# Last entries in the CiteULike library

For the full list: http://www.citeulike.org/group/13962/

EarlierOn the faint-end of the galaxy luminosity function in the Epoch of Reionization: updated constraints from the HST Frontier Fields(14 Nov 2017)Ultra-faint galaxies are hosted by small dark matter halos with shallow gravitational potential wells, hence their star formation activity is more sensitive to feedback effects. The shape of the faint-end of the high-$z$ galaxy luminosity function (LF) contains important information on star formation and its interaction with the [...]Fri, Nov 17, 2017Source: CiteULike Group Cosmo LUTHGalaxy And Mass Assembly: Automatic Morphological Classification of Galaxies Using Statistical Learning(16 Nov 2017)We apply four statistical learning methods to a sample of $7941$ galaxies ($z [...]Fri, Nov 17, 2017Source: CiteULike Group Cosmo LUTHGalaxy and Mass Assembly (GAMA): Small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies(15 Nov 2017)The galaxy pairwise velocity dispersion (PVD) can provide important tests of non-standard gravity and galaxy formation models. We describe measurements of the PVD of galaxies in the Galaxy and Mass Assembly (GAMA) survey as a function of projected separation and galaxy luminosity. Due to the faint magnitude limit [...]Thu, Nov 16, 2017Source: CiteULike Group Cosmo LUTHDisruption of Dark Matter Substructure: Fact or Fiction?(14 Nov 2017)Accurately predicting the demographics of dark matter (DM) substructure is of paramount importance for many fields of astrophysics, including gravitational lensing, galaxy evolution, halo occupation modeling, and constraining the nature of dark matter. Because of its strongly non-linear nature, DM substructure is typically modeled using N-body simulations, which [...]Thu, Nov 16, 2017Source: CiteULike Group Cosmo LUTHEvidence of Neutrino Enhanced Clustering in a Complete Sample of Sloan Survey Clusters, Implying$âˆ‘ m_Î½=0.11Â±0.03eV$(14 Nov 2017)The clustering amplitude of 7143 clusters from the Sloan Digital Sky Survey (SDSS) is found to increase linearly with cluster mass, closely agreeing with the Gaussian random field hypothesis for structure formation. In detail, the observed correlation length exceeds pure cold dark matter (CDM) simulation predictions by$∼eq [...]Wed, Nov 15, 2017Source: CiteULike Group Cosmo LUTHLocalized massive halo properties in Bahamas and Macsis simulations: scalings, log-normality, and covariance(14 Nov 2017)Using tens of thousands of halos realized in the BAHAMAS and MACSIS simulations produced with a consistent astrophysics treatment that includes AGN feedback, we validate a multi-property statistical model for the stellar and hot gas mass behavior in halos hosting groups and clusters of galaxies. The large sample [...]Wed, Nov 15, 2017Source: CiteULike Group Cosmo LUTHCosmic Star Formation: a simple model of the SFRD(z)(9 Nov 2017)We investigate the evolution of the cosmic star formation rate density (SFRD) from redshift z=20 to z=0 and compare it with the observational one by Madau and Dickinson derived from recent compilations of UV and IR data. The theoretical SFRD(z) and its evolution are obtained using a simple [...]Fri, Nov 10, 2017Source: CiteULike Group Cosmo LUTHThe MUSE Hubble Ultra Deep Field Survey VI: The Faint-End of the Lya Luminosity Function at 2.91 < z < 6.64 and Implications for Reionisation(7 Nov 2017), doi:10.1051/0004-6361/201731431We present the deepest study to date of the Lya luminosity function (LF) in a blank field using blind integral field spectroscopy from MUSE. We constructed a sample of 604 Lya emitters (LAEs) across the redshift range 2.91 < z < 6.64 using automatic detection software in [...]Fri, Nov 10, 2017Source: CiteULike Group Cosmo LUTHVery low-luminosity galaxies in the early universe have observed sizes similar to single star