bluuebunny/crossref_metadata_2025_split huggingface dataset:
Who saw it coming? The UK’s great financial crisis
Authors: Hindmoor Andrew , McConnell Allan 
Published: February 2014

AbstractWho foresaw the UK banking crisis? This paper addresses this issue through detailed empirical work on the content of the Chancellor of the Exchequer’s speeches, Bank of EnglandFinancial Stability Reports, Financial Service Authority reports and speeches by Bank of England officials, editorials in theTimesandFinancial Times, bank annual reports and financial statements, credit rating reports, share price movements, Parliamentary questions, Treasury select committee reports and the output of academic economists. We find that few people inside or outside government recognised the existence of significant financial vulnerabilities in the financial system in the years prior to the collapse of Northern Rock in September 2007. We use the conceptual lenses of individual, institutional and paradigmatic pathologies to provide explanations for this failure to detect looming crisis conditions. We argue ultimately that regulators and commentators were blinded by faith in market forces and the risk-tempering properties of securitisation.
Breeding to non-breeding population ratio and breeding performance of the globally Endangered Lear’s MacawAnodorhynchus leari: conservation and monitoring implications
Authors: PACÍFICO ERICA C. , BARBOSA EDUARDO A. , FILADELFO THIAGO , OLIVEIRA KLEBER G. , SILVEIRA LUÍS F. , TELLA JOSÉ L. 
Published: February 2014

SummaryLear’s MacawAnodorhynchus leariis currently listed as “Endangered” by IUCN. Although it only breeds on cliffs at two protected sites in Bahia State, Brazil, there is no accurate information on population parameters such as the number of breeding pairs and their breeding performance. Between 2009 and 2010, we sought to quantify, for the first time, breeding population size and the main breeding parameters for the species in the two known breeding sites, by quantifying the number of active nests and monitoring 75 breeding attempts. Overall, 80% of the breeding attempts were successful with 1.33 (± 0.86 SD) fledglings/breeding attempt (productivity) and 1.67 (± 0.60 SD) fledglings/successful nest (brood size). Breeding success and productivity were higher in 2010, while brood size did not vary between years and breeding sites. By adding 73 estimated nests to the 41 nests monitored, 228 individuals were estimated to be reproductively active in 2010, representing c.20% of the population (1,125 individuals). Given that the species is confined to a single population, further population increases could provoke overcrowding and negative density-dependent effects if it does not expand geographically. Therefore, long-term population monitoring focusing on the fraction of the population that is actually breeding and its breeding performance, rather than solely on the whole population size, is important for a better understanding of the population dynamics and conservation of this species.
A case of parvovirus B19-induced pure red cell aplasia in a child following heart transplant
Authors: Kelleher Eoin , McMahon Corrina , McMahon Colin J. 
Published: February 2014

AbstractWe describe a case of an 11-year-old boy who underwent orthotopic heart transplant for dilated cardiomyopathy. He developed a normocytic, normochromic anaemia with a low reticulocyte count 1 month after transplant. A bone marrow biopsy was performed, which showed a mildly hypocellular bone marrow with few red blood cell precursors with giant pro-erythroblasts indicative of a pure red cell aplasia. Parvovirus B19 polymerase chain reaction in the blood was positive 2 months after transplant. Intravenous immunoglobulin administration resulted in a resolution of the anaemia over several months. Unexplained pure red cell aplasia in immunosuppressed patients should alert one to the possibility of parvovirus B19 infection.
Types of habitat in the Universe
Authors: Cockell Charles S. 
Published: February 2014

AbstractFrom a biological point of view, all environments in the Universe can be categorized into one of three types: uninhabitable, uninhabited habitat or inhabited habitat. This paper describes and defines different habitat types in the Universe with a special focus on environments not usually encountered on the Earth, but which might be common on other planetary bodies. They include uninhabited habitats, subtypes of which are sterile habitats and organic-free habitats. Examples of the different types of environments are provided with reference to the Eyjafjallajökull, Iceland. These habitat types are used to identify testable hypotheses on the abundance of different habitats and the distribution of life in the Universe.
Diffuse Interstellar Bands: Past and Present
Authors: Snow T. P. 
Published: February 2014

