bluuebunny/crossref_metadata_2025_split huggingface dataset:
Selective and efficient extraction of recombinant proteins from the periplasm of Escherichia coli using low concentrations of chemicals
Authors: Jalalirad Reza 
Published: July 2013

Abstract
Experiments were conducted to determine chemicals at low concentrations, which can be utilized for selective release of periplasmic proteins. It was revealed that 80–100 % of the activity of alpha-amylase, beta-lactamase, and Fab D1.3 was retained in the presence of 0.05 and 0.1 % Triton X-100, 0.1 % Tween 20, 0.1 % DOC, 0.01 % BAC, 0.01 % CTAB, 10 mM EDTA, 1 mM and 10 mM DEA, 10 mM NTA, 0.1 and 1 % SHMP, 200 mM urea, 100–500 mM GndCl, and 1 % solvents (hexane, xylene, toluene, benzene, pyridine and isoamyl alcohol). Performance of these chemicals, recognized as generally safe, for selective release of proteins from the periplasm of Escherichia coli was investigated. DOC was a general and very efficient agent, and at concentrations as low as 0.05, 0.1, and 0.025 %, released beta-lactamase, alpha-amylase, and Fab D1.3 selectively with yield factors of 2.7, 2.3, and 3.6 times greater than osmotic shock procedure, respectively. EDTA (1 and 10 mM) discharged Fab D1.3 with efficiency more than osmotic shock (target protein yield of 110 and 138 %, correspondingly). Isoamyl alcohol (10 % v/v) was effective for periplasmic release of alpha-amylase and particularly Fab D1.3, with target protein yields of 75 and 168 %, respectively.
Removal of Copper(II) from a Concentrated Sulphate Medium by Cloud Point Extraction Using an N,N′‐Bis(salicylaldehyde)Ethylenediimine Di‐Schiff Base Chelating Ligand
Authors: Reffas Hasnia , Benabdallah Tayeb , Youcef Mohammed Hadj , Ilikti Hocine 
Published: July 2013

AbstractVarious chelating ligands have been investigated for the cloud point extraction of several metal ions. However, limited studies on the use of the Schiff base ligands have been reported. In this work, cloud point extraction behavior of copper(II) with N,N′‐bis(salicylaldehyde)Ethylenediimine Schiff base chelating ligand, (H2SALEN), was investigated in aqueous concentrated sulphate medium. The extraction process used is based on the formation of hydrophobic H2SALEN–copper(II) complexes that are solubilized in the micellar phase of a non‐ionic surfactant, i.e. ethoxylated (9.5EO) tert‐butylphenol. The copper(II) complexes are then extracted into the surfactant‐rich phase above cloud point temperature. Different parameters affecting the extraction process of Cu(II), such as equilibrium pH, extractant concentration, and non‐ionic surfactant concentration were explored. The extraction of Cu(II) was studied in the pH range of 2–11. The results obtained showed that it was profoundly influenced by the pH of the aqueous medium. The concentration factor, Cf, of about 17 with extraction efficiency of E % ≈100 was achieved. The stoichiometry of the extracted complex of copper(II) was ascertained by the Yoe–Jones method to give a composition of 1:1 (Cu:H2L). The optimum conditions of the extraction‐removal have been established as the following: (1) 1.86 × 10−3 mol/L ligand; (2) 3 wt% surfactant; (3) pH of 8 (4) 0.5 mol/L Na2SO4 and (5) temperature of 60 °C.
The Effect of Monoglyceride Addition on the Rheological Properties of Pistachio Spread
Authors: Shakerardekani Ahmad , Karim Roselina , Ghazali Hasanah Mohd , Chin Nyuk Ling 
Published: July 2013

AbstractPistachio nut (Pistacia vera L.) is one of the most delicious and nutritious nuts in the world. In this study, monoglycerides (0.0–1.5 %) as lipophilic emulsifiers were used to prevent oil separation in pistachio spread A (containing 50.0 % pistachio paste, 30.0 % icing sugar and 20.0 % red palm oil) and B (containing 58.3 % pistachio paste, 25.0 % icing sugar and 16.7 % red palm oil). Changes in rheological behavior of pistachio spreads were investigated. The highest work of shear (which indicates spreadability) was observed in Formulations A and B containing 1.5 % monoglycerides. Addition of emulsifier significantly (P < 0.05) influenced the consistency index (K), thixotropic area (A), yield stress (τ0) and coefficient correlation (R) of pistachio spreads. All the pistachio spreads that contained emulsifier exhibited a higher storage modulus (G′) than the loss modulus (G″).
A gene signature for late distant metastasis in breast cancer identifies a potential mechanism of late recurrences
Authors: Mittempergher Lorenza , Saghatchian Mahasti , Wolf Denise M. , Michiels Stefan , Canisius Sander , Dessen Philippe , Delaloge Suzette , Lazar Vladimir , Benz Stephen C. , Tursz Thomas , Bernards René , van't Veer Laura J. 
Published: July 2013