cluster complexes(6 Nov 2017)We compare the sizes and luminosities of 307 faint z=6-8 sources revealed by the Hubble Frontier Fields (HFF) program with sources in the nearby universe. Making use of the latest lensing models and data from the first four HFF clusters with an extensive suite of public lens models, [...]Wed, Nov 08, 2017Source: CiteULike Group Cosmo LUTHThe Dearth of z~10 Galaxies in all HST Legacy Fields -- The Rapid Evolution of the Galaxy Population in the First 500 Myr(30 Oct 2017)We present an analysis of all prime HST legacy fields spanning >800 arcmin^2 for the search of z~10 galaxy candidates and the study of their UV luminosity function (LF). In particular, we present new z~10 candidates selected from the full Hubble Frontier Field (HFF) dataset. Despite the addition [...]Fri, Nov 03, 2017Source: CiteULike Group Cosmo LUTHDark Energy Survey Year 1 Results: A Precise H0 Measurement from DES Y1, BAO, and D/H Data(1 Nov 2017)We combine Dark Energy Survey Year 1 clustering and weak lensing data with Baryon Acoustic Oscillations (BAO) and Big Bang Nucleosynthesis (BBN) experiments to constrain the Hubble constant. Assuming a flat $Λ$CDM model with minimal neutrino mass ($∑ m_ν = 0.06$ eV) we find $H_0=67.2^+1.2_-1.0$ km/s/Mpc (68% CL). [...]Thu, Nov 02, 2017Source: CiteULike Group Cosmo LUTHStellar mass spectrum within massive collapsing clumps I. Influence of the initial conditions(1 Nov 2017)We conduct numerical experiments in which we systematically vary the initial density over four orders of magnitude and the turbulent velocity over a factor ten. In a companion paper, we investigate the dependence of this distribution on the gas thermodynamics. We performed a series of hydrodynamical numerical simulations [...]Thu, Nov 02, 2017Source: CiteULike Group Cosmo LUTHDust temperature and mid-to-total infrared color distributions for star-forming galaxies at 0<z<4(27 Oct 2017)We present a new, publicly available library of dust spectral energy distributions (SEDs). These SEDs are characterized by only three parameters: the dust mass (Mdust), the dust temperature (Tdust), and the mid-to-total infrared color (IR8=LIR/L8). The latter measures the relative contribution of PAH molecules to the LIR. We [...]Tue, Oct 31, 2017Source: CiteULike Group Cosmo LUTHDoes the Galaxy-Halo Connection Vary with Environment?(25 Oct 2017)SubHalo Abundance Matching (SHAM) assumes that one (sub)halo property, such as mass Mvir or peak circular velocity Vpeak, determines properties of the galaxy hosted in each (sub)halo such as its luminosity or stellar mass. This assumption implies that the dependence of Galaxy Luminosity Functions (GLFs) and the Galaxy [...]Sat, Oct 28, 2017Source: CiteULike Group Cosmo LUTHA census of cool core galaxy clusters in IllustrisTNG(23 Oct 2017)The thermodynamic structure of hot gas in galaxy clusters is sensitive to astrophysical processes and typically difficult to model with galaxy formation simulations. We explore the fraction of cool-core (CC) clusters in a large sample of $370$ clusters from IllustrisTNG, examining six common CC definitions. IllustrisTNG produces continuous [...]Wed, Oct 25, 2017Source: CiteULike Group Cosmo LUTHThe Mass Growth and Stellar Ages of Galaxies: Observations versus Simulations(23 Oct 2017)Using observed stellar mass functions out to $z=5$, we measure the main progenitor stellar mass growth of descendant galaxies with masses of $\logM_*/M_odot=11.5,11.0,10.5,10.0$ at $z∼0.1$ using an evolving cumulative number density selection. From these mass growth histories, we are able to measure the time at which half the [...]Wed, Oct 25, 2017Source: CiteULike Group Cosmo LUTHCosmic Reionization After Planck and Before JWST: An Analytic Approach(20 Oct 2017)The reionization of cosmic hydrogen marks a critical juncture in the history of structure formation in the