Current Semi-analytic Models Research Articles

Massive and old quiescent galaxies at high redshift

Aims. Questions of how massive quiescent galaxies rapidly assembled and how abundant they are at high redshift are increasingly important in the study of galaxy formation. Looking at these systems can shed light on the processes of galaxy mass assembly and quenching of the star formation at early epochs. In order to address these questions, we aim to identify and characterize massive quiescent galaxies from z ∼ 2.5 out to the highest redshifts at which these systems can be found. The final purpose is to compare the results with the predictions of state-of-the-art semi-analytical models of galaxy formation and evolution. Methods. We defined observer-frame color–color diagrams to optimally select quiescent galaxies at z > 2.5 and applied them to the COSMOS2015 catalog. We refined the spectral energy distribution (SED) fitting analysis for the selected candidates to confirm their quiescent nature, then derived their number density, mass density, and stellar mass functions. Finally, we compared the results with previous observations and some current semi-analytic models. Results. We selected candidates for quiescent galaxies in the redshift range 2.5 ≲ z ≲ 4.5 from the COSMOS2015 catalog by means of two color–color diagrams. The additional SED fitting analysis allowed us to select 128 galaxies, consistent with being massive (log(M*/M⊙)≥10.6), old (ages ≳0.5 Gyr), and quiescent (log(sSFR [yr−1]) ≤ −10.5) objects at high redshift (2.5 < z < 4.5). Their number and mass densities are in fair agreement with previous observations and, if confirmed, show a discrepancy with current semi-analytical models of galaxy formation and evolution, that underpredict the number of massive quiescent systems up to a factor of ∼12 at 2.5 ≤ z < 3.0 and ∼10 at z ∼ 4.0. The evolution of the stellar mass functions (SMFs) of these systems is similar to previous estimates and indicates a disagreement with models, particularly with regard to the shape of the SMF. Conclusions. The present results add further evidence to the possibility that massive and quiescent galaxies can exist out to at least z ∼ 4. If future spectroscopic observations carried out with, for example, the James Webb Space Telecope (JWST), confirm the substantial presence of such a population, further work on modeling the stellar mass assembly, as well as supermassive black hole accretion and feedback processes at early cosmic epochs, is needed to understand how these systems formed, evolved, and quenched their star formation.

A productivity model for cyclic steam stimulation for heavy oil with non-Newtonian flow behaviour

A lot of research has been performed and most researchers believe that heavy oil is a Bingham fluid under the condition of a low temperature, which has a threshold pressure gradient (TPG). However, the current analytical and semi-analytical models as well as numerical simulators in cyclic steam stimulation neglect TPG of heavy oil. In this paper, a new model that takes temperature variation and TPG into account is developed and analyzed. During a steam injection period, a reservoir is divided into a latent heat zone, a sensible heat zone and an unheated zone. During a production period, the reservoir is divided into a non-Newtonian fluid zone and a Newtonian fluid zone. Then results of this model are compared with both CMG-STARS results and field data. Finally, a set of sensitivity studies have been conducted to show the relationships between TPG and injection and production rate, steam quality and BHP. [Received: September 19, 2016; Accepted: January 28, 2017]

Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos

We study relation between stellar mass and halo mass for high-mass halos using a sample of galaxy clusters with accurate measurements of stellar masses from optical and IR data and total masses from X-ray observations. We find that stellar mass of the brightest cluster galaxies (BCGs) scales as M*BCG\propto M500^a_BCG with the best fit slope of a_BCG~0.35+-0.1 and scatter of M*BCG at a fixed M500 of ~0.2 dex. We show that M*-M relations from abundance matching or halo modelling reported in recent studies underestimate stellar masses of BCGs by a factor of ~2-4, because these studies used stellar mass functions (SMF) based on photometry that severely underestimates the outer surface brightness profiles of massive galaxies. We show that M*-M relation derived using abundance matching with the recent SMF calibration by Bernardi et al. (2013) based on improved photometry is in a much better agreement with the relation we derive. The total stellar mass of galaxies correlates with total mass M500 with the slope of \approx 0.6+-0.1 and scatter of 0.1 dex. This indicates that efficiency with which baryons are converted into stars decreases with increasing cluster mass. We show that for a fixed choice of the initial mass function (IMF) total stellar fraction in clusters is only a factor of ~3-5 lower than the peak stellar fraction reached in M\approx 10^12 Msun halos, and only a factor of ~1.5-3 if the IMF becomes progressively more bottom heavy with increasing mass in early type galaxies, as indicated by recent observations. The larger normalization and slope of the M*-M relation derived in this study shows that the overall efficiency of star formation in massive halos is suppressed much less than was thought before and that feedback and associated suppression of star formation in massive halos should be weaker than assumed in most of the current semi-analytic models and simulations.

