Towards a more realistic population of bright spiral galaxies in cosmological simulations

We present an update to the multiphase SPH galaxy formation code by Scannapieco et al. We include a more elaborate treatment of the production of metals, cooling rates based on individual element abundances, and a scheme for the turbulent diffusion of metals. Our SN feedback model now transfers energy to the ISM in kinetic and thermal form, and we include a prescription for the effects of radiation pressure from massive young stars on the ISM. We calibrate our new code on the well studied Aquarius haloes and then use it to simulate a sample of 16 galaxies with halo masses between 1x10^11 and 3x10^12 M_sun. In general, the stellar masses of the sample agree well with the stellar mass to halo mass relation inferred from abundance matching techniques for redshifts z=0-4. There is however a tendency to overproduce stars at z>4 and to underproduce them at z<0.5 in the least massive haloes. Overly high SFRs at z<1 for the most massive haloes are likely connected to the lack of AGN feedback in our model. The simulated sample also shows reasonable agreement with observed star formation rates, sizes, gas fractions and gas-phase metallicities at z=0-3. Remaining discrepancies can be connected to deviations from predictions for star formation histories from abundance matching. At z=0, the model galaxies show realistic morphologies, stellar surface density profiles, circular velocity curves and stellar metallicities, but overly flat metallicity gradients. 15 out of 16 of our galaxies contain disk components with kinematic disk fraction ranging between 15 and 65 %. The disk fraction depends on the time of the last destructive merger or misaligned infall event. Considering the remaining shortcomings of our simulations we conclude that even higher kinematic disk fractions may be possible for LambdaCDM haloes with quiet merger histories, such as the Aquarius haloes.Comment: 26 pages, 20 figures, accepted for publication in MNRA

Why stellar feedback promotes disc formation in simulated galaxies

We study how feedback influences baryon infall onto galaxies using cosmological, zoom-in simulations of haloes with present mass $M_{vir}=6.9\times10^{11} M_{\odot}$ to $1.7\times10^{12} M_{\odot}$. Starting at z=4 from identical initial conditions, implementations of weak and strong stellar feedback produce bulge- and disc-dominated galaxies, respectively. Strong feedback favours disc formation: (1) because conversion of gas into stars is suppressed at early times, as required by abundance matching arguments, resulting in flat star formation histories and higher gas fractions; (2) because 50% of the stars form in situ from recycled disc gas with angular momentum only weakly related to that of the z=0 dark halo; (3) because late-time gas accretion is typically an order of magnitude stronger and has higher specific angular momentum, with recycled gas dominating over primordial infall; (4) because 25-30% of the total accreted gas is ejected entirely before z~1, removing primarily low angular momentum material which enriches the nearby inter-galactic medium. Most recycled gas roughly conserves its angular momentum, but material ejected for long times and to large radii can gain significant angular momentum before re-accretion. These processes lower galaxy formation efficiency in addition to promoting disc formation.Comment: 23 pages, 29 figures, accepted for publication in MNRA

