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1. Polarized HLA Class I Expression on Renal Tubules Hinders the Detection of Donor-Specific Urinary Extracellular Vesicles

Author

Wu L, van Heugten MH, van den Bosch TPP, Duimel H, López-Iglesias C, Hesselink DA, Baan CC, and Boer K

Subjects
kidney transplantation, donor-specific biomarker, hla, extracellular vesicles, human urine, renal tubule, Medicine (General), R5-920
Abstract

Liang Wu,1,2 Martijn H van Heugten,3 Thierry PP van den Bosch,4 Hans Duimel,5 Carmen López-Iglesias,5 Dennis A Hesselink,2 Carla C Baan,2 Karin Boer2 1Department of Nephrology, the First Affiliated Hospital of Shaoyang University, Shaoyang, Hunan, People’s Republic of China; 2Erasmus MC Transplant Institute, University Medical Center Rotterdam, Department of Internal Medicine, Division of Nephrology and Transplantation, Rotterdam, the Netherlands; 3University Medical Center Rotterdam, Department of Internal Medicine, Division of Nephrology and Transplantation, Rotterdam, the Netherlands; 4Department of Pathology, University Medical Center Rotterdam, Rotterdam, the Netherlands; 5The Microscopy CORE Laboratory at the Faculty of Health, Medicine and Life Sciences, Maastricht University, Maastricht, the NetherlandsCorrespondence: Liang Wu, Erasmus MC Transplant Institute, Department of Internal Medicine, University Medical Center Rotterdam Erasmus MC, Room No. Na-514, Doctor Molewaterplein 40, 3015 GD, Rotterdam, the Netherlands, Tel +31 0622145029, Email l.wu.1@erasmusmc.nlPurpose: Kidney transplantation is the optimal treatment for patients with end-stage kidney disease. Donor-specific urinary extracellular vesicles (uEVs) hold potential as biomarkers for assessing allograft status. We aimed to develop a method for identifying donor-specific uEVs based on human leukocyte antigen (HLA) mismatching with the kidney transplant recipients (KTRs).Patients and Methods: Urine and plasma were obtained from HLA-A2+ donors and HLA-A2- KTRs pre-transplant. CD9 (tetraspanin, EV marker) and HLA-A2 double-positive (CD9+ HLA-A2+) EVs were quantified using isolation-free imaging flow cytometry (IFCM). Healthy individuals’ urine was used to investigate CD9+ HLA-class-I+ uEV quantification using IFCM, time-resolved fluoroimmunoassay (TR-FIA), and immunogold staining cryo-electron microscopy (cryo-EM). Culture-derived CD9+ HLA-class-I+ EVs were spiked into the urine to investigate urine matrix effects on uEV HLA detection. Deceased donor kidneys and peritumoral kidney tissue were used for HLA class I detection with histochemistry.Results: The concentrations of CD9+ HLA-A2+ EVs in both donor and recipient urine approached the negative (detergent-treated) control levels for IFCM and were significantly lower than those observed in donor plasma. In parallel, universal HLA class I+ uEVs were similarly undetectable in the urine and uEV isolates compared with plasma, as verified by IFCM, TR-FIA, and cryogenic electron microscopy. Culture supernatant containing HLA class I+ vesicles from B, T, and human proximal tubule cells were spiked into the urine, and these EVs remained stable at 37°C for 8 hours. Immunohistochemistry revealed that HLA class I was predominantly expressed on the basolateral side of renal tubules, with limited expression on their urine/apical side.Conclusion: The detection of donor-specific uEVs is hindered by the limited release of HLA class I+ EVs from the kidney into the urine, primarily due to the polarized HLA class I expression on renal tubules. Identifying donor-specific uEVs requires further advancements in recognizing transplant-specific uEVs and urine-associated markers.Keywords: kidney transplantation, donor-specific biomarker, HLA, extracellular vesicles, human urine, renal tubule

Published
2024

2. Gaia Data Release 1. Testing the parallaxes with local Cepheids and RR Lyrae stars

Author

Gaia Collaboration, Clementini, G., Eyer, L., Ripepi, V., Marconi, M., Muraveva, T., Garofalo, A., Sarro, L. M., Palmer, M., Luri, X., Molinaro, R., Rimoldini, L., Szabados, L., Musella, I., Anderson, R. I., Prusti, T., de Bruijne, J. H. J., Brown, A. G. A., Vallenari, A., Babusiaux, C., Bailer-Jones, C. A. L., Bastian, U., Biermann, M., Evans, D. W., Jansen, F., Jordi, C., Klioner, S. A., Lammers, U., Lindegren, L., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H. I., Soubiran, C., Valette, V., van Leeuwen, F., Walton, N. A., Aerts, C., Arenou, F., Cropper, M., Drimmel, R., Høg, E., Katz, D., Lattanzi, M. G., O'Mullane, W., Grebel, E. K., Holland, A. D., Huc, C., Passot, X., Perryman, M., Bramante, L., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., De Angeli, F., Fabricius, C., Guerra, R., Hernández, J., Jean-Azntoine-Piccolo, A., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Ordóñez-Blanco, D., Panuzzo, P., Portell, J., Richards, P. J., Riello, M., Seabroke, G. M., Tanga, P., Thévenin, F., Torra, J., Els, S. G., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Lock, T., Mercier, E., Altmann, M., Andrae, R., Astraatmadja, T. L., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Busso, G., Carry, B., Cellino, A., Cowell, S., Creevey, O., Cuypers, J., Davidson, M., De Ridder, J., de Torres, A., Delchambre, L., Dell'Oro, A., Ducourant, C., Frémat, Y., García-Torres, M., Gosset, E., Halbwachs, J. -L., Hambly, N. C., Harrison, D. L., Hauser, M., Hestroffer, D., Hodgkin, S. T., Huckle, H. E., Hutton, A., Jasniewicz, G., Jordan, S., Kontizas, M., Korn, A. J., Lanzafame, A. C., Manteiga, M., Moitinho, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J. -M., Recio-Blanco, A., Robin, A. C., Siopis, C., Smith, M., Smith, K. W., Sozzetti, A., Thuillot, W., van Reeven, W., Viala, Y., Abbas, U., Aramburu, A. Abreu, Accart, S., Aguado, J. J., Allan, P. M., Allasia, W., Altavilla, G., Álvarez, M. A., Alves, J., Andrei, A. H., Varela, E. Anglada, Antiche, E., Antoja, T., Antón, S., Arcay, B., Bach, N., Baker, S. G., Balaguer-Núñez, L., Barache, C., Barata, C., Barbier, A., Barblan, F., Navascués, D. Barrado y, Barros, M., Barstow, M. A., Becciani, U., Bellazzini, M., García, A. Bello, Belokurov, V., Bendjoya, P., Berihuete, A., Bianchi, L., Bienaymé, O., Billebaud, F., Blagorodnova, N., Blanco-Cuaresma, S., Boch, T., Bombrun, A., Borrachero, R., Bouquillon, S., Bourda, G., Bouy, H., Bragaglia, A., Breddels, M. A., Brouillet, N., Brüsemeister, T., Bucciarelli, B., Burgess, P., Burgon, R., Burlacu, A., Busonero, D., Buzzi, R., Caffau, E., Cambras, J., Campbell, H., Cancelliere, R., Cantat-Gaudin, T., Carlucci, T., Carrasco, J. M., Castellani, M., Charlot, P., Charnas, J., Chiavassa, A., Clotet, M., Cocozza, G., Collins, R. S., Costigan, G., Crifo, F., Cross, N. J. G., Crosta, M., Crowley, C., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., De Cat, P., de Felice, F., de Laverny, P., De Luise, F., De March, R., de Souza, R., Debosscher, J., del Pozo, E., Delbo, M., Delgado, A., Delgado, H. E., Di Matteo, P., Diakite, S., Distefano, E., Dolding, C., Anjos, S. Dos, Drazinos, P., Durán, J., Dzigan, Y., Edvardsson, B., Enke, H., Evans, N. W., Bontemps, G. Eynard, Fabre, C., Fabrizio, M., Faigler, S., Falcão, A. J., Casas, M. Farràs, Federici, L., Fedorets, G., Fernández-Hernánde, J., Fernique, P., Fienga, A., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fouesneau, M., Fraile, E., Fraser, M., Fuchs, J., Gai, M., Galleti, S., Galluccio, L., Garabato, D., García-Sedano, F., Garralda, N., Gavras, P., Gerssen, J., Geyer, R., Gilmore, G., Girona, S., Giuffrida, G., Gomes, M., González-Marcos, A., González-Núñez, J., González-Vidal, J. J., Granvik, M., Guerrier, A., Guillout, P., Guiraud, J., Gúrpide, A., Gutiérrez-Sánchez, R., Guy, L. P., Haigron, R., Hatzidimitriou, D., Haywood, M., Heiter, U., Helmi, A., Hobbs, D., Hofmann, W., Holl, B., Holland, G., Hunt, J. A. S., Hypki, A., Icardi, V., Irwin, M., de Fombelle, G. Jevardat, Jofré, P., Jonker, P. G., Jorissen, A., Julbe, F., Karampelas, A., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, E., Koposov, S. E., Kordopatis, G., Koubsky, P., Krone-Martins, A., Kudryashova, M., Kull, I., Bachchan, R. K., Lacoste-Seris, F., Lanza, A. F., Lavigne, J. -B., Poncin-Lafitte, C. Le, Lebreton, Y., Lebzelter, T., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lemaitre, V., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Lobel, A., Löffler, W., López, M., Lorenz, D., MacDonald, I., Fernandes, T. Magalhães, Managau, S., Mann, R. G., Mantelet, G., Marchal, O., Marchant, J. M., Marinoni, S., Marrese, P. M., Marschalkó, G., Marshall, D. J., Martín-Fleitas, J. M., Martino, M., Mary, N., Matijevič, G., Mazeh, T., McMillan, P. J., Messina, S., Michalik, D., Millar, N. R., Miranda, B. M. H., Molina, D., Molinaro, M., Molnár, L., Moniez, M., Montegriffo, P., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morgenthaler, S., Morris, D., Mulone, A. F., Narbonne, J., Nelemans, G., Nicastro, L., Noval, L., Ordénovic, C., Ordieres-Meré, J., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Parsons, P., Pecoraro, M., Pedrosa, R., Pentikäinen, H., Pichon, B., Piersimoni, A. M., Pineau, F. -X., Plachy, E., Plum, G., Poujoulet, E., Prša, A., Pulone, L., Ragaini, S., Rago, S., Rambaux, N., Ramos-Lerate, M., Ranalli, P., Rauw, G., Read, A., Regibo, S., Reylé, C., Ribeiro, R. A., Riva, A., Rixon, G., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sellés, T. Sagristà, Sahlmann, J., Salgado, J., Salguero, E., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J. C., Segransan, D., Shih, I-C., Smareglia, R., Smart, R. L., Solano, E., Solitro, F., Sordo, R., Nieto, S. Soria, Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I. A., Steidelmüller, H., Stephenson, C. A., Stoev, H., Suess, F. F., Süveges, M., Surdej, J., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M. B., Teixeira, R., Terrett, D., Tingley, B., Trager, S. C., Turon, C., Ulla, A., Utrilla, E., Valentini, G., van Elteren, A., Van Hemelryck, E., van Leeuwen, M., Varadi, M., Vecchiato, A., Veljanoski, J., Via, T., Vicente, D., Vogt, S., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Weingrill, K., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Zucker, S., Zurbach, C., Zwitter, T., Alecu, A., Allen, M., Prieto, C. Allende, Amorim, A., Anglada-Escudé, G., Arsenijevic, V., Azaz, S., Balm, P., Beck, M., Bernstein, H. -H., Bigot, L., Bijaoui, A., Blasco, C., Bonfigli, M., Bono, G., Boudreault, S., Bressan, A., Brown, S., Brunet, P. -M., Bunclark, P., Buonanno, R., Butkevich, A. G., Carret, C., Carrion, C., Chemin, L., Chéreau, F., Corcione, L., Darmigny, E., de Boer, K. S., de Teodoro, P., de Zeeuw, P. T., Luche, C. Delle, Domingues, C. D., Dubath, P., Fodor, F., Frézouls, B., Fries, A., Fustes, D., Fyfe, D., Gallardo, E., Gallegos, J., Gardiol, D., Gebran, M., Gomboc, A., Gómez, A., Grux, E., Gueguen, A., Heyrovsky, A., Hoar, J., Iannicola, G., Parache, Y. Isasi, Janotto, A. -M., Joliet, E., Jonckheere, A., Keil, R., Kim, D. -W., Klagyivik, P., Klar, J., Knude, J., Kochukhov, O., Kolka, I., Kos, J., Kutka, A., Lainey, V., LeBouquin, D., Liu, C., Loreggia, D., Makarov, V. V., Marseille, M. G., Martayan, C., Martinez-Rubi, O., Massart, B., Meynadier, F., Mignot, S., Munari, U., Nguyen, A. -T., Nordlander, T., O'Flaherty, K. S., Ocvirk, P., Sanz, A. Olias, Ortiz, P., Osorio, J., Oszkiewicz, D., Ouzounis, A., Park, P., Pasquato, E., Peltzer, C., Peralta, J., Péturaud, F., Pieniluoma, T., Pigozzi, E., Poels, J., Prat, G., Prod'homme, T., Raison, F., Rebordao, J. M., Risquez, D., Rocca-Volmerange, B., Rosen, S., Ruiz-Fuertes, M. I., Russo, F., Sembay, S., Vizcaino, I. Serraller, Short, A., Siebert, A., Silva, H., Sinachopoulos, D., Slezak, E., Soffel, M., Sosnowska, D., Straižys, V., ter Linden, M., Terrell, D., Theil, S., Tiede, C., Troisi, L., Tsalmantza, P., Tur, D., Vaccari, M., Vachier, F., Valles, P., Van Hamme, W., Veltz, L., Virtanen, J., Wallut, J. -M., Wichmann, R., Wilkinson, M. I., Ziaeepour, H., and Zschocke, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Parallaxes for 331 classical Cepheids, 31 Type II Cepheids and 364 RR Lyrae stars in common between Gaia and the Hipparcos and Tycho-2 catalogues are published in Gaia Data Release 1 (DR1) as part of the Tycho-Gaia Astrometric Solution (TGAS). In order to test these first parallax measurements of the primary standard candles of the cosmological distance ladder, that involve astrometry collected by Gaia during the initial 14 months of science operation, we compared them with literature estimates and derived new period-luminosity ($PL$), period-Wesenheit ($PW$) relations for classical and Type II Cepheids and infrared $PL$, $PL$-metallicity ($PLZ$) and optical luminosity-metallicity ($M_V$-[Fe/H]) relations for the RR Lyrae stars, with zero points based on TGAS. The new relations were computed using multi-band ($V,I,J,K_{\mathrm{s}},W_{1}$) photometry and spectroscopic metal abundances available in the literature, and applying three alternative approaches: (i) by linear least squares fitting the absolute magnitudes inferred from direct transformation of the TGAS parallaxes, (ii) by adopting astrometric-based luminosities, and (iii) using a Bayesian fitting approach. TGAS parallaxes bring a significant added value to the previous Hipparcos estimates. The relations presented in this paper represent first Gaia-calibrated relations and form a "work-in-progress" milestone report in the wait for Gaia-only parallaxes of which a first solution will become available with Gaia's Data Release 2 (DR2) in 2018., Comment: 29 pages, 25 figures. Accepted for publication by A&A