Bio-optical Properties of Cyanobacteria Blooms in Western Lake Erie

There is a growing use of remote sensing observations for detecting and quantifying freshwater cyanobacteria populations, yet the inherent optical properties of these communities in natural settings, fundamental to bio-optical algorithms, are not well known. Towards bridging this knowledge gap, we measured a full complement of optical properties in western Lake Erie during cyanobacteria blooms in the summers of 2013 and 2014. Our measurements focus attention on the optical uniqueness of cyanobacteria blooms, which have consequences for remote sensing and bio-optical modeling. We found the cyanobacteria blooms in the western basin during our field work were dominated by Microcystis, while the waters in the adjacent central basin were dominated by Planktothrix. Chlorophyll concentrations ranged from 1 to over 135 ${\mu}g/L$ across the study area with the highest concentrations associated with Microcystis in the western basin. We observed large, amorphous colonial Microcystis structures in the bloom area characterized by high phytoplankton absorption and high scattering coefficients with a mean particle backscatter ratio at 443nm greater than 0.03, which is higher than other plankton types and more comparable to suspended inorganic sediments. While our samples contained mixtures of both, our analysis suggests high contributions to the measured scatter and backscatter coefficients from cyanobacteria. Our measurements provide new insights into the optical properties of cyanobacteria blooms, and indicate that current semi-analytic models are likely to have problems resolving a closed solution in these types of waters as many of our observations are beyond the range of existing model components. We believe that different algorithm or model approaches are needed for these conditions, specifically for phytoplankton absorption and particle backscatter components. From a remote sensing perspective, this presents a challenge not only in terms of a need for new algorithms, but also for determining when to apply the best algorithm for a given situation. These results are new in the sense that they represent a complete description of the optical properties of freshwater cyanobacteria blooms, and are likely to be representative of bloom conditions for other systems containing Microcystis cells and colonies.

A hybrid semi-analytical model for production from heterogeneous tight oil reservoirs with fractured horizontal well

Fracture networks induced by hydraulic fracturing are highways for fluid flow into the horizontal wellbore in tight formations. Pressure and rate transient responses of fractured horizontal wells in a heterogeneous reservoir are commonly simulated with numerical models by fined grids around the fractures. An alternative to full-scale numerical simulation in heterogeneous formations has been the use of semi-analytical methods for relatively simple forms of heterogeneity, such as composite and compartmental reservoirs. However, flow within the fracture networks is not considered in current semi-analytical models. This paper presents an efficient hybrid method for modeling fluid flow in fractured heterogeneous reservoirs. In this approach, the reservoir is divided into locally homogenous blocks where bounded Green-function solution is employed and coupled at the boundaries between adjacent substructures of reservoir. Green-function solution is employed and coupled at the boundaries between adjacent substructures of reservoir. Locally dual porosity models are implemented to characterize the heterogeneity of small-scale natural fractures, and large-scale fractures are represented explicitly by discrete fracture models. The flow within fracture networks is solved via the finite element method. With a simple direct discretization of the fractures and boundaries, the proposed hybrid model is shown to accurately capture the flow behavior with high computational efficiency. The validation of the approach is demonstrated in comparison to numerical solutions in heterogeneous reservoirs. On the basis of the model, detailed analysis of the flow behavior of a fractured horizontal production well in heterogeneous reservoir are provided. Finally, a field case is investigated to highlight the applicability and computational convenience of the proposed method.

