pinecone/core-2020-05-10-deduplication huggingface dataset:
Syringolin A: action on plants, regulation of biosynthesis, and phylogenetic occurrence of structurally related compounds

Syringolin A, the product of a mixed non-ribosomal peptide/polyketide synthetase, is secreted by  Pseudomonas syringae pv. syringae under in planta conditions and is one of the molecular determinants recognized by nonhost plant species. Spray application of syringolin A onto powdery mildew-infected wheat and Arabidopsis has the remarkable effect of reprogramming epidermal cells that are colonized by the powdery mildew fungi Blumeria graminis f. sp. tritici and Erysiphe cichoracearum, respectively, in a compatible interaction to undergo hypersensitive cell death. No hypersensitive cell death is observed if the compound is applied onto uninfected plants. Transcriptome analyses in wheat and Arabidopsis with regard to powdery mildew inoculation and/or syringolin A spraying lead to a hypothesis about how syringolin A may accomplish to induce the hypersensitive reaction (HR) in colonized cells. The model is supported by transcriptome analyis of an Arabidopsis mutant in which HR is not induced upon syringolin A spraying of powdery mildew-infected plants. Cloning of the syringolin A synthetase genes has allowed us to build a detailed model of syringolin A synthesis based on the gene structure. This model in turn enabled us to clone the genes responsible for the synthesis of glidobactins (syn. cepafungins), antibiotics with a structure related to syringolin A that were reported to have antitumor activity, from an unknown species belonging to the order Burkholderiales. Comparisons to the approximately 700 complete eubacterial genomic sequences known resulted in the identification of  a small but very intriguing group of pathogenic bacteria postulated to produce glidobacting-like molecules
The Local Velocity Anomaly

There is a velocity discontinuity at about 7 Mpc between the galaxies of the
Local Sheet that are moving together with low internal velocity dispersion and
the adjacent structures. The Local Sheet bounds the Local Void. The Local Sheet
is determined to have a peculiar velocity of 260 km/s away from the center of
the void. In order for this large velocity to be generated by an absence of
gravity, the Local Void must be at least 45 Mpc in diameter and be very empty.Comment: Invited review, "Galaxies in the Local Volume", Sydney, 8-13 July,
  2007. eds. B. Koribalski & H. Jerjen, Astrophys. & Space Sci. Proceed. 10
  pages with 7 figure
Magnetic Fields in Irregular Galaxies

Magnetic fields are an important component of the interstellar medium,
especially in low-mass galaxies like irregulars where the magnetic pressure may
be significant. However, few irregular galaxies have observed magnetic field
structures. Using the VLA, the GBT, and the ATCA, we have observed several
irregular galaxies in the radio continuum to determine their magnetic field
structures. Here we report on our results for the galaxies NGC 4214 and NGC
1569.Comment: 4 pages, 1 table, 1 figure, contributed talk at "Galaxies in the
  Local Volume" conference in Sydney, July 200
Outlining the Local Void with the Parkes HI ZOA and Galactic Bulge
  Surveys

The Parkes deep HI ZOA survey has been extended between 2002 and 2004 towards
higher latitudes in the Galactic Bulge region. This area of extreme star
crowding and high extinction levels remains impenetrable at any other waveband
regime.
  Preliminary results of the 3 dimensional distribution based on the combined
HI-surveys are presented. We focus on the extent and "content" of the Local
Void as outlined by these HI surveys, followed by a preliminary discussion of
the properties of the few galaxies detected in the Local Void.Comment: 4 pages, 2 figures (jpg). To be published in ``Galaxies in the Local
  Volume'' (Sydney, July 2007), eds. B. Koribalski & H. Jerjen, Astrophys. &
  Space Scienc
Resolving the Outer Disks and Halos of Nearby Galaxies