Published
2017
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3. Gaia Data Release 1. Open cluster astrometry: performance, limitations, and future prospects

Author

Gaia Collaboration, van Leeuwen, F., Vallenari, A., Jordi, C., Lindegren, L., Bastian, U., Prusti, T., de Bruijne, J. H. J., Brown, A. G. A., Babusiaux, C., Bailer-Jones, C. A. L., Biermann, M., Evans, D. W., Eyer, L., Jansen, F., Klioner, S. A., Lammers, U., Luri, X., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H. I., Soubiran, C., Valette, V., Walton, N. A., Aerts, C., Arenou, F., Cropper, M., Drimmel, R., Høg, E., Katz, D., Lattanzi, M. G., O'Mullane, W., Grebel, E. K., Holland, A. D., Huc, C., Passot, X., Perryman, M., Bramante, L., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., De Angeli, F., Fabricius, C., Guerra, R., Hernández, J., Jean-Antoine-Piccolo, A., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Ordóñez-Blanco, D., Panuzzo, P., Portell, J., Richards, P. J., Riello, M., Seabroke, G. M., Tanga, P., Thévenin, F., Torra, J., Els, S. G., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Lock, T., Mercier, E., Altmann, M., Andrae, R., Astraatmadja, T. L., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Busso, G., Carry, B., Cellino, A., Clementini, G., Cowell, S., Creevey, O., Cuypers, J., Davidson, M., De Ridder, J., de Torres, A., Delchambre, L., Dell'Oro, A., Ducourant, C., Frémat, Y., García-Torres, M., Gosset, E., Halbwachs, J. -L., Hambly, N. C., Harrison, D. L., Hauser, M., Hestroffer, D., Hodgkin, S. T., Huckle, H. E., Hutton, A., Jasniewicz, G., Jordan, S., Kontizas, M., Korn, A. J., Lanzafame, A. C., Manteiga, M., Moitinho, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J. -M., Recio-Blanco, A., Robin, A. C., Sarro, L. M., Siopis, C., Smith, M., Smith, K. W., Sozzetti, A., Thuillot, W., van Reeven, W., Viala, Y., Abbas, U., Aramburu, A. Abreu, Accart, S., Aguado, J. J., Allan, P. M., Allasia, W., Altavilla, G., Álvarez, M. A., Alves, J., Anderson, R. I., Andrei, A. H., Varela, E. Anglada, Antiche, E., Antoja, T., Antón, S., Arcay, B., Bach, N., Baker, S. G., Balaguer-Núñez, L., Barache, C., Barata, C., Barbier, A., Barblan, F., Navascués, D. Barrado y, Barros, M., Barstow, M. A., Becciani, U., Bellazzini, M., García, A. Bello, Belokurov, V., Bendjoya, P., Berihuete, A., Bianchi, L., Bienaymé, O., Billebaud, F., Blagorodnova, N., Blanco-Cuaresma, S., Boch, T., Bombrun, A., Borrachero, R., Bouquillon, S., Bourda, G., Bouy, H., Bragaglia, A., Breddels, M. A., Brouillet, N., Brüsemeister, T., Bucciarelli, B., Burgess, P., Burgon, R., Burlacu, A., Busonero, D., Buzzi, R., Caffau, E., Cambras, J., Campbell, H., Cancelliere, R., Cantat-Gaudin, T., Carlucci, T., Carrasco, J. M., Castellani, M., Charlot, P., Charnas, J., Chiavassa, A., Clotet, M., Cocozza, G., Collins, R. S., Costigan, G., Crifo, F., Cross, N. J. G., Crosta, M., Crowley, C., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., De Cat, P., de Felice, F., de Laverny, P., De Luise, F., De March, R., de Martino, D., de Souza, R., Debosscher, J., del Pozo, E., Delbo, M., Delgado, A., Delgado, H. E., Di Matteo, P., Diakite, S., Distefano, E., Dolding, C., Anjos, S. Dos, Drazinos, P., Durán, J., Dzigan, Y., Edvardsson, B., Enke, H., Evans, N. W., Bontemps, G. Eynard, Fabre, C., Fabrizio, M., Faigler, S., Falcão, A. J., Casas, M. Farràs, Federici, L., Fedorets, G., Fernández-Hernández, J., Fernique, P., Fienga, A., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fouesneau, M., Fraile, E., Fraser, M., Fuchs, J., Gai, M., Galleti, S., Galluccio, L., Garabato, D., García-Sedano, F., Garofalo, A., Garralda, N., Gavras, P., Gerssen, J., Geyer, R., Gilmore, G., Girona, S., Giuffrida, G., Gomes, M., González-Marcos, A., González-Núñez, J., González-Vidal, J. J., Granvik, M., Guerrier, A., Guillout, P., Guiraud, J., Gúrpide, A., Gutiérrez-Sánchez, R., Guy, L. P., Haigron, R., Hatzidimitriou, D., Haywood, M., Heiter, U., Helmi, A., Hobbs, D., Hofmann, W., Holl, B., Holland, G., Hunt, J. A. S., Hypki, A., Icardi, V., Irwin, M., de Fombelle, G. Jevardat, Jofré, P., Jonker, P. G., Jorissen, A., Julbe, F., Karampelas, A., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, E., Koposov, S. E., Kordopatis, G., Koubsky, P., Krone-Martins, A., Kudryashova, M., Kull, I., Bachchan, R. K., Lacoste-Seris, F., Lanza, A. F., Lavigne, J. -B., Poncin-Lafitte, C. Le, Lebreton, Y., Lebzelter, T., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lemaitre, V., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Lobel, A., Löffer, W., López, M., Lorenz, D., MacDonald, I., Fernandes, T. Magalhães, Managau, S., Mann, R. G., Mantelet, G., Marchal, O., Marchant, J. M., Marconi, M., Marinoni, S., Marrese, P. M., Marschalkó, G., Marshall, D. J., Martín-Fleitas, J. M., Martino, M., Mary, N., Matijevič, G., Mazeh, T., McMillan, P. J., Messina, S., Michalik, D., Millar, N. R., Miranda, B. M. H., Molina, D., Molinaro, R., Molinaro, M., Molnár, L., Moniez, M., Montegrio, P., Mor, R., Mora, A., Morbidelli, R., Morel, T., Morgenthaler, S., Morris, D., Mulone, A. F., Muraveva, T., Musella, I., Narbonne, J., Nelemans, G., Nicastro, L., Noval, L., Ordénovic, C., Ordieres-Meré, J., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Parsons, P., Pecoraro, M., Pedrosa, R., Pentikäinen, H., Pichon, B., Piersimoni, A. M., Pineau, F. -X., Plachy, E., Plum, G., Poujoulet, E., Prša, A., Pulone, L., Ragaini, S., Rago, S., Rambaux, N., Ramos-Lerate, M., Ranalli, P., Rauw, G., Read, A., Regibo, S., Reylé, C., Ribeiro, R. A., Rimoldini, L., Ripepi, V., Riva, A., Rixon, G., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sellés, T. Sagristà, Sahlmann, J., Salgado, J., Salguero, E., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J. C., Segransan, D., Shih, I-C., Smareglia, R., Smart, R. L., Solano, E., Solitro, F., Sordo, R., Nieto, S. Soria, Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I. A., Steidelmüller, H., Stephenson, C. A., Stoev, H., Suess, F. F., Süveges, M., Surdej, J., Szabados, L., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M. B., Teixeira, R., Terrett, D., Tingley, B., Trager, S. C., Turon, C., Ulla, A., Utrilla, E., Valentini, G., van Elteren, A., Van Hemelryck, E., van Leeuwen, M., Varadi, M., Vecchiato, A., Veljanoski, J., Via, T., Vicente, D., Vogt, S., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Weingril, K., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Zucker, S., Zurbach, C., Zwitter, T., Alecu, A., Allen, M., Prieto, C. Allende, Amorim, A., Anglada-Escudé, G., Arsenijevic, V., Azaz, S., Balm, P., Beck, M., Bernsteiny, H. -H., Bigot, L., Bijaoui, A., Blasco, C., Bonfigli, M., Bono, G., Boudreault, S., Bressan, A., Brown, S., Brunet, P. -M., Bunclarky, P., Buonanno, R., Butkevich, A. G., Carret, C., Carrion, C., Chemin, L., Chéreau, F., Corcione, L., Darmigny, E., de Boer, K. S., de Teodoro, P., de Zeeuw, P. T., Luche, C. Delle, Domingues, C. D., Dubath, P., Fodor, F., Frézouls, B., Fries, A., Fustes, D., Fyfe, D., Gallardo, E., Gallegos, J., Gardio, D., Gebran, M., Gomboc, A., Gómez, A., Grux, E., Gueguen, A., Heyrovsky, A., Hoar, J., Iannicola, G., Parache, Y. Isasi, Janotto, A. -M., Joliet, E., Jonckheere, A., Keil, R., Kim, D. -W., Klagyivik, P., Klar, J., Knude, J., Kochukhov, O., Kolka, I., Kos, J., Kutka, A., Lainey, V., LeBouquin, D., Liu, C., Loreggia, D., Makarov, V. V., Marseille, M. G., Martayan, C., Martinez-Rubi, O., Massart, B., Meynadier, F., Mignot, S., Munari, U., Nguyen, A. -T., Nordlander, T., O'Flaherty, K. S., Ocvirk, P., Sanz, A. Olias, Ortiz, P., Osorio, J., Oszkiewicz, D., Ouzounis, A., Palmer, M., Park, P., Pasquato, E., Peltzer, C., Peralta, J., Péturaud, F., Pieniluoma, T., Pigozzi, E., Poelsy, J., Prat, G., Prod'homme, T., Raison, F., Rebordao, J. M., Risquez, D., Rocca-Volmerange, B., Rosen, S., Ruiz-Fuertes, M. I., Russo, F., Sembay, S., Vizcaino, I. Serraller, Short, A., Siebert, A., Silva, H., Sinachopoulos, D., Slezak, E., Soffel, M., Sosnowska, D., Straižys, V., ter Linden, M., Terrell, D., Theil, S., Tiede, C., Troisi, L., Tsalmantza, P., Tur, D., Vaccari, M., Vachier, F., Valles, P., Van Hamme, W., Veltz, L., Virtanen, J., Wallut, J. -M., Wichmann, R., Wilkinson, M. I., Ziaeepour, H., and Zschocke, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Context. The first Gaia Data Release contains the Tycho-Gaia Astrometric Solution (TGAS). This is a subset of about 2 million stars for which, besides the position and photometry, the proper motion and parallax are calculated using Hipparcos and Tycho-2 positions in 1991.25 as prior information. Aims. We investigate the scientific potential and limitations of the TGAS component by means of the astrometric data for open clusters. Methods. Mean cluster parallax and proper motion values are derived taking into account the error correlations within the astrometric solutions for individual stars, an estimate of the internal velocity dispersion in the cluster, and, where relevant, the effects of the depth of the cluster along the line of sight. Internal consistency of the TGAS data is assessed. Results. Values given for standard uncertainties are still inaccurate and may lead to unrealistic unit-weight standard deviations of least squares solutions for cluster parameters. Reconstructed mean cluster parallax and proper motion values are generally in very good agreement with earlier Hipparcos-based determination, although the Gaia mean parallax for the Pleiades is a significant exception. We have no current explanation for that discrepancy. Most clusters are observed to extend to nearly 15 pc from the cluster centre, and it will be up to future Gaia releases to establish whether those potential cluster-member stars are still dynamically bound to the clusters. Conclusions. The Gaia DR1 provides the means to examine open clusters far beyond their more easily visible cores, and can provide membership assessments based on proper motions and parallaxes. A combined HR diagram shows the same features as observed before using the Hipparcos data, with clearly increased luminosities for older A and F dwarfs., Comment: Accepted for publication by A&A. 21 pages main text plus 46 pages appendices. 34 figures main text, 38 figures appendices. 8 table in main text, 19 tables in appendices

