@article{CassanBeaulieuBrillantetal.2004, author = {Cassan, A. and Beaulieu, Jean-Philippe and Brillant, Stephane and Coutures, C. and Dominik, M. and Donatowicz, J. and Jorgensen, Uffe Grae and Kubas, Daniel and Albrow, Michael D. and Caldwell, John A. R. and Fouque, P. and Greenhill, John and Hill, K. and Horne, Keith and Kane, Stephen R. and Martin, Ralph and Menzies, J. W. and Pollard, K. R. and Sahu, K. C. and Vinter, C. and Wambsganss, Joachim and Watson, R. and Williams, A. and Fendt, Christian and Hauschildt, P. and Heinmueller, Janine and Marquette, Jean-Baptiste and Thurl, C.}, title = {Probing the atmosphere of the bulge G5III star OGLE-2002-BUL-069 by analysis of microlensed H alpha line}, year = {2004}, abstract = {We discuss high-resolution, time-resolved spectra of the caustic exit of the binary microlensing event OGLE 2002-BLG-069 obtained with UVES on the VLT. The source star is a G5III giant in the Galactic Bulge. During such events, the source star is highly magnified, and a strong differential magnification around the caustic resolves its surface. Using an appropriate model stellar atmosphere generated by the PHOENIX v2.6 code we obtain a model light curve for the caustic exit and compare it with a dense set of photometric observations obtained by the PLANET microlensing follow up network. We further compare predicted variations in the Halpha equivalent width with those measured from our spectra. While the model and observations agree in the gross features, there are discrepancies suggesting shortcomings in the model, particularly for the Halpha line core, where we have detected amplified emission from the stellar chromosphere after the source star's trailing limb exited the caustic. This achievement became possible by the provision of the very efficient OGLE-III Early Warning System, a network of small telescopes capable of nearly-continuous round-the-clock photometric monitoring, on-line data reduction, daily near-real-time modelling in order to predict caustic crossing parameters, and a fast and efficient response of a 8 m class telescope to a "Target-of-Opportunity" observation request}, language = {en} } @article{JiangDePoyGalYametal.2004, author = {Jiang, G. F. and DePoy, D. L. and Gal-Yam, A. and Gaudi, B. S. and Gould, A. and Han, C. and Lipkin, Y. and Maoz, D. and Ofek, E. O. and Park, B. G. and Pogge, R. W. and Udalski, A. and Kubiak, Marcin and Szymanski, M. K. and Szewczyk, O. and Zerbrun, K. and Wyrzykowski, L. and Soszynski, I. and Pietrzynski, G. and Albrow, Michael D. and Beaulieu, Jean-Philippe and Caldwell, John A. R. and Cassan, A. and Coutures, C. and Dominik, M. and Donatowicz, J. and Fouque, P. and Greenhill, John and Hill, K. and Horne, Keith and Jorgensen, S. F. and Jorgensen, Uffe Grae and Kane, Stephen R. and Kubas, Daniel and Martin, Ralph and Menzies, J. W. and Pollard, R. and Sahu, K. C. and Wambsganss, Joachim and Watson, R. and Williams, A.}, title = {OGLE-2003-BLG-238 : Microlensing mass estimate of an isolated star}, issn = {0004-637X}, year = {2004}, abstract = {Microlensing is the only known direct method to measure the masses of stars that lack visible companions. In terms of microlensing observables, the mass is given by M (c(2)/4G)(r) over tilde (E)theta(E) and so requires the measurement of both the angular Einstein radius theta(E) and the projected Einstein radius (r) over tilde (E). Simultaneous measurement of these two parameters is extremely rare. Here we analyze OGLE-2003-BLG-238, a spectacularly bright (I-min 10.3), high-magnification (A(max) 170) microlensing event. Pronounced finite-source effects permit a measurement of theta(E) = 650 muas. Although the timescale of the event is only t(E) 38 days, one can still obtain weak constraints on the microlens parallax: 4.4 AU < <(r)over tilde>(E) < 18 AU at the 1 \σ level. Together these two parameter measurements yield a range for the lens mass of 0.36 M-\&ODOT; < M < 1.48 M-\&ODOT;. As was the case for MACHO- LMC-5, the only other single star (apart from the Sun) whose mass has been determined from its gravitational effects, this estimate is rather crude. It does, however, demonstrate the viability of the technique. We also discuss future prospects for single-lens mass measurements}, language = {en} } @article{TreatKleinenBroothaertsetal.2019, author = {Treat, Claire C. and Kleinen, Thomas and Broothaerts, Nils and Dalton, April S. and Dommain, Rene and Douglas, Thomas A. and Drexler, Judith Z. and Finkelstein, Sarah A. and Grosse, Guido and Hope, Geoffrey and Hutchings, Jack and Jones, Miriam C. and Kuhry, Peter and Lacourse, Terri and Lahteenoja, Outi and