IntroductionBreast cancer risk of recurrence is known to span 20 years, yet existing prognostic signatures are best at predicting early recurrences (≤5 years). There is a critical need to identify those patients at risk of late‐relapse (>5 years), in order to select potential candidates for further treatment and to identify molecular targets for such treatment.MethodsA total of 252 breast primary tumors were selected at the Netherlands Cancer Institute from a retrospective series of ER+, HER2− breast cancer patients with a follow‐up of at least 10 years. Gene expression analysis was performed using Agilent 4x44K microarrays. Patients were classified in 3 groups: no relapse (M0); relapse before 5 years (M0‐5) or after 5 years (M5‐15). We assessed the correlation of clinico‐pathological variables with late Distant Metastases (DM). We divided the patient series into a training set of untreated patients (n = 140) and a test set of treated patients (n = 112), to investigate whether a gene‐signature or single genes could be identified for predicting late DM. Pathway level late DM correlates were identified using PARADIGM and DAVID.ResultsOf the clinico‐pathologic variables tested, only lymph node status associated with late DM. A 241‐gene signature developed on the NKI training set was able to classify M5‐15 patients in the test set with a sensitivity of 77% and a specificity of 33% (AUC 0.654). This signature showed enrichment in genes involved in immune response and extracellular matrix. An alternative analysis of individual genes identified CH25H as an independent predictor of distant metastasis in our patient series.ConclusionsWe identified a gene signature for late metastasis in breast cancer. Our data are consistent with a model in which suppressed anti‐tumoral immunity enables dormant tumor cells to re‐enter the cell cycle to form metastases in response to extrinsic events in the microenvironment.
Bat conservation in China: should protection of subterranean habitats be a priority?
Authors: Luo Jinhong , Jiang Tinglei , Lu Guanjun , Wang Lei , Wang Jing , Feng Jiang 
Published: July 2013

AbstractSubterranean environments are essential for the survival of many bat species and other cave fauna but these places are subject to increasing human disturbance. To examine the significance of subterranean habitats for the conservation of bats in China we surveyed bat species in 225 underground sites during 2003–2011. Our results show that 77% of bat species in China, including 30 nationally Endangered or Vulnerable species and nine endemic species, roost in caves and other subterranean habitats. The number of species in occupied roosts was 1–15. Almost 90% of the roosts surveyed contained signs of human disturbance, most of which was from recreational activities. One hundred and twenty-one roosts merit special concern because they harbour ≥ 6 species or > 1,000 individuals, or species of special concern (threatened or endemic species). Generally, larger roosts support more species and a greater abundance of bats than smaller roosts but there is no direct correlation between the presence of species of special concern and roost size. Disused tourist caves have significantly more bat species than other types of roosts. Our data demonstrate that roost disturbance by recreational activities has pronounced detrimental effects on the number of bat species and the presence of species of special concern. We discuss the social, economic and political issues that could adversely affect bat conservation in caves in China, and we recommend that protection of subterranean habitats should be a high priority for bat conservation.
Impact of the First Stars to the First Galaxy Formation
Authors: Chen Ke-Jung , Jeon Myoungwon , Greif Thomas , Bromm Volker , Heger Alexander 
Published: July 2013

AbstractWe present the results from our cosmological simulations of the first stages of galaxy formation. We use Gadget-2 (Springel 2005), modified to include detailed cooling, chemistry, and radiative transfer of primordial gas to study the impact of the first stars on galaxy formation. In contrast to previous work, we apply a realistic treatment of stellar feedback by using updated stellar models for the first stars. In this proceeding, we briefly summarize how stellar feedback from the first stars affects the primordial IGM inside the first galaxies.
Discovery of bright z ~ 7 galaxies in the UltraVISTA survey
Authors: Bowler Rebecca A. A. , Dunlop James S. , McLure Ross J. 
Published: July 2013