Simulating the formation and evolution of disc galaxies in a LambdaCDM universe

The majority of stars in the universe has formed in disc galaxies with masses similar to that of the Milky Way. Ab-initio cosmological hydrodynamical simulations of the formation and evolution of galaxies in a Lambda Cold Dark Matter universe have long suffered from serious problems in correctly modelling the star-formation history and structure of disc galaxies. We first use idealized semi-cosmological simulations to gain a better understanding of processes leading to problems in disc formation simulations. We add rotating spheres of hot gas to cosmological dark-matter-only simulations of individual haloes and follow the formation and evolution of galaxy discs from the cooling gas. The initial orientation of the baryonic angular momentum with respect to the halo has a major effect on disc formation. Despite the coherently rotating initial conditions, the orientations of the disc and the outer gas and the relative angle between the components can all change by more than 90 degrees over several billion years. Dominant discs with realistic structural and kinematical properties form preferentially if slow cooling times shift disc formation to later times, if the initial angular momentum is aligned with the halo minor axis and if there is little reorientation of the disc. We then present a new set of fully cosmological simulations with an updated multiphase smoothed particle hydrodynamics galaxy formation code. The update includes improved treatment of metal-line cooling, metal production, turbulent diffusion of metals, kinetic and thermal supernova feedback and radiation pressure from massive young stars. We compare the models to a variety of observations at high and low redshifts and find good agreement for morphologies, stellar-to-dark-matter mass ratios, star formation rates, gas fractions and heavy element abundances. Agreement is better at redshift z=1 than at present day as discrepancies in star formation histories for the lowest and highest simulated galaxy masses become apparent at late times. 18 out of 19 of our model galaxies at z=0 contain stellar discs with kinematic disc fractions up to 65 %, higher than in any previous simulations. We finally compare our model galaxies in detail with recent observations of the structural evolution of stellar galactic discs and the structure of z=0 gas discs. Stellar surface density profiles agree well with observations at z>1, but reveal too little central growth afterwards. This is likely connected to a lack of bars in our simulations resulting from overly strong feedback. Discs at z=0 are too extended by a factor \sim 2. The discs have diverse formation histories ranging from pure inside-out growth in systems with quiescent merger histories to continuous mass growth at all radii. Central mass growth in our models is driven by mergers and misaligned infall events, which leave signatures in the present day distributions of radii and element abundances as functions of stellar age. Gas discs agree well with observations in terms of sizes and profile shapes, but on average have overly high gas-to-stellar mass ratios. Our models agree well with the observed neutral hydrogen mass-size relation. Despite significant progress, our models continue to suffer from various problems illustrating that we are still far away from capturing all relevant physical processes accurately

An observational and theoretical view of the radial distribution of HI gas in galaxies

We analyze the radial distribution of HI gas for 23 disk galaxies with unusually high HI content from the Bluedisk sample, along with a similar-sized sample of "normal" galaxies. We propose an empirical model to fit the radial profile of the HI surface density, an exponential function with a depression near the center. The radial HI surface density profiles are very homogeneous in the outer regions of the galaxy; the exponentially declining part of the profile has a scale-length of $\sim 0.18$ R1, where R1 is the radius where the column density of the HI is 1 M$_{\odot}$ pc$^{-2}$. This holds for all galaxies, independent of their stellar or HI mass. The homogenous outer profiles, combined with the limited range in HI surface density in the non-exponential inner disk, results in the well-known tight relation between HI size and HI mass. By comparing the radial profiles of the HI-rich galaxies with those of the control systems, we deduce that in about half the galaxies, most of the excess gas lies outside the stellar disk, in the exponentially declining outer regions of the HI disk. In the other half, the excess is more centrally peaked. We compare our results with existing smoothed-particle hydrodynamical simulations and semi-analytic models of disk galaxy formation in a $\Lambda$ Cold Dark Matter universe. Both the hydro simulations and the semi-analytic models reproduce the HI surface density profiles and the HI size-mass relation without further tuning of the simulation and model inputs. In the semi-analytic models, the universal shape of the outer HI radial profiles is a consequence of the {\em assumption} that infalling gas is always distributed exponentially. The conversion of atomic gas to molecular form explains the limited range of HI surface densities in the inner disk. These two factors produce the tight HI mass-size relation.Comment: 15 pages, 14 figures, submitted to MNRA

Pet attitudes predicting preferences for pets over people

The preference for animal companionship over human companionship may be predicted by attitudes about pet ownership. We hypothesized that pet attitudes could predict preferences for relationships with pets over humans. We sampled 182 people who named a person and a pet they love and care about. Participants rated their feelings of love, time spent, enjoyment, and equity in both their human and pet relationships. We also presented seven hypothetical negative event scenarios that involve both the pet and human and asked participants to predict their feelings and reactions based on these events. The Pet Attitudes Scale (Templer et al., 1981) was used to assess attitudes towards pets. People had similar positive feelings about their pet‑human and human‑human relationships. However, people were more likely to react negatively towards a human compared to a pet. Positive pet a;itudes predicted more positive and less negative reactions to pets. Positive pet a;itudes can predict preference for pet relationships over human relationships and may help researchers identify what relationships work best depending on a personʹs pet attitudes

