@article{ReadKegelKluteetal.2013, author = {Read, Betsy A. and Kegel, Jessica and Klute, Mary J. and Kuo, Alan and Lefebvre, Stephane C. and Maumus, Florian and Mayer, Christoph and Miller, John and Monier, Adam and Salamov, Asaf and Young, Jeremy and Aguilar, Maria and Claverie, Jean-Michel and Frickenhaus, Stephan and Gonzalez, Karina and Herman, Emily K. and Lin, Yao-Cheng and Napier, Johnathan and Ogata, Hiroyuki and Sarno, Analissa F. and Shmutz, Jeremy and Schroeder, Declan and de Vargas, Colomban and Verret, Frederic and von Dassow, Peter and Valentin, Klaus and Van de Peer, Yves and Wheeler, Glen and Dacks, Joel B. and Delwiche, Charles F. and Dyhrman, Sonya T. and Gl{\"o}ckner, Gernot and John, Uwe and Richards, Thomas and Worden, Alexandra Z. and Zhang, Xiaoyu and Grigoriev, Igor V. and Allen, Andrew E. and Bidle, Kay and Borodovsky, M. and Bowler, C. and Brownlee, Colin and Cock, J. Mark and Elias, Marek and Gladyshev, Vadim N. and Groth, Marco and Guda, Chittibabu and Hadaegh, Ahmad and Iglesias-Rodriguez, Maria Debora and Jenkins, J. and Jones, Bethan M. and Lawson, Tracy and Leese, Florian and Lindquist, Erika and Lobanov, Alexei and Lomsadze, Alexandre and Malik, Shehre-Banoo and Marsh, Mary E. and Mackinder, Luke and Mock, Thomas and M{\"u}ller-R{\"o}ber, Bernd and Pagarete, Antonio and Parker, Micaela and Probert, Ian and Quesneville, Hadi and Raines, Christine and Rensing, Stefan A. and Riano-Pachon, Diego Mauricio and Richier, Sophie and Rokitta, Sebastian and Shiraiwa, Yoshihiro and Soanes, Darren M. and van der Giezen, Mark and Wahlund, Thomas M. and Williams, Bryony and Wilson, Willie and Wolfe, Gordon and Wurch, Louie L.}, title = {Pan genome of the phytoplankton Emiliania underpins its global distribution}, series = {Nature : the international weekly journal of science}, volume = {499}, journal = {Nature : the international weekly journal of science}, number = {7457}, publisher = {Nature Publ. Group}, address = {London}, organization = {Emiliania Huxleyi Annotation}, issn = {0028-0836}, doi = {10.1038/nature12221}, pages = {209 -- 213}, year = {2013}, abstract = {Coccolithophores have influenced the global climate for over 200 million years(1). These marine phytoplankton can account for 20 per cent of total carbon fixation in some systems(2). They form blooms that can occupy hundreds of thousands of square kilometres and are distinguished by their elegantly sculpted calcium carbonate exoskeletons (coccoliths), rendering them visible from space(3). Although coccolithophores export carbon in the form of organic matter and calcite to the sea floor, they also release CO2 in the calcification process. Hence, they have a complex influence on the carbon cycle, driving either CO2 production or uptake, sequestration and export to the deep ocean(4). Here we report the first haptophyte reference genome, from the coccolithophore Emiliania huxleyi strain CCMP1516, and sequences from 13 additional isolates. Our analyses reveal a pan genome (core genes plus genes distributed variably between strains) probably supported by an atypical complement of repetitive sequence in the genome. Comparisons across strains demonstrate that E. huxleyi, which has long been considered a single species, harbours extensive genome variability reflected in different metabolic repertoires. Genome variability within this species complex seems to underpin its capacity both to thrive in habitats ranging from the equator to the subarctic and to form large-scale episodic blooms under a wide variety of environmental conditions.