Published
2017
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4. A survey of Phlebotomine sand flies across their northern distribution range limit in Western Europe

Author

Risueño, J., primary, Bersihand, S., additional, Bender, C., additional, Cornen, T., additional, De Boer, K., additional, Ibáñez-Justicia, A., additional, Rey, D., additional, Rozier, Y., additional, Schneider, A., additional, Stroo, A., additional, Vanslembrouck, A., additional, Van Bortel, W., additional, Weigand, A., additional, Zambianchi, D., additional, Pérez Cutillas, P., additional, Oerther, S., additional, Braks, M., additional, Wint, G.R.W., additional, Berriatua, E., additional, and Schaffner, F., additional

Published
2024
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5. Adjuvant abemaciclib combined with endocrine therapy for high-risk early breast cancer: updated efficacy and Ki-67 analysis from the monarchE study

Author

Jimenez, M.M., Johnston, S., Boyle, F., Steger, G.G., Neven, P., Jiang, Z., Campone, M., Huober, J., Shimizu, C., Cicin, I., Wardley, A., Tolaney, S.M., Abuin, G.G., Zarba, J., Lim, E., Sant, P., Liao, N., Christiansen, B., Eigeliene, N., Martin-Babau, J., Ettl, J., Mavroudis, D., Chiu, J., Boer, K., Nagarkar, R., Paluch-Shimon, S., Moscetti, L., Sagara, Y., Kim, S.-B., Maciel, M.M., Tjan-Heijnen, V., Broom, R., Lacko, A., Schenker, M., Volkov, N., Sim Yap, Y., Coccia-Portugal, M., Ángel García Sáenz, J., Andersson, A., Chao, T.-Y., Gokmen, E., Harputluoglu, H., Berzoy, O., Patt, D., McArthur, H., Chew, H., Chalasani, P., Kaufman, P., Tedesco, K., Graff, S.L., Harbeck, N., Rastogi, P., Martin, M., Shao, Z.M., Fasching, P.A., Huang, C.S., Jaliffe, G.G., Tryakin, A., Goetz, M.P., Rugo, H.S., Senkus, E., Testa, L., Andersson, M., Tamura, K., Del Mastro, L., Kreipe, H., Hegg, R., Sohn, J., Guarneri, V., Cortés, J., Hamilton, E., André, V., Wei, R., Barriga, S., Sherwood, S., Forrester, T., Munoz, M., Shahir, A., San Antonio, B., Nabinger, S.C., Toi, M., Johnston, S.R.D., and O’Shaughnessy, J.

Published
2021
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6. Final results from the PERUSE study of first-line pertuzumab plus trastuzumab plus a taxane for HER2-positive locally recurrent or metastatic breast cancer, with a multivariable approach to guide prognostication

