed rotation curves can better be described by the cored pseudo-isothermal halo than by the NFW halo. The slopes of the dark matter density profiles confirm this result and are in good agreement with previous studies. The quality of the fits can often be improved when including baryons, which suggests that they contribute significantly to the inner part of the density profile of dwarf galaxies.