bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Age-Redshift Relation For LRGs
Authors: Liu Gaochao , Lu Youjun , Chen Xuelei , Zhao Yongheng , Du Wei , Meng Xianmin 
Published: July 2013

AbstractThe relative age of galaxies at different redshifts can be used to infer the Hubble parameter and put constraints on cosmological models. We select 23,883 quiescent luminous red galaxies (LRGs) from the SDSS DR7, dividing them into four sub-samples according to their velocity dispersions. Each sub-sample was further divided into 12 redshift bins. The spectra of the LRGs in each redshift and velocity bin were co-added. Adopting the GalexEV/SteLib model, we estimate the mean ages of the LRGs from these combined spectra by the full-spectrum fitting method and find it is consistent with the well known “downsizing” formation of galaxies. Based on the age–redshift relation, we further estimate the Hubble parameter.
Discriminating Quasars from Stars Based on SDSS and UKIDSS Databases
Authors: Ma He , Zhang Yanxia , Zhao Yongheng , Zhang Bo 
Published: July 2013

AbstractIn this work, two different algorithms: Linear Discriminant Analysis (LDA) and Support Vector Machines (SVMs) are combined for the classification of unresolved sources from SDSS DR8 and UKIDSS DR8. The experimental result shows that this joint approach is effective for our case.
Studying Luminous Red Galaxies to probe H(z) at high redshift
Authors: Ratsimbazafy A. , Cress C. , Crawford S. ,   SCALPEL team
Published: July 2013

AbstractLuminous Red Galaxies (LRGs) have old, red stellar populations often interpreted as evidence of a formation scenario in which these galaxies form in a single intense burst of star formation at high redshift. By measuring the average age of LRGs at two different redshifts, one can potentially measure the redshift interval corresponding to a time interval and thus measure the Hubble parameter H(z) ≈ −(1 + z)−1 Δ z/Δt (as in Jimenez & Loeb). The goal of this project is to measure directly the expansion rate of the universe at the redshift range 0.1 < z < 1.0 within 3% precision. We explore the age-dating of Sloan Digital Sky Survey LRGs using the stellar population models of Lick absorption line indices after stacking spectra in redshift bins to increase the signal-to-noise. We also use the method of full spectral fitting to measure the ages of LRGs observed with the Southern Africa Large Telescope (SALT).
The hierarchical evolution of Brightest Cluster Galaxies: red galaxies in a young universe
Authors: Tonini Chiara 
Published: July 2013

AbstractWe investigate the evolution of Brightest Cluster Galaxies (BCGs) from redshift z ~ 1.6 to z = 0. We upgrade the hierarchical semi-analytic model of Croton et al. (2006) with a new spectro-photometric model that produces realistic galaxy spectra, making use of the Maraston (2005) stellar populations and a new recipe for the dust extinction. We compare the model predictions of the K-band luminosity evolution and the J-K, V-I and I-K colour evolution with a series of datasets, including Collins et al. (Nature, 2009) who argued that semi-analytic models based on the Millennium simulation cannot reproduce the red colours and high luminosity of BCGs at z > 1. We show instead that the model is well in range of the observed luminosity and correctly reproduces the colour evolution of BCGs in the whole redshift range up to z ~ 1.6. We argue that the success of the semi-analytic model is in large part due to the implementation of a more sophisticated spectro-photometric model. An analysis of the model BCGs shows an increase in mass by a factor 2-3 since z ~ 1, and star formation activity down to low redshifts. While the consensus regarding BCGs is that they are passively evolving, we argue that this conclusion is affected by the degeneracy between star formation history and stellar population models used in SED-fitting, and by the inefficacy of toy-models of passive evolution to capture the complexity of real galaxies, especially those with rich merger histories like BCGs. Following this argument, we also show that in the semi-analytic model, the BCGs show a realistic mix of stellar populations, and that these stellar populations are mostly old. In addition, the age-redshift relation of the model BCGs follows that of the Universe, meaning that given their merger history and star formation history, the ageing of BCGs is always dominated by the ageing of their stellar populations. In a ΛCDM Universe, we define such evolution as ‘passive in the hierarchical sense’.
A Possible Stream of Accreted Globular Clusters in M 31
Authors: Yuan H.-B. 
Published: July 2013