}, language = {en} } @inproceedings{GonzalezRiedelsbergerMoralesNavarroetal.2012, author = {Gonzalez, W. and Riedelsberger, J. and Morales-Navarro, S. E. and Caballero, Julio and Alzate-Morales, Jans H. and Gonzalez-Nilo, F. D. and Dreyer, Ingo}, title = {The pH sensor of the plant K plus uptake channel KAT1 is built from a sensory cloud rather than from single key amino acids}, series = {The FEBS journal}, volume = {279}, booktitle = {The FEBS journal}, publisher = {Wiley-Blackwell}, address = {Hoboken}, issn = {1742-464X}, pages = {455 -- 455}, year = {2012}, language = {en} } @article{GonzalezManriqueKuckeinPastorYabaretal.2016, author = {Gonzalez Manrique, Sergio Javier and Kuckein, Christoph and Pastor Yabar, A. and Collados Vera, M. and Denker, Carsten and Fischer, C. E. and G{\"o}m{\"o}ry, P. and Diercke, Andrea and Gonzalez, N. Bello and Schlichenmaier, R. and Balthasar, H. and Berkefeld, T. and Feller, A. and Hoch, S. and Hofmann, A. and Kneer, F. and Lagg, A. and Nicklas, H. and Orozco Suarez, D. and Schmidt, D. and Schmidt, W. and Sigwarth, M. and Sobotka, M. and Solanki, S. K. and Soltau, D. and Staude, J. and Strassmeier, Klaus G. and Verma, Meetu and Volkmer, R. and von der L{\"u}he, O. and Waldmann, T.}, title = {Fitting peculiar spectral profiles in He I 10830 angstrom absorption features}, series = {Astronomische Nachrichten = Astronomical notes}, volume = {337}, journal = {Astronomische Nachrichten = Astronomical notes}, publisher = {Wiley-VCH}, address = {Weinheim}, issn = {0004-6337}, doi = {10.1002/asna.201512433}, pages = {1057 -- 1063}, year = {2016}, abstract = {The new generation of solar instruments provides better spectral, spatial, and temporal resolution for a better understanding of the physical processes that take place on the Sun. Multiple-component profiles are more commonly observed with these instruments. Particularly, the He i 10830 triplet presents such peculiar spectral profiles, which give information on the velocity and magnetic fine structure of the upper chromosphere. The purpose of this investigation is to describe a technique to efficiently fit the two blended components of the He i 10830 triplet, which are commonly observed when two atmospheric components are located within the same resolution element. The observations used in this study were taken on 2015 April 17 with the very fast spectroscopic mode of the GREGOR Infrared Spectrograph (GRIS) attached to the 1.5-m GREGOR solar telescope, located at the Observatorio del Teide, Tenerife, Spain. We apply a double-Lorentzian fitting technique using Levenberg-Marquardt least-squares minimization. This technique is very simple and much faster than inversion codes. Line-of-sight Doppler velocities can be inferred for a whole map of pixels within just a few minutes. Our results show sub-and supersonic downflow velocities of up to 32 km s(-1) for the fast component in the vicinity of footpoints of filamentary structures. The slow component presents velocities close to rest. (C) 2016 WILEY-VCH Verlag GmbH\& Co. KGaA, Weinheim}, language = {en} } @article{VermaDenkerBoehmetal.2016, author = {Verma, Meetu and Denker, Carsten and B{\"o}hm, F. and Balthasar, H. and Fischer, C. E. and Kuckein, Christoph and Gonzalez, N. Bello and Berkefeld, T. and Collados Vera, M. and Diercke, Andrea and Feller, A. and Gonzalez Manrique, Sergio Javier and Hofmann, A. and Lagg, A. and Nicklas, H. and Orozco Suarez, D. and Pator Yabar, A. and Rezaei, R. and Schlichenmaier, R. and Schmidt, D. and Schmidt, W. and Sigwarth, M. and Sobotka, M. and Solanki, S. K. and Soltau, D. and Staude, J. and Strassmeier, Klaus G. and Volkmer, R. and von der L{\"u}he, O. and Waldmann, T.