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854 results on '"Vogt, S."'

1. Constraints on $f(R)$ gravity from tSZE-selected SPT galaxy clusters and weak lensing mass calibration from DES and HST

Author

Vogt, S. M. L., Bocquet, S., Davies, C. T., Mohr, J. J., Schmidt, F., Ruan, C. -Z., Li, B., Hernández-Aguayo, C., Grandis, S., Bleem, L. E., Klein, M., Schrabback, T., Aguena, M., Brooks, D., Burke, D. L., Campos, A., Rosell, A. Carnero, Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gatti, M., Giannini, G., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Lee, S., Lima, M., Marshall, J. L., Mena-Fernández, J., Miquel, R., Myles, J., Paterno, M., Pieres, A., Malagón, A. A. Plazas, Reichardt, C. L., Romer, A. K., Samuroff, S., Sarkar, A., Sanchez, E., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vikram, V., Weaverdyck, N., and Weller, J.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present constraints on the $f(R)$ gravity model using a sample of 1,005 galaxy clusters in the redshift range $0.25 - 1.78$ that have been selected through the thermal Sunyaev-Zel'dovich effect (tSZE) from South Pole Telescope (SPT) data and subjected to optical and near-infrared confirmation with the Multi-component Matched Filter (MCMF) algorithm. We employ weak gravitational lensing mass calibration from the Dark Energy Survey (DES) Year 3 data for 688 clusters at $z < 0.95$ and from the Hubble Space Telescope (HST) for 39 clusters with $0.6 < z < 1.7$. Our cluster sample is a powerful probe of $f(R)$ gravity, because this model predicts a scale-dependent enhancement in the growth of structure, which impacts the halo mass function (HMF) at cluster mass scales. To account for these modified gravity effects on the HMF, our analysis employs a semi-analytical approach calibrated with numerical simulations. Combining calibrated cluster counts with primary cosmic microwave background (CMB) temperature and polarization anisotropy measurements from the Planck2018 release, we derive robust constraints on the $f(R)$ parameter $f_{R0}$. Our results, $\log_{10} |f_{R0}| < -5.32$ at the 95 % credible level, are the tightest current constraints on $f(R)$ gravity from cosmological scales. This upper limit rules out $f(R)$-like deviations from general relativity that result in more than a $\sim$20 % enhancement of the cluster population on mass scales $M_\mathrm{200c}>3\times10^{14}M_\odot$., Comment: 21 pages, 6 figures, submitted to Phys. Rev. D

Published
2024

4. A multiple planet system of super-Earths orbiting the brightest red dwarf star GJ887

Author

Jeffers, S. V., Dreizler, S., Barnes, J. R., Haswell, C. A., Nelson, R. P., Rodríguez, E., Lopez-Gonzalez, M. J., Morales, N., Luque, R., Zechmeister, M., Vogt, S. S., Jenkins, J. S., Palle, E., Berdinas, Z. M., Coleman, G. A. L., Diaz, M. R., Ribas, I., Jones, H. R. A., Butler, R. P., Tinney, C. G., Bailey, J., Carter, B. D., O'Toole, S., Wittenmyer, R. A., Crane, J. D., Feng, F., Shectman, S. A., Teske, J., Reiners, A., Amado, P. J., and Anglada-Escude, G.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The nearest exoplanets to the Sun are our best possibilities for detailed characterization. We report the discovery of a compact multi-planet system of super-Earths orbiting the nearby red dwarf GJ 887, using radial velocity measurements. The planets have orbital periods of 9.3 and 21.8~days. Assuming an Earth-like albedo, the equilibrium temperature of the 21.8 day planet is approx 350 K; which is interior, but close to the inner edge, of the liquid-water habitable zone. We also detect a further unconfirmed signal with a period of 50 days which could correspond to a third super-Earth in a more temperate orbit. GJ 887 is an unusually magnetically quiet red dwarf with a photometric variability below 500 parts-per-million, making its planets amenable to phase-resolved photometric characterization., Comment: Published by Science

Published
2020
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5. Measuring the Orbital Parameters of Radial Velocity Systems in Mean Motion Resonance---a Case Study of HD 200964