AbstractThe diffuse interstellar bands (DIBs) have come to the fore as an important mystery. This paper presents the history of DIB discovery and research; their importance; a summary of their properties; constraints on proposed identifications; a survey of DIB papers (including graduate student's theses); and a web site that lists DIBs paper from 1922 to 2011 (to be extended to the present).
New Infrared Diffuse Interstellar Bands in the Galactic Center and Elsewhere
Authors: Geballe T. R. 
Published: February 2014

AbstractThis paper updates the recent discovery of over a dozen new diffuse interstellar bands (DIBs), first in H-band spectra of stars in the Galactic center (GC) and toward stars in the Cygnus OB2 Association. The H-band DIBs, which currently number 15, are the longest wavelength DIBs reported to date and are the first found on sightlines toward the Galactic center. K-band (2.0-2.5 μm) spectra of the GC stars do not reveal additional DIBs. Comparison of the velocity profile of the strongest of the new DIBs in the sightline toward GCS3-2 (in the GC) with that toward Cygnus OB2 No. 9 and also with the broad velocity profiles of H3+ lines toward GCS3-2 confirm that a significant fraction of the diffuse material producing the DIB absorptions on sightlines to the GC is located within the central few hundred parsecs of the Galaxy.
Spatial Correlations of Selected DIBs to the CH and CH+ Molecules
Authors: Weselak T. , Krełowski J. 
Published: February 2014

AbstractThe analysis of radial velocities in the spectra of HD 151932 and HD 152233, performed for the optical lines of interstellar CH and CH+ molecules on one hand, and for the diffuse bands 4964 and 6196 Å on the other hand, suggests that the carrier of the former DIB is spatially related to CH, while the carrier of the latter - to CH+. A further analysis, based on the sample of 106 reddened OB stars, partly confirms this suggestion, showing that the CH column density correlates indeed much better with the equivalent width of the 4964 DIB than with that of the 6196 DIB.
Diffuse Interstellar Bands: How are they related to known Gas-Phase Constituents of the ISM?
Authors: Welty D. E. 
Published: February 2014

AbstractIn this brief review of recent work relating the DIBs to other gas-phase constituents of the ISM, we explore correlations between DIB equivalent widths and the column densities of various atomic and molecular species, drawn from a large database constructed for that purpose. The tightness and slopes of the correlations can provide information on how the DIBs might be related to those species (physically, chemically, spatially) and on various properties of the DIB carriers. Deviations from the mean relationships can reveal dependences of DIB strengths on other parameters, regional variations in DIB behavior, and individual sight lines where unusual environmental conditions affect the DIBs. Variations in DIB profiles (e.g., wings, substructure) and relative strengths may be related to differences in physical conditions inferred from atomic and/or molecular absorption lines.
The Infrared Emission Bands
Authors: Peeters E. 
Published: February 2014

AbstractUp to 10% of the total power output of star-forming galaxies is emitted in the infrared emission features at 3.3, 6.2, 7.7, 8.6 and 11.2 μm. Here, I will review the spectral characteristics of these IR emission bands, their dependence on the local environment, the implications for the physical and chemical characteristics of the carriers, and their applicability as a diagnostic tool.
Detection of the Buckminsterfullerene Cation (C60+) in Space
Authors: Berné O. , Mulas G. , Joblin C. 
Published: February 2014

AbstractIn the early 90's, C60+was proposed as the carrier of two diffuse interstellar bands (DIBs) at 9577 and 9632 Å, but a firm identification still awaits gas-phase spectroscopic data. Neutral C60, on the other hand, was recently detected through its infrared emission bands in the interstellar medium and evolved stars. In this contribution, we present the detection of C60+through its infrared vibrational bands in the NGC 7023 nebula, based on spectroscopic observations with theSpitzerspace telescope, quantum chemistry calculation, and laboratory data from the literature. This detection supports the idea that C60+could be a DIB carrier, and provides robust evidence that fullerenes exist in the gas-phase in the interstellar medium. Modeling efforts to design specific observations, combined with new gas-phase data, will be essential to confirm this proposal. A definitive attribution of the 9577 and 9632 Å DIBs to C60+would represent a significant step forward in the field.
Unidentified Species in Envelopes around Carbon Stars
Authors: Jiang B. W. , Li A. , Zhang K. , Liu J. M. , Gao J. , Mishra A. 
Published: February 2014