AbstractGlobular clusters (GCs) are excellent tracers for the formation, assembly and evolutionary history of their host galaxies. However, their origin and their role in galaxy evolution are still unclear. There are accumulating evidences that a significant fraction of GCs in massive galaxies (e.g., M 31) are accreted during their assembly history (e.g., Mackey et al. 2010). In this contribution, we report the discovery of a possible stream of accreted GCs in M 31 using data from the literature. Unlike previous substructures of GCs identified as clumps in the phase and metallicity space (Ashman, Keith & Christina 1993), the members of this stream are widely spread but tightly correlated in the position-velocity space (see Fig. 1). The tight correlation suggests that they possibly follow very similar orbits. A number of stellar streams have been discovered in the outer halo of M 31 (e.g., Ibata et al. 2001; McConnachie et al. 2009), one of which may be physically associated with the GC stream. If the association is established, it will not only provide a key evidence for accretion origins of some GCs in M 31, but also place a strong constraint on the mass distribution of M 31.
Supermassive black holes: Coevolution (or not) of black holes and host galaxies
Authors: Kormendy John 
Published: July 2013

AbstractSupermassive black holes (BHs) have been found in 75 galaxies by observing spatially resolved dynamics. The Hubble Space Telescope (HST) revolutionized BH work by advancing the subject from its ‘proof of concept’ phase into quantitative studies of BH demographics. Most influential was the discovery of a tight correlation between BH masses M• and the velocity dispersions σ of stars in the host galaxy bulge components at radii where the stars mostly feel each other and not the BH. Together with correlations between M• and bulge luminosity, with the ‘missing light’ that defines galaxy cores, and with numbers of globular clusters, this has led to the conclusion that BHs and bulges coevolve by regulating each other's growth. This simple picture with one set of correlations for all galaxies dominated BH work in the past decade.New results are now replacing the above, simple story with a richer and more plausible picture in which BHs correlate differently with different kinds of galaxy components. BHs with masses of 105—106M⊙ live in some bulgeless galaxies. So classical (merger-built) bulges are not necessary equipment for BH formation. On the other hand, while they live in galaxy disks, BHs do not correlate with galaxy disks or with disk-grown pseudobulges. They also have no special correlation with dark matter halos beyond the fact that halo gravity controls galaxy formation. This leads to the suggestion that there are two modes of BH feeding, (1) local, secular and episodic feeding of small BHs in largely bulgeless galaxies that involves too little energy feedback to drive BH–host-galaxy coevolution and (2) global feeding in major galaxy mergers that rapidly grows giant BHs in short-duration events whose energy feedback does affect galaxy formation. After these quasar-like phases, maintenance-mode BH feedback into hot, X-ray-emitting gas continues to have a primarily negative effect in preventing late-time star formation when cold gas or gas-rich galaxies get accreted. Finally, the highest-mass galaxies inherit coevolution effects from smaller galaxies; the tightness of their BH correlations is caused mainly by averaging during dissipationless major mergers.
Hot Gas and AGN Feedback in Galaxies and Nearby Groups
Authors: Jones Christine , Forman William , Bogdan Akos , Randall Scott , Kraft Ralph , Churazov Eugene 
Published: July 2013

AbstractMassive galaxies harbor a supermassive black hole at their centers. At high redshifts, these galaxies experienced a very active quasar phase, when, as their black holes grew by accretion, they produced enormous amounts of energy. At the present epoch, these black holes still undergo occasional outbursts, although the mode of their energy release is primarily mechanical rather than radiative. The energy from these outbursts can reheat the cooling gas in the galaxy cores and maintain the red and dead nature of the early-type galaxies. These outbursts also can have dramatic effects on the galaxy-scale hot coronae found in the more massive galaxies. We describe research in three areas related to the hot gas around galaxies and their supermassive black holes. First we present examples of galaxies with AGN outbursts that have been studied in detail. Second, we show that X-ray emitting low-luminosity AGN are present in 80% of the galaxies studied. Third, we discuss the first examples of extensive hot gas and dark matter halos in optically faint galaxies.
Quasar activity in the neighbor Universe
Authors: Falomo R. , Bettoni D. , Karhunen K. , Kotilainen J. , Uslenghi M. 
Published: July 2013