Author

Rosenthal, M. M., Jacobson-Galan, W., Nelson, B., Murray-Clay, R. A., Burt, J. A., Holden, B., Chang, E., Kaaz, N., Yant, J., Butler, R. P., and Vogt, S. S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The presence of mean motion resonances (MMRs) complicates analysis and fitting of planetary systems observed through the radial velocity (RV) technique. MMR can allow planets to remain stable in regions of phase space where strong planet-planet interactions would otherwise destabilize the system. These stable orbits can occupy small phase space volumes, allowing MMRs to strongly constrain system parameters, but making searches for stable orbital parameters challenging. Furthermore, libration of the resonant angle and dynamical interaction between the planets introduces another, long period variation into the observed RV signal, complicating analysis of the periods of the planets in the system. We discuss this phenomenon using the example of HD 200964. By searching through parameter space and numerically integrating each proposed set of planetary parameters to test for long term stability, we find stable solutions in the 7:5 and 3:2 MMRs in addition to the originally identified 4:3 MMR. The 7:5 configuration provides the best match to the data, while the 3:2 configuration provides the most easily understood formation scenario. In reanalysis of the originally published shorter-baseline data, we find fits in both the 4:3 and 3:2 resonances, but not the 7:5. Because the time baseline of the data is less than the resonant libration period, the current best fit to the data may not reflect the actual resonant configuration. In the absence of a full sample of the longer libration period, we find that it is of paramount importance to incorporate long term stability when fitting for the system's orbital configuration., Comment: 26 pages, 23 figures

Published
2019
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6. Frequency of planets orbiting M dwarfs in the Solar neighbourhood

Author

Tuomi, M., Jones, H. R. A., Butler, R. P., Arriagada, P., Vogt, S. S., Burt, J., Laughlin, G., Holden, B., Shectman, S. A., Crane, J. D., Thompson, I., Keiser, S., Jenkins, J. S., Berdiñas, Z., Diaz, M., Kiraga, M., and Barnes, J. R.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The most abundant stars in the Galaxy, M dwarfs, are very commonly hosts to diverse systems of low-mass planets. Their abundancy implies that the general occurrence rate of planets is dominated by their occurrence rate around such M dwarfs. In this article, we combine the M dwarf surveys conducted with the HIRES/Keck, PFS/Magellan, HARPS/ESO, and UVES/VLT instruments supported with data from several other instruments. We analyse the radial velocities of an approximately volume- and brightness-limited sample of 426 nearby M dwarfs in order to search for Doppler signals of cadidate planets. In addition, we analyse spectroscopic activity indicators and ASAS photometry to rule out radial velocity signals corresponding to stellar activity as Doppler signals of planets. We calculate estimates for the occurrence rate of planets around the sample stars and study the properties of this occurrence rate as a function of stellar properties. Our analyses reveal a total of 118 candidate planets orbiting nearby M dwarfs. Based on our results accounting for selection effects and sample detection threshold, we estimate that M dwarfs have on average at least 2.39$^{+4.58}_{-1.36}$ planets per star orbiting them. Accounting for the different sensitivities of radial velocity surveys and Kepler transit photometry implies that there are at least 3.0 planets per star orbiting M dwarfs. We also present evidence for a population of cool mini-Neptunes and Neptunes with indications that they are found an order of magnitude more frequently orbiting the least massive M dwarfs in our sample., Comment: Manuscript submitted to AAS journals. 338 pages, including 66 pages of tables summarising data properties, target properties, and selected parameter estimates