universe. Here we present a new formulation of the standard reionization equation for the evolution of the volume-averaged HII fraction that is more consistent with the accepted conceptual model of inhomogeneous [...]Wed, Oct 25, 2017Source: CiteULike Group Cosmo LUTHMultiDark-Galaxies: data release and first results(23 Oct 2017)We present the public release of the MultiDark-Galaxies: three distinct galaxy catalogues derived from one of the Planck cosmology MultiDark simulations (i.e. MDPL2, with a volume of (1 Gpc/$h$)$^3$ and mass resolution of $1.5 × 10^9 M_odot/h$) by applying the semi-analytic models GALACTICUS, SAG, and SAGE to it. [...]Wed, Oct 25, 2017Source: CiteULike Group Cosmo LUTHDisturbed galaxy clusters are more abundant in an X-ray volume-limited sample(10 Oct 2017)We present first strong observational evidence that the X-ray cool-core bias or the apparent bias in the abundance of relaxed clusters is absent in our REFLEX volume-limited sample (ReVols). We show that these previously observed biases are due to the survey selection method such as for an flux-limited [...]Thu, Oct 12, 2017Source: CiteULike Group Cosmo LUTHClassicality and Quantum Break-Time for Cosmic Axions(2 Oct 2017)We investigate the length of the period of validity of a classical description for the cosmic axion field. To this end, we first show that we can understand the oscillating axion solution as expectation value over an underlying coherent quantum state. Once we include self-interaction of the axion, [...]Wed, Oct 04, 2017Source: CiteULike Group Cosmo LUTHThe Grism Lens-Amplified Survey from Space (GLASS). XII. Spatially Resolved Galaxy Star Formation Histories and True Evolutionary Paths at z > 1(2 Oct 2017)Modern data empower observers to describe galaxies as the spatially and biographically complex objects they are. We illustrate this through case studies of four, $z∼1.3$ systems based on deep, spatially resolved, 17-band + G102 + G141 Hubble Space Telescope grism spectrophotometry. Using full spectrum rest-UV/-optical continuum fitting, we [...]Wed, Oct 04, 2017Source: CiteULike Group Cosmo LUTHGalaxy Cluster Mass Reconstruction Project: III. The impact of dynamical substructure on cluster mass estimates(28 Sep 2017)With the advent of wide-field cosmological surveys, we are approaching samples of hundreds of thousands of galaxy clusters. While such large numbers will help reduce statistical uncertainties, the control of systematics in cluster masses becomes ever more crucial. Here we examine the effects of an important source of [...]Mon, Oct 02, 2017Source: CiteULike Group Cosmo LUTHConnecting the first galaxies with ultra faint dwarfs in the Local Group: chemical signatures of Population~III stars(25 Sep 2017)We investigate the star formation history and chemical evolution of isolated analogues of Local Group (LG) ultra faint dwarf galaxies (UFDs; stellar mass range of 10^2 solar mass < M_star [...]Wed, Sep 27, 2017Source: CiteULike Group Cosmo LUTHHidden universality in the merger rate distribution in the primordial black hole scenario(26 Sep 2017)Primordial black holes (PBHs) form binaries in the radiation dominated era. Once formed, some fraction of them merge within the age of the Universe by gravitational radiation reaction. We investigate the merger rate of the PBH binaries when the PBHs have a distribution of masses around $\cal O(10) [...]Wed, Sep 27, 2017Source: CiteULike Group Cosmo LUTHComparing galaxy formation in semi-analytic models and hydrodynamical simulations(25 Sep 2017)It is now possible for hydrodynamical simulations to reproduce a representative galaxy population. Accordingly, it is timely to assess critically some of the assumptions of traditional semi-analytic galaxy formation models. We use the Eagle simulations to assess assumptions built into the Galform semi-analytic model, focussing on those