The tight empirical relation between dark matter halo mass and flat rotation velocity for late-type galaxies
Monthly Notices of the Royal Astronomical Society: Letters Oxford University Press 483:1 (2018) L98-L103
Abstract:
We present a new empirical relation between galaxy dark matter halo mass (Mhalo) and the velocity along the flat portion of the rotation curve (Vflat), derived from 120 late-type galaxies from the SPARC data base. The orthogonal scatter in this relation is comparable to the observed scatter in the baryonic Tully–Fisher relation (BTFR), indicating a tight coupling between total halo mass and galaxy kinematics at r ≪ Rvir. The small vertical scatter in the relation makes it an extremely competitive estimator of total halo mass. We demonstrate that this conclusion holds true for different priors on M*/L[3.6μ] that give a tight BTFR, but requires that the halo density profile follow DC14 rather than NFW. We provide additional relations between Mhalo and other velocity definitions at smaller galactic radii (i.e. V2.2, Veff, and Vmax) which can be useful for estimating halo masses from kinematic surveys, providing an alternative to abundance matching. Furthermore, we constrain the dark matter analogue of the radial acceleration relation and also find its scatter to be small, demonstrating the fine balance between baryons and dark matter in their contribution to galaxy kinematics.Stellar feedback and the energy budget of late-type Galaxies: Missing baryons and core creation
Monthly Notices of the Royal Astronomical Society Oxford University Press 480:4 (2018) 4287-4301
Abstract:
In a ΛCDM cosmology, galaxy formation is a globally inefficient process: it is often the case that far fewer baryons are observed in galaxy discs than expected from the cosmic baryon fraction. The location of these ‘missing baryons’ is unclear. By fitting halo profiles to the rotation curves of galaxies in the SPARC data set, we measure the ‘missing baryon’ mass for individual late-type systems. Assuming that haloes initially accrete the cosmological baryon fraction, we show that the maximum energy available from supernovae is typically not enough to completely eject these ‘missing baryons’ from a halo, but it is often sufficient to heat them to the virial temperature. The energy available from supernovae has the same scaling with galaxy mass as the energy needed to heat or eject the ‘missing baryons’, indicating that the coupling efficiency of the feedback to the ISM may be constant with galaxy virial mass. We further find that the energy available from supernova feedback is always enough to convert a primordial cusp into a core and has magnitude consistent with what is required to heat the ‘missing baryons’ to the virial temperature. Taking a census of the baryon content of galaxies with 109 < Mvir/M⊙ < 1012 reveals that ∼86 per cent of baryons are likely to be in a hot phase surrounding the galaxies and possibly observable in the X-ray, ∼7 per cent are in the form of cold gas, and ∼7 per cent are in stars.A Census of the LyC Photons that Form the UV Background During Reionization
Monthly Notices of the Royal Astronomical Society Oxford University Press 478:4 (2018) 4986-5005
Abstract:
We present a new, on-the-fly photon flux and absorption tracer algorithm designed to directly measure the contribution of different source populations to the metagalactic ultraviolet (UV) background and to the ionization fraction of gas in the Universe. We use a suite of multifrequency radiation hydrodynamics simulations that are carefully calibrated to reproduce a realistic reionization history and galaxy properties at z ⩾ 6, to disentangle the contribution of photons emitted by different mass haloes and by stars with different metallicities and ages to the UV background during reionization. While at very early cosmic times low-mass, metal-poor haloes provide most of the Lyman continuum photons, their contribution decreases steadily with time. At z = 6 it is the photons emitted by massive systems ( Mhalo/M⊙>1010h−1 ) and by the metal enriched stars (10−3 < Z/Z⊙ < 10−1.5) that provide the largest contribution to the ionising UV background. We demonstrate that there are large variations in the escape fraction depending on the source, with the escape fraction being highest ( ∼45--60percent ) for photons emitted by the oldest stars that penetrate into the intergalactic medium via low opacity channels carved by the ionising photons and supernova from younger stars. Before H II regions begin to overlap, the photoionization rate strongly fluctuates between different, isolated H II bubbles, depending on the embedded ionising source, which we suggest may result in spatial variations in the properties of dwarf galaxies.The SPHINX Cosmological Simulations of the First Billion Years: the Impact of Binary Stars on Reionization★
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2018)
Impact of Lyman alpha pressure on metal-poor dwarf galaxies
Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 475:4 (2018) 4617-4635