Author

Bachelot, T., Bouzid, K., Campone, M., Desmoulins, I., Coudert, B., Bondarenko, I., Nowecki, Z., Glogowska, I., Ciruelos Gil, E., Errihani, H., Dalenc, F., Ricci, F., Dieras, V., Kaufman, B., Paluch-Shimon, S., Wardley, A., Schneeweiss, A., Ferreira, A., Mano, M., Kalofonos, H., Andreetta, C., Puglisi, F., Montemurro, F., Barrett, S., Zhang, Q., Mavroudis, D., Matus, J., Villarreal Garza, C., Beato, C., Ismael, G., Hu, X., Abdel Azeem, H., Gaafar, R., Perrin, C., Kerbrat, P., Ettl, J., Paepke, S., Hitre, E., Lang, I., Trudeau, M., Verma, S., Li, H., Hoffmann, O., Aktas, B., Cariello, A., Cruciani, G., Tienghi, A., Tondini, C., Al-Twegieri, T., Loman, N., Laing, R., Miles, D., Brain, E., Fasching, P., Lux, M., Frassoldati, A., Aziz, Z., Salas, J., Streb, J., Krzemieniecki, K., Wronski, A., Garcia Garcia, J., Menjon Beltran, S., Cicin, I., Schmid, P., Gallagher, C., Turner, N., Tong, Z., Boer, K., Juhász, B., Horvath, Z., Bianchini, G., Gianni, L., Curigliano, G., Juarez Ramiro, A., Susnjar, S., Matos, E., Sevillano, E., Garcia Estevez, L., Gokmen, E., Uslu, R., Wildiers, H., Schutz, F., Cruz, M., Bourgeois, H., von Schumann, R., Stemmer, S., Dominguez, A., Morales-Vásques, F., Wojtukiewicz, M., Trifunovic, J., Echarri Gonzalez, M.J., Illarramendi Mañas, J., Martinez De Dueñas, E., Voitko, N., Hicks, J., Waters, S., Barrett-Lee, P., Wheatley, D., De Boer, R., Cocquyt, V., Jerusalem, G., Barrios, C., Panasci, L., Mattson, J., Tanner, M., Gozy, M., Vasilopoulos, G., Papandreou, C., Revesz, J., Battelli, N., Benedetti, G., Latini, L., Gridelli, C., Lazaro Leon, J., Alarcón Company, J., Arance Fernandez, A., Barnadas Molins, A., Calvo Plaza, I., Bratos, R., Gonzalez Martin, A., Izarzugaza Peron, Y., Klint, L., Kovalev, A., McCarthy, N., Yeo, B., Kee, D., Thomson, J., White, S., Greil, R., Wang, S., Artignan, X., Juhasz-Böess, I., Rody, A., Ngan, R., Dourleshter, F., Goldberg, H., Doni, L., Di Costanzo, F., Ferraù, F., Drobniene, M., Aleknavicius, E., Rashid, K., Costa, L., de la Cruz Merino, L., Garcia Saenz, J., López, R., Del Val Munoz, O., Ozyilkan, O., Azribi, F., Jaafar, H., Baird, R., Verrill, M., Beith, J., Petzer, A., Moreira de Andrade, J., Bernstein, V., Macpherson, N., Rayson, D., Saad Eldin, I., Achille, M., Augereau, P., Müller, V., Rasco, A., Evron, E., Katz, D., Berardi, R., Cascinu, S., De Censi, A., Gennari, A., El-Saghir, N., Ghosn, M., Oosterkamp, H.M., Van den Bosch, J., Kukulska, M., Kalinka, E., Alonso, J., Dalmau Portulas, E., Del Mar Gordon Santiago, M., Pelaez Fernandez, I., Aksoy, S., Altundag, K., Senol Coskun, H., Bozcuk, H., Shparyk, Y., Barraclough, L., Levitt, N., Panwar, U., Kelly, S., Rigg, A., Varughese, M., Castillo, C., Fein, L., Malik, L., Stuart-Harris, R., Singer, C., Stoeger, H., Samonigg, H., Feng, J., Cedeño, M., Ruohola, J., Berdah, J.-F., Goncalves, A., Orfeuvre, H., Grischke, E.-M., Simon, E., Wagner, S., Koumakis, G., Papazisis, K., Ben Baruch, N., Fried, G., Geffen, D., Karminsky, N., Peretz, T., Cavanna, L., Pedrazzioli, P., Grasso, D., Ruggeri, E., D’Auria, G., Moscetti, L., Juozaityte, E., Rodriguez Cid, J., Roerdink, H., Siddiqi, N., Passos Coelho, J., Arcediano Del Amo, A., Garcia Garre, E., García Gonzalez, M., Garcia-Palomo Perez, A., Herenandez Perez, C., Lopez Alvarez, P., Lopez De Ceballos, M.H., Martínez Jañez, N., Mele Olive, M., McAdam, K., Perren, T., Dunn, G., Humphreys, A., Taylor, W., Vera, R., Kaen, L., Andel, J., Steger, G., De Grève, J., Huizing, M., Hegg, R., Joy, A., Kuruvilla, P., Sehdev, S., Smiljanic, S., Kütner, R., Alexandre, J., Grosjean, J., Laplaige, P., Largillier, R., Maes, P., Martin, P., Pottier, V., Christensen, B., Khandan, F., Lück, H.-J., Zahm, D.-M., Fountzilas, G., Karavasilis, V., Safra, T., Inbar, M., Ryvo, L., Bonetti, A., Seles, E., Giacobino, A., Chavarri Guerra, Y., de Jongh, F., van der Velden, A., van Warmerdam, L., Vrijaldenhoven, S., Smorenburg, C.H., Cavero, M., Andres Conejero, R., Oltra Ferrando, A., Redondo Sanchez, A., Ribelles Entrena, N., Saura Grau, S., Viñas Vilaro, G., Bachmeier, K., Beresford, M., Butt, M., Joffe, J., Poole, C., Woodings, P., Chakraborti, P., Yordi, G., Woodward, N., Nobre, A., Luiz Amorim, G., Califaretti, N., Fox, S., Robidoux, A., Li, E., Li, N., Jiang, J., Soria, T., Padrik, P., Lahdenpera, O., Barletta, H., Dohollou, N., Genet, D., Prulhiere, K., Coeffic, D., Facchini, T., Vieillot, S., Catala, S., Teixeira, L., Hesse, T., Kühn, T., Ober, A., Repp, R., Schröder, W., Pectasides, D., Bodoky, G., Kahan, Z., Jiveliouk, I., Rosengarten, O., Rossi, V., Alabiso, O., Pérez Martínez, M., van de Wouw, A.J., Smok-Kalwat, J., Damasecno, M., Augusto, I., Sousa, G., Saadein, A., Abdelhafiez, N., Abulkhair, O., Antón Torres, A., Corbellas Aparicio, M., Llorente Domenech, R., Florián Jerico, J., Garcia Mata, J., Gil Raga, M., Galan Brotons, A., Llombart Cussac, A., Llorca Ferrandiz, C., Martinez Del Prado, P., Olier Garate, C., Rodriguez Sanchez, C., Sanchez Gomez, R., Santisteban Eslava, M., Soberino, J., Vidal Losada Garcia, M., Soto de Prado, D., Torrego Garcia, J., Vicente Rubio, E., Garcia, M., Murias Rosales, A., Granstam Björneklett, H., Narbe, U., Jafri, M., Rea, D., Newby, J., Jones, A., Westwell, S., Ring, A., Alonso, I., Rodríguez, R., Ciruelos, E., Peretz-Yablonski, T., Merot, J.-L., Trask, P., du Toit, Y., Pena-Murillo, C., Revelant, V., and Klingbiel, D.

Published
2021
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7. Congenital heart disease in the ESC EORP Registry of Pregnancy and Cardiac disease (ROPAC)

Author

Hall, Roger, Roos-Hesselink, Jolien, Stein, Joerg, Parsonage, William Anthony, Budts, Werner, De Backer, Julie, Grewal, Jasmin, Marelli, Ariane, Kaemmerer, Harald, Jondeau, Guillaume, Johnson, Mark, Maggioni, Aldo P., Tavazzi, Luigi, Thilen, Ulf, Elkayam, Uri, Otto, Catherine, Sliwa, Karen, Aquieri, A., Saad, A., Vega, H. Ruda, Hojman, J., Caparros, J.M., Blanco, M. Vazquez, Arstall, M., Chung, C.M., Mahadavan, G., Aldridge, E., Wittwer, M., Chow, Y.Y., Parsonage, W.A., Lust, K., Collins, N., Warner, G., Hatton, R., Gordon, A., Nyman, E., Stein, J., Donhauser, E., Gabriel, H., Bahshaliyev, A., Guliyev, F., Hasanova, I., Jahangirov, T., Gasimov, Z., Salim, A., Ahmed, C.M., Begum, F., Hoque, M.H., Mahmood, M., Islam, M.N., Haque, P.P., Banerjee, S.K., Parveen, T., Morissens, M., De Backer, J., Demulier, L., de Hosson, M., Budts, W., Beckx, M., Kozic, M., Lovric, M., Kovacevic-Preradovic, T., Chilingirova, N., Kratunkov, P., Wahab, N., McLean, S., Gordon, E., Walter, L., Marelli, A., Montesclaros, A.R., Monsalve, G., Rodriguez, C., Balthazar, F., Quintero, V., Palacio, W., Cadavid, L.A. Mejía, Ortiz, E. Munoz, Hoyos, F. Fortich, Guerrero, E. Arevalo, Ricardo, J. Gandara, Penagos, J. Velasquez, Vavera, Z., Prague, Popelova, J., Vejlstrup, N., Grønbeck, L., Johansen, M., Ersboll, A., Elrakshy, Y., Eltamawy, K., Abd-El Aziz, M. Gamal, El Nagar, A., Ebaid, H., Elenin, H. Abo, Saed, M., Farag, S., Makled, W., Sorour, K., Ashour, Z., El-Sayed, G., Meguid Mahdy, M. Abdel, Taha, N., Dardeer, A., Shabaan, M., Ali, M., Moceri, P., Duthoit, G., Gouton, M., Nizard, J., Baris, L., Cohen, S., Ladouceur, M., Khimoud, D., Iung, B., Berger, F., Olsson, A., Gembruch, U., Merz, W.M., Reinert, E., Clade, S., Kliesch, Y., Wald, C., Sinning, C., Kozlik-Feldmann, R., Blankenberg, S., Zengin-Sahm, E., Mueller, G., Hillebrand, M., Hauck, P., von Kodolitsch, Y., Zarniko, N., Baumgartner, Muenster H., Schmidt, R., Hellige, A., Tutarel, O., Kaemmerer, H., Kuschel, B., Nagdyman, N., Motz, R., Maisuradze, D., Frogoudaki, A., Iliodromitis, E., Anastasiou-Nana, M., Marousi, Triantafyllis, D., Bekiaris, G., Karvounis, H., Giannakoulas, G., Ntiloudi, D., Mouratoglou, S.A., Temesvari, A., Balint, H., Kohalmi, D., Merkely, B., Liptai, C., Nemes, A., Forster, T., Kalapos, A., Berek, K., Havasi, K., Ambrus, N., Shelke, A., Kawade, R., Patil, S., Martanto, E., Aprami, T.M., Purnomowati, A., Cool, C.J., Hasan, M., Akbar, R., Hidayat, S., Dewi, T.I., Permadi, W., Soedarsono, D.A., Ansari-Ramandi, M.M., Samiei, N., Tabib, A., Kashfi, F., Ansari-Ramandi, S., Rezaei, S., Farhan, H. Ali, Al-Hussein, A., Al-Saedi, G., Mahmood, G., Yaseen, I.F., Al-Yousuf, L., AlBayati, M., Mahmood, S., Raheem, S., AlHaidari, T., Dakhil, Z., Thornton, P., Donnelly, J., Bowen, M., Blatt, A., Elbaz-Greener, G., Shotan, A., Yalonetsky, S., Goland, S., Biener, M., Assenza, G. Egidy, Bonvicini, M., Donti, A., Bulgarelli, A., Prandstraller, D., Romeo, C., Crepaz, R., Sciatti, E., Metra, M., Orabona, R., Ali, L. Ait, Festa, P., Fesslova, V., Bonanomi, C., Calcagnino, M., Lombardi, F., Colli, A.M., Ossola, M.W., Gobbi, C., Gherbesi, E., Tondi, L., Schiavone, M., Squillace, M., Carmina, M.G., Maina, A., Macchi, C., Gollo, E., Comoglio, F.M., Montali, N., Re, P., Bordese, R., Todros, T., Donvito, V., Marra, W. Grosso, Sinagra, G., D'Agata Mottolese, B., Bobbo, M., Gesuete, V., Rakar, S., Ramani, F., Niwa, K., Mekebekova, D., Mussagaliyeva, A., Lee, T., Mirrakhimov, E., Abilova, S., Bektasheva, E., Neronova, K., Lunegova, O., Žaliūnas, R., Jonkaitienė, R., Petrauskaitė, J., Laucevicius, A., Jancauskaite, D., Lauciuviene, L., Gumbiene, L., Lankutiene, L., Glaveckaite, S., Laukyte, M., Solovjova, S., Rudiene, V., Chee, K.H., Yim, C.C.-W., Ang, H.L., Kuppusamy, R., Watson, T., Caruana, M., Estensen, M.-E., Kayani, M.G.A. Mahmood, Munir, R., Tomaszuk-Kazberuk, A., Sobkowicz, B., Przepiesc, J., Lesniak-Sobelga, A., Tomkiewicz-Pajak, L., Komar, M., Olszowska, M., Podolec, P., Wisniowska-Smialek, S., Lelonek, M., Faflik, U., Cichocka-Radwan, A., Plaskota, K., Trojnarska, O., Guerra, N., de Sousa, L., Cruz, C., Ribeiro, V., Jovanova, S., Petrescu, V., Jurcut, R., Ginghina, C., Coman, I. Mircea, Musteata, M., Osipova, O., Golivets, T., Khamnagadaev, I., Golovchenko, O., Nagibina, A., Ropatko, I., Gaisin, I.R., Shilina, L. Valeryevna, Sharashkina, N., Shlyakhto, E., Irtyuga, O., Moiseeva, O., Karelkina, E., Zazerskaya, I., Kozlenok, A., Sukhova, I., Jovovic, L., Prokšelj, K., Koželj, M., Askar, A.O., Abdilaahi, A.A., Mohamed, M.H., Dirir, A.M., Sliwa, K., Manga, P., Pijuan-Domenech, A., Galian-Gay, L., Tornos, P., Subirana, M.T., T, M., Subirana, Oliver, J.M., Garcia-Aranda Dominguez, B., Gonzalez, I. Hernandez, Jimenez, J.F. Delgado, Subias, P. Escribano, Murga, N., Elbushi, A., Suliman, A., Jazzar, K., Murtada, M., Ahamed, N., Dellborg, M., Furenas, E., Jinesjo, M., Skoglund, K., Eriksson, P., Gilljam, T., Thilen, U., Tobler, D., Wustmann, K., Schwitz, F., Schwerzmann, M., Rutz, T., Bouchardy, J., Greutmann, M., Lopes, B.M. Santos, Meier, L., Arrigo, M., de Boer, K., Konings, T., Wajon, E., Wagenaar, L.J., Polak, P., Pieper, E.P.G., Roos-Hesselink, J., van Hagen, I., Duvekot, H., Cornette, J.M.J., De Groot, C., van Oppen, C., Sarac, L., Esen, O. Batukan, Enar, S. Catirli, Mondo, C., Ingabire, P., Nalwanga, B., Semu, T., Salih, B.T., Almahmeed, W.A.R., Wani, S., Farook, F.S. Mohamed, Ain, Al, Gerges, F., Komaranchath, A.M., Al bakshi, F., Al Mulla, A., Yusufali, A.H., Al Hatou, E.I., Bazargani, N., Hussain, F., Hudsmith, L., Thompson, P., Thorne, S., Bowater, S., Money-Kyrle, A., Clifford, P., Ramrakha, P., Firoozan, S., Chaplin, J., Bowers, N., Adamson, D., Schroeder, F., Wendler, R., Hammond, S., Nihoyannopoulos, P., Norfolk, Norwich, Hall, R., Freeman, L., Veldtman, G., Kerr, J., Tellett, L., Scott, N., Bhatt, A.B., DeFaria Yeh, D., Youniss, M.A., Wood, M., Sarma, A.A., Tsiaras, S., Stefanescu, A., Duran, J.M., Stone, L., Majdalany, D.S., Chapa, J., Chintala, K., Gupta, P., Botti, J., Ting, J., Davidson, W.R., Wells, G., Sparks, D., Paruchuri, V., Marzo, K., Patel, D., Wagner, W., Ahanya, S.N., Colicchia, L., Jentink, T., Han, K., Loichinger, M., Parker, M., Longtin, C., Yetman, A., Erickson, K., Cramer, J., Tsai, S., Fletcher, B., Warta, S., Cohen, C., Lindblade, C., Puntel, R., Nagaran, K., Croft, N., Gurvitz, M., Otto, C., Talluto, C., Murphy, D., Perlroth, M.G., Ramlakhan, Karishma P., Johnson, Mark R., Lelonek, Malgorzata, Saad, Aly, Gasimov, Zaur, Sharashkina, Natalia V., Thornton, Patrick, Arstall, Margaret, and Roos-Hesselink, Jolien W.

