bluuebunny/crossref_metadata_2025_split huggingface dataset:
Protein Kinase C Activators as Synaptogenic and Memory Therapeutics
Authors: Sun Miao‐Kun , Alkon Daniel L. 
Published: November 2009

AbstractThe last decade has witnessed a rapid progress in understanding of the molecular cascades that may underlie memory and memory disorders. Among the critical players, activity of protein kinase C (PKC) isoforms is essential for many types of learning and memory and their dysfunction, and is critical in memory disorders. PKC inhibition and functional deficits lead to an impairment of various types of learning and memory, consistent with the observations that neurotoxic amyloid inhibits PKC activity and that transgenic animal models with PKCβ deficit exhibit impaired capacity in cognition. In addition, PKC isozymes play a regulatory role in amyloid production and accumulation. Restoration of the impaired PKC signal pathway pharmacologically results in an enhanced memory capacity and synaptic remodeling / repair and synaptogenesis, and, therefore, represents a potentially important strategy for the treatment of memory disorders, including Alzheimer's dementia. The PKC activators, especially those that are isozyme‐specific, are a new class of drug candidates that may be developed as future memory therapeutics.
Contrast in usage of FCAT‐approved anatomical terminology between members of two anatomy associations in North America
Authors: Martin Bradford D. , Thorpe Donna , Merenda Victoria , Finch Brian , Anderson‐Smith Wendy , Consiglio‐Lahti Zane 
Published: November 2009

AbstractAlmost 12 years since the publishing of Terminologia Anatomica (TA) by the Federative Committee on Anatomical Terminology (FCAT), there has yet to be a unified adoption of FCAT‐recommended anatomical terms by North American anatomists. A survey was sent to members of the Human Anatomy & Physiology Society (HAPS) to compare the frequency of FCAT term usage with a previous study involving the American Association of Anatomists (AAA). The HAPS differed from AAA in being composed mostly of biologists (56.5%) who teach anatomy with only 18.3% of respondents having terminal degrees in anatomy. The survey included the same 25 sets of synonymic names for selected gross anatomical structures or related terms used for the AAA survey. Overall results indicate that the FCAT preferred term had the highest frequency of usage in only 40.0% of the survey questions, demonstrating 4% lower compliance than AAA respondents. Compliance with FCAT preferred terms ranged from 92.2% to 1.7% usage. When compared with AAA anatomists, there were reversals in predominant usage between FCAT and non‐FCAT terms for six sets of anatomical structures: HAPS respondents predominantly used non‐FCAT terms for adrenal gland (88.7%), antecubital fossa (57.4%), patellar tendon (65.2%), ligamentum capitis femoris (36.5%), while preferring the FCAT anterior circumflex humeral artery (45.2%) and anterior/posterior preferred over ventral/dorsal (41.7%). Almost 54% of HAPS anatomists were not familiar with the FCAT, nearly 21% higher than the AAA. Anat Sci Educ 3:25–32, 2010. © 2009 American Association of Anatomists.
An index to measure a scientist's specific impact
Authors: De Visscher Alex 
Published: November 2009

AbstractThe specific impact index, or s‐index, is introduced as a measure of a scientist's projected impact per paper. The index is complementary to other indices that measure overall impact as it can distinguish between authors maximizing the quantity of their output and authors maximizing the quality of their output. It also can be used to monitor career progress. The main advantage of the new index is that it reduces age bias from older papers that have more time to accumulate citations than do more recent papers. The index was tested on 24 scientists in different fields and of different statures. The overall projected impact estimated from the index correlates well with Hirsch's h‐index squared (r2=0.99). The impact of different aging models was evaluated as well.
Simulations of the formation and evolution of dwarf galaxies
Authors: Valcke S. , De Rijcke S. , Dejonghe H. 
Published: November 2009