AbstractWe have exploited the new, deep, near-infrared Y,J,H,Ks UltraVISTA imaging of the COSMOS field, in tandem with deep optical and mid-infrared imaging, to conduct a new search for luminous galaxies at redshifts z ≃ 7. We have utilised this unique multi-wavelength dataset to select galaxy candidates at redshifts z > 6.5 by searching first for Y+J-detected objects which are undetected in the CFHT and HST optical data. This sample was then refined using a photometric redshift fitting code, enabling the rejection of lower-redshift galaxy contaminants and cool galactic M, L, T dwarf stars. The final result of this process is a small sample of (at most) ten credible galaxy candidates at z > 6.5 (from over 200,000 galaxies detected in the year-one UltraVISTA data). The new z ≃ 7 galaxies reported here are the first credible z ≃ 7 Lyman-break galaxies discovered in the COSMOS field and, as the most UV-luminous discovered to date at these redshifts, are prime targets for deep follow-up spectroscopy. We explore their physical properties, and briefly consider the implications of their inferred number density for the form of the galaxy luminosity function at z ≃ 7.
Evolution of the galaxy merger rate since z=2 from the UKIDSS Ultra-Deep Survey
Authors: Foucaud S. , Wang P.-W. , Almaini O. , Grützbauch R. , Hartley W. G. , Simpson C. , Conselice C. J. 
Published: July 2013

AbstractIt is now clear that the epoch when the Universe was half of its current age is a crucial period during which galaxies assembled their mass and evolved into the galaxies we observe in the local Universe. However, so far only very few direct studies of mass assembly in action, hence galaxy merging, were conducted over z=1 and usually relied on very small or biased samples. Based on very deep near infrared survey data, the latest UKIDSS-UDS DR8, combined with the optical data conducted by Subaru and CFHT and Spitzer IRAC observations, we explored the evolution of the merging rate up to z = 2, over the largest volume of the Universe at 0.4<z<2 ever sampled. The pair fraction is found to decrease by a factor of two during this period, and wet (gas rich) mergers dominate largely. The dry mergers are very rare, ruling it out as the main mechanism for the mass assembly of passive massive galaxies. Also while massive galaxies undergo a decrease of their pair fraction during this period, less massive systems follow an increase during the same period.
Clustering of EROs from UKIDSS DXS and Pan-STARRS PS1
Authors: Kim J.-W. , Edge A. C. , Wake D. A. , Gonzalez-Perez V. , Baugh C. M , Lacey C. G. 
Published: July 2013

AbstractWe have measured the angular two-point correlation function of EROs. The halo model is fitted to the observed clustering, and dark matter halo mass, bias and satellite fraction are estimated in three redshift bins. We also compare our results with the semi-analytical galaxy formation model. This work illustrates the power of clustering analysis in providing observational constraints on simulations.
Galaxies in most dense environments at redshift 1.4
Authors: Strazzullo V. 
Published: July 2013

AbstractAt a cosmic time when galaxy clusters start showing evidence of a still active galaxy population, the X-ray luminous, massive cluster XMMU J2235-2557 at z=1.39, already hosts massive, quiescent, early-type galaxies on a tight red sequence dominating the cluster core. XMMU J2235-2557 is among the most massive of the very distant clusters, which may explain the evolved status of the system itself, and of its host galaxy populations. It remains a unique laboratory to observe environment-biased galaxy evolution already 9 billion years ago.
The effects of binary stars on the colors of galaxies at z~2.0
Authors: Zhang Y. , Liu J. , Zhang F. 
Published: July 2013

AbstractUsing the Monte Carlo simulations and a set of theoretical galaxy templates, which are built on the Yunnan evolutionary population synthesis models with and without binary interactions, we compare the optical color-color (C-C) relations for passive and star-forming galaxies at redshift z~2.0, and study the effect of binary interactions on this relation. We find that the influence of binary interactions on the C-C relation is insignificant for passive galaxies at z~2.0.
The intriguing life of star-forming galaxies in the redshift range 1 ≤ z ≤ 2 using MASSIV
Authors: Amram P. , López-Sanjuan C. , Epinat B. , Contini T. , Vergani D. , Tasca L. , Le Fèvre O. , Garilli B. , Divoy C. , Queyrel J. , Kissler-Patig M. , Moultaka J. , Paioro L. , Tresse L. , Perret V. , Bournaud F. 
Published: July 2013