In a hierarchical merging scenario, the outer parts of a galaxy are a fossil
record of the galaxy's early history. Observations of the outer disks and halos
of galaxies thus provide a tool to study individual galaxy histories and test
formation theories. Locally, an impressive effort has been made to understand
the halo of the Milky Way, Andromeda, and M33. However, due to the stochastic
nature of halo formation, a better understanding of this process requires a
large sample of galaxies with known halo properties. The GHOSTS project (PI: R.
de Jong) aims to characterize the halos and outer portions of 14 nearby (D=4-14
Mpc) spiral galaxies using the Hubble Space Telescope. Detection of individual
stars in the outer parts of these galaxies enables us to study both the
morphological properties of the galaxies, and determine the stars' metallicity
and age.Comment: Contributed talk; to appear in the proceedings of "Galaxies in the
  Local Volume" Sydney 8-13 July 200
Modeling Non-Circular Motions in Disk Galaxies: A Bar in NGC 2976

We give a brief description of a new model for non-circular motions in disk
galaxy velocity fields, that does not invoke epicycles. We assume non-circular
motions to stem from a bar-like or oval distortion to the potential, as could
arise from a triaxial halo or a bar in the mass distribution of the baryons. We
apply our model to the high-quality CO and Halpha kinematics of NGC 2976
presented by Simon et al. 2003; it fits the data as well as their model with
unrealistic radial flows, but yields a steeper rotation curve. Our analysis and
other evidence suggests that NGC 2976 hosts a bar, implying a large baryonic
contribution to the potential and thus limiting the allowed dark matter halo
density.Comment: 4 pages, 3 color figures, contribution to "Galaxies in the Local
  Volume" conference proceedings, eds. B. Koribalski and H. Jerje
Gravitational stability in the disk of M51

Star formation laws, like i.e. the Schmidt law relating star formation rate
and total gas density, have been studied in several spiral galaxies but the
underlying physics are not yet well understood. M51, as a nearby face-on, grand
design spiral galaxy studied in many line transitions, is an ideal target to
study the connection between physical conditions of the gas and star formation
activity. In this contribution we combine molecular, atomic, total gas and
stellar surface densities and study the gravitational stability of the gas
(Schuster et al.2007, Hitschfeld et al. in prep.). From our IRAM-30m 12 CO2-1
map and complementary HI-, Radio Continuum- and ACS-HST B-band-data we derive
maps of the total gas density and the stellar surface density to study the
gravitational stability of the gas via the Toomre Q parameter.Comment: 4 pages, 3 Figures: Galaxies in the Local Volume, Sydney, Conference
  Proceedings Contributio
Mining the Local Volume

After recent systematic optical, IR, and HI surveys, the total number of
known galaxies within 10 Mpc has increased from 179 to 550. About half this
Local Volume (LV) sample is now been imaged with HST, yielding the galaxy
distances with an accuracy of about 8%. For the majority of the LV galaxies we
currently have H-alpha fluxes that allow us to reconstruct the star formation
history of our neighbourhood.
  For the late-type LV galaxies their HI masses and angular momentum follow the
linear relation in the range of 4 orders, which is expected for rotating
gaseous disks being near the gravitational instability threshold.
  The data obtained on the LV galaxies imply important cosmological parameters,
in particular, the mean local matter density and HI mass density, as well as
SFR density.
  Surprisingly, the local Hubble flow around the LV groups is very quiet, with
1D rms deviations of 25 km/s,which is a signature of the Universe
vacuum-dominated on small scales. The cold infall pattern around nearby groups
provides us with a new method to determine the total mass of the groups
independent from virial mass estimates.Comment: 10 pages, 6 figures, proceedings Symposium "Galaxies in the Local
  Volume", Sydney, 8 - 13 July 2007, B. Koribalski and H. Jerjen, ed
First Results From the Large Binocular Telescope: Deep Photometry of New
  dSphs

This contribution describes photometry for two Galactic dSphs obtained with
the Large Binocular Telescope to a magnitude of ~25.5. Using the Large
Binocular Camera, a purpose-built wide-field imager for the LBT, we have
examined the structure and star formation histories of two newly-discovered
Local Group members, the Hercules dSph and the Leo T dSph/dIrr system. We have
constructed a structural map for the Hercules system using three-filter
photometry to V ~ 25.5. This is the first deep photometry for this system, and
it indicates that Hercules is unusually elongated, possibly indicating
distortion due to the Galactic tidal field. We have also derived the first star
formation history for the Leo T system, and find that its oldest population of
stars (age ~ 13 Gyr) were relatively metal-rich, with [Fe/H] ~ -1.5.Comment: Four pages, two figures. To appear in the proceedings of "Galaxies in
  the Local Volume", Astrophysics and Space Science, editors B. Koribalski and
  H. Jerje
Proper Motions in the Andromeda Subgroup