}, title = {Flow and magnetic field properties in the trailing sunspots of active region NOAA 12396}, series = {Astronomische Nachrichten = Astronomical notes}, volume = {337}, journal = {Astronomische Nachrichten = Astronomical notes}, publisher = {Wiley-VCH}, address = {Weinheim}, issn = {0004-6337}, doi = {10.1002/asna.201612447}, pages = {1090 -- 1098}, year = {2016}, abstract = {Improved measurements of the photospheric and chromospheric three-dimensional magnetic and flow fields are crucial for a precise determination of the origin and evolution of active regions. We present an illustrative sample of multi-instrument data acquired during a two-week coordinated observing campaign in August 2015 involving, among others, the GREGOR solar telescope (imaging and near-infrared spectroscopy) and the space missions Solar Dynamics Observatory (SDO) and Interface Region Imaging Spectrograph (IRIS). The observations focused on the trailing part of active region NOAA 12396 with complex polarity inversion lines and strong intrusions of opposite polarity flux. The GREGOR Infrared Spectrograph (GRIS) provided Stokes IQUV spectral profiles in the photospheric Si i.1082.7 nm line, the chromospheric He I lambda 1083.0 nm triplet, and the photospheric Ca I lambda 1083.9 nm line. Carefully calibrated GRIS scans of the active region provided maps of Doppler velocity and magnetic field at different atmospheric heights. We compare quick-look maps with those obtained with the " Stokes Inversions based on Response functions" (SIR) code, which furnishes deeper insight into the magnetic properties of the region. We find supporting evidence that newly emerging flux and intruding opposite polarity flux are hampering the formation of penumbrae, i.e., a penumbra fully surrounding a sunspot is only expected after cessation of flux emergence in proximity to the sunspots. (C) 2016 WILEY-VCH Verlag GmbH\& Co.KGaA, Weinheim}, language = {en} } @article{GonzalezFortesTassiTrucchietal.2019, author = {Gonzalez-Fortes, Gloria M. and Tassi, F. and Trucchi, E. and Henneberger, K. and Paijmans, Johanna L. A. and Diez-del-Molino, D. and Schroeder, H. and Susca, R. R. and Barroso-Ruiz, C. and Bermudez, F. J. and Barroso-Medina, C. and Bettencourt, A. M. S. and Sampaio, H. A. and Salas, A. and de Lombera-Hermida, A. and Fabregas Valcarce, Ram{\´o}n and Vaquero, M. and Alonso, S. and Lozano, Marina and Rodriguez-Alvarez, Xose Pedro and Fernandez-Rodriguez, C. and Manica, Andrea and Hofreiter, Michael and Barbujani, Guido}, title = {A western route of prehistoric human migration from Africa into the Iberian Peninsula}, series = {Proceedings of the Royal Society of London : B, Biological sciences}, volume = {286}, journal = {Proceedings of the Royal Society of London : B, Biological sciences}, number = {1895}, publisher = {Royal Society}, address = {London}, issn = {0962-8452}, doi = {10.1098/rspb.2018.2288}, pages = {10}, year = {2019}, abstract = {Being at the western fringe of Europe, Iberia had a peculiar prehistory and a complex pattern of Neolithization. A few studies, all based on modern populations, reported the presence of DNA of likely African origin in this region, generally concluding it was the result of recent gene flow, probably during the Islamic period. Here, we provide evidence of much older gene flow from Africa to Iberia by sequencing whole genomes from four human remains from northern Portugal and southern Spain dated around 4000 years BP (from the Middle Neolithic to the Bronze Age). We found one of them to carry an unequivocal sub-Saharan mitogenome of most probably West or West-Central African origin, to our knowledge never reported before in prehistoric remains outside Africa. Our analyses of ancient nuclear genomes show small but significant levels of sub-Saharan African affinity in several ancient Iberian samples, which indicates that what we detected was not an occasional individual phenomenon, but an admixture event recognizable at the population level. We interpret this result as evidence of an early migration process from Africa into the Iberian Peninsula through a western route, possibly across the Strait of Gibraltar.