relating [...]Wed, Sep 27, 2017Source: CiteULike Group Cosmo LUTHThe merger rate of primordial-black-hole binaries(19 Sep 2017)Primordial black holes (PBHs) have long been a candidate for the elusive dark matter (DM), and remain poorly constrained in the ~20-100 Msun mass range. PBH binaries were recently suggested as the possible source of LIGO's first detections. In this paper, we thoroughly revisit existing estimates of the [...]Thu, Sep 21, 2017Source: CiteULike Group Cosmo LUTHInteractions between multiple supermassive black holes in galactic nuclei: a solution to the final parsec problem(19 Sep 2017)Using few-body simulations, we investigate the evolution of supermassive black holes (SMBHs) in galaxies ($M_∗=10^10-10^12 M_odot$at$z=0$) at$0 [...]Wed, Sep 20, 2017Source: CiteULike Group Cosmo LUTHGLASS: A General Likelihood Approximate Solution Scheme(28 Aug 2017)We present a technique for constructing suitable posterior probability distributions in situations for which the sampling distribution of the data is not known. This is very useful for modern scientific data analysis in the era of "big data", for which exact likelihoods are commonly either unknown, computationally prohibitively [...]Wed, Aug 30, 2017Source: CiteULike Group Cosmo LUTHSpatial Clustering of Dark Matter Halos: Secondary Bias, Neighbor Bias, and the Influence of Massive Neighbors on Halo Properties(28 Aug 2017)We explore the phenomenon commonly known as halo assembly bias, whereby dark matter halos of the same mass are found to be more or less clustered when a second halo property is considered, for halos in the mass range $3.7 × 10^11 \; h^-1 \mathrmM_odot - 5.0 × [...]Wed, Aug 30, 2017Source: CiteULike Group Cosmo LUTHThe concentration-mass relation of clusters of galaxies from the OmegaWINGS survey(24 Aug 2017)The relation between a cosmological halo concentration and its mass (cMr) is a powerful tool to constrain cosmological models of halo formation and evolution. On the scale of galaxy clusters the cMr has so far been determined mostly with X-ray and gravitational lensing data. The use of independent [...]Fri, Aug 25, 2017Source: CiteULike Group Cosmo LUTHTree-based solvers for adaptive mesh refinement code FLASH - I: gravity and optical depths(21 Aug 2017)We describe an OctTree algorithm for the MPI-parallel, adaptive mesh-refinement code \sc FLASH, which can be used to calculate the gas self-gravity, and also the angle-averaged local optical depth, for treating ambient diffuse radiation. The algorithm communicates to the different processors only those parts of the tree that [...]Tue, Aug 22, 2017Source: CiteULike Group Cosmo LUTHAccurate Modelling of Galaxy Clustering on Small Scales: Testing the Standard$Î›\mathrmCDM$+ Halo Model(16 Aug 2017)Interpreting the small-scale clustering of galaxies with halo models can elucidate the connection between galaxies and dark matter halos. Unfortunately, the modelling is typically not sufficiently accurate for ruling out models in a statistical sense. It is thus difficult to use the information encoded in small scales to [...]Thu, Aug 17, 2017Source: CiteULike Group Cosmo LUTHSmall-scale Intensity Mapping: Extended Halos as a Probe of the Ionizing Escape Fraction and Faint Galaxy Populations during Reionization(24 Jul 2017)We present a new method to quantify the value of the escape fraction of ionizing photons, and the existence of ultra-faint galaxies clustered around brighter objects during the epoch of cosmic reionization, using the diffuse Ly$α$, continuum and H$α$emission observed around galaxies at$z∼6$. We model the [...]Wed, Jul 26, 2017Source: CiteULike Group Cosmo LUTHAttractive vs. repulsive interactions in the Bose-Einstein condensation dynamics of relativistic field theories(24 Jul 2017)We study the impact of attractive self-interactions on the nonequilibrium dynamics of relativistic quantum fields with large occupancies at low momenta. Our primary focus is on Bose-Einstein condensation and nonthermal fixed points in such systems. As a model system we consider O(N)-symmetric scalar field theories. We use classical-statistical [...]Wed, Jul 26, 2017Source: CiteULike Group Cosmo LUTHActive Galactic Nuclei: what's in a name?