Loisel, Julie and Notebaert, Bastiaan and Payne, Richard J. and Peteet, Dorothy M. and Sannel, A. Britta K. and Stelling, Jonathan M. and Strauss, Jens and Swindles, Graeme T. and Talbot, Julie and Tarnocai, Charles and Verstraeten, Gert and Williams, Christopher J. and Xia, Zhengyu and Yu, Zicheng and Valiranta, Minna and Hattestrand, Martina and Alexanderson, Helena and Brovkin, Victor}, title = {Widespread global peatland establishment and persistence over the last 130,000 y}, series = {Proceedings of the National Academy of Sciences of the United States of America}, volume = {116}, journal = {Proceedings of the National Academy of Sciences of the United States of America}, number = {11}, publisher = {National Acad. of Sciences}, address = {Washington}, issn = {0027-8424}, doi = {10.1073/pnas.1813305116}, pages = {4822 -- 4827}, year = {2019}, abstract = {Glacial-interglacial variations in CO2 and methane in polar ice cores have been attributed, in part, to changes in global wetland extent, but the wetland distribution before the Last Glacial Maximum (LGM, 21 ka to 18 ka) remains virtually unknown. We present a study of global peatland extent and carbon (C) stocks through the last glacial cycle (130 ka to present) using a newly compiled database of 1,063 detailed stratigraphic records of peat deposits buried by mineral sediments, as well as a global peatland model. Quantitative agreement between modeling and observations shows extensive peat accumulation before the LGM in northern latitudes (> 40 degrees N), particularly during warmer periods including the last interglacial (130 ka to 116 ka, MIS 5e) and the interstadial (57 ka to 29 ka, MIS 3). During cooling periods of glacial advance and permafrost formation, the burial of northern peatlands by glaciers and mineral sediments decreased active peatland extent, thickness, and modeled C stocks by 70 to 90\% from warmer times. Tropical peatland extent and C stocks show little temporal variation throughout the study period. While the increased burial of northern peats was correlated with cooling periods, the burial of tropical peat was predominately driven by changes in sea level and regional hydrology. Peat burial by mineral sediments represents a mechanism for long-term terrestrial C storage in the Earth system. These results show that northern peatlands accumulate significant C stocks during warmer times, indicating their potential for C sequestration during the warming Anthropocene.}, language = {en} } @article{ToySutherlandTownendetal.2017, author = {Toy, Virginia Gail and Sutherland, Rupert and Townend, John and Allen, Michael J. and Becroft, Leeza and Boles, Austin and Boulton, Carolyn and Carpenter, Brett and Cooper, Alan and Cox, Simon C. and Daube, Christopher and Faulkner, D. R. and Halfpenny, Angela and Kato, Naoki and Keys, Stephen and Kirilova, Martina and Kometani, Yusuke and Little, Timothy and Mariani, Elisabetta and Melosh, Benjamin and Menzies, Catriona D. and Morales, Luiz and Morgan, Chance and Mori, Hiroshi and Niemeijer, Andre and Norris, Richard and Prior, David and Sauer, Katrina and Schleicher, Anja Maria and Shigematsu, Norio and Teagle, Damon A. H. and Tobin, Harold and Valdez, Robert and Williams, Jack and Yeo, Samantha and Baratin, Laura-May and Barth, Nicolas and Benson, Adrian and Boese, Carolin and C{\´e}l{\´e}rier, Bernard and Chamberlain, Calum J. and Conze, Ronald and Coussens, Jamie and Craw, Lisa and Doan, Mai-Linh and Eccles, Jennifer and Grieve, Jason and Grochowski, Julia and Gulley, Anton and Howarth, Jamie and Jacobs, Katrina and Janku-Capova, Lucie and Jeppson, Tamara and Langridge, Robert and Mallyon, Deirdre and Marx, Ray and Massiot, C{\´e}cile and Mathewson, Loren and Moore, Josephine and Nishikawa, Osamu and Pooley, Brent and Pyne, Alex and Savage, Martha K. and Schmitt, Doug and Taylor-Offord, Sam and Upton, Phaedra and Weaver, Konrad C. and Wiersberg, Thomas and Zimmer, Martin}, title = {Bedrock geology of DFDP-2B, central Alpine Fault, New Zealand}, series = {New Zealand journal of geology and geophysics : an international journal of the geoscience of New Zealand, the Pacific Rim, and Antarctica ; NZJG}, volume = {60}, journal = {New Zealand journal of geology and geophysics : an international journal of the geoscience of New Zealand, the Pacific Rim, and Antarctica ; NZJG}, number = {4}, publisher = {Taylor \& Francis}, address = {Abingdon}, organization = {DFDP-2 Sci Team}, issn = {0028-8306}, doi = {10.1080/00288306.2017.1375533}, pages = {497 -- 518}, year = {2017}, abstract = {During the second phase of the Alpine Fault, Deep Fault Drilling Project (DFDP) in the