Published
2019

7. Stellar activity analysis of Barnard's Star: Very slow rotation and evidence for long-term activity cycle

Author

Toledo-Padrón, B., Hernández, J. I. González, Rodríguez-López, C., Mascareño, A. Suárez, Rebolo, R., Butler, R. P., Ribas, I., Anglada-Escudé, G., Johnson, E. N., Reiners, A., Caballero, J. A., Quirrenbach, A., Amado, P. J., Béjar, V. J. S., Morales, J. C., Perger, M., Jeffers, S. V., Vogt, S., Teske, J., Shectman, S., Crane, J., Díaz, M., Arriagada, P., Holden, B., Burt, J., Rodríguez, E., Herrero, E., Murgas, F., Pallé, E., Morales, N., López-González, M. J., Alonso, E. Díez, Tuomi, M., Kiraga, M., Engle, S. G., Guinan, E. F., Strachan, J. B. P., Aceituno, F. J., Aceituno, J., Casanova, V. M., Martín-Ruiz, S., Montes, D., Ortiz, J. L., Sota, A., Briol, J., Barbieri, L., Cervini, I., Deldem, M., Dubois, F., Hambsch, F. -J., Harris, B., Kotnik, C., Logie, L., Lopez, J., McNeely, M., Ogmen, Y., Pérez, L., Rau, S., Rodríguez, D., Urquijo, F. S., and Vanaverbeke, S.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The search for Earth-like planets around late-type stars using ultra-stable spectrographs requires a very precise characterization of the stellar activity and the magnetic cycle of the star, since these phenomena induce radial velocity (RV) signals that can be misinterpreted as planetary signals. Among the nearby stars, we have selected Barnard's Star (Gl 699) to carry out a characterization of these phenomena using a set of spectroscopic data that covers about 14.5 years and comes from seven different spectrographs: HARPS, HARPS-N, CARMENES, HIRES, UVES, APF, and PFS; and a set of photometric data that covers about 15.1 years and comes from four different photometric sources: ASAS, FCAPT-RCT, AAVSO, and SNO. We have measured different chromospheric activity indicators (H$\alpha$, Ca~{\sc II}~HK and Na I D), as well as the FWHM of the cross-correlation function computed for a sub-set of the spectroscopic data. The analysis of Generalized Lomb-Scargle periodograms of the time series of different activity indicators reveals that the rotation period of the star is 145 $\pm$ 15 days, consistent with the expected rotation period according to the low activity level of the star and previous claims. The upper limit of the predicted activity-induced RV signal corresponding to this rotation period is about 1 m/s. We also find evidence of a long-term cycle of 10 $\pm$ 2 years that is consistent with previous estimates of magnetic cycles from photometric time series in other M stars of similar activity levels. The available photometric data of the star also support the detection of both the long-term and the rotation signals., Comment: 16 pages, 20 figures

Published
2018
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9. A candidate super-Earth planet orbiting near the snow line of Barnard's star

Author

Ribas, I., Tuomi, M., Reiners, A., Butler, R. P., Morales, J. C., Perger, M., Dreizler, S., Rodríguez-López, C., Hernández, J. I. González, Rosich, A., Feng, F., Trifonov, T., Vogt, S. S., Caballero, J. A., Hatzes, A., Herrero, E., Jeffers, S. V., Lafarga, M., Murgas, F., Nelson, R. P., Rodríguez, E., Strachan, J. B. P., Tal-Or, L., Teske, J., Toledo-Padrón, B., Zechmeister, M., Quirrenbach, A., Amado, P. J., Azzaro, M., Béjar, V. J. S., Barnes, J. R., Berdiñas, Z. M., Burt, J., Coleman, G., Cortés-Contreras, M., Crane, J., Engle, S. G., Guinan, E. F., Haswell, C. A., Henning, Th., Holden, B., Jenkins, J., Jones, H. R. A., Kaminski, A., Kiraga, M., Kürster, M., Lee, M. H., López-González, M. J., Montes, D., Morin, J., Ofir, A., Pallé, E., Rebolo, R., Reffert, S., Schweitzer, A., Seifert, W., Shectman, S. A., Staab, D., Street, R. A., Mascareño, A. Suárez, Tsapras, Y., Wang, S. X., and Anglada-Escudé, G.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