Published
2021
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8. High-velocity gas towards the LMC resides in the Milky Way halo

Author

Richter, P., de Boer, K. S., Werner, K., and Rauch, T.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

To explore the origin of high-velocity gas in the direction of the Large Magellanic Cloud (LMC) we analyze absorption lines in the ultraviolet spectrum of a Galactic halo star that is located in front of the LMC at d=9.2 kpc distance. We study the velocity-component structure of low and intermediate metal ions in the spectrum of RXJ0439.8-6809, as obtained with the Cosmic Origins Spectrograph (COS) onboard HST, and measure equivalent widths and column densities for these ions. We supplement our COS data with a Far-Ultraviolet Spectroscopic Explorer spectrum of the nearby LMC star Sk-69 59 and with HI 21cm data from the Leiden-Argentina-Bonn (LAB) survey. Metal absorption towards RXJ0439.8-6809 is unambiguously detected in three different velocity components near v_LSR=0,+60, and +150 km/s. The presence of absorption proves that all three gas components are situated in front of the star, thus being located in the disk and inner halo of the Milky Way. For the high-velocity cloud (HVC) at v_LSR=+150 km/s we derive an oxygen abundance of [O/H]=-0.63 (~0.2 solar) from the neighbouring Sk-69 59 sightline, in accordance with previous abundance measurements for this HVC. From the observed kinematics we infer that the HVC hardly participates in the Galactic rotation. Our study shows that the HVC towards the LMC represents a Milky Way halo cloud that traces low-column density gas with relatively low metallicity. It rules out scenarios in which the HVC represents material close to the LMC that stems from a LMC outflow., Comment: 4 pages, 3 figures; submitted to A&A Letters

Published
2015
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11. A systematic review and meta-analysis of the relationship between obsessive-compulsive symptoms and symptoms of proposed orthorexia nervosa: The contribution of assessments

Author

Huynh, PA, Miles, S, de Boer, K, Meyer, D, Nedeljkovic, M, Huynh, PA, Miles, S, de Boer, K, Meyer, D, and Nedeljkovic, M

Abstract

OBJECTIVE: This systematic review and meta-analysis aimed to update the literature on orthorexia nervosa (ON), a proposed diagnosis of pathologically 'healthy' eating, by critically analysing the current evidence for the relationship between ON and obsessive-compulsive (OC) symptoms. Further, this paper aimed to compare the ON/OC relationship significance and strength based on when the ON measurement tool was developed. METHOD: PsycINFO, PubMed and Web of Science databases were queried for quantitative, peer-reviewed studies recruiting adult participants, published in English up to April 2023. Studies not directly comparing ON and OC symptoms were excluded. After full-text review and quality assessment, 40 studies were included in the systematic review and 31 studies in the meta-analysis. RESULTS: ON assessments created prior to the 2016 revised ON diagnostic criteria do not appear to fully capture OC symptoms. Studies using earlier developed ON assessments demonstrated inconsistent ON/OC relationships whereas studies implementing more recent assessments (from 2018 onwards) found consistently significant, larger relationships, highlighting a previously underrated OC component of ON. CONCLUSIONS: Early ON studies, and studies utilising early ON assessments should be interpreted with caution, particularly in relation to OC symptom involvement in ON. Future research should validate novel ON assessments and investigate common underlying factors.

Published
2024

13. Can filamentary accretion explain the orbital poles of the Milky Way satellites?

Author

Pawlowski, M. S., Kroupa, P., Angus, G., de Boer, K. S., Famaey, B., and Hensler, G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Several scenarios have been suggested to explain the phase-space distribution of the Milky Way (MW) satellite galaxies in a disc of satellites (DoS). To quantitatively compare these different possibilities, a new method analysing angular momentum directions in modelled data is presented. It determines how likely it is to find sets of angular momenta as concentrated and as close to a polar orientation as is observed for the MW satellite orbital poles. The method can be easily applied to orbital pole data from different models. The observed distribution of satellite orbital poles is compared to published angular momentum directions of subhalos derived from six cosmological state-of-the-art simulations in the Aquarius project. This tests the possibility that filamentary accretion might be able to naturally explain the satellite orbits within the DoS. For the most likely alignment of main halo and MW disc spin, the probability to reproduce the MW satellite orbital pole properties turns out to be less than 0.5 per cent in Aquarius models. Even an isotropic distribution of angular momenta has a higher likelihood to produce the observed distribution. The two Via Lactea cosmological simulations give results similar to the Aquarius simulations. Comparing instead with numerical models of galaxy-interactions gives a probability of up to 90 per cent for some models to draw the observed distribution of orbital poles from the angular momenta of tidal debris. This indicates that the formation as tidal dwarf galaxies in a single encounter is a viable, if not the only, process to explain the phase-space distribution of the MW satellite galaxies., Comment: 14 pages, 4 figures, 3 tables. Accepted for publication in MNRAS

Published
2012
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14. Making Counter-Orbiting Tidal Debris: The Origin of the Milky Way Disc of Satellites

Author

Pawlowski, M. S., Kroupa, P., and de Boer, K. S.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Using stellar-dynamical calculations it is shown for the first time that counter-orbiting material emerges naturally in tidal interactions of disc galaxies. Model particles on both pro- and retrograde orbits can be formed as tidal debris in single encounters with disc galaxies of 1-to-1 and 4-to-1 mass ratios. A total of 74 model calculations are performed for a range of different initial parameters. Interactions include fly-by and merger cases. The fraction of counter-orbiting material produced varies over a wide range (from a few up to 50 percent). All fly-by models show a similar two-phase behaviour, with retrograde material forming first. Properties of the prograde and retrograde populations are extracted to make an observational discrimination possible. During such encounters the tidal debris occupies a certain region in phase space. In this material, tidal-dwarf galaxies may form. The modelling therefore can explain why galaxies may have dwarf galaxies orbiting counter to the bulk of their dwarf galaxies. An example is the Sculptor dwarf of the Milky Way, which orbits counter to the bulk of the disc of satellites. The modelling thus supports the scenario of the MW satellites being ancient tidal-dwarf galaxies formed from gaseous material stripped from another galaxy during an encounter with the young MW. A possible candidate for this galaxy is identified as the Magellanic Cloud progenitor galaxy. Its angular motion fits the angular motion of the MW disc of satellites objects. This scenario is in agreement with Lynden-Bell's original suggestion for the origin of the dSph satellites and the near-unbound orbit of the LMC., Comment: 26 pages, 13 figures. Accepted for publication in Astronomy and Astrophysics

Published
2011
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15. Hysteresis of atmospheric parameters of 12 RR Lyrae stars based on multichannel simultaneous Stroemgren photometry

Author

de Boer, K. S. and Maintz, G.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

RR Lyrae stars have been observed to improve the insight into the processes at work in their atmospheres. Simultaneous Stroemgren-photometry allows to obtain a rapid sequence of measurements in which photometric indices are unaffected by non-optimum observing conditions. The indices y, b-y, and c_1 are used with an established calibration to derive T_eff and to derive the gravity, log g_BJ from the Balmer jump, throughout the pulsation cycle. By employing the equations for stellar structure, additional parameters can be derived. Stroemgren photometry and its calibration in terms of T_eff and log g can be used to determine the run of R and the atmosphere pulsation velocity. We find that the Balmer-line strengths are correlated with T_eff and that the strength of the Ca_ii K line correlates well with the radius of the star and thus the pulsation-dependent density of the atmosphere. The density in the stellar atmosphere fluctuates as indicated by the changes in the gravity log g_BJ, derived from c_1, between 2.3 and 4.5 dex. Also the Stroemgren metal index, m_1, fluctuates. We find a disagreement between log g(T,L,M), the gravity calculated from T_eff, L, and the mass M,and the gravity log g_BJ. This can be used to reassess the mass and the absolute magnitude of an individual star.The curves derived for the pulsational velocity V_pul differ from curves obtained from spectra needed to apply the Baade-Wesselink method; we think these differences are due to phase dependent differences in the optical depth levels sampled in continuum photometry and in spectroscopy. We find an atmospheric oscillation in these fundamental mode RR Lyrae stars of periodicity P/7., Comment: 12 pages, 11 figures

Published
2010
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16. Local-Group tests of dark-matter Concordance Cosmology: Towards a new paradigm for structure formation

Author

Kroupa, P., Famaey, B., de Boer, K. S., Dabringhausen, J., Pawlowski, M. S., Boily, C. M., Jerjen, H., Forbes, D., Hensler, G., and Metz, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology
Abstract

(abridged) Predictions of the Concordance Cosmological Model (CCM) of the structures in the environment of large spiral galaxies are compared with observed properties of Local Group galaxies. Five new most probably irreconcilable problems are uncovered. However, the Local Group properties provide hints that may lead to a solution of the above problems The DoS and bulge--satellite correlation suggest that dissipational events forming bulges are related to the processes forming phase-space correlated satellite populations. Such events are well known to occur since in galaxy encounters energy and angular momentum are expelled in the form of tidal tails, which can fragment to form populations of tidal-dwarf galaxies (TDGs) and associated star clusters. If Local Group satellite galaxies are to be interpreted as TDGs then the sub-structure predictions of CCM are internally in conflict. All findings thus suggest that the CCM does not account for the Local Group observations and that therefore existing as well as new viable alternatives have to be further explored. These are discussed and natural solutions for the above problems emerge., Comment: A and A, in press, 25 pages, 9 figures; new version contains minor text adjustments for conformity with the published version and additional minor changes resulting from reader's feedback. The speculation on a dark force has been added. Also, the Fritz Zwicky Paradox is now included to agree with the published version

Published
2010
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17. Kinematics of RHB stars to trace the structure of the galaxy

Author

Kaempf, T. A., de Boer, K. S., and Altmann, M.