Whataroa River, South Westland, New Zealand, bedrock was encountered in the DFDP-2B borehole from 238.5-893.2 m Measured Depth (MD). Continuous sampling and meso- to microscale characterisation of whole rock cuttings established that, in sequence, the borehole sampled amphibolite facies, Torlesse Composite Terrane-derived schists, protomylonites and mylonites, terminating 200-400 m above an Alpine Fault Principal Slip Zone (PSZ) with a maximum dip of 62°. The most diagnostic structural features of increasing PSZ proximity were the occurrence of shear bands and reduction in mean quartz grain sizes. A change in composition to greater mica:quartz + feldspar, most markedly below c. 700 m MD, is inferred to result from either heterogeneous sampling or a change in lithology related to alteration. Major oxide variations suggest the fault-proximal Alpine Fault alteration zone, as previously defined in DFDP-1 core, was not sampled.}, language = {en} } @article{vanDrielGesztelyiBakerToeroeketal.2014, author = {van Driel-Gesztelyi, L. and Baker, Daniel N. and Toeroek, T. and Pariat, E. and Green, L. M. and Williams, D. R. and Carlyle, J. and Valori, G. and Demoulin, Pascal and Kliem, Bernhard and Long, D. M. and Matthews, S. A. and Malherbe, J. -M.}, title = {Coronal magnetic reconnection driven by CME expansion-the 2011 June 7 event}, series = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, volume = {788}, journal = {The astrophysical journal : an international review of spectroscopy and astronomical physics}, number = {1}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {0004-637X}, doi = {10.1088/0004-637X/788/1/85}, pages = {12}, year = {2014}, abstract = {Coronal mass ejections (CMEs) erupt and expand in a magnetically structured solar corona. Various indirect observational pieces of evidence have shown that the magnetic field of CMEs reconnects with surrounding magnetic fields, forming, e.g., dimming regions distant from the CME source regions. Analyzing Solar Dynamics Observatory (SDO) observations of the eruption from AR 11226 on 2011 June 7, we present the first direct evidence of coronal magnetic reconnection between the fields of two adjacent active regions during a CME. The observations are presented jointly with a data-constrained numerical simulation, demonstrating the formation/intensification of current sheets along a hyperbolic flux tube at the interface between the CME and the neighboring AR 11227. Reconnection resulted in the formation of new magnetic connections between the erupting magnetic structure from AR 11226 and the neighboring active region AR 11227 about 200 Mm from the eruption site. The onset of reconnection first becomes apparent in the SDO/AIA images when filament plasma, originally contained within the erupting flux rope, is redirected toward remote areas in AR 11227, tracing the change of large-scale magnetic connectivity. The location of the coronal reconnection region becomes bright and directly observable at SDO/AIA wavelengths, owing to the presence of down-flowing cool, dense (1010 cm(-3)) filament plasma in its vicinity. The high-density plasma around the reconnection region is heated to coronal temperatures, presumably by slow-mode shocks and Coulomb collisions. These results provide the first direct observational evidence that CMEs reconnect with surrounding magnetic structures, leading to a large-scale reconfiguration of the coronal magnetic field.}, language = {en} } @misc{DrielGesztelyiBakerToeroeketal.2013, author = {Driel-Gesztelyi, L. van and Baker, Daniel N. and T{\"o}r{\"o}k, Tibor and Pariat, Etienne and Green, L. M. and Williams, D. R. and Carlyle, J. and Valori, G. and D{\´e}moulin, Pascal and Matthews, S. A. and Kliem, Bernhard and Malherbe, J.-M.}, title = {Magnetic reconnection driven by filament eruption in the 7 June 2011 event}, series = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, journal = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, number = {608}, doi = {10.25932/publishup-41567}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-415671}, pages = {502 -- 503}, year = {2013}, abstract = {During an unusually massive filament eruption on 7 June 2011, SDO/AIA imaged for the first time significant EUV emission around a magnetic reconnection region in the solar corona. The reconnection occurred between magnetic fields of the laterally expanding CME and a neighbouring active region. A pre-existing quasi-separatrix layer was activated in the process. This scenario is supported by data-constrained numerical simulations of the eruption. Observations show that dense cool filament plasma was re-directed and heated in situ, producing coronal-temperature emission around the reconnection region. These results provide the first direct observational evidence, supported by MHD simulations and magnetic modelling, that a large-scale re-configuration of the coronal magnetic field takes place during solar eruptions via the process of magnetic reconnection.