(22 Jul 2017)Active Galactic Nuclei (AGN) are energetic astrophysical sources powered by accretion onto supermassive black holes in galaxies, and present unique observational signatures that cover the full electromagnetic spectrum over more than twenty orders of magnitude in frequency. The rich phenomenology of AGN has resulted in a large number [...]Tue, Jul 25, 2017Source: CiteULike Group Cosmo LUTHSelf-shielding of hydrogen in the IGM during the epoch of reionization(21 Jul 2017)We investigate self-shielding of intergalactic hydrogen against ionizing radiation in radiative transfer simulations of cosmic reionization carefully calibrated with Lyman alpha forest data. While self-shielded regions manifest as Lyman-limit systems in the post-reionization Universe, here we focus on their evolution during reionization (redshifts z=6-10). At these redshifts, the [...]Mon, Jul 24, 2017Source: CiteULike Group Cosmo LUTHElucidating$Î›$CDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy(20 Jul 2017)We examine the impact of baryon acoustic oscillation (BAO) scale measurements on the discrepancy between the value of the Hubble constant ($H_0$) inferred from the local distance ladder and from Planck cosmic microwave background (CMB) data. While the BAO data alone cannot constrain$H_0$, we show that combining [...]Fri, Jul 21, 2017Source: CiteULike Group Cosmo LUTHKiDS-450 + 2dFLenS: Cosmological parameter constraints from weak gravitational lensing tomography and overlapping redshift-space galaxy clustering(20 Jul 2017)We perform a combined analysis of cosmic shear tomography, galaxy-galaxy lensing tomography, and redshift-space multipole power spectra (monopole and quadrupole) using 450 deg$^2$of imaging data by the Kilo Degree Survey (KiDS) overlapping with two spectroscopic surveys: the 2-degree Field Lensing Survey (2dFLenS) and the Baryon Oscillation Spectroscopic [...]Fri, Jul 21, 2017Source: CiteULike Group Cosmo LUTHThe core-cusp problem: a matter of perspective(19 Jul 2017)The existence of two kinematically and chemically distinct stellar subpopulations in the Sculptor and Fornax dwarf galaxies offers the opportunity to constrain the density profile of their matter haloes by measuring the mass contained within the well-separated half-light radii of the two metallicity subpopulations. Walker and Peñarrubia have [...]Fri, Jul 21, 2017Source: CiteULike Group Cosmo LUTHA Moving Mesh Hydrodynamic Solver for ChaNGa(17 Jul 2017)We describe the structure and implementation of a moving-mesh hydrodynamics solver in the large-scale parallel code, Charm N-body GrAvity solver (ChaNGa). While largely based on the algorithm described by Springel (2010) that is implemented in AREPO, our algorithm differs a few aspects. We describe our use of the [...]Wed, Jul 19, 2017Source: CiteULike Group Cosmo LUTHFinding structure in the dark: coupled dark energy, weak lensing, and the mildly nonlinear regime(18 Jul 2017)We reexamine interactions between the dark sectors of cosmology, with a focus on robust constraints that can be obtained using only mildly nonlinear scales. While it is well known that couplings between dark matter and dark energy can be constrained to the percent level when including the full [...]Wed, Jul 19, 2017Source: CiteULike Group Cosmo LUTHLight and color curve properties of type Ia supernovae: Theory vs. Observations(17 Jul 2017)We study optical light curve(LC) relations of type Ia supernovae(SNe~Ia) for their use in cosmology using high-quality photometry