A local leaky-box model for the local stellar surface density–gas surface density–gas phase metallicity relation

We revisit the relation between the stellar surface density, the gas surface density, and the gas-phase metallicity of typical disk galaxies in the local Universe with the SDSS-IV/MaNGA survey, using the star formation rate surface density as an indicator for the gas surface density. We show that these three local parameters form a tight relationship, confirming previous works (e.g., by the PINGS and CALIFA surveys), but with a larger sample. We present a new local leaky-box model, assuming star formation history and chemical evolution is localized except for outflowing materials. We derive closed-form solutions for the evolution of stellar surface density, gas surface density and gas-phase metallicity, and show that these parameters form a tight relation independent of initial gas density and time. We show that, with canonical values of model parameters, this predicted relation match the observed one well. In addition, we briefly describe a pathway to improving the current semi-analytic models of galaxy formation by incorporating the local leaky-box model in the cosmological context, which can potentially explain simultaneously multiple properties of Milky Way-type disk galaxies, such as the size growth and the global stellar mass-gas metallicity relation.

On the physical origin of galactic conformity

Correlations between the star formation rates (SFRs) of nearby galaxies (so-called galactic conformity) have been observed for projected separations up to 4 Mpc, an effect not predicted by current semi-analytic models. We investigate correlations between the mass accretion rates (dMvir/dt) of nearby halos as a potential physical origin for this effect. We find that pairs of host halos "know about" each others' assembly histories even when their present-day separation is greater than thirty times the virial radius of either halo. These distances are far too large for direct interaction between the halos to explain the correlation in their dMvir/dt. Instead, halo pairs at these distances reside in the same large-scale tidal environment, which regulates dMvir/dt for both halos. Larger halos are less affected by external forces, which naturally gives rise to a mass dependence of the halo conformity signal. SDSS measurements of galactic conformity exhibit a qualitatively similar dependence on stellar mass, including how the signal varies with distance. Based on the expectation that halo accretion and galaxy SFR are correlated, we predict the scale-, mass- and redshift-dependence of large-scale galactic conformity, finding that the signal should drop to undetectable levels by z > 1. These predictions are testable with current surveys to z ~ 1; confirmation would establish a strong correlation between dark matter halo accretion rate and central galaxy SFR.

The clustering of galaxies as a function of their photometrically estimated atomic gas content

We introduce a new photometric estimator of the HI mass fraction (M_HI/M_*) in local galaxies, which is a linear combination of four parameters: stellar mass, stellar surface mass density, NUV-r colour, and g-i colour gradient. It is calibrated using samples of nearby galaxies (0.025<z<0.05) with HI line detections from the GASS and ALFALFA surveys, and it is demonstrated to provide unbiased M_HI/M_* estimates even for HI-rich galaxies. We apply this estimator to a sample of ~24,000 galaxies from the SDSS/DR7 in the same redshift range. We then bin these galaxies by stellar mass and HI mass fraction and compute projected two point cross-correlation functions with respect to a reference galaxy sample. Results are compared with predictions from current semi-analytic models of galaxy formation. The agreement is good for galaxies with stellar masses larger than 10^10 M_sun, but not for lower mass systems. We then extend the analysis by studying the bias in the clustering of HI-poor or HI-rich galaxies with respect to galaxies with normal HI content on scales between 100 kpc and ~5 Mpc. For the HI-deficient population, the strongest bias effects arise when the HI-deficiency is defined in comparison to galaxies of the same stellar mass and size. This is not reproduced by the semi-analytic models, where the quenching of star formation in satellites occurs by "starvation" and does not depend on their internal structure. HI-rich galaxies with masses greater than 10^10 M_sun are found to be anti-biased compared to galaxies with "normal" HI content. Interestingly, no such effect is found for lower mass galaxies.