}, language = {en} } @article{SackettAlbrowBeaulieuetal.2003, author = {Sackett, Penny D. and Albrow, Michael D. and Beaulieu, Jean-Philippe and Caldwell, John A. R. and Coutures, C. and Dominik, M. and Greenhill, John and Hill, K. and Horne, Keith and Jorgensen, Uffe Grae and Kane, Stephen R. and Kubas, Daniel and Martin, Ralph and Menzies, J. W. and Pollard, K. R. and Sahu, K. C. and Wambsganß, Joachim and Watson, R. and Williams, A.}, title = {PLANET II : a microlensing and transit search for extrasolar planets}, year = {2003}, abstract = {Due to their extremely small luminosity compared to the stars they orbit, planets outside our own Solar System are extraordinarily difficult to detect directly in optical light. Careful photometric monitoring of distant stars, however, can reveal the presence of exoplanets via the microlensing or eclipsing effects they induce. The international PLANET collaboration is performing such monitoring using a cadre of semi-dedicated telescopes around the world. Their results constrain the number of gas giants orbiting 1-7 AU from the most typical stars in the Galaxy. Upgrades in the program are opening regions of ''exoplanet discovery space'' - toward smaller masses and larger orbital radii - that are inaccessible to the Doppler velocity technique.}, language = {en} } @article{FurnissWorseckFumagallietal.2019, author = {Furniss, Amy and Worseck, Gabor and Fumagalli, Michele and Johnson, Caitlin A. and Williams, David A. and Pontrelli, P. and Prochaska, J. Xavier}, title = {Spectroscopic Redshift of the Gamma-Ray Blazar B2 1215+30 from Ly alpha Emission}, series = {The astronomical journal}, volume = {157}, journal = {The astronomical journal}, number = {2}, publisher = {IOP Publ. Ltd.}, address = {Bristol}, issn = {0004-6256}, doi = {10.3847/1538-3881/aaf28b}, pages = {4}, year = {2019}, abstract = {We report on Cosmic Origin Spectrograph observations of the gamma-ray bright blazar B2 1215+30, collected in 2015 November. These observations allow for the confirmation of the source redshift from the detection of a Lyα emission feature at λ ~ 1374 {\AA}. The emission feature places the source at a redshift of z = 0.1305 ± 0.003, confirming the source's ground-based spectral measurement. The gamma-ray emission of the source is discussed in the context of the source distance, required for the accurate reconstruction of the intrinsic gamma-ray emission taking the absorption by the extragalactic background light into account. The source distance is found to be low enough that the previously reported detection of an exceptional flaring event from B2 1215+30 in 2014 cannot be used to investigate opacity-specific spectral and variability characteristics introduced by possible ultra-high-energy cosmic-ray propagation.}, language = {en} } @article{MaddockChilderstoneFryetal.2017, author = {Maddock, Simon T. and Childerstone, Aaron and Fry, Bryan Grieg and Williams, David J. and Barlow, Axel and Wuester, Wolfgang}, title = {Multi-locus phylogeny and species delimitation of Australo-Papuan blacksnakes (Pseudechis Wagler, 1830: Elapidae: Serpentes)}, series = {Molecular phylogenetics and evolution}, volume = {107}, journal = {Molecular phylogenetics and evolution}, publisher = {Elsevier}, address = {San Diego}, issn = {1055-7903}, doi = {10.1016/j.ympev.2016.09.005}, pages = {48 -- 55}, year = {2017}, abstract = {Genetic analyses of Australasian organisms have resulted in the identification of extensive cryptic diversity across the continent. The venomous elapid snakes are among the best-studied organismal groups in this region, but many knowledge gaps persist: for instance, despite their iconic status, the species-level diversity among Australo-Papuan blacksnakes (Pseudechis) has remained poorly understood due to the existence of a group of cryptic species within the P. australis species complex, collectively termed "pygmy mulga snakes". Using two mitochondrial and three nuclear loci we assess species boundaries within the genus using Bayesian species delimitation methods and reconstruct their phylogenetic history using multispecies coalescent approaches. Our analyses support the recognition of 10 species, including all of the currently described pygmy mulga snakes and one undescribed species from the Northern Territory of Australia. Phylogenetic relationships within the genus are broadly consistent with previous work, with the recognition of three major groups, the viviparous red-bellied black snake P. porphyriacus forming the sister species to two clades consisting of ovoviviparous species.