AbstractThe infrared (IR) spectra of many evolved carbon-rich stars exhibit two prominent dust emission features peaking around 21μm and 30μm, with the former exclusively seen in proto-planetary nebulae (PPNe), while the latter seen in a much wider range of objects, including AGB stars, PPNe and planetary nebulae (PNe). The 30μm feature is seen in all the 21μm sources, but no correlation is found between these two features. Over a dozen carrier candidates have been proposed for the 21μm feature, but none of them has been widely accepted and the nature of the 21μm feature remains a mystery. The carrier of the 30μm feature also remains unidentified. MgS dust, once widely accepted as a valid carrier, was ruled out because of the sulfur budget problem. In this work we examine nano-sized FeO dust as a carrier for the 21μm feature. We calculate the IR emission spectrum of FeO nanodust which undergoes single-photon heating in PPNe. It is found that the 21μm feature emitted by FeO nanodust is too broad to explain the observed feature. For the 30μm feature, we argue that graphite could be a viable carrier. Graphite, provided its d.c. conductivity σd.c. exceeds ~100ohm−1cm−1, exhibits a pronounced band at 30μm.
Two GeV-TeV Supernova Remnants without Associated Neutral and Molecular Clouds
Authors: Tian W. , Leahy D. , Zhu H. , Su H. 
Published: February 2014

AbstractTeV gamma ray emissions have been detected at the directions of supernova remnants (SNRs) W51C and Tycho SNR. We analyze the Hi absorption spectra towards W51C, Tycho SNR and their nearby compact sources. We conclude that W51C is at a distance of about 4.3 kpc and Tycho SNR has a distance of 2.5 ~ 3.0 kpc. Our study detects high-velocity Hi clouds which coincide with star formation region W51B, but finds that the clouds are behind W51B which argues against previous claims that W51C has shocked the high velocity Hi clouds. We argue that Tycho SNR is naked Ia SNR (lack of evidence of interacting with adjacent neutral and molecular cloud). This gives two examples that the very high gamma ray emission from SNRs does not likely originate from SNR-cloud interaction.
Laboratory Electronic Spectra of Carbon Chains and Rings
Authors: Zack L. N. , Maier J. P. 
Published: February 2014

AbstractCarriers of the diffuse interstellar bands (DIBs) cannot be definitively identified without laboratory spectra. Several techniques, including matrix isolation, cavity ringdown spectroscopy, resonance enhanced multiphoton ionization, and ion trapping, have been used to measure the electronic spectra of carbon chains and their derivatives. The gas-phase laboratory spectra could then be compared to the astronomical data of known DIBs. The choice of molecules studied in the gas phase depends on the presence of strong electronic transitions at optical wavelengths, the lifetimes of excited electronic states, and chemical feasibility in diffuse astrophysical environments. Collisional-radiative rate models have also be used in conjunction with laboratory spectra to predict absorption profiles under interstellar conditions.
Laboratory Studies on the Role of PAHs as DIB Carriers
Authors: Huisken F. , Rouillé G. , Steglich M. , Carpentier Y. , Jäger C. , Henning Th. 
Published: February 2014

AbstractThe electronic spectroscopy of various polycyclic aromatic hydrocarbon (PAH) molecules has been studied in the laboratory at low temperatures using both molecular beam and matrix isolation spectroscopy techniques. While molecular beam spectra can be readily compared to astronomical observations, the band positions measured in Ne and Ar matrices are extrapolated to obtain rather good estimates for the same transitions in the gas phase. Absolute absorption cross sections are determined for gas-phase and matrix spectra by comparing them with calibrated solution spectra. All laboratory results are analyzed and discussed in view of the role that PAHs can play as carriers of the diffuse interstellar bands (DIBs). Our studies suggest that regular neutral PAHs are not responsible for any of the known strong DIBs.
Developments of Optical Spectrometers as Approaches to Diffuse Interstellar Bands
Authors: Araki M. , Uchida S. , Kondo N. , Matsushita Y. , Abe K. , Ito K. , Tsukiyama K. 
Published: February 2014