Subjects
Astrophysics
Abstract

Red horizontal-branch (RHB) stars have been selected from the HIPPARCOS catalogue to investigate their kinematics and spatial distribution. HIPPARCOS parallaxes, literature radial velocities and HIPPARCOS proper motions, together with models for the gravitational potential of the Milky Way allow a calculation of the actual velocity vectors and the orbits of the RHB stars. The velocity characteristics are used to define a halo population sample (HPS) in the collection of RHBs. The orbits lead statistically to an overall z-distance probability distribution, showing that the RHBs exhibit two populations, a disk one having a scale height of h_disk ~0.6 kpc and a halo one of ~4 kpc. We have investigated the influence on our results of parallax accuracy and of a demarcation line in the HRD between the RHB and the red-giant (RG) star region. Neither of them show marked effects. We have performed the orbit analysis using the potential model of Allen & Santillan as well as of Dehnen & Binney. The results differ only slightly for the disk population, showing that these potential models are not a critical part of such orbit investigations. RHB scale height values are smaller than those found earlier for sdB stars, most likely because the samples of stars used had different spatial distributions a priori. The data do not allow us to specify a trend in the kinematic behaviour of star types along the horizontal branch., Comment: 10 pages, 10 figures, accepted by A&A 16/11/2004

Published
2004
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18. Intermediate scale structure of the interstellar medium towards NGC 6231 in Sco OB1 with FUSE

Author

Marggraf, O., Bluhm, H., and de Boer, K. S.

Subjects
Astrophysics
Abstract

The FUSE far-ultraviolet interstellar spectra toward seven targets in NGC 6231 show that the molecules H_2, HD, and CO as well as various atomic species are distributed in several clouds. The main absorption component found on the sight lines lies in the Lupus cloud region at a distance of about 150 pc, and there is a weaker second one, presumably in the Sco OB1 shell surrounding NGC 6231 (d~1.8 kpc). H_2 excitation modelling is used to constrain the radiation field and the density in the gas; HD is used to estimate the abundance of H+. The small angular separation of the target stars allows column density variations to be probed over the field of view, on scales of 0.05 pc in the case of the Lupus cloud distance. They are 40% for H_2 and 60% for H I. A rather strong radiation field inside the molecular clouds suggests a separation of the gas into smaller cloudlets also along the line of sight., Comment: 12 pages, accepted for publication in Astronomy & Astrophysics

Published
2003
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19. Studying the populations of our Galaxy using the kinematics of sdB stars

Author

Altmann, M., Edelmann, H., and de Boer, K. S.

Subjects
Astrophysics
Abstract

We have analysed the kinematics of a sample of 114 hot subdwarf stars, for 2/3 of which we present new proper motions, spectroscopic and photometric data. The vast majority of the stars show a kinematic behaviour that is similar to that of Thick Disk stars. Some stars have velocities rather fitting to solar, i.e. Thin Disk, kinematics. 16 objects have orbital velocities which differ considerably from those of Disk stars. These are members of the Galactic Halo. We analysed the velocity dispersions and calculated orbits. Most stars feature orbits with disk character (eccentricity <= 0.5), a few reach far above the Galactic plane and have very eccentric orbits (ecc >= 0.7). The intermediate eccentricity range is poorly populated. This indicates that the (Thick) Disk and the Halo are kinematically disjunct. Plotting a histogram of the orbit data points along z leads to the z-distance probability distribution of the star; doing this for all stars leads to the z-distance probability distribution of the sample. The logarithmic histogram shows two slopes, each representing the scale height of a population. The disk component has a scale height of 0.9 (0.1) kpc, which is consistent with earlier results and is similar to that of the Thick Disk. The other slope represents a component with a scale height ~7 kpc, a much flatter gradient than for the disk component. This shows that the vast majority of the sdBs are Disk stars, but a Halo minority is present, too. The kinematic history and population membership of the sdB stars on the whole is different from that of the cooler HBA stars, which are predominantly or even exclusively Halo objects. This leads to the question, whether the Halo sdB stars are of similar origin as the HBAs, or whether their kinematical behaviour possibly represents another origin, such as infalling stellar aggregates., Comment: accepted for publication in Astronomy and Astrophysics (A&A), 20 pages, 9 figures, 4 tables

Published
2003
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20. ROSAT X-ray sources in the field of the LMC. III.The log N -- log S of background AGN and the LMC gas

Author

Kahabka, P., de Boer, K. S., and Bruens, C.

Subjects
Astrophysics
Abstract

We use 50 (candidate) background X-ray sources (AGN) in the LMC field observed in ROSAT PSPC observations to derive the observed log N - log S relation. We correct for the varying PSPC exposure and the absorption due to the galactic and the LMC gas. We compare the observed log N - log S with a theoretical log N - log S of the soft extragalactic X-ray background (AGN and a cluster of galaxy contribution). We find that the observed log N - log S has a deficiency with respect to the theoretical log N - log S. Factors which can account for such a deficiency are: (1) incompleteness of the selected AGN and cluster of galaxies sample, (2) deviation of the log N - log S in the LMC field from the log N - log S derived from a large sample of AGN in several fields, (3) existence of gas additional to the HI represented in the Parkes HI map of the LMC field. We investigate the likely contribution of these effects and find that (1) a fraction of at most 30% of the background sources may not have been found in this analysis and may contribute to the observed deficiency. (2) We cannot exclude a deviation of the log N - log S in the field of the LMC from a theoretical log N - log S, especially the cluster of galaxy contribution may show variations across the sky. (3) If LMC gas (restricted to >10^21 cm^-2 columns) in addition to the HI represented in the Parkes map would be responsible for the deficiency, then a factor of >0.3 (at 90% confidence) of additional gas would be required. This would equal a molecular mass fraction of >21%, which would be larger than, but within the uncertainties consistent with a molecular mass fraction of ~30% derived from CO observations (for columns >10^21 cm^-2)., Comment: 14 pages, accepted for publication in A&A, March 22 2002

Published
2002
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21. ROSAT X-ray sources in the field of the LMC I.Total LMC gas from the background AGN spectral fits

Author

Kahabka, P., de Boer, K. S., and Bruens, C.

Subjects
Astrophysics
Abstract

We analyzed a sample of 26 background X-ray sources in a ~60 square degree field of the Large Magellanic Cloud observed with the ROSAT PSPC. The sample has been selected from previously classified and optically identified X-ray sources. In addition pointlike and spectrally hard sources with at least 100 to 200 observed counts have been used for the analysis. We performed X-ray spectral fitting and derived total hydrogen absorbing column densities due to LMC gas in the range 10^20 - 2. 10^21 cm^-2. We compared these columns with the HI columns derived from a 21-cm Parkes survey of the LMC. For 7 optically identified sources we find, within the uncertainties derived from the X-ray spectral fit, agreement for both columns. For further 19 sources we constrain the LMC columns from the X-ray spectral fit assuming that the powerlaw photon index is that of AGN type spectra. We derive for 20 sources gas columns which are within the uncertainties in agreement with the HI columns. We derive for two background sources (RX J0536.9-6913 and RX J0547.0-7040) hydrogen absorbing column densities due to LMC gas, which are in excess to the HI columns. These sources - located in regions of large (~3. 10^21 cm^-2) LMC HI column densities - could be seen through additional gas which may be warm and diffuse, cold or molecular. For 10 sources we derive upper limits for the gas columns additional to HI and constrain the molecular mass fraction to <(30-140)%., Comment: Accepted by A&A

Published
2001
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22. HI spectra and column densities toward HVC and IVC probes

Author

Wakker, B. P., Kalberla, P. M. W., van Woerden, H., de Boer, K. S., and Putman, M. E.

Subjects
Astrophysics
Abstract

We show 21-cm line profiles in the direction of stars and extragalactic objects, lying projected on high- and intermediate-velocity clouds (HVCs and IVCs). About half of these are from new data obtained with the Effelsberg 100-m telescope, about a quarter are extracted from the Leiden-Dwingeloo Survey (LDS) and the remaining quarter were observed with other single-dish telescopes. HI column densities were determined for each HVC/IVC. Wakker (2001) (Paper I) uses these in combination with optical and ultraviolet high-resolution measurements to derive abundances. Here, an analysis is given of the difference and ratio of N(HI) as observed with a 9 arcmin versus a 35 arcmin beam. For HVCs and IVCs the ratio N(HI-9 arcmin)/N(HI-35 arcmin) lies in the range 0.2-2.5. For low-velocity gas this ratio ranges from 0.75 to 1.3 (the observed ratio is 0.85-1.4, but it appears that the correction for stray radiation is slightly off). The smaller range for the low-velocity gas may be caused by confusion in the line of sight, so that a low ratio in one component can be compensated by a high ratio in another -- for 11 low-velocity clouds fit by one component the distribution of ratios has a larger dispersion. Comparison with higher angular resolution data is possible for sixteen sightlines. Eight sightlines with HI data at 1 arcmin-2 arcmin resolution show a range of 0.75-1.25 for N(HI-2 arcmin)/N(HI-9 arcmin), while in eight other sightlines N(HI-Ly-alpha)/N(HI-9 arcmin) ranges from 0.74 to 0.98., Comment: To appear in the "Astrophysical Journal Supplement"; 45 pages; degraded figures (astro-ph restriction) - ask for good versions

Published
2001
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23. GAIA: Composition, Formation and Evolution of the Galaxy

Author

Perryman, M. A. C., de Boer, K. S., Gilmore, G., Høg, E., Lattanzi, M. G., Lindegren, L., Luri, X., Mignard, F., Pace, O., and de Zeeuw, P. T.