This article presents results of VLBI observations of regions of H2O maser
activity in the Local Group galaxies M33 and IC10. Since all position
measurements were made relative to extragalactic background sources, the proper
motions of the two galaxies could be measured. For M33, this provides this
galaxy's three dimensional velocity, showing that this galaxy is moving with a
velocity of 190 +/- 59 km\s relative to the Milky Way. For IC10, we obtain a
motion of 215 +/- 42 km/s relative to the Milky Way. These measurements promise
a new handle on dynamical models for the Local Group and the mass and dark
matter halo of Andromeda and the Milky Way.Comment: 4 pages 1 figures, to appear in the proceedings of "Galaxies in the
  Local Volume", Astrophysics and Space Science, editors B. Koribalski and H.
  Jerjen also available at
  http://www.mpifr-bonn.mpg.de/staff/abrunthaler/pub.shtm
Properties of voids in the Local Volume

Current explanation of the overabundance of dark matter subhalos in the Local
Group (LG) indicates that there maybe a limit on mass of a halo, which can host
a galaxy. This idea can be tested using voids in the distribution of galaxies:
at some level small voids should not contain any (even dwarf) galaxies. We use
observational samples complete to M_B=-12 with distances less than 8 Mpc to
construct the void function (VF): the distribution of sizes of voids empty of
any galaxies. There are ~ 30 voids with sizes ranging from 1 to 5 Mpc. We also
study the distribution of dark matter halos in very high resolution simulations
of the LCDM model. The theoretical VF matches the observations remarkably well
only if we use halos with circular velocities larger than 45 +/- 10 km/s. This
agrees with the Local Group predictions. Small voids look quite similar to heir
giant cousins: the density has a minimum at the center of a void and it
increases as we get closer to the border. Thus, both the Local Group data and
the nearby voids indicate that isolated halos below 45 +/- 10 km/s must not
host galaxies and that small (few Mpc) voids are truly dark.Comment: 5 pages 1 figure. To appear in proceedings of the conference
  "Galaxies in the Local Volume", Sydney, 8 to 13 July 200
Young star clusters in M31

In our study of M31's globular cluster system with MMT/Hectospec, we have
obtained high-quality spectra of 85 clusters with ages less than 1 Gyr. With
the exception of Hubble V, the young cluster in NGC 205, we find that these
young clusters have kinematics and spatial distribution consistent with
membership in M31's young disk. Preliminary estimates of the cluster masses and
structural parameters, using spectroscopically derived ages and HST imaging,
confirms earlier suggestions that M31 has clusters similar to the LMC's young
populous clusters.Comment: 4 pages, 1 figure, contributed talk at "Galaxies in the Local Volume"
  conference in Sydney, July 200
Evolution of the Small Magellanic Cloud

Based on the results of N-body simulations on the last 2.5 Gyr evolution of
the Large and Small Magellanic Clouds (LMC and SMC, respectively) interacting
with the Galaxy, we firstly show when and where the leading arms (LAs) of the
Magellanic stream (MS) can pass through the Galactic plane after the MS
formation. We secondly show collisions between the outer Galactic HI disk and
the LAs of the MS can create giant HI holes and chimney-like structures in the
disk about 0.2 Gyr ago. We thirdly show that a large amount of metal-poor gas
is stripped from the SMC and transfered to the LMC during the tidal interaction
between the Clouds and the Galaxy about 0.2 and 1.3 Gyr ago. We thus propose
that this metal-poor gas can closely be associated with the origin of LMC's
young and intermediate-age stars and star clusters with distinctively
low-metallicities with [Fe/H] < -0.6.Comment: 4 pages, 3 figures, to appear in the proceedings of ``Galaxies in the
  Local Volume'', Sydney, 8 to 13 July, 200
Using Local Volume data to constrain Dark Matter dynamics