AbstractMASSIV (Mass Assembly Survey with SINFONI in VVDS) is an ESO large program which consists of 84 star-forming galaxies, spanning a wide range of stellar masses, observed with the IFU SINFONI on the VLT, in the redshift range 1 ≤ z ≤ 2. To be representative of the normal galaxy population, the sample has been selected from a well-defined, complete and representative parent sample. The kinematics of individual galaxies reveals that 58% of the galaxies are slow rotators, which means that a high fraction of these galaxies should probably be formed through major merger processes which might have produced gaseous thick or spheroidal structures supported by velocity dispersion rather than by rotation. Computations on the major merger rate from close pairs indicate that a typical star-forming galaxy underwent ~0.4 major mergers in the last ~9.5 Gyr, showing that merging is a major process driving mass assembly into the red sequence galaxies. These objects are also intriguing due to the fact that more than one galaxy over four is more metal-rich in its outskirts than in its center.
Spatially-Resolved View of High-Redshift Starbursts: the case of Sub-mm Galaxies
Authors: Menéndez-Delmestre Karín , Blain Andrew W. , Swinbank Mark , Smail Ian , Ivison Rob J. , Chapman Scott C. 
Published: July 2013

AbstractUltra-luminous infrared galaxies (LIR > 1012 L⊙) are locally rare, but appear to dominate the co-moving energy density at higher redshifts (z>2). Many of these are optically-faint, dust-obscured galaxies that have been identified by the detection of their thermal dust emission at sub-mm wavelengths. Multi-wavelength spectroscopic follow-up observations of these sub-mm galaxies (SMGs) have shown that they are massive (Mstellar ~ 1011 M⊙) objects undergoing intense star-formation (SFRs ~ 102−103 M⊙ yr−1) with a mean redshift of z ~ 2, coinciding with the epoch of peak quasar activity. The large fraction of AGNs in SMGs and the derived SMBH masses (M• < 108 M⊙) in these galaxies suggest that the submm phase may play an important role in the rapid growth of SMBHs. When both AGN and star-formation activity are present, long-slit spectroscopic techniques face difficulties in disentangling their contributions and may result in SFR and mass overestimates. We present an integral field view of the Hα emission in a sample of 3 SMGs at z~1.4–2.4 with the IFU instrument OSIRIS on Keck. Designed to be used with Laser Guide Star Adaptive Optics, OSIRIS allows a spatial resolution of up to 10× higher than what has been possible in previous seeing-limited studies of the ionized gas in these galaxies. Our main results are the following: (1) We detect multiple galactic-scale sub-components: the compact, broad Hα emission (FWHM >1000 km s−1) likely associated with an AGN, the more extended narrow-line Hα emission (FWHM ≲500 km s−1) of star-forming regions; the latter are dominated by multiple 1–2 kpc sized Hα-bright clumps, each contributing 1-25% of the total clump-integrated Hα emission. (2) We derive clump dynamical masses ~1–10×109M⊙, 1–2 orders of magnitude larger than the kpc-scaled stellar clumps uncovered in optically-selected z ~ 2 star-forming galaxies. (3) We determine high star-formation rate surface densities (ΣSFR~1–50 M⊙yr−1 kpc−2, after extinction correction), similar to local starbursts and luminous infrared galaxies. In contrast to these local environments, SMGs undergo such intense activity on significantly larger spatial scales as revealed by extended Hα emission over 4–16 kpc. (4) We find no evidence of ordered global motion as it would be found in a disk, but rather large velocity offsets (~ few × 100 km s−1) between the distinct stellar clumps. The merger interpretation is likely the most accurate scenario for the SMGs in our sample. However, the final test of whether an underlying disk structure is present will come from studies of the cold gas at the high spatial resolutions possible with ALMA.We refer the reader to Menéndez-Delmestre et al. (2012) for more details.
The evolution of galaxy sizes
Authors: Poggianti Bianca M. , Calvi Rosa , Bindoni Daniele , D'Onofrio Mauro , Moretti Alessia , Valentinuzzi Tiziano , Fasano Giovanni , Fritz Jacopo , De Lucia Gabriella , Vulcani Benedetta , Bettoni Daniela , Gullieuszik Marco , Omizzolo Alessandro 
Published: July 2013

AbstractWe present a study of galaxy sizes in the local Universe as a function of galaxy environment, comparing clusters and the general field. Galaxies with radii and masses comparable to high-z massive and compact galaxies represent 4.4% of all galaxies more massive than 3 × 1010M⊙ in the field. Such galaxies are 3 times more frequent in clusters than in the field. Most of them are early-type galaxies with intermediate to old stellar populations. There is a trend of smaller radii for older luminosity-weighted ages at fixed galaxy mass. We show the relation between size and luminosity-weighted age for galaxies of different stellar masses and in different environments. We compare with high-z data to quantify the evolution of galaxy sizes. We find that, once the progenitor bias due to the relation between galaxy size and stellar age is removed, the average amount of size evolution of individual galaxies between high- and low-z is mild, of the order of a factor 1.6.
Quenching star formation at intermediate redshifts: downsizing of the mass flux density in the green valley
Authors: Gonçalves Thiago S. , Martin D. Christopher , Menéndez-Delmestre Karín , Wyder Ted K. , Koekemoer Anton 
Published: July 2013

