# Last entries in the CiteULike library

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

EarlierDisturbed 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 LUTHDensity distribution of the cosmological matter field(6 Jun 2017)The one-point probability distribution function (PDF) of the matter density field in the universe is a fundamental property that plays an essential role in cosmology for estimates such as gravitational weak lensing, non-linear clustering, massive production of mock galaxy catalogs, and testing predictions of cosmological models. Here we [...]Thu, Jun 08, 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$). Here we present 1D non-LTE time-dependent radiative transfer simulations of pure central detonations of carbon-oxygen WDs with a [...]Thu, Jun 08, 2017Source: CiteULike Group Cosmo LUTHGas Cooling in Hydrodynamic Simulations with An Exact Time Integration Scheme(31 May 2017)We implement and test the exact time integration method proposed by Townsend 2009 for gas cooling in cosmological hydrodynamic simulations. The errors using this time integrator for the internal energy are limited by the resolution of the cooling tables and are insensitive to the size of the timestep, [...]Fri, Jun 02, 2017Source: CiteULike Group Cosmo LUTHThe structural evolution of galaxies with both thin and thick discsMonthly Notices of the Royal Astronomical Society (25 May 2017), doi:10.1093/mnras/stx1300We perform controlled N-body simulations of disc galaxies growing within live dark matter (DM) haloes to present-day galaxies that contain both thin and thick discs. We consider two types of models: a) thick disc initial conditions to which stars on [...]Fri, May 26, 2017Source: CiteULike Group Cosmo LUTHSelf-consistent semi-analytic models of the first stars(25 May 2017)We have developed a semi-analytic framework to model the large-scale evolution of the first Population III (Pop III) stars and the transition to Population II (Pop II) star formation. Our model follows dark matter halos from cosmological N-body simulations, utilizing their individual merger histories and three-dimensional positions, and [...]Fri, May 26, 2017Source: CiteULike Group Cosmo LUTHHalo Histories vs. Galaxy Properties at z=0, III: The Properties of Star-Forming Galaxies(23 May 2017)We measure how the properties of star-forming central galaxies correlate with large-scale environment,$δ$, measured on$10$Mpc/h scales. We use group catalogs to isolate a robust sample of central galaxies with high purity and completeness. The properties we investigate are star formation rate (SFR), exponential disk scale length [...]Thu, May 25, 2017Source: CiteULike Group Cosmo LUTHEMERGE - An empirical model for the formation of galaxies since$zâˆ¼10$(15 May 2017)We present EMERGE, an Empirical ModEl for the foRmation of GalaxiEs, describing the evolution of individual galaxies in large volumes from$z∼10$to the present day. We assign a star formation rate to each dark matter halo based on its growth rate, which specifies how much baryonic material [...]Wed, May 17, 2017Source: CiteULike Group Cosmo LUTHBeyond Assembly Bias: Exploring Secondary Halo Biases for Cluster-size Haloes(10 May 2017)Secondary halo bias, commonly known as "assembly bias," is the dependence of halo clustering on a halo property other than mass. This prediction of the Lambda-Cold Dark Matter cosmology is essential to modelling the galaxy distribution to high precision and interpreting clustering measurements. As the name suggests, different [...]Fri, May 12, 2017Source: CiteULike Group Cosmo LUTHPrecision cosmology with redshift-space bispectrum: a perturbation theory based model at one-loop order(7 May 2017)The large-scale matter distribution in the late-time Universe exhibits gravity-induced non-Gaussianity, and the bispectrum, three-point cumulant is expected to contain significant cosmological information. In particular, the measurement of the bispectrum helps to tighten the constraints on dark energy and modified gravity through the redshift-space distortions (RSD). In this [...]Tue, May 09, 2017Source: CiteULike Group Cosmo LUTHRevisiting HOD model assumptions: the impact of AGN feedback and assembly bias(1 May 2017)The standard Halo Occupation Distribution (HOD) models were originally developed based on results from semi-analytic and hydrodynamical galaxy formation models. Those models have since progressed, in particular to include AGN feedback to match the galaxy