The peculiar velocity reconstruction methods allow one to have a deeper
insight into the distribution of dark matter: both to measure mean matter
density and to obtain the primordial density fluctuations. We present here the
Monge-Ampere-Kantorovitch method applied to mock catalogues mimicking in both
redshift and distance catalogues. After having discussed the results obtained
for a class of biases that may be corrected for, we focus on the systematics
coming from the unknown distribution of unobserved mass and from the
statistical relationship between mass and luminosity. We then show how to use
these systematics to put constraints on the dark matter distribution. Finally a
preliminary application to an extended version (c z < 3000 km/s) of the
Neighbour Galaxy Catalogue is presented. We recover the peculiar velocities in
our neighbourhood and present a preliminary measurement of the local Omega_M.Comment: 4 pages, 2 figures. To be published in the proceedings of ``Galaxies
  in the Local Volume'', Sydney 8 to 13 July 200
Deepest Near-IR Surface Photometry of Galaxies in the Local Sphere of
  Influence

We present near-IR, deep (4 mag deeper than 2MASS) imaging of 56 Local Volume
galaxies. Global parameters such as total magnitudes and stellar masses have
been derived and the new near-IR data combined with existing 21cm and optical
B-band data. We present multiwavelength relations such as the HI mass-to-light
ratio and investigate the maximum total baryonic mass a galaxy can have.Comment: 4 pages, 3 figures, To be published in the proceedings of "Galaxies
  in the Local Volume", ed. B. Koribalski, H. Jerje
Galaxy Clusters in the Radio: Relativistic Plasma and ICM/Radio Galaxy Interaction Processes

The organization of this paper is as follows: the basic formulae used to derive the age of synchrotron sources and the equipartition parameters are presented in Section 2, while the observational properties of diffuse radio sources (Radio halos, Radio relics, and Mini-halos) are presented in Section 3. Then in Section 4 we give a general outline of the models of the relativistic particle origin and re-acceleration; while the current results on cluster magnetic fields are described in Section 5. Finally, Section 6 reports the properties of cluster radio emitting galaxies
Cosmology with clusters of galaxies

In this Chapter I review the role that galaxy clusters play as tools to constrain cosmological parameters. I will concentrate mostly on the application of the mass function of galaxy clusters, while other methods, such as that based on the baryon fraction, are covered by other Chapters of the book. Since most of the cosmological applications of galaxy clusters rely on precise measurements of their masses, a substantial part of my Lectures concentrates on the different methods that have been applied so far to weight galaxy clusters. I provide in Section 2 a short introduction to the basics of cosmic structure formation. In Section 3 I describe the Press--Schechter (PS) formalism to derive the cosmological mass function, then discussing extensions of the PS approach and the most recent calibrations from N--body simulations. In Section 4 I review the methods to build samples of galaxy clusters at different wavelengths. Section 5 is devoted to the discussion of different methods to derive cluster masses. In Section 6 I describe the cosmological constraints, which have been obtained so far by tracing the cluster mass function with a variety of methods. Finally, I describe in Section 7 the future perspectives for cosmology with galaxy clusters and the challenges for clusters to keep playing an important role in the era of precision cosmology
The Nature and the Extent of the Market for Technology in Biopharmaceuticals

This paper explored an unusually comprehensive dataset of more than 2,000 drug R&D projects all over the world during the 1990s. This enabled us to characterise several features of the innovation process in pharmaceuticals, particularly the different role and comparative R&D performance of the large established drug companies vis-à-vis smaller high-tech specialist firms - the so-called New Biotechnology Firms (NBFs). Our results can be summarised as follows:
a)The NBFs are largely an American phenomenon. More than half of the drug R&D projects originated in the US are by NBFs, while almost 90% of the drug R&D projects originated in Europe are from established pharmaceutical firms;
b)Collaborative R&D projects are consistently more likely to occur in the US than in Europe. However, in-house projects are a significant majority of the drug R&D projects that entered the clinical stages.
c)The established pharmaceutical companies have comparative advantages with respect to the NBFs in drug development (clinical trials). In drug discovery there is no advantage related to scale. Unlike clinical developments, where the large firms seem to have superior capabilities when compared to the NBFs, in discovery there is no inherent superiority (in terms of ultimate probability of success of the compounds) of either the NBFs or the large firms.
d)The NBFs are not specialized in more risky R&D projects. In fact, more risky drug projects (i.e. drugs for which there is no or there are few existing remedies) are more likely to be undertaken by the larger pharmaceutical companies. This suggests that scale, market power, and the ability to moblise large amounts of resources are key factors in enabling the firms to sustain such higher risks.
e)Other things being equal, the projects originated by the NBFs are more likely to fail in the earlier clinical stages. This suggests that the NBFs perform a good deal of exploration without incurring the higher costs of failing at later stages.
Developing re-usable interactive storytelling technologies