At a distance of 1.8 parsecs, Barnard's star (Gl 699) is a red dwarf with the largest apparent motion of any known stellar object. It is the closest single star to the Sun, second only to the alpha Centauri triple stellar system. Barnard's star is also among the least magnetically active red dwarfs known and has an estimated age older than our Solar System. Its properties have made it a prime target for planet searches employing techniques such as radial velocity, astrometry, and direct imaging, all with different sensitivity limits but ultimately leading to disproved or null results. Here we report that the combination of numerous measurements from high-precision radial velocity instruments reveals the presence of a low-amplitude but significant periodic signal at 233 days. Independent photometric and spectroscopic monitoring, as well as the analysis of instrumental systematic effects, show that this signal is best explained as arising from a planetary companion. The candidate planet around Barnard's star is a cold super-Earth with a minimum mass of 3.2 Earth masses orbiting near its snow-line. The combination of all radial velocity datasets spanning 20 years additionally reveals a long-term modulation that could arise from a magnetic activity cycle or from a more distant planetary object. Because of its proximity to the Sun, the proposed planet has a maximum angular separation of 220 milli-arcseconds from Barnard's star, making it an excellent target for complementary direct imaging and astrometric observations., Comment: 38 pages, 7 figures, 4 tables, author's version of published paper in Nature journal

Published
2018
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10. Gaia Data Release 2: Observational Hertzsprung-Russell diagrams