}, language = {en} } @article{KefiBerlowWietersetal.2012, author = {Kefi, Sonia and Berlow, Eric L. and Wieters, Evie A. and Navarrete, Sergio A. and Petchey, Owen L. and Wood, Spencer A. and Boit, Alice and Joppa, Lucas N. and Lafferty, Kevin D. and Williams, Richard J. and Martinez, Neo D. and Menge, Bruce A. and Blanchette, Carol A. and Iles, Alison C. and Brose, Ulrich}, title = {More than a meal ... integrating non-feeding interactions into food webs}, series = {Ecology letters}, volume = {15}, journal = {Ecology letters}, number = {4}, publisher = {Wiley-Blackwell}, address = {Hoboken}, issn = {1461-023X}, doi = {10.1111/j.1461-0248.2011.01732.x}, pages = {291 -- 300}, year = {2012}, abstract = {Organisms eating each other are only one of many types of well documented and important interactions among species. Other such types include habitat modification, predator interference and facilitation. However, ecological network research has been typically limited to either pure food webs or to networks of only a few (<3) interaction types. The great diversity of non-trophic interactions observed in nature has been poorly addressed by ecologists and largely excluded from network theory. Herein, we propose a conceptual framework that organises this diversity into three main functional classes defined by how they modify specific parameters in a dynamic food web model. This approach provides a path forward for incorporating non-trophic interactions in traditional food web models and offers a new perspective on tackling ecological complexity that should stimulate both theoretical and empirical approaches to understanding the patterns and dynamics of diverse species interactions in nature.}, language = {en} } @article{BoitMartinezWilliamsetal.2012, author = {Boit, Alice and Martinez, Neo D. and Williams, Richard J. and Gaedke, Ursula}, title = {Mechanistic theory and modelling of complex food-web dynamics in Lake Constance}, series = {Ecology letters}, volume = {15}, journal = {Ecology letters}, number = {6}, publisher = {Wiley-Blackwell}, address = {Hoboken}, issn = {1461-023X}, doi = {10.1111/j.1461-0248.2012.01777.x}, pages = {594 -- 602}, year = {2012}, abstract = {Mechanistic understanding of consumer-resource dynamics is critical to predicting the effects of global change on ecosystem structure, function and services. Such understanding is severely limited by mechanistic models inability to reproduce the dynamics of multiple populations interacting in the field. We surpass this limitation here by extending general consumer-resource network theory to the complex dynamics of a specific ecosystem comprised by the seasonal biomass and production patterns in a pelagic food web of a large, well-studied lake. We parameterised our allometric trophic network model of 24 guilds and 107 feeding relationships using the lakes food web structure, initial spring biomasses and body-masses. Adding activity respiration, the detrital loop, minimal abiotic forcing, prey resistance and several empirically observed rates substantially increased the model's fit to the observed seasonal dynamics and the size-abundance distribution. This process illuminates a promising approach towards improving food-web theory and dynamic models of specific habitats.}, language = {en} } @article{RichardsonShenarRoyLoubieretal.2016, author = {Richardson, Noel D. and Shenar, Tomer and Roy-Loubier, Olivier and Schaefer, Gail and Moffat, Anthony F. J. and St-Louis, Nicole and Gies, Douglas R. and Farrington, Chris and Hill, Grant M. and Williams, Peredur M. and Gordon, Kathryn and Pablo, Herbert and Ramiaramanantsoa, Tahina}, title = {The CHARA Array resolves the long-period Wolf-Rayet binaries WR 137 and WR 138}, series = {Monthly notices of the Royal Astronomical Society}, volume = {461}, journal = {Monthly notices of the Royal Astronomical Society}, publisher = {Oxford Univ. Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1093/mnras/stw1585}, pages = {4115 -- 4124}, year = {2016}, abstract = {We report on interferometric observations with the CHARAArray of two classical Wolf-Rayet (WR) stars in suspected binary systems, namely WR 137 and WR 138. In both cases, we resolve the component stars to be separated by a few milliarcseconds. The data were collected in the H band, and provide a measure of the fractional flux for both stars in each system. We find that the WR star is the dominant H-band light source in both systems (fWR, 137 = 0.59 +/- 0.04; fWR, 138 = 0.67 +/- 0.01), which is confirmed through both comparisons with estimated fundamental parameters for WR stars and O dwarfs, as well as through spectral modelling of each system. Our spectral modelling also provides fundamental parameters for the stars and winds in these systems. The results on WR 138 provide evidence that it is a binary system which may have gone through a previous mass-transfer episode to create the WR star. The separation and position of the stars in the WR 137 system together with previous results from the IOTA interferometer provides evidence that the binary is seen nearly edgeon. The possible edge-on orbit of WR 137 aligns well with the dust production site imaged by the Hubble Space Telescope during a previous periastron passage, showing that the dust production may be concentrated in the orbital plane.}, language = {en} } @article{HommesSchattmannNeffeAhmadetal.2017, author = {Hommes-Schattmann, Paul J. and Neffe, Axel T. and Ahmad, Bilal and Williams, Gareth R. and Vanneaux, Valerie and Menasche, Philippe and Kalfa, David and Lendlein, Andreas}, title = {RGD constructs with physical anchor groups as polymer co-electrospinnable cell adhesives}, series = {Polymers for advanced technologies}, volume = {28}, journal = {Polymers for advanced technologies}, publisher = {Wiley}, address = {Hoboken}, issn = {1042-7147}, doi = {10.1002/pat.3963}, pages = {1312 -- 1317}, year = {2017}, abstract = {The tissue integration of synthetic polymers can be promoted by displaying RGD peptides at the biointerface with the objective of enhancing colonization of the material by endogenous cells. A firm but flexible attachment of the peptide to the polymer matrix, still allowing interaction with receptors, is therefore of interest. Here, the covalent coupling of flexible physical anchor groups, allowing for temporary immobilization on polymeric surfaces via hydrophobic or dipole-dipole interactions, to a RGD peptide was investigated. For this purpose, a stearate or an oligo(ethylene glycol) (OEG) was attached to GRGDS in 51-69\% yield. The obtained RGD linker constructs were characterized by NMR, IR and MALDI-ToF mass spectrometry, revealing that the commercially available OEG and stearate linkers are in fact mixtures of similar compounds. The RGD linker constructs were co-electrospun with poly(p-dioxanone) (PPDO). After electrospinning, nitrogen could be detected on the surface of the PPDO fibers by X-ray photoelectron spectroscopy. The nitrogen content exceeded the calculated value for the homogeneous material mixture suggesting a pronounced presentation of the peptide on the fiber surface. Increasing amounts of RGD linker constructs in the electrospinning solution did not lead to a detection of an increased amount of peptide on the scaffold surface, suggesting inhomogeneous distribution of the peptide on the PPDO fiber surface. Human adipose-derived stem cells cultured on the patches showed similar viability as when cultured on PPDO containing pristine RGD. The fully characterized RGD linker constructs could serve as valuable tools for the further development of tissue-integrating polymeric scaffolds. Copyright (c) 2016 John Wiley \& Sons, Ltd.}, language = {en} } @misc{GvaramadzeKniazevMiroshnichenkoetal.2012, author = {Gvaramadze, V. V. and Kniazev, A. Y. and Miroshnichenko, A. S. and Berdnikov, Leonid N. and Langer, N. and Stringfellow, G. S. and Todt, Helge Tobias and Hamann, Wolf-Rainer and Grebel, E. K. and Buckley, D. and Crause, L. and Crawford, S. and Gulbis, A. and Hettlage, C. and Hooper, E. and Husser, T. -O. and Kotze, P. and Loaring, N. and Nordsieck, K. H. and O'Donoghue, D. and Pickering, T. and Potter, S. and Colmenero, E. Romero and Vaisanen, P. and Williams, T. and Wolf, M. and Reichart, D. E. and Ivarsen, K. M. and Haislip, J. B. and Nysewander, M. C. and LaCluyze, A. P.}, title = {Discovery of two new Galactic candidate luminous blue variables with Wide-field Infrared Survey Explorer}, series = {Monthly notices of the Royal Astronomical Society}, volume = {421}, journal = {Monthly notices of the Royal Astronomical Society}, number = {4}, publisher = {Oxford Univ. Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1111/j.1365-2966.2012.20556.x}, pages = {3325 -- 3337}, year = {2012}, abstract = {We report the discovery of two new Galactic candidate luminous blue variable (LBV) stars via detection of circular shells (typical of confirmed and candidate LBVs) and follow-up spectroscopy of their central stars. The shells were detected at 22 mu m in the archival data of the Mid-Infrared All Sky Survey carried out with the Wide-field Infrared Survey Explorer (WISE). Follow-up optical spectroscopy of the central stars of the shells conducted with the renewed Southern African Large Telescope (SALT) showed that their spectra are very similar to those of the well-known LBVs P Cygni and AG Car, and the recently discovered candidate LBV MN112, which implies the LBV classification for these stars as well. The LBV classification of both stars is supported by detection of their significant photometric variability: one of them brightened in the R and I bands by 0.68 +/- 0.10 and 0.61 +/- 0.04 mag, respectively, during the last 1318 years, while the second one (known as Hen 3-1383) varies its B, V, R, I and Ks brightnesses by similar or equal to 0.50.9 mag on time-scales from 10 d to decades. We also found significant changes in the spectrum of Hen 3-1383 on a time-scale of similar or equal to 3 months, which provides additional support for the LBV classification of this star. Further spectrophotometric monitoring of both stars is required to firmly prove their LBV status. We discuss a connection between the location of massive stars in the field and their fast rotation, and suggest that the LBV activity of the newly discovered candidate LBVs might be directly related to their possible runaway status.}, language = {en} } @article{LuetzowHommesSchattmannNeffeetal.2018, author = {L{\"u}tzow, Karola and Hommes-Schattmann, Paul J. and Neffe, Axel T. and Ahmad, Bilal and Williams, Gareth R. and Lendlein, Andreas}, title = {Perfluorophenyl azide functionalization of electrospun poly(para-dioxanone)}, series = {Polymers for advanced technologies}, volume = {30}, journal = {Polymers for advanced technologies}, number = {5}, publisher = {Wiley}, address = {Hoboken}, issn = {1042-7147}, doi = {10.1002/pat.4331}, pages = {1165 -- 1172}, year = {2018}, abstract = {Strategies to surface-functionalize scaffolds by covalent binding of biologically active compounds are of fundamental interest to control the interactions between scaffolds and biomolecules or cells. Poly(para-dioxanone) (PPDO) is a clinically established polymer that has shown potential as temporary implant, eg, for the reconstruction of the inferior vena cava, as a nonwoven fiber mesh. However, PPDO lacks suitable chemical groups for covalent functionalization. Furthermore, PPDO is highly sensitive to hydrolysis, reflected by short in vivo half-life times and degradation during storage. Establishing a method for covalent functionalization without degradation of this hydrolyzable polymer is therefore important to enable the surface tailoring for tissue engineering applications. It was hypothesized that treatment of PPDO with an N-hydroxysuccinimide ester group bearing perfluorophenyl azide (PFPA) under UV irradiation would allow efficient surface functionalization of the scaffold. X-ray photoelectron spectroscopy and attenuated total reflectance Fourier-transformed infrared spectroscopy investigation revealed the successful binding, while a gel permeation chromatography study showed that degradation did not occur under these conditions. Coupling of a rhodamine dye to the N-hydroxysuccinimide esters on the surface of a PFPA-functionalized scaffold via its amine linker showed a homogenous staining of the PPDO in laser confocal microscopy. The PFPA method is therefore applicable even to the surface functionalization of hydrolytically labile polymers, and it was demonstrated that PFPA chemistry may serve as a versatile tool for the (bio-)functionalization of PPDO scaffolds.}, language = {en} } @article{ThiedeArrowsmithBookhagenetal.2006, author = {Thiede, Rasmus Christoph and Arrowsmith, J. Ram{\´o}n and Bookhagen, Bodo and McWilliams, Michael O. and Sobel, Edward and Strecker, Manfred}, title = {Dome formation and extension in the Tethyan Himalaya, Leo Pargil, northwest India}, doi = {10.1130/B25872.1}, year = {2006}, abstract = {Metamorphic dome complexes occur within the internal structures of the northern Himalaya and southern Tibet. Their origin, deformation, and fault displacement patterns are poorly constrained. We report new field mapping, structural data, and cooling ages from the western flank of the Leo Pargil dome in the northwestern Himalaya in an attempt to characterize its post-middle Miocene structural development. The western flank of the dome is characterized by shallow, west-dipping pervasive foliation and WNW-ESE mineral lineation. Shear-sense indicators demonstrate that it is affected by east-west normal faulting that facilitated