AbstractWe present models of the formation and evolution of isolated dwarf galaxies. The models follow the evolution of an initially homogeneous gas cloud collapsing in a pre‐existing dark‐matter halo. These simplified initial conditions are supported by the merger trees of isolated dwarf galaxies extracted from the milli‐Millennium Simulation. An extensive comparison of the models to observations was made. The models' surface brightness profiles are well fitted by Sérsic profiles and the correlations between the models' Sérsic parameters and luminosity agree with the observations. We have also compared model predictions for the half‐light radius Re, central velocity dispersion σc, broad band colour B – V, metallicity [Z/Z⊙] versus luminosity relations and for the location relative to the fundamental plane with the available data. In all cases the models give the correct slope, in most cases we also get the zero‐point right (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Ram pressure stripping of disk galaxies in galaxy clusters
Authors: Roediger E. 
Published: November 2009

AbstractWhile galaxies move through the intracluster medium of their host cluster, they experience a ram pressure which removes at least a significant part of their interstellar medium. This ram pressure stripping appears to be especially important for spiral galaxies: this scenario is a good candidate to explain the differences observed between cluster spirals in the nearby universe and their field counterparts. Thus, ram pressure stripping of disk galaxies in clusters has been studied intensively during the last decade. I review advances made in this area, concentrating on theoretical work, but continuously comparing to observations (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Luminosity function of galaxies in rich and poor galaxy clusters
Authors: Krywult J. 
Published: November 2009

AbstractUsing photometric data from SDSS survey we study the galaxy luminosity function in the 75 rich and poor Abell clusters. The integrated Schechter functions were fitted to unbinned data in the four g, r, i, and z photometric passbands. We find that the luminosity function differs with Abell richness class (R). In all bands the faint‐end slope α is steeper in poor clusters than in rich clusters. Moreover, the value of characteristic magnitude M * decreasing with richness class R (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Metal enrichment of the intracluster medium: SN‐driven galactic winds
Authors: Baumgartner V. , Breitschwerdt D. 
Published: November 2009

AbstractWe investigate the role of supernova (SN)‐driven galactic winds in the chemical enrichment of the intracluster medium (ICM). Such outflows on galactic scales have their origin in huge star forming regions and expel metal enriched material out ofthe galaxies into their surroundings as observed, for example, in the nearby starburst galaxy NGC 253. As massive stars in OB‐associations explode sequentially, shock waves are driven into the interstellar medium (ISM) of a galaxy and merge, forming a superbubble (SB). These SBs expand in a direction perpendicular to the disk plane following the density gradient of the ISM. We use the 2D analytical approximation by Kompaneets (1960) to model the expansion of SBs in an exponentially stratified ISM. This is modified in order to describe the sequence of SN‐explosions as a time‐dependent process taking into account the main‐sequence life‐time of the SN‐progenitors and using an initial mass function to get the number of massive stars per mass interval. The evolution of the bubble in space and time is calculated analytically, from which the onset of Rayleigh‐Taylor instabilities in the shell can be determined. In its further evolution, the shell will break up and high‐metallicity gas will be ejected into the halo ofthe galaxy and even into the ICM. We derive the number of stars needed for blow‐out depending on the scale height and density ofthe ambient medium, as well as the fraction of alpha‐ and iron peak elements contained in the hot gas. Finally, the amount of metals injected by Milky Way‐type galaxies to the ICM is calculated confirming the importance ofthis enrichment process (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
High relative velocity central dumbbells in poor clusters
Authors: Quintana H. , Proust D. , Hertling G. , Ramírez A. , Toledo I. , Way M.J. 
Published: November 2009

AbstractWe propose that some high relative velocity dumbbell galaxies are the centers of poor clusters or groups that are coming into a merging process. The components of these galaxies closely follow the incoming velocity of the merging groups, as revealed by the bimodality of the velocity histograms. Only mergers in a direction with a small angle to the line of sight can show the large velocity difference of the components and the velocity separation of incoming subgroups in the histograms. In this case the simple interpretation would be that the dumbbells components are also in an early phase of their merger, as they still keep the information of the incoming orbits, but analysis of a numerous sample is needed to prove this suggestion (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
ToPoS view of the Perseus cluster
Authors: Ryś S. , Siemieniec‐Oziȩbło G. , Urbanik M. , Soida M. , Kus A. 
Published: November 2009