}, language = {en} } @article{HubrigSchoellerIlyinetal.2013, author = {Hubrig, Swetlana and Schoeller, M. and Ilyin, Ilya and Kharchenko, N. V. and Oskinova, Lidia M. and Langer, N. and Gonzalez, J. F. and Kholtygin, A. F. and Briquet, Maryline}, title = {Exploring the origin of magnetic fields in massive stars - II. New magnetic field measurements in cluster and field stars}, series = {Astronomy and astrophysics : an international weekly journal}, volume = {551}, journal = {Astronomy and astrophysics : an international weekly journal}, publisher = {EDP Sciences}, address = {Les Ulis}, organization = {MAGORI Collaboration}, issn = {0004-6361}, doi = {10.1051/0004-6361/201220721}, pages = {13}, year = {2013}, abstract = {Context. Theories on the origin of magnetic fields in massive stars remain poorly developed, because the properties of their magnetic field as function of stellar parameters could not yet be investigated. Additional observations are of utmost importance to constrain the conditions that are conducive to magnetic fields and to determine first trends about their occurrence rate and field strength distribution. Aims. To investigate whether magnetic fields in massive stars are ubiquitous or appear only in stars with a specific spectral classification, certain ages, or in a special environment, we acquired 67 new spectropolarimetric observations for 30 massive stars. Among the observed sample, roughly one third of the stars are probable members of clusters at different ages, whereas the remaining stars are field stars not known to belong to any cluster or association. Methods. Spectropolarimetric observations were obtained during four different nights using the low-resolution spectropolarimetric mode of FOcal Reducer low dispersion Spectrograph (FORS 2) mounted on the 8-m Antu telescope of the VLT. Furthermore, we present a number of follow-up observations carried out with the high-resolution spectropolarimeters SOFIN mounted at the Nordic Optical Telescope (NOT) and HARPS mounted at the ESO 3.6 m between 2008 and 2011. To assess the membership in open clusters and associations, we used astrometric catalogues with the highest quality kinematic and photometric data currently available. Results. The presence of a magnetic field is confirmed in nine stars previously observed with FORS 1/2: HD36879, HD47839, CPD-28 2561, CPD-47 2963, HD93843, HD148937, HD149757, HD328856, and HD164794. New magnetic field detections at a significance level of at least 3 sigma were achieved in five stars: HD92206c, HD93521, HD93632, CPD-46 8221, and HD157857. Among the stars with a detected magnetic field, five stars belong to open clusters with high membership probability. According to previous kinematic studies, five magnetic O-type stars in our sample are candidate runaway stars.}, language = {en} } @article{StarkenburgMartinYouakimetal.2017, author = {Starkenburg, Else and Martin, Nicolas and Youakim, Kris and Aguado, David S. and Allende Prieto, Carlos and Arentsen, Anke and Bernard, Edouard J. and Bonifacio, Piercarlo and Caffau, Elisabetta and Carlberg, Raymond G. and Cote, Patrick and Fouesneau, Morgan and Francois, Patrick and Franke, Oliver and Gonzalez Hernandez, Jonay I. and Gwyn, Stephen D. J. and Hill, Vanessa and Ibata, Rodrigo A. and Jablonka, Pascale and Longeard, Nicolas and McConnachie, Alan W. and Navarro, Julio F. and Sanchez-Janssen, Ruben and Tolstoy, Eline and Venn, Kim A.}, title = {The Pristine survey - I. Mining the Galaxy for the most metal-poor stars}, series = {Monthly notices of the Royal Astronomical Society}, volume = {471}, journal = {Monthly notices of the Royal Astronomical Society}, publisher = {Oxford Univ. Press}, address = {Oxford}, issn = {0035-8711}, doi = {10.1093/mnras/stx1068}, pages = {2587 -- 2604}, year = {2017}, abstract = {We present the Pristine survey, a new narrow-band photometric survey focused on the metallicity-sensitive Ca H\&K lines and conducted in the Northern hemisphere with the wide-field imager MegaCam on the Canada-France-Hawaii Telescope. This paper reviews our overall survey strategy and discusses the data processing and metallicity calibration. Additionally we review the application of these data to the main aims