exhumation of high-grade metamorphic rocks in a contractional setting. Sustained top-to-northwest normal faulting during exhumation is observed in a progressive transition from ductile to brittle deformation. Garnet and kyanite indicate that the Leo Pargil dome was exhumed from the mid-crust. Ar- 40/Ar-39 mica and apatite fission track (AFT) ages constrain cooling and exhumation pathways front 350 to 60 degrees C and suggest that the dome cooled in three stages since the middle Miocene. Ar-40/Ar-39 white mica ages of 16-14 Ma suggest a first phase of rapid cooling and provide minimum estimates for the onset of dome exhumation. AFT ages between 10 and 8 Ma suggest that ductile fault displacement had ceased by then, and AFT track-length data from high-elevation samples indicate that the rate of cooling had decreased significantly. We interpret this to indicate decreased fault displacement along the Leo Pargil shear zone and possibly a transition to the Kaurik-Chango normal fault system between 10 and 6 Ma. AFT ages from lower elevations indicate accelerated cooling since the Pliocene that cannot be related to pure fault displacement, and therefore may reflect more pronounced regionally distributed and erosion-driven exhumation}, language = {en} } @article{ThiedeArrowsmithBookhagenetal.2005, author = {Thiede, Rasmus Christoph and Arrowsmith, J. Ram{\´o}n and Bookhagen, Bodo and McWilliams, Michael O. and Sobel, Edward and Strecker, Manfred}, title = {From tectonically to erosionally controlled development of the Himalayan orogen}, issn = {0091-7613}, year = {2005}, abstract = {Whether variations in the spatial distribution of erosion influence the location, style, and magnitude of deformation within the Himalayan orogen is a matter of debate. We report new Ar-40/Ar-39 white mica and apatite fission- track (AFT) ages that measure the vertical component of exhumation rates along an similar to 120-km-wide NE-SW transect spanning the greater Sutlej region of northwest India. The Ar-40/Ar-39 data indicate that first the High Himalayan Crystalline units cooled below their closing temperature during the early to middle Miocene. Subsequently, Lesser Himalayan Crystalline nappes cooled rapidly, indicating southward propagation of the orogen during late Miocene to Pliocene time. The AFT data, in contrast, imply synchronous exhumation of a NE-SW-oriented similar to 80 x 40 km region spanning both crystalline nappes during the Pliocene-Quaternary. The locus of pronounced exhumation defined by the AFT data correlates with a region of high precipitation, discharge, and sediment flux rates during the Holocene. This correlation suggests that although tectonic processes exerted the dominant control on the denudation pattern before and until the middle Miocene; erosion may have been the most important factor since the Pliocene}, language = {en} } @article{HokeGarzioneAraneoetal.2009, author = {Hoke, Gregory D. and Garzione, Carmala N. and Araneo, Diego C. and Latorre, Claudio and Strecker, Manfred and Williams, Kendra J.}, title = {The stable isotope altimeter : do quaternary pedogenic carbonates predict modern elevations?}, issn = {0091-7613}, doi = {10.1130/G30308a.1}, year = {2009}, abstract = {Stable isotope altimetry is a useful tool for estimating paleoelevation in sedimentary records. Yet questions remain regarding how source moisture, climate, and local topography can influence these estimates. Here we present stable isotope altimetry results on late Quaternary pedogenic carbonates of known elevation on both flanks of the Andean orogen at 33 degrees S. We measured delta O-18 values of pedogenic carbonates and river water samples from small drainages at regular elevation increments within the Rio Aconcagua (Chile) and Rio Mendoza (Argentina) catchments. The delta O-18 values of river waters correlate well with elevation and show similar isotopic gradients between the Chilean (-3.7 parts per thousand/km) and Argentine (-4.8 parts per thousand/km) sides of the range. Uncertainties associated with scatter in the river water data and assumptions about the temperature of carbonate formation indicate that elevation estimates have 1 sigma errors of 350-450 m. We estimate the isotopic composition of soil water from pedogenic carbonates on both sides of the range by assuming mean annual temperatures based the modern temperature lapse rate from meteorological station data. Combined, our data show that stable isotope altimetry produces reasonable estimates of modern elevation, with the majority of our samples (60\%) within the 1 sigma uncertainties and 77\% within 2 sigma.}, language = {en} }