451 research outputs found
Nuclear star cluster formation in energy-space
In a virialized stellar system, the mean-square velocity is a direct tracer
of the energy per unit mass of the system. Here, we exploit this to estimate
and compare root-mean-square velocities for a large sample of nuclear star
clusters and their host (late- or early-type) galaxies. Traditional
observables, such as the radial surface brightness and second-order velocity
moment profiles, are subject to short-term variations due to individual
episodes of matter infall and/or star formation. The total mass, energy and
angular momentum, on the other hand, are approximately conserved. Thus, the
total energy and angular momentum more directly probe the formation of galaxies
and their nuclear star clusters, by offering access to more fundamental
properties of the nuclear cluster-galaxy system than traditional observables.
We find that there is a strong correlation, in fact a near equality, between
the root-mean-square velocity of a nuclear star cluster and that of its host.
Thus, the energy per unit mass of a nuclear star cluster is always comparable
to that of its host galaxy. We interpret this as evidence that nuclear star
clusters do not form independently of their host galaxies, but rather that
their formation and subsequent evolution are coupled. We discuss how our
results can potentially be used to offer a clear and observationally testable
prediction to distinguish between the different nuclear star cluster formation
scenarios, and/or quantify their relative contributions.Comment: 12 pages, 3 figures, 4 tables; accepted for publication in MNRA
Explaining two circumnuclear star forming rings in NGC5248
The distribution of gas in the central kiloparsec of a galaxy has a
dynamically rapid evolution. Nonaxisymmetries in the gravitational potential of
the galactic disk, such as a large scale stellar bar or spiral, can lead to
significant radial motion of gaseous material from larger radii to the central
region. The large influx of gas and the subsequent star formation keep the
central region constantly changing. However, the ability of gas to reach the
nucleus proper to fuel an AGN phase is not guaranteed. Gas inflow can be halted
at a circumnuclear star forming ring several hundred parsec away. The nearby
galaxy NGC5248 is especially interesting in this sense since it is said to host
2 circumnuclear star forming rings at 100pc and 370pc from its quiescent
nucleus. Here we present new subarcsecond PdBI+30m CO(2-1) emission line
observations of the central region. For the first time the molecular gas
distribution at the smallest stellar ring is resolved into a gas ring,
consistent with the presence of a quiescent nucleus. However, the molecular gas
shows no ring structure at the larger ring. We combine analyses of the gaseous
and stellar content in the central kiloparsec of this galaxy to understand the
gas distribution and dynamics of this star forming central region. We discuss
the probability of two scenarios leading to the current observations, given our
full understanding of this system, and discuss whether there are really two
circumnuclear star forming rings in this galaxy.Comment: Accepted for publication in A&A, 14pages + long tabl
Neural correlates of ‘pessimistic' attitude in depression
Background Preparing for potentially threatening events in the future is essential for survival. Anticipating the future to be unpleasant is also a cognitive key feature of depression. We hypothesized that ‘pessimism'-related emotion processing would characterize brain activity in major depression. Method During functional magnetic resonance imaging, depressed patients and a healthy control group were cued to expect and then perceive pictures of known emotional valences - pleasant, unpleasant and neutral - and stimuli of unknown valence that could have been either pleasant or unpleasant. Brain activation associated with the ‘unknown' expectation was compared with the ‘known' expectation conditions. Results While anticipating pictures of unknown valence, activation patterns in depressed patients within the medial and dorsolateral prefrontal areas, inferior frontal gyrus, insula and medial thalamus were similar to activations associated with expecting unpleasant pictures, but not with expecting positive pictures. The activity within a majority of these areas correlated with the depression scores. Differences between healthy and depressed persons were found particularly for medial and dorsolateral prefrontal and insular activations. Conclusions Brain activation in depression during expecting events of unknown emotional valence was comparable with activation while expecting certainly negative, but not positive events. This neurobiological finding is consistent with cognitive models supposing that depressed patients develop a ‘pessimistic' attitude towards events with an unknown emotional meaning. Thereby, particularly the role of brain areas associated with the processing of cognitive and executive control and of the internal state is emphasized in contributing to major depressio
Old Technology Meets New Technology: Complementarities, Similarities, and Alliance Formation
Alliance formation is commonplace in many high-technology industries experiencing radical technological change, where
established firms use alliances with new entrants to adapt to technological change, while new entrants benefit from the
ability of established players to commercialize the new technology. Despite the prevalence of these alliances, we know little
about how these firms choose to ally with specific firms given the range of possible partners they may choose from. This
study explores factors that lead to alliance formation between pharmaceutical and biotechnology companies. We focus on
the alliance tie as the unit of analysis and argue that dyadic complementarities and similarities directly influence alliance
formation. We then introduce a contingency model in which the positive effect of complementarities and similarities on
alliance formation is moderated by the age of the new technology firm. We draw theoretical attention to the intersection
between levels of analysis, in particular, the intersection between dyadic and firm-level constructs. We find that a
pharmaceutical and a biotechnology firm are more likely to enter an alliance based on complementarities when the
biotechnology firm is younger. Another noteworthy contribution is the finding that proxies for broad capabilities appear to
be at least as, if not more, effective in predicting alliance formation compared to fine-grained science and technology-related
indicators, like patent cross citations or patent common citations. We conclude by suggesting that future studies on alliance
formation need to take into account interactions across levels; for example, how dyadic capabilities interact with firm-level
factors
HST/WFPC2 imaging of the circumnuclear structure of LLAGNs. I Data and nuclear morphology
To advance our knowledge of the nature of the central source in LLAGNs and
its relation with stellar clusters, we are carrying out several imaging
projects with HST at near-UV, optical and near-IR wavelengths. In this paper,
we present the first results obtained with observations of the central regions
of 57 LLAGNs imaged with the WFPC2 through any of the V (F555W, F547M, F614W)
and I (F791W, F814W) filters that are available in the HST archive. The sample
contains 34% of the LINERs and 36% of the TOs in the Palomar sample. The mean
spatial resolution of these images is 10 pc. With these data we have built an
atlas that includes structural maps for all the galaxies, useful to identify
compact nuclear sources and, additionally, to characterize the circumnuclear
environment of LLAGNs, determining the frequency of dust and its morphology.
The main results obtained are: 1) We have not found any correlation between the
presence of nuclear compact sources and emission-line type. Thus, nucleated
LINERs are as frequent as nucleated TOs. 2) The nuclei of "Young-TOs" are
brighter than the nuclei of "Old-TOs" and LINERs. These results confirm our
previous results that Young-TOs are separated from other LLAGNs classes in
terms of their central stellar population properties and brightness. 3)
Circumnuclear dust is detected in 88% of the LLAGNs, being almost ubiquitous in
TOs. 4) The dust morphology is complex and varied, from nuclear spiral lanes to
chaotic filaments and nuclear disk-like structures. Chaotic filaments are as
frequent as dust spirals; but nuclear disks are mainly seen in LINERs. These
results suggest an evolutionary sequence of the dust in LLAGNs, LINERs being
the more evolved systems and Young-TOs the youngest. The full collection of
figures are at http://www.iaa.es/~rosa/research/LLAGNs2007/LLAGNs-HSTIma1.htmlComment: Paper accepted in AJ, pdf file and the full collection of figures are
at the ULR: http://www.iaa.es/~rosa/research/LLAGNs2007/LLAGNs-HSTIma1.htm
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