of the survey, which are to gather a large sample of the most metal-poor stars in the Galaxy, to further characterize the faintest Milky Way satellites, and to map the (metal-poor) substructure in the Galactic halo. The current Pristine footprint comprises over 1000 deg(2) in the Galactic halo ranging from b similar to 30 degrees to similar to 78 degrees and covers many known stellar substructures. We demonstrate that, for Sloan Digital Sky Survey (SDSS) stellar objects, we can calibrate the photometry at the 0.02-mag level. The comparison with existing spectroscopic metallicities from SDSS/Sloan Extension for Galactic Understanding and Exploration (SEGUE) and Large Sky Area Multi-Object Fiber Spectroscopic Telescope shows that, when combined with SDSS broad-band g and i photometry, we can use the CaHK photometry to infer photometric metallicities with an accuracy of similar to 0.2 dex from [Fe/H] = -0.5 down to the extremely metal-poor regime ([Fe/H] < -3.0). After the removal of various contaminants, we can efficiently select metal-poor stars and build a very complete sample with high purity. The success rate of uncovering [Fe/H](SEGUE) < -3.0 stars among [Fe/H](Pristine) < -3.0 selected stars is 24 per cent, and 85 per cent of the remaining candidates are still very metal poor ([Fe/H]<-2.0). We further demonstrate that Pristine is well suited to identify the very rare and pristine Galactic stars with [Fe/H] < -4.0, which can teach us valuable lessons about the early Universe.}, language = {en} } @article{DenglerWagnerDembiczetal.2018, author = {Dengler, J{\"u}rgen and Wagner, Viktoria and Dembicz, Iwona and Garcia-Mijangos, Itziar and Naqinezhad, Alireza and Boch, Steffen and Chiarucci, Alessandro and Conradi, Timo and Filibeck, Goffredo and Guarino, Riccardo and Janisova, Monika and Steinbauer, Manuel J. and Acic, Svetlana and Acosta, Alicia T. R. and Akasaka, Munemitsu and Allers, Marc-Andre and Apostolova, Iva and Axmanova, Irena and Bakan, Branko and Baranova, Alina and Bardy-Durchhalter, Manfred and Bartha, Sandor and Baumann, Esther and Becker, Thomas and Becker, Ute and Belonovskaya, Elena and Bengtsson, Karin and Benito Alonso, Jose Luis and Berastegi, Asun and Bergamini, Ariel and Bonini, Ilaria and Bruun, Hans Henrik and Budzhak, Vasyl and Bueno, Alvaro and Antonio Campos, Juan and Cancellieri, Laura and Carboni, Marta and Chocarro, Cristina and Conti, Luisa and Czarniecka-Wiera, Marta and De Frenne, Pieter and Deak, Balazs and Didukh, Yakiv P. and Diekmann, Martin and Dolnik, Christian and Dupre, Cecilia and Ecker, Klaus and Ermakov, Nikolai and Erschbamer, Brigitta and Escudero, Adrian and Etayo, Javier and Fajmonova, Zuzana and Felde, Vivian A. and Fernandez Calzado, Maria Rosa and Finckh, Manfred and Fotiadis, Georgios and Fracchiolla, Mariano and Ganeva, Anna and Garcia-Magro, Daniel and Gavilan, Rosario G. and Germany, Markus and Giladi, Itamar and Gillet, Francois and Giusso del Galdo, Gian Pietro and Gonzalez, Jose M. and Grytnes, John-Arvid and Hajek, Michal and Hajkova, Petra and Helm, Aveliina and Herrera, Mercedes and Hettenbergerova, Eva and Hobohm, Carsten and Huellbusch, Elisabeth M. and Ingerpuu, Nele and Jandt, Ute and Jeltsch, Florian and Jensen, Kai and Jentsch, Anke and Jeschke, Michael and Jimenez-Alfaro, Borja and Kacki, Zygmunt and Kakinuma, Kaoru and Kapfer, Jutta and Kavgaci, Ali and Kelemen, Andras and Kiehl, Kathrin and Koyama, Asuka and Koyanagi, Tomoyo F. and Kozub, Lukasz and Kuzemko, Anna and Kyrkjeeide, Magni Olsen and Landi, Sara and Langer, Nancy and Lastrucci, Lorenzo and Lazzaro, Lorenzo and Lelli, Chiara and Leps, Jan and Loebel, Swantje and Luzuriaga, Arantzazu L. and Maccherini, Simona and Magnes, Martin and Malicki, Marek and Marceno, Corrado and Mardari, Constantin and Mauchamp, Leslie and May, Felix and Michelsen, Ottar and Mesa, Joaquin Molero and Molnar, Zsolt and Moysiyenko, Ivan Y. and Nakaga, Yuko