THE IMPACT OF GAS STRIPPING AND STELLAR MASS LOSS ON SATELLITE GALAXY EVOLUTION

Current semi-analytic models (SAMs) of galaxy formation over-predict the fraction of passive small late-type satellite galaxies in dense environments by a factor of two to three. We hypothesize that this is due to inaccurate prescriptions on cold gas evolution. In the hope of solving this problem we apply detailed prescriptions on the evolution of diffuse hot gases in satellites and on stellar mass loss, both of which are critical to model cold gas evolution. We replace the conventional shock-heating motivated instant stripping with a realistic gradual prescription based on ram pressure and tidal stripping. We also carefully consider stellar mass loss in our model. When both mechanisms are included, the fraction of passive late types matches the data much more closely. The satellite over-quenching problem is still present in small galaxies in massive haloes, however. In terms of the detectable residual star formation rates, gradual diffuse gas stripping appears to be much more important than stellar mass loss in our model. The implications of these results and other possibilities, such as redshift-dependent merging geometry and tidal disruption, are also discussed.

SPIDER - II. The Fundamental Plane of early-type galaxies in grizYJHK

We present a complete analysis of the Fundamental Plane of early-type galaxies (ETGs) in the nearby universe. The sample, as defined in paper I, comprises 39,993 ETGs located in environments covering the entire domain in local density (from field to cluster). We derive the FP of ETGs in the grizYJHK wavebands with a detailed discussion on fitting procedure, bias due to selection effects and bias due to correlated errors on r_e and mue as key factors in obtaining meaningful FP coefficients. Studying the Kormendy relation we find that its slope varies from g (3.44+-0.04) to K (3.80+-0.02) implying that smaller size ETGs have a larger ratio of optical/NIR radii than galaxies with larger re. We also examine the Faber-Jackson relation and find that its slope is similar for all wavebands, within the uncertainties, with a mean value of 0.198+-0.007. The variation of the FP coefficients for the magnitude selected sample from g through K amounts to 11%, negligible, and 10%, respectively. We find that the tilt of the FP becomes larger for higher Sersic index and larger axis ratios, independent of the waveband we measured the FP variables. This suggests that these variations are likely related to structural and dynamical differences of galaxian properties. We also show that the current semi-analytical models of galaxy formation reproduce very well the variation of age and metallicity of the stellar populations present in massive ETGs as a function of the stellar mass in these systems. In particular, we find that massive ETGs have coeval stellar pops with age varying only by a few % per decade in mass, while metallicity increases with stellar mass by 23% per mass decade.

Ray-tracing through the Millennium Simulation: Born corrections and lens-lens coupling in cosmic shear and galaxy-galaxy lensing

(abridged) We study the accuracy of various approximations to cosmic shear and weak galaxy-galaxy lensing and investigate effects of Born corrections and lens-lens coupling. We use ray-tracing through the Millennium Simulation to calculate various cosmic-shear and galaxy-galaxy-lensing statistics. We compare the results from ray-tracing to semi-analytic predictions. We find: (i) The linear approximation provides an excellent fit to cosmic-shear power spectra as long as the actual matter power spectrum is used as input. Common fitting formulae, however, strongly underestimate the cosmic-shear power spectra. Halo models provide a better fit to cosmic shear-power spectra, but there are still noticeable deviations. (ii) Cosmic-shear B-modes induced by Born corrections and lens-lens coupling are at least three orders of magnitude smaller than cosmic-shear E-modes. Semi-analytic extensions to the linear approximation predict the right order of magnitude for the B-mode. Compared to the ray-tracing results, however, the semi-analytic predictions may differ by a factor two on small scales and also show a different scale dependence. (iii) The linear approximation may under- or overestimate the galaxy-galaxy-lensing shear signal by several percent due to the neglect of magnification bias, which may lead to a correlation between the shear and the observed number density of lenses. We conclude: (i) Current semi-analytic models need to be improved in order to match the degree of statistical accuracy expected for future weak-lensing surveys. (ii) Shear B-modes induced by corrections to the linear approximation are not important for future cosmic-shear surveys. (iii) Magnification bias can be important for galaxy-galaxy-lensing surveys.