AbstractWe present the first map of the Perseus Cluster obtained within the Toruń Polarimetric Survey (ToPoS). The maps indicate that there is a large scale polarized radiation located at the periphery of classic radius of this cluster. It seems that an investigation of the magnetic structures we should take into account the contribution from circularly polarized radiation. Few pictures presented here seems to support such a point of view (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The evolution of cluster early‐type galaxies over the past 8 Gyr
Authors: Fritz A. , Jørgensen I. , Schiavon R.P. , Chiboucas K. 
Published: November 2009

AbstractWe present the Fundamental Plane (FP) of early‐type galaxies in the clusters of galaxies RXJ1415.1+3612 at z = 1.013. This is the first detailed FP investigation of cluster early‐type galaxies at redshift z = 1. The distant cluster galaxies follow a steeper FP relation compared to the local FP. The change in the slope of the FP can be interpreted as a massdependent evolution. To analyse in more detail the galaxy population in high redshift galaxy clusters at 0.8 < z < 1, we combine our sample with a previous detailed spectroscopic study of 38 early‐type galaxies in two distant galaxy clusters, RXJ0152.7–1357 at z = 0.83 and RXJ1226.9+3332 at z = 0.89. For all clusters Gemini/GMOS spectroscopy with high signal‐to‐noise and intermediate‐resolution has been acquired to measure the internal kinematics and stellar populations of the galaxies. From HST/ACS imaging, surface brightness profiles, morphologies and structural parameters were derived for the galaxy sample. The least massive galaxies (M = 2 x 1010 M⊙) in our sample have experienced their most recent major star formation burst at zform ∼ 1.1. For massive galaxies (M > 2 x 1011 M⊙) the bulk of their stellar populations have been formed earlier zform ≳ 1.6. Our results confirm previous findings by Jørgensen et al. This suggests that the less massive galaxies in the distant clusters have much younger stellar populations than their more massive counterparts. One explanation is that low‐mass cluster galaxies have experienced more extended star formation histories with more frequent bursts of star formation with shorter duration compared to the formation history of high‐mass cluster galaxies (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
A continuum of structure and stellar content from Virgo cluster earlytype dwarfs to giants?
Authors: Janz J. , Lisker T. 
Published: November 2009

AbstractBased on the wealth of multiwavelength imaging data from the SDSS, we investigate whether dwarf and giant early‐type galaxies in the Virgo cluster follow a continuum in their structural parameters and their stellar population characteristics. More specifically we study the relation between size and brightness for the galaxies and their color magnitude relation. In both cases, we find noticeable deviations from a simple joint behavior of dwarfs and giants. We discuss these findings in the light of the different formation mechanisms commonly assumed for dwarf and giant early types, thereby taking into account the existence of several distinct early‐type dwarf subclasses. By comparing our results to a semianalytic model of galaxy formation, we argue that the analyzed relations might be reproduced by processes that form dwarfs and giants altogether. The work presented here is based on Janz & Lisker (2008, 2009) (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The evolution of cluster dwarfs
Authors: Harsono D. , De Propris R. 
Published: November 2009

AbstractWe summarize the results from analyzing six clusters of galaxies at 0.14 < z < 0.40 observed with the Hubble Space Telescope Advanced Camera for Surveys. We derive deep composite luminosity functions in B, g, V, r, i, and z down to absolute magnitude of ∼ –14 + 5 log h mag. The luminosity functions are fitted by a single Schechter function with MBgVriz * = –19.8, –20.9, –21.9, –22.0, –21.7, and –22.3 mag, and α ∼ –1.3 for all bands. The data suggests red sequence dominates the luminosity function down to ≥6 mag below L*, the dwarf spheroidals regime. Hence, at least at z 0.3, the red sequence is well established and galaxies down to dwarf spheroidals are assembled within these clusters. We do not detect the faint‐end upturn (M > –16) that is observed in lower redshift clusters. If this is real, the faint‐end population has originated since z = 0.3 (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Post‐starburst galaxies and the transformation of blue into red galaxies
Authors: De Rijcke S. , Buyle P. , Pisano D.J. , Freeman K. , Dejonghe H. 
Published: November 2009