K. and Natcheva, Rayna and Noroozi, Jalil and Pakeman, Robin J. and Palpurina, Salza and Partel, Meelis and Paetsch, Ricarda and Pauli, Harald and Pedashenko, Hristo and Peet, Robert K. and Pielech, Remigiusz and Pipenbaher, Natasa and Pirini, Chrisoula and Pleskova, Zuzana and Polyakova, Mariya A. and Prentice, Honor C. and Reinecke, Jennifer and Reitalu, Triin and Pilar Rodriguez-Rojo, Maria and Rolecek, Jan and Ronkin, Vladimir and Rosati, Leonardo and Rosen, Ejvind and Ruprecht, Eszter and Rusina, Solvita and Sabovljevic, Marko and Maria Sanchez, Ana and Savchenko, Galina and Schuhmacher, Oliver and Skornik, Sonja and Sperandii, Marta Gaia and Staniaszek-Kik, Monika and Stevanovic-Dajic, Zora and Stock, Marin and Suchrow, Sigrid and Sutcliffe, Laura M. E. and Swacha, Grzegorz and Sykes, Martin and Szabo, Anna and Talebi, Amir and Tanase, Catalin and Terzi, Massimo and Tolgyesi, Csaba and Torca, Marta and Torok, Peter and Tothmeresz, Bela and Tsarevskaya, Nadezda and Tsiripidis, Ioannis and Tzonev, Rossen and Ushimaru, Atushi and Valko, Orsolya and van der Maarel, Eddy and Vanneste, Thomas and Vashenyak, Iuliia and Vassilev, Kiril and Viciani, Daniele and Villar, Luis and Virtanen, Risto and Kosic, Ivana Vitasovic and Wang, Yun and Weiser, Frank and Went, Julia and Wesche, Karsten and White, Hannah and Winkler, Manuela and Zaniewski, Piotr T. and Zhang, Hui and Ziv, Yaron and Znamenskiy, Sergey and Biurrun, Idoia}, title = {GrassPlot - a database of multi-scale plant diversity in Palaearctic grasslands}, series = {Phytocoenologia}, volume = {48}, journal = {Phytocoenologia}, number = {3}, publisher = {Cramer}, address = {Stuttgart}, issn = {0340-269X}, doi = {10.1127/phyto/2018/0267}, pages = {331 -- 347}, year = {2018}, abstract = {GrassPlot is a collaborative vegetation-plot database organised by the Eurasian Dry Grassland Group (EDGG) and listed in the Global Index of Vegetation-Plot Databases (GIVD ID EU-00-003). GrassPlot collects plot records (releves) from grasslands and other open habitats of the Palaearctic biogeographic realm. It focuses on precisely delimited plots of eight standard grain sizes (0.0001; 0.001;... 1,000 m(2)) and on nested-plot series with at least four different grain sizes. The usage of GrassPlot is regulated through Bylaws that intend to balance the interests of data contributors and data users. The current version (v. 1.00) contains data for approximately 170,000 plots of different sizes and 2,800 nested-plot series. The key components are richness data and metadata. However, most included datasets also encompass compositional data. About 14,000 plots have near-complete records of terricolous bryophytes and lichens in addition to vascular plants. At present, GrassPlot contains data from 36 countries throughout the Palaearctic, spread across elevational gradients and major grassland types. GrassPlot with its multi-scale and multi-taxon focus complements the larger international vegetationplot databases, such as the European Vegetation Archive (EVA) and the global database " sPlot". Its main aim is to facilitate studies on the scale-and taxon-dependency of biodiversity patterns and drivers along macroecological gradients. GrassPlot is a dynamic database and will expand through new data collection coordinated by the elected Governing Board. We invite researchers with suitable data to join GrassPlot. Researchers with project ideas addressable with GrassPlot data are welcome to submit proposals to the Governing Board.}, language = {en} } @article{HubrigFossatiCarrolletal.2014, author = {Hubrig, Swetlana and Fossati, Luca and Carroll, Thorsten Anthony and Castro, Norberto and Gonzalez, J. F. and Ilyin, Ilya and Przybilla, Norbert and Schoeller, M. and Oskinova, Lidia M. and Morel, T. and Langer, N. and Scholz, Ralf-Dieter and Kharchenko, N. V. and Nieva, M. -F.