Dynamical Treatment of Virialization Heating in Galaxy Formation

In a hierarchical picture of galaxy formation virialization continually transforms gravitational potential energy into kinetic energies of the baryonic and dark matter. For the gaseous component the kinetic, turbulent energy is transformed eventually into internal thermal energy through shocks and viscous dissipation. Traditionally this virialization and shock heating has been assumed to occur instantaneously, allowing an estimate of the gas temperature to be derived from the virial temperature defined from the embedding dark matter halo velocity dispersion. As the mass grows the virial temperature of a halo grows. Mass accretion hence can be translated into a heating term. We derive this heating rate from the extended Press Schechter formalism and demonstrate its usefulness in semianalytical models of galaxy formation. Our method explicitly conserves energy, unlike the previous impulsive heating assumptions. Our formalism can trivially be applied in all current semianalytical models as the heating term can be computed directly from the underlying merger trees. Our analytic results for the first cooling halos and the transition from cold to hot accretion are in agreement with numerical simulations.

Galaxy morphology and evolution from SWAN adaptive optics imaging

We present the results from adaptive optics (AO) assisted imaging in the Ks band of an area of 15 arcmin^2 for SWAN (Survey of a Wide Area with NACO). We derive the high resolution near-IR morphology of ~400 galaxies up to Ks~23.5 in the first 21 SWAN fields around bright guide stars, carefully taking into account the survey selection effects and using an accurate treatment of the anisoplanatic AO PSF. The detected galaxies are sorted into two morphological classes according to their Sersic index. The extracted morphological properties and number counts of the galaxies are compared with the predictions of different galaxy formation and evolution models, both for the whole galaxy population and separately for late-type and early-type galaxies. This is one of the first times such a comparison has been done in the near-IR, as AO observations and accurate PSF modeling are needed to obtain reliable morphological classification of faint field galaxies at these wavelengths. For early-type galaxies we find that a pure luminosity evolution model, without evidence for relevant number and size evolution, better reproduces the observed properties of our Ks-selected sample than current semi-analytic models based on the hierarchical picture of galaxy formation. In particular, we find that the observed flattening of elliptical galaxy counts at Ks~20 is quantitatively in good agreement with the prediction of the pure luminosity evolution model that was calculated prior to the observation. For late-type galaxies, while both models are able to reproduce the number counts, we find some hints of a possible size growth. These results demonstrate the unique power of AO observations to derive high resolution details of faint galaxies' morphology in the near-IR and drive studies of galaxy evolution.

SpitzerObservations ofz∼ 3 Lyman Break Galaxies: Stellar Masses and Mid‐Infrared Properties

We describe the spectral energy distributions (SEDs) of Lyman break galaxies (LBGs) at z ~ 3, using deep mid-infrared and optical observations of the extended Groth strip, obtained with IRAC and MIPS on board Spitzer and from the ground, respectively. We focus on LBGs with detections at all four IRAC bands, in particular the 26 galaxies with IRAC 8 μm band (rest-frame K-band) detections. We use stellar population-synthesis models and probe the stellar content of these galaxies. Based on best-fit continuous star formation models, we derive estimates of the stellar mass for these LBGs. As in previous studies, we find that a fraction of LBGs have very red colors and large estimated stellar masses (M_* > 5 × 10^(10) M_⊙); the current Spitzer data allow us, for the first time, to study these massive LBGs in detail. We discuss the link between these LBGs and submillimeter-luminous galaxies, and we find that the number density of these massive LBGs at high redshift is higher than predicted by current semianalytic models of galaxy evolution.

SPIFFI Observations of the Starburst SMM J14011+0252:Already Old, Fat, and Rich by z =2.565

Using the SPectrometer for Infrared Faint Field Imaging on the ESO Very Large Telescope, we have obtained J-, H-, and K-band integral field spectroscopy of the luminous submillimeter galaxy SMM J140110252. z p 2.565 A global spectrum reveals the brighter of this spatially resolved system’s two components as an intense starburst that is remarkably old, massive, and metal-rich for the early epoch at which it is observed. We see a strong Balmer break implying a ≥100 Myr timescale for continuous star formation as well as nebular emission-line ratios implying a supersolar oxygen abundance on large spatial scales. Overall, the system is rapidly converting a large baryonic mass into stars over the course of only a few hundred megayears. Our study thus adds new arguments to the growing evidence that submillimeter galaxies are more massive than Lyman break galaxies and more numerous at high redshift than predicted by current semianalytic models of galaxy evolution. Subject headings: galaxies: abundances — galaxies: evolution — galaxies: formation