AbstractWe investigate the properties of the galaxies hosting quasars in ~400 low redshift (z < 0.5) SDSS QSO that are in the “Stripe 82” sky area. For this region deep (r ~ 22.4 mag) u, b, v, r and i images are available and allow us to study both the host galaxies and the Mpc scale environments. This sample outnumbers previous studies of low-z QSOs. We present preliminary results of the properties of quasars activity and in particular we focus on the relationships among host galaxy luminosity, black hole mass, radio emission and the surrounding galaxy environments. We select from the SDSS - QSO Catalogue all the QSOs in the range of redshift 0.1<z<0.5 and in the Stripe82 region. This gives a total of 416 QSO. In this sample we are dominated by radio quiet quasars (about 5% are radio loud). In Fig. 1 we report the distribution of QSO in the plane redshift-MR (H0 = 70). The mean redshift of the sample is <z> = 0.39 and the average absolute magnitude is: <Mi> = −22.68. We implemented an automated procedure using AIDA (Uslenghi & Falomo 2011) to decompose the QSO images into nucleus and host galaxy luminosity. After masking of all contaminating sources in the field a 2D fitting is performed using PSF + galaxy model. In Fig. 1 we show an example of a QSO image in the sample and the distribution of the host galaxy absolute magnitude of the resolved objects.
Galaxy spectra from the UV to the mid-IR
Authors: Brown Michael J. I. , Moustakas John , Smith J.-D. T. , da Cunha Elisabete , Imanishi Masatoshi , Armus Lee , Brandl Bernhard R. 
Published: July 2013

AbstractTemplates and models of galaxy spectra are often essential for determining the physical properties of galaxies. Many commonly used templates have large systematic errors, which significantly impact photometric redshifts and k-corrections. We present a new library of 110 galaxy template spectra spanning from the ultraviolet to the mid-infrared. The templates combine optical, Spitzer and Akari spectra with MAGPHYS models, all normalised and verified with matched aperture photometry. Our library contains more galaxies, spans a broader range of colours and has smaller systematic errors than previous libraries of galaxy spectra.
The stellar populations of massive galaxies in the local Universe
Authors: McDermid Richard M. 
Published: July 2013

AbstractI present a brief review of the stellar population properties of massive galaxies, focusing on early-type galaxies in particular, with emphasis on recent results from the ATLAS3D Survey. I discuss the occurence of young stellar ages, cold gas, and ongoing star formation in early-type galaxies, the presence of which gives important clues to the evolutionary path of these galaxies. Consideration of empirical star formation histories gives a meaningful picture of galaxy stellar population properties, and allows accurate comparison of mass estimates from populations and dynamics. This has recently provided strong evidence of a non-universal IMF, as supported by other recent evidences. Spatially-resolved studies of stellar populations are also crucial to connect distinct components within galaxies to spatial structures seen in other wavelengths or parameters. Stellar populations in the faint outer envelopes of early-type galaxies are a formidable frontier for observers, but promise to put constraints on the ratio of accreted stellar mass versus that formed ‘in situ’ - a key feature of recent galaxy formation models. Galaxy environment appears to play a key role in controlling the stellar population properties of low mass galaxies. Simulations remind us, however, that current day galaxies are the product of a complex assembly and environment history, which gives rise to the trends we see. This has strong implications for our interpretation of environmental trends.
Stellar population gradients in brightest cluster galaxies
Authors: Loubser S. I. , Sánchez-Blázquez P. 
Published: July 2013

AbstractWe present the stellar population and velocity dispersion gradients for a sample of 24 brightest cluster galaxies (BCGs) in the nearby Universe for which we have obtained high quality long-slit spectra at the Gemini telescopes. With the aim of studying the possible connection between the formation of the BCGs and their host clusters, we explore the relations between the stellar population gradients and properties of the host clusters, as well as the possible connections between the stellar population gradients and other properties of the galaxies. We find mean stellar population gradients (negative Δ[Z/H]/log r gradient of − 0.285 ± 0.064; small positive Δlog(age)/log r gradient of +0.069 ± 0.049; and null Δ[E/Fe]/log r gradient of -0.008 ± 0.032), that are consistent with those of normal massive elliptical galaxies. However, we find a trend between metallicity gradients and velocity dispersion (with a negative slope of − 1.616 ± 0.539), that is not found for the most massive ellipticals. Furthermore, we find trends between the metallicity gradients and K-band luminosities (with a slope of 0.173 ± 0.081) as well as the distance from the BCG to the X-ray peak of the host cluster (with a slope of − 7.546 ± 2.752). The latter indicates a possible relation between the formation of the cluster and that of the central galaxy.
The stellar metallicity distribution in intermediate-latitude fields
Authors: Peng Xiyan , Du Cuihua , Wu Zhenyu 
Published: July 2013