AbstractA discharge-emission spectrometer and a cavity ringdown spectrometer have been developed to aid in the solution to the diffuse interstellar band (DIB) problem. A hollow cathode was used to generate molecular ions in a discharge because it has been suggested that molecular ions are probable DIB candidates. The discharge was produced by a pulsed voltage of 1300–1500 V. A wide wavelength range of optical emission from the discharge was examined by a HORIBA Jobin Yvon iHR320 monochromator. The dispersed discharge emission was detected by a photomultiplier and was recorded via a lock-in amplifier. The 2B3u–X2B2g electronic transition of the butatriene cation H2CCCCH2+ was observed in the discharge emission of 2-butyne H3CCCCH3. The frequency of the electronic transition was measured to be 20381 cm−1, and a comparison study was made with known DIB spectra.The resolution of the discharge-emission spectrometer is insufficient to make precise comparisons between laboratory frequencies and astronomically observed DIB spectra. We therefore developed the cavity ringdown spectrometer using the same hollow cathode. The high sensitivity of this spectrometer was confirmed by the observation of the forbidden band of O2.
The 4051 Å Comet Band of 13C3
Authors: Haddad M.A. , Zhao D. , Linnartz H. , Ubachs W. 
Published: February 2014

AbstractThe tricarbon C3 molecule has been detected in a number of translucent interstellar clouds via its $A^1\Pi_{u}-X^1\Sigma_{g}^{+}$ (000-000) electronic ‘comet’ band around 4051 Å. So far, it is the largest molecule unambiguously identified in the diffuse interstellar medium. In this work, rotationally resolved laboratory spectra are presented for the corresponding transition of the 13C3 isotopologue. The spectra are recorded in direct absorption using cavity ring-down spectroscopy in combination with a supersonic plasma jet. A rotational analysis yields accurate spectroscopic parameters. In contrast to 12C3, no significant perturbations are found for (e− or f-parity) levels up to J' = 18 in the A1Π upper electronic state.
Observational Constraints for Modeling Diffuse Molecular Clouds
Authors: Federman S. R. 
Published: February 2014

AbstractGround-based and space-borne observations of diffuse molecular clouds suggest a number of areas where further improvements to modeling efforts is warranted. I will highlight those that have the widest applicability. The range in CO fractionation caused by selective isotope photodissociation, in particular the large 12C16O/13C16O ratios observed toward stars in Ophiuchus, is not reproduced well by current models. Our ongoing laboratory measurements of oscillator strengths and predissociation rates for Rydberg transitions in CO isotopologues may help clarify the situtation. The CH+ abundance continues to draw attention. Small scale structure seen toward ζ Per may provide additional constraints on the possible synthesis routes. The connection between results from optical transitions and those from radio and sub-millimeter wave transitions requires further effort. A study of OH+ and OH toward background stars reveals that these species favor different environments. This brings to focus the need to model each cloud along the line of sight separately, and to allow the physical conditions to vary within an individual cloud, in order to gain further insight into the chemistry. Now that an extensive set of data on molecular excitation is available, the models should seek to reproduce these data to place further constraints on the modeling results.
The Stability of Cosmic Fullerenes and Fullerenic Aggregates
Authors: Micelotta E. R. , Cami J. , Peeters E. , Zettergren H. , Schmidt H. T. , Cederquist H. , Jones A. P. , Tielens A. G. G. M. 
Published: February 2014

AbstractEstablishing the stability of cosmic fullerenes and fullerenic aggregates is extremely relevant for a variety of reasons. For instance, the emission features of C60 and C70 fall in the same spectral region as the Un-identified InfraRed (UIR) bands, which they could contribute to. To be able to contribute to the UIR emission, however, fullerenes must be able to survive long enough against the destruction mechanisms operating in the interstellar medium. In this study we focus on the effects of collisional processing, i.e., the bombardment by energetic ions and electrons. A recent experimental/theoretical study has shown that ion collisions with C60 clusters result in the dissociation of the cluster with the simultaneous formation of covalent fullerene dimers, which could play a role as DIBs carriers. We present here our first results about the collisional processing of C60 molecules and clusters by H, He and C ions in interstellar shocks. We have adapted the models that have previously been developed to successfully treat the collisional processing of PAHs in space. The nature of the interaction and the similarities between PAHs and fullerenes make this approach appropriate. In addition, our study shows that the formation of covalent dimers following ion collisions with C60 clusters is compatible with the astrophysical conditions under consideration.
Theoretical Investigation of PAHs: Implications to Diffuse Interstellar Bands
Authors: Pathak A. , Buragohain M. , Hammonds M. , Sarre P. J. 
Published: February 2014