Observational Tests of the Galaxy Formation Process

The mutual feedback between star formation and nuclear activity in large spheroidal galaxies may be a key ingredient to overcome several difficulties plaguing current semi-analytic models for galaxy formation. We discuss some observational implications of the model by Granato et al. (2003) for the co-evolution of galaxies and active nuclei at their centers and stress the potential of the forthcoming surveys of the Sunyaev-Zeldovich effect on arcminute scales, down to $\mu$K levels, to investigate the early galaxy formation phases, difficult to access by other means.

Near-Infrared Bright Galaxies at z 2. Entering the Spheroid Formation Epoch?

Spectroscopic redshifts have been measured for nine K-band luminous galaxies at 1.7 < z < 2.3, selected with Ks < 20 in the K20 survey region of the Great Observatories Origins Deep Survey (GOODS) area. Star formation rates (SFRs) of ~100-500 M? yr-1 are derived when dust extinction is taken into account. The fitting of their multicolor spectral energy distributions indicates stellar masses of M 1011 M? for most of the galaxies. Their rest-frame UV morphology is highly irregular, suggesting that merging-driven starbursts are going on in these galaxies. Morphologies tend to be more compact in the near-IR, a hint for the possible presence of older stellar populations. Such galaxies are strongly clustered, with seven out of nine belonging to redshift spikes, which indicates a correlation length of r0 ~ 9-17 h-1 Mpc (1 ? range). Current semianalytical models of galaxy formation appear to underpredict by a large factor (30) the number density of such a population of massive and powerful starburst galaxies at z ~ 2. The high masses and SFRs, together with the strong clustering, suggest that at z ~ 2 we may have started to explore the major formation epoch of massive early-type galaxies.

The Evolution of the Galaxy Luminosity Function: Theoretical Predictions vs. Observations

We show that the canonical prescriptions adopted by current semi-analytic models (SAMs) of hierarchical galaxy formation lead to luminosity functions (LFs) too steep when compared with existing data (obtained from deep multicolor surveys in the HDF-N, HDF-S, NTT-DF in rest-frame B and UV (1700 A) bands) at redshifts z > 1; the discrepancy grows to a factor ~ 8 at z ≈ 3. Such result is robust with respect to different recipes for the feedback if this is assumed to arise from the effect of Supernovae contained in the galaxies. When the depletion of satellite galaxies in common haloes due to binary aggregations is taken into account, the discrepancy of SAM predictions with the observed LFs at z > 1 and at z ~ 3 is appreciably reduced. At z ≈ 0 the effect of binary aggregations is to yield a flatter LF for −20 −16.

The connection between spheroidal galaxies and QSOS

In view of the extensive evidence of tight inter-relationships between spheroidal galaxies (and galactic bulges) with massive black holes hosted at their centers, a consistent model must deal jointly with the evolution of the two components. We describe one such model, which successfully accounts for the local luminosity function of spheroidal galaxies, for their photometric and chemical properties, for deep galaxy counts in different wavebands, including those in the (sub)-mm region which proved to be critical for current semi-analytic models stemming from the standard hierarchical clustering picture, for clustering properties of SCUBA galaxies, of EROs, and of LBGs, as well as for the local mass function of massive black holes and for quasar evolution. Predictions that can be tested by surveys carried out by SIRTF are presented.

Analytical Modelling of Galaxy Formation

We present an analytical model of galaxy formation in hierarchical cosmogonies with new prescriptions for the clustering of dark matter halos, their internal structure, and the modelling of galaxies. These improvements with respect to current semi-analytical models allows us, respectively, to follow more accurately the evolution of halos, to study the spatial segregation of galactic properties within clusters, and to obtain more confident predictions on the Tully-Fisher and the Fundamental Plane relations.