AbstractBased on BATC and SDSS photometric data, we adopt the spectral energy distribution (SED) fitting method to evaluate stellar metallicities in the Galaxy. We find that the mean metallicity shifts from metal-rich to metal-poor with the increase of distance from the Galactic Centre.
Plasma diagnostics of emission-line galaxies in SDSS
Authors: Zhang Zhitai , Liang Yanchun , Hammer François 
Published: July 2013

AbstractWe analyse a sample of 15,019 narrow emission-line galaxies, i.e. Seyferts, LINERs, composites and star-forming galaxies, from SDSS DR7 to study the differences between the different emission-line classes. We report two clear sequences of electron temperature (Te) and density (ne): Te-LINER ≳ Te-composite > Te-Seyfert > Te-star-forming and ne-Seyfert ≳ ne-LINER > ne-composite > ne-star-forming. General transitions of ne and Te from central regions to disks are quantitatively confirmed.
Assembly Histories and Observational Properties of Simulated Early-type Galaxies
Authors: Johansson Peter H. 
Published: July 2013

AbstractWe demonstrate that massive simulated galaxies assemble in two phases, with the initial growth dominated by compact in situ star formation, whereas the late growth is dominated by accretion of old stars formed in subunits outside the main galaxy. We also show that 1) gravitational feedback strongly suppresses late star formation in massive galaxies contributing to the observed galaxy colour bimodality that 2) the observed galaxy downsizing can be explained naturally in the two-phased model and finally that 3) the details of the assembly histories of massive galaxies are directly connected to their observed kinematic properties.
Probing the mass assembly of massive nearby galaxies with deep imaging
Authors: Duc P.–A. , Cuillandre J.-C. , Alatalo K. , Blitz L. , Bois M. , Bournaud F. , Bureau M. , Cappellari M. , Côté P. , Davies R. L. , Davis T. A. , de Zeeuw P. T. , Emsellem E. , Ferrarese L. , Ferriere E. , Gwyn S. , Khochfar S. , Krajnovic D. , Kuntschner H. , Lablanche P.-Y. , McDermid R. M. , Michel-Dansac L. , Morganti R. , Naab T. , Oosterloo T. , Sarzi M. , Scott N. , Serra P. , Weijmans A. , Young L. M. 
Published: July 2013

AbstractAccording to a popular scenario supported by numerical models, the mass assembly and growth of massive galaxies, in particular the Early-Type Galaxies (ETGs), is, below a redshift of 1, mainly due to the accretion of multiple gas–poor satellites. In order to get observational evidence of the role played by minor dry mergers, we are obtaining extremely deep optical images of a complete volume limited sample of nearby ETGs. These observations, done with the CFHT as part of the ATLAS3D, NGVS and MATLAS projects, reach a stunning 28.5 – 29 mag.arcsec−2 surface brightness limit in the g' band. They allow us to detect the relics of past collisions such as faint stellar tidal tails as well as the very extended stellar halos which keep the memory of the last episodes of galactic accretion. Images and preliminary results from this on-going survey are presented, in particular a possible correlation between the fine structure index (which parametrizes the amount of tidal perturbation) of the ETGs, their stellar mass, effective radius and gas content.
Economic and Social Implications of Regulating Alcohol Availability in Grocery Stores
Authors: Rickard Bradley J. , Costanigro Marco , Garg Teevrat 
Published: July 2013

AbstractThe availability of alcoholic beverages in grocery stores varies across the United States due to state‐level regulations. Recently there have been a number of controversial legislative proposals to expand the distribution of certain alcoholic beverages, most notably wine. Our econometric results show that, holding constant the total quantity of alcohol consumed, a higher share of wine correlates with lower traffic fatality rates, while the opposite is true for beer. These findings suggest that arguments against the wider distribution of wine as an approach to reduce social problems may not be fully justified.
A new theoretical analysis of deindustrialisation
Authors: Tregenna Fiona 
Published: July 2013