Subjects
Astrophysics
Abstract

The GAIA astrometric mission has recently been approved as one of the next two `cornerstones' of ESA's science programme, with a launch date target of not later than mid-2012. GAIA will provide positional and radial velocity measurements with the accuracies needed to produce a stereoscopic and kinematic census of about one billion stars throughout our Galaxy (and into the Local Group), amounting to about 1 per cent of the Galactic stellar population. GAIA's main scientific goal is to clarify the origin and history of our Galaxy, from a quantitative census of the stellar populations. It will advance questions such as when the stars in our Galaxy formed, when and how it was assembled, and its distribution of dark matter. The survey aims for completeness to V=20 mag, with accuracies of about 10 microarcsec at 15 mag. Combined with astrophysical information for each star, provided by on-board multi-colour photometry and (limited) spectroscopy, these data will have the precision necessary to quantify the early formation, and subsequent dynamical, chemical and star formation evolution of our Galaxy. Additional products include detection and orbital classification of tens of thousands of extra-Solar planetary systems, and a comprehensive survey of some 10^5-10^6 minor bodies in our Solar System, through galaxies in the nearby Universe, to some 500,000 distant quasars. It will provide a number of stringent new tests of general relativity and cosmology. The complete satellite system was evaluated as part of a detailed technology study, including a detailed payload design, corresponding accuracy assesments, and results from a prototype data reduction development., Comment: Accepted by A&A: 25 pages, 8 figures

Published
2001
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24. Stellar Associations and their Field East of LMC 4 in the Large Magellanic Cloud

Author

Gouliermis, D., de Boer, K. S., Keller, S. C., Kontizas, M., and Kontizas, E.

Subjects
Astrophysics
Abstract

We report about the stellar content and the luminosity and mass functions of three stellar associations and their field located on the north-east edge of the super-bubble LMC 4 in the Large Magellanic Cloud., Comment: To be appeared in the meeting Proceedings of ``Modes of Star Formation and the Origin of Field Populations'', Heidelberg, Germany, October 2000; to be published in the ASP Conference Series, edited by E. K. Grebel and W. Brandner

Published
2001

25. ORFEUS II Echelle spectra: Molecular hydrogen at high velocities toward HD 93521

Author

Gringel, W., Barnstedt, J., de Boer, K. S., Grewing, M., Kappelmann, N., and Richter, P.

Subjects
Astrophysics
Abstract

Absorption lines of interstellar molecular hydrogen in the far ultraviolet (FUV) have been observed in the spectrum of the O9.5 halo star HD 93521, located some 1500 pc from the Galactic plane. During the second flight of the ORFEUS-SPAS mission a spectrum with the Echelle spectrometer has been recorded with a total integration time of 1740 s. The resolution achieved was about 10.000 with a signal-to-noise ratio of up to 25. For the first time two components of molecular hydrogen have been observed in absorption at velocities of -12 km/s in the Galactic disk and at -62 km/s located presumably in the Galactic halo. The column densities derived from a standard curve of growth analysis were found to be N(H_2) = 10^17.0 cm^-2 for the disk component and N(H_2) = 10^14.6 cm^-2 respectively for the component located in the Galactic halo., Comment: 4 pages, 5 figures, accepted for publication in A&A Letters

Published
2000

26. Discovery of molecular hydrogen in a high-velocity cloud of the Galactic halo

Author

Richter, P., de Boer, K. S., Widmann, H., Kappelmann, N., Gringel, W., Grewing, M., and Barnstedt, J.

Subjects
Astrophysics
Abstract

We report the discovery of molecular hydrogen absorption in a Galactic high-velocity cloud (HVC) in the direction of the Large Magellanic Cloud. For the same HVC we derive an iron abundance which is half of the solar value. Thus, all evidence points to a Galactic origin for high-velocity cloud complex in front of the LMC., Comment: Published in Nature, this week; 14 pages, 3 figures

Published
1999
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27. ORFEUS II echelle spectra: deuterium and molecular hydrogen in the ISM towards BD +39 3226

Author

Bluhm, H., Marggraf, O., de Boer, K. S., Richter, P., and Heber, U.

Subjects
Astrophysics
Abstract

In ORFEUS II spectra of the sdO star BD +39 3226 interstellar hydrogen and deuterium is detected. From Ly alpha profile fitting and a curve of growth analysis of the Lyman series of H I and D I we derive the column densities N(H)=1.20(+0.28/-0.22)*10^20 cm^(-2) and N(D)=1.45(+0.50/-0.38)*10^(15) cm^(-2). From the analysis of metal absorption lines in ORFEUS and IUE spectra we obtain column densities for 11 elements. In addition, we examine absorption lines of H_2 for rotational excitation states up to J=7. We find an H_2 ortho-to-para ratio of 2.5, the fractional abundance of molecular hydrogen has a low value of log f=-4.08 for a total amount of N(H_2)=4.8(+2.0/-1.6)*10^15 cm^(-2). The column densities of the excitation states reveal a moderate Boltzmann excitation temperature of 130 K and an equivalent excitation temperature for the excited upper states due to UV pumping of <1800 K., Comment: 10 pages, 10 figures, accepted for publication in A&A main journal

Published
1999

28. ORFEUS II echelle spectra: On the H_2/CO ratio in the LMC towards LH 10

Author

Richter, P., de Boer, K. S., Bomans, D. J., Chin, Y. -N., Heithausen, A., and Koornneef, J.

Subjects
Astrophysics
Abstract

ORFEUS far UV echelle spectra have been used to investigate HI, H_2 and CO absorption lines along the line of sight towards LH 10:3120 in the LMC, extending the study presented by de Boer et al. (1998). While H_2 absorption is clearly visible, no CO absorption at LMC velocities is detected, but an upper limit of N(CO) < 3.3 10^13 cm^-2 for the CO column density is derived for the C-X band near 1088 A. The detected H_2 absorption features were used to determine a limit for the H_2/CO ratio of N(H_2)/N(CO) > 2.0 10^5 for the LMC gas along this individual line of sight. Generally, the fraction of gas in molecular form in the LMC is low compared to interstellar gas in the Milky Way with the same total gas quantity. We compare the absorption spectroscopy with SEST CO emission line measurements. It is found that most of the CO emission comes from gas behind LH 10:3120. We discuss our results in view of the possible scenario, in which the low dust content limits the amount of molecular hydrogen in the diffuse LMC gas., Comment: 7 pages, 3 figures; accepted for publication in A&A main journal

Published
1999

29. BUSCA: A Telescope Instrumentation for Simultaneous Imaging in 4 Optical Bands

Author

Reif, K., Bagschik, K., de Boer, K. S., Schmoll, J., Mueller, Ph., Poschmann, H, Klink, G, Kohley, R, Heber, U., and Mebold, U.

Subjects
Astrophysics
Abstract

The "Bonn University Simultaneous CAmera" (BUSCA) is a CCD camera system which allows simultaneous direct imaging of the same sky area in four colors. The optics are designed for an f/8 beam and four 4Kx4K CCDs with 15m pixels covering a field of view of 12 arcmin x 12 arcmin at a 2m class telescope. In September 1998 BUSCA has seen "First Light". The instrument is based on three dichroic beam splitters which separate optical wavelength bands such (at 430nm, 540nm, 730nm) that standard astronomical intermediate-band filter systems can be used. The dichroics are made of plane-parallel glass plates mounted at an angle of 45 degrees. Astigmatism in the transmitted beams (f/8) is completely cancelled by identical plane-parallel glass plates of suitable orientation. BUSCA offers new perspectives in astronomical multicolor photometry: i) The broadband spectral properties (e.g. color indices) of astronomical objects in the optical can be determined with high reliability even in non-photometric atmospheric conditions. ii) Precious observing time is used very efficiently. iii) With the large field of view, extended objects like globular and open star clusters or galaxies are covered in a single exposure. iv) Each exposure results in a complete data set., Comment: HTML document with 9 figures (.jpg's, .gif's). To appear in SPIE, Vol. 3649, gziped Postscript document (1.1MB) with full resolution diagrams at: ftp://www.astro.uni-bonn.de/pub/reif/busca/busca.ps.gz

Published
1999
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30. ORFEUS II echelle spectra: Absorption by H_2 in the LMC

Author

de Boer, K. S., Richter, P., Bomans, D. J., Heithausen, A., and Koornneef, J.

Subjects
Astrophysics
Abstract

We present the first detection of molecular hydrogen (H_2) UV absorption profiles on the line of sight to the LMC. The star LH 10:3120 in the LMC was measured with the ORFEUS telescope and the Tuebingen echelle spectrograph during the space shuttle mission of Nov./Dec. 1996. 16 absorption lines from the Lyman band are used to derive the column densities of H_2 for the lowest 5 rotational states in the LMC gas. For these states we find a total column density of N(H_2)=6.6 x 10^18$ cm^-2 on this individual line of sight. We obtain equivalent excitation temperatures of T < 50 K for the rotational ground state and T = 470 K for 0 < J < 6 by fitting the population densities of the rotational states to theoretical Boltzmann distributions. We conclude that UV pumping dominates the population of the higher rotational levels, as known from the H_2 gas in the Milky Way. (Research supported in part by the DARA), Comment: Astronomy & Astrophysics, Letter, in press

Published
1998

31. ORFEUS II echelle spectra: The scale height of interstellar O VI in the halo

Author

Widmann, H., de Boer, K. S., Richter, P., Kraemer, G., Appenzeller, I., Barnstedt, J., Goelz, M., Grewing, M., Gringel, W., Mandel, H., and Werner, K.

Subjects
Astrophysics
Abstract

FUV high resolution spectra of 18 stars, particularly chosen to observe the interstellar medium (ISM), were obtained during the second ORFEUS-SPAS free flight space shuttle mission in December 1996. Among these were 6 objects with a distance to the galactic plane larger than 1 kpc, one SMC and 4 LMC stars. This selction of targets is part of the ORFEUS program to explore the galactic halo. As the most important tracer of the hot gas we analyzed the stronger component of the important O VI doublet in all our ISM spectra. We found an average N(O VI) x sin |b| = 3.5 x 10^14 /cm^2 on the lines of sight to the 4 LMC stars. Assuming an exponential distribution of O VI we calculated a midplane density n(o) of 2.07 x 10^-8 /cm^3 and a scle height h(o) of 5.50 kpc. (Research supported in part by the DARA), Comment: Astronomy & Astrophysics, Letter, in press

Published
1998

32. ORFEUS II echelle spectra: Detection of H_2 absorption in SMC gas

Author

Richter, P., Widmann, H., de Boer, K. S., Appenzeller, I., Barnstedt, J., Goelz, M., Grewing, M., Gringel, W., Kappelmann, N., Kraemer, G., and Werner, K.

Subjects
Astrophysics
Abstract

We present a study of molecular hyrogen (H_2) in the SMC gas, based on space shuttle Far UV spectroscopy with ORFEUS and the Tuebingen echelle spectrograph, in the line of sight to the SMC star HD 5980. 17 absorption lines from the Lyman band have been analysed. Our line of sight crosses two clouds within the SMC. We detect a cool molecular component near +120 km/s, where the H_2 from the lowest 3 rotational states (J<3) is found. For this cloud we derive an excitation temperature of 70 K, probably the kinetic temerature of the gas. The cloud is located in the SMC foreground. Another SMC component is visible at +160 km/s. Here we find unblended H_2 absorption lines from levels 4 < J < 8. For this component we obtain an equivalent excitation temperature T > 2350 K and conclude that this cloud must be highly excited by strong UV radiation from its energetic environment. (Research supported in part by the DARA), Comment: Astronomy & Astrophysics, Letter, in press

Published
1998

33. NGS panel analysis in 24 ectopia lentis patients; a clinically relevant test with a high diagnostic yield

Author

Overwater, E., Floor, K., van Beek, D., de Boer, K., van Dijk, T., Hilhorst-Hofstee, Y., Hoogeboom, A.J.M., van Kaam, K.J., van de Kamp, J.M., Kempers, M., Krapels, I.P.C., Kroes, H.Y., Loeys, B., Salemink, S., Stumpel, C.T.R.M., Verhoeven, V.J.M., Wijnands-van den Berg, E., Cobben, J.M., van Tintelen, J.P., Weiss, M.M., Houweling, A.C., and Maugeri, A.