}, title = {B fields in OB stars (BOB): The discovery of a magnetic field in a multiple system in the Trifid nebula, one of the youngest star forming regions}, series = {Astronomy and astrophysics : an international weekly journal}, volume = {564}, journal = {Astronomy and astrophysics : an international weekly journal}, publisher = {EDP Sciences}, address = {Les Ulis}, organization = {BOB Collaboration}, issn = {0004-6361}, doi = {10.1051/0004-6361/201423490}, pages = {5}, year = {2014}, abstract = {Aims. Recent magnetic field surveys in O- and B-type stars revealed that about 10\% of the core-hydrogen-burning massive stars host large-scale magnetic fields. The physical origin of these fields is highly debated. To identify and model the physical processes responsible for the generation of magnetic fields in massive stars, it is important to establish whether magnetic massive stars are found in very young star-forming regions or whether they are formed in close interacting binary systems. Methods. In the framework of our ESO Large Program, we carried out low-resolution spectropolarimetric observations with FORS 2 in 2013 April of the three most massive central stars in the Trifid nebula, HD 164492A, HD 164492C, and HD 164492D. These observations indicated a strong longitudinal magnetic field of about 500-600 G in the poorly studied component HD 164492C. To confirm this detection, we used HARPS in spectropolarimetric mode on two consecutive nights in 2013 June. Results. Our HARPS observations confirmed the longitudinal magnetic field in HD 164492C. Furthermore, the HARPS observations revealed that HD 164492C cannot be considered as a single star as it possesses one or two companions. The spectral appearance indicates that the primary is most likely of spectral type B1-B1.5 V. Since in both observing nights most spectral lines appear blended, it is currently unclear which components are magnetic. Long-term monitoring using high-resolution spectropolarimetry is necessary to separate the contribution of each component to the magnetic signal. Given the location of the system HD 164492C in one of the youngest star formation regions, this system can be considered as a Rosetta Stone for our understanding of the origin of magnetic fields in massive stars.}, language = {en} } @misc{HofreiterPaijmansGoodchildetal.2015, author = {Hofreiter, Michael and Paijmans, Johanna L. A. and Goodchild, Helen and Speller, Camilla F. and Barlow, Axel and Gonzalez-Fortes, Gloria M. and Thomas, Jessica A. and Ludwig, Arne and Collins, Matthew J.}, title = {The future of ancient DNA}, series = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, journal = {Postprints der Universit{\"a}t Potsdam : Mathematisch Naturwissenschaftliche Reihe}, number = {908}, issn = {1866-8372}, doi = {10.25932/publishup-43881}, url = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus4-438816}, pages = {284 -- 295}, year = {2015}, abstract = {Technological innovations such as next generation sequencing and DNA hybridisation enrichment have resulted in multi-fold increases in both the quantity of ancient DNA sequence data and the time depth for DNA retrieval. To date, over 30 ancient genomes have been sequenced, moving from 0.7x coverage (mammoth) in 2008 to more than 50x coverage (Neanderthal) in 2014. Studies of rapid evolutionary changes, such as the evolution and spread of pathogens and the genetic responses of hosts, or the genetics of domestication and climatic adaptation, are developing swiftly and the importance of palaeogenomics for investigating evolutionary processes during the last million years is likely to increase considerably. However, these new datasets require new methods of data processing and analysis, as well as conceptual changes in interpreting the results. In this review we highlight important areas of future technical and conceptual progress and discuss research topics in the rapidly growing field of palaeogenomics.}, language = {en} }