Abstract
The analysis of deindustrialisation has been led by heterodox economists, especially those in the structuralist and Kaldorian traditions, based on a conception of sectoral specificity and the role of manufacturing in growth. Sectors are not the units of Marxian economic analysis, but thinking through the meaning of sectors in Marxian terms allows for an analysis of the meaning and implications of a change in sectoral structure. Deindustrialisation is the sectoral shift that has been most prominent in recent decades and which is likely to have significant implications for the future of capitalism. This article develops an original Marxian theorisation of deindustrialisation. This conceptualisation includes a distinction between two forms of deindustrialisation. As well as taking into account changes in sectoral structure, the proposed typology considers whether such changes are associated with a shift between those activities that produce surplus value and those that do not or only a shift in the composition of surplus-value-producing activities. The distinction between different forms of deindustrialisation allows for an arguably richer analysis of this phenomenon than in more narrowly sector-based approaches.
A New Somphospondylan Sauropod (Dinosauria, Titanosauriformes) from the Late Cretaceous of Ganzhou, Jiangxi Province of Southern China
Authors: Junchang LÜ , Laiping YI , Hui ZHONG , Xuefang WEI 
Published: July 2013

Abstract:A new somphospondylan sauropod (Dinosauria, Titanosauriformes): Gannansaurus sinensis gen. et sp. nov. from the Late Cretaceous Nanxiong Formation of Ganzhou Basin, Jiangxi Province of southern China is erected based on one nearly complete dorsal vertebra and a mid‐caudal vertebra. It is characterized by two centroprezygapophyseal lamina fossae; large, square‐shaped concavity formed by centroprezygapophyseal lamina and dorsal margin of the centrum; large infraparapophyseal fossa; three openings present within the large lateral concavity, which occupy 65% length of the centrum; the posterior centroparapophyseal lamina (PCPL) and the anterior centroparapophyseal lamina (ACPL) weakly developed; the posterior centrodiapophyseal lamina (PCDL) separated by an infradiapophyseal fossa into two branches dorsally; parapophyseal and diapophyseal laminae cross to form “K” configuration. It shares some characters with the Early Cretaceous form‐Euhelopus, indicating that it is more closely related to Euhelopus rather than to other titanosauriform sauropods. This means Gannansaurus may have a close phylogenetic relationship with Euhelopus.
A New Material of Lindera (Lauraceae) of the Late Pliocene from Tengchong, Yunnan and the Genus' Biogeography Significance
Authors: Kequn DAO , Junlin CHEN , Peihong JIN , Chong DONG , Yi YANG , Xiaohui XU , Jingyu WU , Sanping XIE , Zhicheng LIN , Bainian SUN 
Published: July 2013

Abstract:Lindera is a large genus of graceful, pleasantly scented and common native trees and shrubs of southern China and neighboring regions of SE Asia. There is a well‐documented Cenozoic fossil record not only in these regions but also from elsewhere. A new fossil leaf record has been found in diatomite beds from the Upper Pliocene Mangbang Formation of Tuantian, Tengchong County, Yunnan. The leaves are identified and assigned to Lindera acuminatissima K. Q. Dao et B. N. Sun sp. nov., by comparing their leaf architecture and epidermal characteristics with those of 51 extant Lauraceae species and with 15 known fossil Lindera taxa. The specimens have well‐preserved cuticles, with typical leaf architecture and epidermal characteristics of the Lauraceae, including entire leaf margin, intramarginal veins, basal ternate acrodromous primary veins, one‐cell trichome base, paracytic stomatal apparatus, sunken guard cells, subsidiary hardly staining cells and presence of oil cells. These characteristics are consistent with Lindera sect. Daphnidium but are different from reported fossil and extant species of Lindera. The cuticles of Lindera are fragile and delicate with only three Lindera fossils reported based on this tissue. In terms of paleobiogeography, the fossil record indicates that Lindera is distributed in high‐ to mid‐latitude regions of the Late Cretaceous to Paleocene northern hemisphere. Coincidentally, the records of Lindera located on both sides of the Bering Land Bridge possibly support the hypothesis that ancient plants extended via transcontinental exchanges through the Bering Corridor. In the Eocene, ancient Lindera spread to Europe through the Northern Degeer Route and the Southern Thulian Route. At the same time, ancient Lindera spread into Central Asia. Climatic changes and tectonization since the Neogene prevented the propagation of Lindera throughout Asia, North America and Europe, and hence the distribution areas have just regressed to the low‐latitude regions in Asia and North America. From the Paleogene to the Neogene, Lindera has changed its distribution by surviving extreme climate changes. Quaternary glaciations ultimately led to Lindera becoming extinct in Europe. The new record from Tengchong, Yunnan, with its lower latitude located in tropical and subtropical regions, indicates that Lindera has lived in those regions since the late Pliocene.