AbstractWe present deep single‐dish radio observations of a sample of nearby post‐starburst galaxies (0.05 < z < 0.1). About 50% of these post‐starburst galaxies are detected at 21 cm, with HI masses of ∼109 M⊙, up to ∼1010 M⊙. These post‐starburst galaxies are as gas‐rich as spiral galaxies with comparable luminosities. There appears to exist no direct correlation between the amount of H I present in a post‐starburst galaxy and its star formation rate as traced by radio continuum emission. Moreover, the end of the starburst clearly does not necessarily require the complete exhaustion of the neutral gas reservoir. High‐resolution radio observations of one post‐starburst binary system suggest that most of the neutral gas resides outside the stellar bodies of the galaxies. Most likely, the gas was expelled by supernova and/or AGN feedback. This effectively stops star formation, even though copious amounts of diffuse neutral gas remain in the immediate vicinity. This remaining H I reservoir may eventually lead to further episodes of star formation. This may indicate that some post‐starbursts are observed in the inactive phase ofthe star formation duty cycle (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Stellar populations of seven early‐type dwarf galaxies and their nuclei
Authors: Paudel S. , Lisker T. 
Published: November 2009

AbstractDwarf galaxies are the numerically dominating population in the dense regions of the universe. Although they seem to be simple systems at first view, the stellar populations of dwarf elliptical galaxies (dEs) might be fairly complex. Nucleated dEs are of particular interest, since a number of objects exhibit different stellar populations in their nuclei and host galaxy. We present stellar population parameters obtained from integrated optical spectra using a Lick index analysis of seven nucleated dwarf elliptical galaxies and their nuclei. After subtracting the scaled galaxy spectra from the nucleus spectra, we compared them with one another and explore their stellar populations. As a preliminary result, we find that the luminosity weighted ages of the nuclei slightly lower than those of galaxies, however, we do not see any significant difference in metallicity of the host galaxies and their nuclei (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
The properties of fossil groups of galaxies
Authors: Eigenthaler P. , Zeilinger W.W. 
Published: November 2009

AbstractNumerical simulations as well as optical and X‐ray observations over the last few years have shown that poor groups of galaxies can evolve to what is called a fossil group. Dynamical friction as the driving process leads to the coalescence of individual galaxies in ordinary poor groups leaving behind nothing more than a central, massive elliptical galaxy supposed to contain the merger history of the whole group. Due to merging timescales for less‐massive galaxies and gas cooling timescales of the X‐ray intragroup medium exceeding a Hubble time, a surrounding faint‐galaxy population having survived this galactic cannibalism as well as an extended X‐ray halo similar to that found in ordinary groups, is expected. Recent studies suggest that fossil groups are very abundant and could be the progenitors of brightest cluster galaxies (BCGs) in the centers of rich galaxy clusters. However, only a few objects are known to the literature. This article aims to summarize the results of observational fossil group research over the last few years and presents ongoing work by the authors. Complementary to previous research, the SDSS and RASS surveys have been cross‐correlated to identify new fossil structures yielding 34 newly detected fossil group candidates. Observations with ISIS at the 4.2 m William Herschel Telescope on La Palma have been carried out to study the stellar populations of the central ellipticals of 6 fossil groups. In addition multi‐object spectroscopy with VLTs VIMOS has been performed to study the shape of the OLF of one fossil system (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Dwarf spheroidal galaxies in the M81 group of galaxies
Authors: Lianou S. , Grebel E.K. , Koch A. 
Published: November 2009

AbstractWe study the properties of the dwarf galaxy population in the nearby interacting M81 group of galaxies. In particular, we are deriving the metallicity distribution functions, the ages and the star formation histories of these dwarf galaxies based on data from the Hubble Space Telescope's Advanced Camera for Surveys and the Sloan Digital Sky Survey. We are correlating this information with the dwarf galaxies' position in the group in order to derive the impact of interactions and environment on their evolution. Here we present preliminary results on the metallicity distribution functions of dwarf spheroidals in the M81 group (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Testing of the dwarf galaxy content and the evolutionary status of nearby groups of galaxies
Authors: Vennik J. , Hopp U. 
Published: November 2009