Despite the growing interest in Interactive Storytelling (IS), there have been only a small number of implemented demonstrators and few have attempted at developing a re-usable IS technology. In this paper we describe such an IS engine, which is the result of several years of experimentation in the field. The system is based on a game engine for its visualisation component, while the narrative generation component implements a variant of HTN Planning. After an introduction to the principles underlying the system, we introduce the associated production process and discuss authoring problems as well as tools we have developed to facilitate the use of the technology
Thermal Vibrational Convection in a Porous Medium Saturated by a Pure or Binary Fluid

What is Thermal Vibration? The importance of mechanical vibration, as a source of pattern generating mech-anism on the surface of a container filled with liquid, was recognized as early as the beginning of the 19th century by Faraday (1831). However, its importance as a mechanism controlling the convective motion has only been recognized during the 20th century. Originally, mechanical vibration was used in mathematical modeling aimed at increasing the stability threshold of thermo-fluid system (Gershuni et al. 1970, Gresho and Sani 1970). The space exploration and especially the benefits expected from material production in space stations accelerated its development (Alexander 1994). Formally, the thermo-vibrational convection studies concern the form of a mean flowin a confined cavity filled with a fluid presenting temperature non-homogeneities. Compared to the gravity-induced convection, this type of convection presents the advantage that it may exist under weightlessness condition. Under micro-gravity conditions, the gravitational force is reduced drastically. However this situation may cause other forces, which under earth conditions are of minor importance, to be more significant
Seismic parameters re-determined from historical seismograms of 1935-Erdek–Marmara Island and 1963-Çınarcık Earthquakes

In this study, the original seismograms of the 1935-Erdek–Marmara Island and 1963-Çınarcık Earthquakes, recorded at local and regional distances, were vectorized. The epicentral locations have been calculated using available readings from original records and also ISS and seismic station bulletins for 04.01.1935-14:41 and 16:20 Marmara Island–Erdek Earthquakes and 18.09.1963-16:58 Çınarcık Earthquake. The epicenter determinations show that the first event in 04.01.1935 was located at 40.72N–27.72E, while the second one occurred at 40.61N–27.43E, indicating that both were located near the Marmara Island. Another finding is that the 1963 event was located at 40.80N–29.18E, near the Princes’ Island fault. Furthermore, moment tensor inversion method was applied on these earthquakes by using original seismograms, which provided an opportunity to illuminate the seismotectonic features of Marmara Region based on the retrieved fault mechanism solutions. For the first time, the fault mechanisms for 04.01.1935-14:41 and 16:20 Earthquakes were determined using moment tensor inversion from the original seismic waveforms. Likewise, the result obtained for the fault mechanism of 1963 Çınarcık Earthquake showed normal fault mechanism with much shallower depth than estimated before. Our preferred solutions showed that the fault mechanisms for the three events are normal faults and coincide with the seismotectonic structure of the Marmara Region
Questioning the binary divide: non-university higher education in Flanders (Belgium)

In this paper, I will show how the government created a framework to bring universities and colleges closer to each other, and thus cast the binary divide into question.
 Although the first few steps in this process had already been taken in the College Decree in 1994, this process was more stimulated by the Bologna Process. Bologna, after all, stressed the internationalisation of higher education with its consequences for the structure of the  curriculum and the titles of the diplomas. Within this process, new structures emerged (e.g. associations between universities and colleges), and special financing was provided for the
 academic upgrading of college curricula. A comparable financing system for universities and colleges was planned. Nevertheless, the binary divide is still present. First, I will  take a look at the structure of the colleges; second, I will give a picture of their governing structure; third, I will discuss their level of autonomy; and fourth, I will highlight their future development and challenges.status: publishe