Understanding Dwarf Galaxies in order to Understand Dark Matter

Much progress has been made in recent years by the galaxy simulation community in making realistic galaxies, mostly by more accurately capturing the effects of baryons on the structural evolution of dark matter halos at high resolutions. This progress has altered theoretical expectations for galaxy evolution within a Cold Dark Matter (CDM) model, reconciling many earlier discrepancies between theory and observations. Despite this reconciliation, CDM may not be an accurate model for our Universe. Much more work must be done to understand the predictions for galaxy formation within alternative dark matter models.Comment: Refereed contribution to the Proceedings of the Simons Symposium on Illuminating Dark Matter, to be published by Springe

Discovering a New Standard for Treating Depressive Symptoms

Integrated Health Hawaii established evidence-based standards for an engagement-focused care coordination model to treat depression that can contribute significantly to alleviating symptoms and preventing more costly care. Attempting to reach a patient at least seven times resulted in the greatest improvement in outcome measures. Depression is currently ranked as the third leading contributor to global disease burden, and it is estimated that it will be number one by 2030. Care coordination models have been shown to help improve patient outcomes and reduce costs. Yet evidence-based standards for successfully contacting and engaging patients through care coordination are lacking. This study examines Integrated Health Hawaii’s engagement-focused care coordination model to provide evidence for the most effective utilization of care coordination with those suffering from depression in a diverse population. The current standard of making a “good effort,” three attempts, may only be reaching 60\% of patients. To reach at least 75\% of patients, seven attempts should be made; and to reach 95\% of patients, 10 attempts should be made. These attempts can be made within a 2-week period, and the outcomes prevented are substantial in terms of alleviating symptoms, reducing Patient Health Questionnaire-9 scores, and preventing more costly care, including ER visits and self-harm

Mixed-methods analysis of cultural influences on the attitudes of love and hate

This version of the article has been accepted for publication, after peer review (when applicable) and is subject to Springer Nature’s AM terms of use, but is not the Version of Record and does not reflect post-acceptance improvements, or any corrections. The Version of Record is available online at: http://dx.doi.org/10.1007/s12144-023-04460-0Objectives The religious influence on the construction of emotions like love and hate have lacked empirical attention. This study sought to address this issue by exploring the influence of culture and religion on love and hate using both quantitative and qualitative measures. Method Samples from Japan (n = 397), Thailand (n = 258), the U.S. (n = 198), and Sweden (n = 80) took an online survey on either love or hate. Quantitative measures were used to assess either positive or negative attitudes towards love and hate while qualitative measures were used to assess differences in the concepts of love and hate. Results Quantitative measures revealed that cultures (Japan and Thailand) with stronger Buddhist influence tend to have more moderate views of love and hate, while cultures with stronger Christian (Sweden and the U.S.) influence tend to have more polarized views of love and hate. Qualitative measures revealed that although the universal presence of love and hate share similar qualities across cultures, there are unique elements of both that may be lost when measuring love and hate. Conclusions These findings demonstrate a need to consider the religious influence on emotions. Especially when it comes to emotions like love and hate which have considerable influence over relationships, formation of family, and dissolution of alliances, religion may have a significantly broader influence than currently considered in the empirical literature

A single SNP turns a social honey bee (Apis mellifera) worker into a selfish parasite

The evolution of altruism in complex insect societies is arguably one of the major transitions in evolution and inclusive fitness theory plausibly explains why this is an evolutionary stable strategy. Yet, workers of the South African Cape honey bee (Apis mellifera capensis) can reverse to selfish behavior by becoming social parasites and parthenogenetically producing female offspring (thelytoky). Using a joint mapping and population genomics approach, in combination with a time-course transcript abundance dynamics analysis, we show that a single nucleotide polymorphism at the mapped thelytoky locus (Th) is associated with the iconic thelytokous phenotype. Th forms a linkage group with the ecdysis-triggering hormone receptor (Ethr) within a nonrecombining region under strong selection in the genome. A balanced detrimental allele system plausibly explains why the trait is specific to A. m. capensis and cannot easily establish itself into genomes of other honey bee subspecies.The Deutsche Forschungsgemeinschaft (to R.F.A.M.) and the National Research Foundation of South Africa (to C.W.W.P.)http://mbe.oxfordjournals.orghj2020Zoology and Entomolog