luminosity function in a universe with the observed baryon fraction. AGN feedback affects [...]Mon, May 08, 2017Source: CiteULike Group Cosmo LUTHPhase-space Analysis in the Group and Cluster environment: Time since Infall and Tidal Mass Loss(13 Apr 2017)Using the latest cosmological hydrodynamic N-body simulations of groups and clusters, we study how location in phase-space coordinates at$z$$=$$0$can provide information on environmental effects acting in clusters. We confirm the results of previous authors showing that galaxies tend to follow a typical path in phase-space as [...]Mon, Apr 17, 2017Source: CiteULike Group Cosmo LUTHDark-ages Reionization and Galaxy Formation Simulation - XIII. AGN quenching of high redshift star formation in ZF-COSMOS-20115(11 Apr 2017)Massive quiescent galaxies are thought to have formed stars rapidly at early times followed by a long period of quiescence. The recent discovery of a massive quiescent galaxy, ZF-COSMOS-20115 at$z∼4$, only 1.5 Gyr after the Big Bang, places new constraints on galaxy growth and the role of [...]Wed, Apr 12, 2017Source: CiteULike Group Cosmo LUTHFormation of Globular Cluster Candidates in Merging Proto-galaxies at High Redshift: A View from the FIRE Cosmological Simulations(10 Apr 2017)Using a state-of-the-art cosmological simulation of merging proto-galaxies at high redshift from the FIRE project, with explicit treatments of star formation and stellar feedback in the interstellar medium, we investigate the formation of star clusters and examine one of the formation hypothesis of present-day metal-poor globular clusters. We [...]Wed, Apr 12, 2017Source: CiteULike Group Cosmo LUTHGrowth of First Galaxies: Impacts of Star Formation and Stellar Feedback(11 Apr 2017)We present the results of cosmological hydrodynamic simulations with zoom-in initial conditions, and investigate the formation of the first galaxies and their evolution towards observable galaxies at$z ∼ 6$. We focus on three different galaxies which end up in halos with masses$M_h = 2.4 ×10^10~h^-1\; M_odot$[...]Wed, Apr 12, 2017Source: CiteULike Group Cosmo LUTHHigh-redshift galaxies and black holes in the eyes of JWST: a population synthesis model from infrared to X-rays(3 Apr 2017)The first billion years of the Universe is a pivotal time: stars, black holes (BHs) and galaxies form and assemble, sowing the seeds of galaxies as we know them today. Detecting, identifying and understand- ing the first galaxies and BHs is one of the current observational and theoretical [...]Wed, Apr 05, 2017Source: CiteULike Group Cosmo LUTHStar formation in a galactic outflowNature (24 Mar 2017), doi:10.1038/nature21677Recent observations have revealed massive galactic molecular outflows that may have physical conditions (high gas densities) required to form stars. Indeed, several recent models predict that such massive galactic outflows may ignite star formation within the outflow itself. This star-formation mode, in which stars form with [...]Tue, Mar 28, 2017Source: CiteULike Group Cosmo LUTHThe HI-to-H2 Transition in a Turbulent Medium(24 Mar 2017)We study the effect of density fluctuations induced by turbulence on the HI/H$_2$structure in photodissociation regions (PDRs) both analytically and numerically. We perform magnetohydrodynamic numerical simulations for both subsonic and supersonic turbulent gas and chemical HI/H$_2$balance calculations. We derive atomic-to-molecular density profiles and the HI column [...]Tue, Mar 28, 2017Source: CiteULike Group Cosmo LUTHCore or cusps: The central dark matter profile of a redshift one strong lensing cluster with a bright central image(24 Mar 2017)We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at$z=1.06$. The arc system is notable for the presence of a bright central image. The source is a Lyman Break galaxy at$z_s=2.39\$ and the mass enclosed within the 14 arc second radius Einstein [...]Mon, Mar 27, 2017Source: CiteULike Group Cosmo LUTHMassive star formation by accretion II. Rotation: how to circumvent the angular momentum barrier?Astronomy & Astrophysics (24 Mar 2017), doi:10.1051/0004-6361/201630149Rotation plays a key role in the star-formation process, from pre-stellar cores to pre-main-sequence (PMS) objects. Understanding the formation of massive stars requires taking into account the accretion of angular momentum during their PMS phase. We study the PMS evolution of objects destined to [...]Mon, Mar 27, 2017Source: CiteULike Group Cosmo LUTH