AbstractAbout a thousand optical absorption features on the interstellar extinction curve popularly known as the Diffuse Interstellar Bands (DIBs) have been observed. The numbers are increasing every year, thanks to the improvement in telescope and spectroscopic technology. Ultra-high resolution spectroscopic observations and emission features corresponding to some of the DIBs suggest that, some if not all, of these features are due to large molecules. The strength of DIBs depend on the amount of reddening which is directly proportional to the amount of material present between the background star and the observer. Since, the strengths of the DIBs are not strongly correlated with each other, there must be several carriers. Time Dependent Density Functional Theory (TDDFT) calculations are useful in narrowing down molecular systems that may be further investigated in the laboratory.The observations of the unidentified infrared (UIR) bands point towards the widespread presence of Polycyclic Aromatic Hydrocarbon (PAH) molecules. Though, not a single PAH has been discovered in interstellar space, these are the largest molecules suspected to be present. PAHs are stable towards energetic environment prevailing under interstellar conditions rendering these molecules to be good candidates as DIB carriers. We report TDDFT calculations to predict electronic transitions of neutral, protonated-deuteronated and PAHs with five member rings with various sites of protonation and deuteronation. Compared to their neutral forms, these charged isoelectronic forms of PAHs are predicted to have active transitions in the visible region, which means they are suitable candidates as carriers for some of the DIBs and laboratory studies are warranted for these systems.
Dynamics of Synthesis of Large Carbon Structures in the Interstellar Medium
Authors: Patra N. , Sadeghpour H. R. 
Published: February 2014

AbstractWe investigate the nucleation of carbon and hydrogen atoms in the gas phase to form large carbon chains, clusters and cages by reactive molecular dynamics simulations. We study how temperature, particle density, presence of hydrogen, and carbon inflow affect the nucleation of molecular moieties with different characteristics.
Can Fullerene Analogues be the Carriers of the Diffuse Interstellar Bands?
Authors: Cami J. 
Published: February 2014

AbstractFullerenes and their derivatives are amongst the most stable carbonaceous species known and have therefore been proposed as ideal candidates to carry some of the diffuse interstellar bands (DIBs). Evidence for these species in space first came from a few DIBs that have been tentatively identified with electronic transitions of C60+; in recent years, infrared observations have furthermore revealed fullerenes in a variety of circumstellar and interstellar environments. With the presence of the fullerene family in space established, we review what is known about cosmic fullerenes and their derivatives and what role they could play as potential DIB carriers.
The Promise of Recent and Future Observatories and Instruments
Authors: Kaper L 
Published: February 2014

AbstractThe identification of the carrier(s) of diffuse interstellar bands (DIBs) is one of the oldest mysteries in stellar spectroscopy. With the advent of 8-10m-class telescopes substantial progress has been made in measuring the properties of DIBs in the optical and near-infrared wavelength domain, not only in the Galaxy, but also in different environments encountered in Local Group galaxies and beyond. Still, the DIB carriers have remained unidentified. The coming decade will witness the development of extremely large telescopes (GMT, TMT and E-ELT) and their instrumentation. In this overview I will highlight the current instrumentation plan of these future observatories, emphasizing their potential role in solving the enigma of the DIBs.
Diffuse Interstellar Bands: The Way Forward
Authors: Tielens A. G. G. M. 
Published: February 2014

AbstractRather than a summary of the conference, I present here an overview of the status of the field and our progress over the last two decades from the points of view of astronomy, molecular physics, spectroscopy, and astrochemistry. While at first sight, progress may seem slow, actually, we have made an important stride forward. We have recognized now that the problem is very complex and identifying the carriers of the Diffuse Interstellar Bands will require a concerted effort of astronomers, molecular physicists, spectroscopists, and astrochemists. While this is a daunting prospect, we have identified the tools that we need to make this happen.