published by the Carnegie-Supernovae-Project (CSP-I). We revisit the classical luminosity-decline-rate ($Δ m_15$) relation and the Lira-relation, as well as investigate the time evolution of the ($B-V$) color and$B(B-V)$, which [...]Wed, Jul 19, 2017Source: CiteULike Group Cosmo LUTHSmall-Scale Challenges to the$Î›$CDM ParadigmAnnual Review of Astronomy and Astrophysics, Vol. 55, No. 1. (13 Jul 2017), doi:10.1146/annurev-astro-091916-055313The dark energy plus cold dark matter ($Λ$CDM) cosmological model has been a demonstrably successful framework for predicting and explaining the large-scale structure of Universe and its evolution with time. Yet on length scales smaller than$∼ [...]Mon, Jul 17, 2017Source: CiteULike Group Cosmo LUTHThe optimally-sampled galaxy-wide stellar initial mass function - Observational tests and the publicly available GalIMF code(13 Jul 2017)Here we present a full description of the integrated galaxy-wide initial mass function (IGIMF) theory in terms of the optimal sampling and compare it with available observations. Optimal sampling is the method we use to discretize the IMF into stellar masses deterministically. Evidence has been indicating that nature [...]Mon, Jul 17, 2017Source: CiteULike Group Cosmo LUTHConstraining the HI-Halo Mass Relation From Galaxy Clustering(7 Jul 2017)We study the dependence of galaxy clustering on atomic gas mass using a sample of $∼$16,000 galaxies with redshift in the range of $0.0025 [...]Mon, Jul 10, 2017Source: CiteULike Group Cosmo LUTHSmall-N collisional dynamics III: The battle for the realm of not-so-small-N(6 Jul 2017)In this paper, the third in the series, we continue our study of combinatorics in chaotic Newtonian dynamics. We study the chaotic four-body problem in Newtonian gravity assuming finite-sized particles, and we focus on interactions that produce direct collisions between any two stars. Our long-term goal is to [...]Mon, Jul 10, 2017Source: CiteULike Group Cosmo LUTHSimulating galaxies in the reionization era with FIRE-2: galaxy scaling relations, stellar mass functions, and luminosity functions(20 Jun 2017)We present a suite of cosmological zoom-in simulations at z>5 from the Feedback In Realistic Environments project, spanning a halo mass range M_halo~10^8-10^12 M_sun at z=5. We predict the stellar mass-halo mass relation, stellar mass function, and luminosity function in several bands from z=5-12. The median stellar mass-halo [...]Thu, Jun 22, 2017Source: CiteULike Group Cosmo LUTHDark matter haloes: a multistream view(9 Jun 2017)Mysterious dark matter constitutes about 85% of all mass in the Universe. Clustering of dark matter plays the dominant role in the formation of all observed structures on scales from a fraction to a few hundreds of Mega-parsecs. Galaxies play a role of lights illuminating these structures so [...]Wed, Jun 14, 2017Source: CiteULike Group Cosmo LUTHEIG - II. Intriguing characteristics of the most extremely isolated galaxiesMonthly Notices of the Royal Astronomical Society, Vol. 469, No. 1. (6 Jun 2017), pp. 347-382, doi:10.1093/mnras/stx689We have selected a sample of 41 extremely isolated galaxies (EIGs) from the local universe using both optical and HI ALFALFA redshifts (Spector & Brosch 2016). Narrow band H$_α$and wide band imaging along [...]Thu, Jun 08, 2017Source: CiteULike Group Cosmo LUTHEvidence for sub-Chandrasekhar-mass progenitors of Type Ia supernovae at the faint end of the width-luminosity relation(6 Jun 2017)The faster light-curve evolution of low-luminosity Type Ia supernovae (SNe Ia) suggests that they could result from the explosion of white dwarf (WD) progenitors below the Chandrasekhar mass ($M_ Ch\$). Here we present 1D non-LTE time-dependent radiative transfer simulations of pure central detonations of carbon-oxygen WDs with a [...]Thu, Jun 08, 2017Source: CiteULike Group Cosmo LUTH