AbstractWe carried out visual and parametric searches for dwarf galaxies in five loose groups of galaxies. Follow‐up spectroscopy with the HET has shown a 50% success rate of morphological selection. The evolutionary status of the studied groups differs: while the NGC 6962 group has a partially relaxed core, surrounded by an infall region, the NGC 5005/5033 group and the IC 65 group, which consist only of late‐type galaxies, are probably still assembling (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Evolution of dwarf galaxies in the Centaurus A group
Authors: Crnojević D. , Grebel E.K. , Koch A. 
Published: November 2009

AbstractThe study of (dwarf) galaxies in nearby groups is one among the most powerful tools that can be used to investigate galaxy evolution, chemical enrichment and environmental effects on these objects. The Centaurus A group (at a distance of ∼4 Mpc) is dynamically evolved and contains about 30 dwarf companions of different morphologies and stellar contents. Here we present the first results for the dwarf spheroidal galaxy population in this group. We use archival HST/ACS data to study their resolved stellar content. The resulting metallicity distribution functions reveal metal‐poor populations and wide metallicity spreads for each galaxy. We find no clear trend of the derived physical properties as a function of galaxy position in the group. Finally, we compare our results to the dwarf population of the Local Group, and find no outstanding differences (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Galaxy‐galaxy interactions as triggers of star formation
Authors: Popescu N.A. 
Published: November 2009

AbstractGalaxy‐galaxy interactions represent the main physical processes that trigger substantial star formation in galaxies. In order to study the galaxy interactions effects on color and morphology of the galaxies in the fields of two radio galaxies at z ∼ 1, we combined optical‐NIR photometry and HST/WFPC2 morphology data from the Stanford et al. (2002) catalog, with HST/WFPC2 archival images. Using a strong pair isolation criterion in terms of the apparent angular separation and rest‐frame line‐of‐sight velocity difference, we obtained a sample of galaxy pairs in the studied fields. The fact that close interactions and mergers induce star‐forming episodes is confirmed by the presence of morphological disturbances and bluer optical‐NIR colors at many analyzed galaxies (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
A study of major mergers using a multi‐phase ISM code
Authors: Weniger J. , Theis Ch. , Harfst S. 
Published: November 2009

AbstractGalaxy interactions are a common phenomenon in clusters of galaxies. Especially major mergers are of particular importance, because they can change the morphological type of galaxies. They have an impact on the mass function of galaxies and they trigger star formation – the main driver of the Galactic Matter Cycle. Therefore, we conducted a study of major mergers by means of a multi‐phase ISM code. This code is based on a TREE‐SPH‐code combined with a sticky particle method allowing for star formation controlled by the properties of a multi‐phase ISM. This is in contrast to the usually implemented Schmidt law depending mainly on the gas density. Previously, this code was used on isolated galaxies. Since our star formation recipe is not restricted to a special type of galaxy, it is interesting to apply it to interacting galaxies, too. Our study on major mergers includes a research of global properties of the interacting system, namely the star formation rate and the star formation efficiency, the evaporation and condensation rates, as well as the mass exchange of distinct components, namely stars, diffuse ISM, and clouds. Investigating these properties provides insight to interrelations between various physical processes. The results indicate that the star formation efficiency as well as the evaporation and condensation rates are influenced by the interaction (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
IC 1370: A merger candidate at the periphery of a z ∼ 0.05 cluster
Authors: Temporin S. , Ciroi S. 
Published: November 2009

AbstractRecent studies show evidence of galaxy pre‐processing within groups and/or filaments before infall in galaxy clusters. We present VIMOS/IFU observations of IC1370, a galaxy that shows morphological signatures of a recent merger and is located at a projected distance of ∼1.2 Mpc to the center of the cluster II Zw108 at z ∼ 0.05. This galaxy shows two opposite tidal tails, a boxy bulge with a de Vaucouleurs light profile, and a disk component that contributes ∼50 % of the total luminosity. We investigate the history of the galaxy by applying the spectral synthesis technique to the integral field observations and combining the resulting information with morphological and photometric parameters. The same observations allow us to investigate a background (z ∼ 0.09) compact group of 6 galaxies, ofwhich IC 1370 was initially thought to be the central, brightest member (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)