AbstractThe bimodality in galaxy properties has been observed at low and high redshift, with a clear distinction between star-forming galaxies in the blue cloud and passively evolving objects in the red sequence; the absence of galaxies with intermediate properties indicates that the quenching of star formation and subsequent transition between populations must happen rapidly. In this work, we present a study of over 100 transiting galaxies in the so-called “green valley” at intermediate redshifts (z ~ 0.8). By using very deep spectroscopy with the DEIMOS instrument at the Keck telescope, we are able to infer the star formation histories of these objects and measure the stellar mass flux density transiting from the blue cloud to the red sequence when the Universe was half its current age. Our results indicate that the process happened more rapidly, affecting more massive galaxies in the past, suggesting a top-down scenario whereby the massive end of the red sequence assembles first. This represents another aspect of downsizing, with the mass flux density moving towards smaller galaxies in recent times.
The Intriguing Life of Massive Galaxies: The Connections between αs, β and Merging
Authors: Peng Ying-jie , Lilly Simon J. , Renzini Alvio , Carollo Marcella 
Published: July 2013

AbstractIn this proceeding paper, we discuss the important underlying connections between the faint end slope αs of the stellar mass function of star-forming galaxies, the logarithmic slope β of the sSFR-mass relation and merging through the continuity approach, as we introduced in Peng et al. (2010, hereafter P10) and (2012, hereafter P12).
Massive galaxies: born as disks, dead as spheroids
Authors: Buitrago Fernando 
Published: July 2013

AbstractPresent day massive (Mstellar > 1011 M⊙) galaxies are composed mostly of early-type objects. To ascertain whether this was also the case at higher redshift, we have compiled over a thousand massive galaxies at 0 < z < 3 with HST imaging and spectroscopic redshifts for the majority of them. We have also analyzed using 3D spectroscopy another sample of 10 massive galaxies at z = 1.4. Both works highlight the progressive change between a late-type/peculiar nature at z > 2 and a predominance of early-type morphologies only since z = 1.
Which Galaxy Property Best Predicts Quiescence?
Authors: Leja Joel , van Dokkum Pieter ,   the 3D-HST Collaboration
Published: July 2013

AbstractIt is generally accepted that local elliptical galaxies assembled most of their mass in a burst of star formation between 1 < z < 3, yet today, their star formation has been almost entirely quenched. In order to constrain this quenching mechanism, we measure Hα line emission in galaxies sorted by multiple galaxy properties as a function of redshift to what galaxy parameter best predicts quiescence. This is done for samples of the most massive, most luminous, and galaxies with the highest velocity dispersion both locally (0.05 < z < 0.07 in the SDSS) and at high redshift (0.7 < z < 1.5 in 3D-HST). It is demonstrated through spectral stacking that velocity dispersion results in the lowest Hα line equivalent width both locally and at high redshift. The spatial distribution of the emission line flux is available from grism spectroscopy: the line flux from the high dispersion stack is centrally peaked and thus likely associated with AGN activity rather than star formation, strengthening this conclusion. Since velocity dispersion may also be the best predictor of halo mass (Wake et al. 2012), this may imply that the quenching mechanism is directly related to halo mass.
Dynamically Close Pairs of Galaxies Selected in the NIR
Authors: Keenan Ryan C. , Foucaud Sebastien , De Propris Roberto , Lin Jing-Hua 
Published: July 2013

AbstractStudies of dynamically close pairs of galaxies can serve as a powerful probe of the galaxy merger rate and its evolution. Here we present a large sample of dynamically close pairs of galaxies selected in the K-band from the UKIDSS LAS. These data span ~ 175 deg2 on the sky in the 2dFGRS equatorial region (10h < RA < 14h). Combining the 2dFGRS redshifts with those from the SDSS, our K-band selected catalog is > 90% spectroscopically complete at KAB < 16.4. In this study, we focus on quantifying the relative contributions of wet, dry, and mixed mergers to the stellar mass buildup of galaxies over the past 1-2 Gyr.
Updated catalog of 132,684 galaxy clusters and evolution of brightest cluster galaxies
Authors: Wen Z. L. , Han J. L. 
Published: July 2013

AbstractWe identified 132,684 clusters in the redshift range of 0.05 < z < 0.8 from SDSS DR8. The spectroscopic redshifts of 52,683 clusters have been included in the catalog using SDSS DR9 data. We found that BCGs are more luminous in richer clusters and at higher redshifts.