Published
2017
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34. Hot subdwarf stars - galactic orbits and distribution perpendicular to the plane

Author

de Boer, K. S., Sanchez, Y. Aguilar, Altmann, M., Geffert, M., Odenkirchen, M., Schmidt, J. H. K., and Colin, J.

Subjects
Astrophysics
Abstract

The spatial distribution and the population nature of subdwarf B type stars in the galaxy is investigated based on the kinematics of these stars. The orbits of 41 stars have been calculated using a galactic mass model. These are well behaved and 10 stars reach to |z| > 2 kpc. Many orbits are very eccentric, reaching in to just 2 kpc from the galactic centre, or veering out to beyond 20 kpc. None of the stars can be identified uniquely as classical Population II objects. The average eccentricity ECC of the orbits of our sample is 0.24, the average normalised z-extent NZE of the orbits is 0.16, and the asymmetric drift of our sample is -36 km s^-1. The distribution in z shows a relative minimum near z=0 pc and has maxima near z=300 pc. This reflects the smaller probability to find the stars IN the disk than away from the disk., Comment: 11 pages, LaTeX (epsf, l-aa), incl. 5 Postscript figures; Accepted by A&A (Main Journal)

Published
1997

35. CIV absorption from hot gas inside supergiant shell LMC4 observed with HST and IUE

Author

Bomans, D. J., de Boer, K. S., Koornneef, J., and Grebel, E. K.

Subjects
Astrophysics
Abstract

High resolution ultraviolet spectra with HST-GHRS of two stars in the direction of the supergiant shell LMC4 unambiguously show absorption by substantial quantities of CIV gas at velocities near the the systemic velocity of the LMC. In combination with the detection of diffuse X-rays from the LMC4 by ROSAT and other supporting data, this demonstrates that the interior of LMC4 is filled with tenuous hot gas. CIV interstellar absorption is seen over a large velocity range, having at least 2 components at about 280 and 320 km/s. The strong component at 280 km/s has a width of 40 km/s and a column density in the order of 3 times 10^13 cm^-2. The width of the absorption is best explained by bulk motions of CIV-containing gas clouds inside LMC4. These hot clouds or layers around cold clouds have to have a relatively high filling factor inside LMC4 to fit the observations. The characteristics of the CIV gas component at 320 km/s are such that they trace a blast wave from a recent supernova within the LMC4 cavity. Galactic CIV absorption is also present, as to be expected for these lines of sight., Comment: 13 pages, LaTeX (l-aa.sty, epsf.sty), 6 Postscript figures in one gzip tar archive, Astronomy and Astrophysics, in press

Published
1996

36. NGC 4526 gas, High Velocity Clouds, and Galactic Halo gas: the Interstellar Medium towards SN 1994D

Author

King, D. L., Vladilo, G., Lipman, K., de Boer, K. S., Centurion, M, Moritz, P., and Walton, N. A.

Subjects
Astrophysics
Abstract

We present spectroscopic observations of supernova 1994D in NGC 4526, an S0$_3$ galaxy in the Virgo cluster 15 Mpc distant. The datasets consist of the interstellar Ca\II\ and Na\I\ lines towards the supernova at high spectral resolution (FWHM 6 \kms), \halpha\ and [N\,II] observations at lower resolution (FWHM 33 \kms) of the nucleus of NGC 4526 and the supernova, obtained with the WHT at La Palma, and 21 cm spectra obtained with the 100 m Effelsberg Radiotelescope in the field of NGC 4526. The velocity of the gas in NGC 4526 determined from our \halpha\ spectra is +625 \kms\ at the centre and +880 \kms\ at the supernova position. Our value of the systemic velocity is higher than the previous value of +450 \kms. In our high resolution spectra we detect Ca\II\ and Na\I\ absorption at +714 \kms\ which is produced in interstellar gas in NGC 4526. To our knowledge this is the first detection of interstellar absorption originating in a galaxy of early morphological type. We detect multi-component Ca\II\ and Na\I\ absorption lines in the range from +204 to +254 \kms\ which originate in a complex of High Velocity Clouds (HVCs) located at a distance $\ll$ 1 Mpc, in the surroundings of the Milky Way. The gas appears to have near solar abundances, low dust content, and a diluted UV radiation field. At $-$29 \kms, we find weak Ca\II\ absorption and weak H\I\ emission. This component may originate in gas infalling onto the Galactic disk. Finally, close to rest velocity, we find both warm and cold gas located beyond 65 pc, probably associated with high latitude gas at the border of Loop I. The total reddening of the supernova, estimated using the standard Milky Way gas-to-dust ratio, is $E$(B$-$V) $\simeq$ 0.05., Comment: Submitted to A&A. 10 pages, including 4 figures; uuencoded compressed postscipt

Published
1994

38. Single- versus double-layer closure of the caesarean (uterine) scar in the prevention of gynaecological symptoms in relation to niche development – the 2Close study: a multicentre randomised controlled trial

Author

Stegwee, S. I., Jordans, I. P. M., van der Voet, L. F., Bongers, M. Y., de Groot, C. J. M., Lambalk, C. B., de Leeuw, R. A., Hehenkamp, W. J. K., van de Ven, P. M., Bosmans, J. E., Pajkrt, E., Bakkum, E. A., Radder, C. M., Hemelaar, M., van Baal, W. M., Visser, H., van Laar, J. O. E. H., van Vliet, H. A. A. M., Rijnders, R. J. P., Sueters, M., Janssen, C. A. H., Hermes, W., Feitsma, A. H., Kapiteijn, K., Scheepers, H. C. J., Langenveld, J., de Boer, K., Coppus, S. F. P. J., Schippers, D. H., Oei, A. L. M., Kaplan, M., Papatsonis, D. N. M., de Vleeschouwer, L. H. M., van Beek, E., Bekker, M. N., Huisjes, A. J. M., Meijer, W. J., Deurloo, K. L., Boormans, E. M. A., van Eijndhoven, H. W. F., and Huirne, J. A. F.

Published
2019
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39. Advancing enhanced wood manufacturing industries in Laos and Australia - Final Report

Author

Smith, H, Leggate, W, KANOWSKI, P, Boer, K, Ling, S, Midgley, S, Belleville, B, Faircloth, A, Robinson, R, Lattanvongkot, B, Boupha, L, Phonetip, K, Smith, H, Leggate, W, KANOWSKI, P, Boer, K, Ling, S, Midgley, S, Belleville, B, Faircloth, A, Robinson, R, Lattanvongkot, B, Boupha, L, and Phonetip, K

Abstract

ACIAR invested in Lao PDR's plantation and wood products sector in 2005, with the third project, FST/2016/151 – Advancing enhanced wood manufacturing industries in Laos and Australia (VALTIP3), building on the results. The VALTIP3 project conducted research on plantation-wood value chains, mapping plantations, exploring actors like traders and women, developing innovative wood products, and implementing processing technologies. It also assessed policy, regulatory, and strategic settings in these areas. The projects built local capacity to meet the demand of plantation-wood processing companies in Laos for NUoL FFS graduates and government stakeholders seeking VALTIP3 team members' knowledge for policy changes.

Published
2023

42. Extracellular vesicles released during normothermic machine perfusion are associated with human donor kidney characteristics

Author

Woud, W.W., Arykbaeva, A.S., Alwayn, I.P.J., Baan, C.C., Minnee, R.C., Hoogduijn, M.J., Boer, K., Internal Medicine, and Surgery

Subjects
Perfusion, Extracellular Vesicles, Transplantation, Cold Ischemia, Humans, Kidney
Abstract

Background: Extracellular vesicles (EVs) are tissue-specific particles released by cells containing valuable diagnostic information in the form of various biomolecules. The characterization of EVs released by kidney grafts during normothermic machine perfusion (NMP) may present a promising avenue to assess graft status before transplantation. Methods: We phenotyped and determined the concentrations of EVs in the perfusate of 8 discarded expanded-criteria donor human Kidneys during 6h of NMP. Perfusate samples were taken at 0/60/180/360min and examined with nanoparticle tracking analysis and imaging flow cytometry (IFCM). Using IFCM, EVs were identified by their expression of common EV markers CD9, CD63, and CD81 (tetraspanins) in combination with either platelet endothelial cell adhesion molecule (CD31), pan-leukocyte protein (CD45), or carboxyfluorescein succiminidyl ester (CFSE) fluorescence. Results: Nanoparticle tracking analysis measurements revealed the release of nanoparticles

Published
2022

44. Random walks on Arakelov class groups

Author

Boer, K. de, Ducas, L., Cramer, R., Wesolowski, B., Haas, F.A.J. de, Kirshanova, E., Luijk, R.M. van, Schoof, R., Stehlé, D., and Leiden University

Subjects
Ideal lattice, Cryptanalysis, Sampling ideals, Worst-case to average-case reduction, Power residue symbol, Quantum algorithm, Continuous hidden subgroup problem, Lattice-based cryptography
Abstract

The main topic of this PhD thesis is the Arakelov ray class group of a number field, an algebraic object that contains both the ideal class group structure and the unit group structure. The main result consists of the fact that certain specific random walks on the Arakelov ray class group result in a target point that is uniformly distributed on this group, under the assumption of an extended version of the Riemann Hypothesis. Almost all other results of this work are consequences of this fact.

Published
2022

48. Induction versus expectant monitoring for intrauterine growth restriction at term: randomised equivalence trial (DIGITAT)

Author

Boers, K E, Vijgen, S M C, Bijlenga, D, van der Post, J A M, Bekedam, D J, Kwee, A, van der Salm, P C M, van Pampus, M G, Spaanderman, M E A, de Boer, K, Duvekot, J J, Bremer, H A, Hasaart, T H M, Delemarre, F M C, Bloemenkamp, K W M, van Meir, C A, Willekes, C, Wijnen, E J, Rijken, M, le Cessie, S, Roumen, F J M E, Thornton, J, van Lith, J M M, Mol, B W J, and Scherjon, S A

Published
2011

49. The structure of the local hot bubble toward l = 165°, b = 0° using IUE and ROSAT data

Author

de Boer, K. S., Kerp, J., Araki, H., editor, Beig, R., editor, Ehlers, J., editor, Frisch, U., editor, Hepp, K., editor, Jaffe, R. L., editor, Kippenhahn, R., editor, Weidenmüller, H. A., editor, Wess, J., editor, Zittartz, J., editor, Beiglböck, W., editor, Lehr, Sabine, editor, Breitschwerdt, Dieter, editor, Freyberg, Michael, editor, and Trümper, Joachim, editor

Published
1998
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