Author

Gaia Collaboration, Babusiaux, C., van Leeuwen, F., Barstow, M. A., Jordi, C., Vallenari, A., Bossini, D., Bressan, A., Cantat-Gaudin, T., van Leeuwen, M., Brown, A. G. A., Prusti, T., de Bruijne, J. H. J., Bailer-Jones, C. A. L., Biermann, M., Evans, D. W., Eyer, L., Jansen, F., Klioner, S. A., Lammers, U., Lindegren, L., Luri, X., Mignard, F., Panem, C., Pourbaix, D., Randich, S., Sartoretti, P., Siddiqui, H. I., Soubiran, C., Walton, N. A., Arenou, F., Bastian, U., Cropper, M., Drimmel, R., Katz, D., Lattanzi, M. G., Bakker, J., Cacciari, C., Castañeda, J., Chaoul, L., Cheek, N., DeAngeli, F., Fabricius, C., Guerra, R., Holl, B., Masana, E., Messineo, R., Mowlavi, N., Nienartowicz, K., Panuzzo, P., Portell, J., Riello, M., Seabroke, G. M., Tanga, P., Thévenin, F., Gracia-Abril, G., Comoretto, G., Garcia-Reinaldos, M., Teyssier, D., Altmann, M., Andrae, R., Audard, M., Bellas-Velidis, I., Benson, K., Berthier, J., Blomme, R., Burgess, P., Busso, G., Carry, B., Cellino, A., Clementini, G., Clotet, M., Creevey, O., Davidson, M., DeRidder, J., Delchambre, L., Dell'Oro, A., Ducourant, C., Fernández-Hernández, J., Fouesneau, M., Frémat, Y., Galluccio, L., García-Torres, M., González-Núñez, J., González-Vidal, J. J., Gosset, E., Guy, L. P., Halbwachs, J. -L., Hambly, N. C., Harrison, D. L., Hernández, J., Hestroffer, D., Hodgkin, S. T., Hutton, A., Jasniewicz, G., Jean-Antoine-Piccolo, A., Jordan, S., Korn, A. J., Krone-Martins, A., Lanzafame, A. C., Lebzelter, T., Löffler, W., Manteiga, M., Marrese, P. M., Martín-Fleitas, J. M., Moitinho, A., Mora, A., Muinonen, K., Osinde, J., Pancino, E., Pauwels, T., Petit, J. -M., Recio-Blanco, A., Richards, P. J., Rimoldini, L., Robin, A. C., Sarro, L. M., Siopis, C., Smith, M., Sozzetti, A., Süveges, M., Torra, J., vanReeven, W., Abbas, U., Aramburu, A. Abreu, Accart, S., Aerts, C., Altavilla, G., Álvarez, M. A., Alvarez, R., Alves, J., Anderson, R. I., Andrei, A. H., Varela, E. Anglada, Antiche, E., Antoja, T., Arcay, B., Astraatmadja, T. L., Bach, N., Baker, S. G., Balaguer-Núñez, L., Balm, P., Barache, C., Barata, C., Barbato, D., Barblan, F., Barklem, P. S., Barrado, D., Barros, M., Muñoz, S. Bartholomé, Bassilana, J. -L., Becciani, U., Bellazzini, M., Berihuete, A., Bertone, S., Bianchi, L., Bienaymé, O., Blanco-Cuaresma, S., Boch, T., Boeche, C., Bombrun, A., Borrachero, R., Bouquillon, S., Bourda, G., Bragaglia, A., Bramante, L., Breddels, M. A., Brouillet, N., Brüsemeister, T., Brugaletta, E., Bucciarelli, B., Burlacu, A., Busonero, D., Butkevich, A. G., Buzzi, R., Caffau, E., Cancelliere, R., Cannizzaro, G., Carballo, R., Carlucci, T., Carrasco, J. M., Casamiquela, L., Castellani, M., Castro-Ginard, A., Charlot, P., Chemin, L., Chiavassa, A., Cocozza, G., Costigan, G., Cowell, S., Crifo, F., Crosta, M., Crowley, C., Cuypers, J., Dafonte, C., Damerdji, Y., Dapergolas, A., David, P., David, M., deLaverny, P., DeLuise, F., DeMarch, R., deMartino, D., deSouza, R., deTorres, A., Debosscher, J., delPozo, E., Delbo, M., Delgado, A., Delgado, H. E., Diakite, S., Diener, C., Distefano, E., Dolding, C., Drazinos, P., Durán, J., Edvardsson, B., Enke, H., Eriksson, K., Esquej, P., Bontemps, G. Eynard, Fabre, C., Fabrizio, M., Faigler, S., Falcão, A. J., Casas, M. Farràs, Federici, L., Fedorets, G., Fernique, P., Figueras, F., Filippi, F., Findeisen, K., Fonti, A., Fraile, E., Fraser, M., Frézouls, B., Gai, M., Galleti, S., Garabato, D., García-Sedano, F., Garofalo, A., Garralda, N., Gavel, A., Gavras, P., Gerssen, J., Geyer, R., Giacobbe, P., Gilmore, G., Girona, S., Giuffrida, G., Glass, F., Gomes, M., Granvik, M., Gueguen, A., Guerrier, A., Guiraud, J., Gutiérrez-Sánchez, R., Haigron, R., Hatzidimitriou, D., Hauser, M., Haywood, M., Heiter, U., Helmi, A., Heu, J., Hilger, T., Hobbs, D., Hofmann, W., Holland, G., Huckle, H. E., Hypki, A., Icardi, V., Janßen, K., JevardatdeFombelle, G., Jonker, P. G., Juhász, Á. L., Julbe, F., Karampelas, A., Kewley, A., Klar, J., Kochoska, A., Kohley, R., Kolenberg, K., Kontizas, M., Kontizas, E., Koposov, S. E., Kordopatis, G., Kostrzewa-Rutkowska, Z., Koubsky, P., Lambert, S., Lanza, A. F., Lasne, Y., Lavigne, J. -B., LeFustec, Y., LePoncin-Lafitte, C., Lebreton, Y., Leccia, S., Leclerc, N., Lecoeur-Taibi, I., Lenhardt, H., Leroux, F., Liao, S., Licata, E., Lindstrøm, H. E. P., Lister, T. A., Livanou, E., Lobel, A., López, M., Managau, S., Mann, R. G., Mantelet, G., Marchal, O., Marchant, J. M., Marconi, M., Marinoni, S., Marschalkó, G., Marshall, D. J., Martino, M., Marton, G., Mary, N., Massari, D., Matijevič, G., Mazeh, T., McMillan, P. J., Messina, S., Michalik, D., Millar, N. R., Molina, D., Molinaro, R., Molnár, L., Montegriffo, P., Mor, R., Morbidelli, R., Morel, T., Morris, D., Mulone, A. F., Muraveva, T., Musella, I., Nelemans, G., Nicastro, L., Noval, L., O'Mullane, W., Ordénovic, C., Ordóñez-Blanco, D., Osborne, P., Pagani, C., Pagano, I., Pailler, F., Palacin, H., Palaversa, L., Panahi, A., Pawlak, M., Piersimoni, A. M., Pineau, F. -X., Plachy, E., Plum, G., Poggio, E., Poujoulet, E., Prša, A., Pulone, L., Racero, E., Ragaini, S., Rambaux, N., Ramos-Lerate, M., Regibo, S., Reylé, C., Riclet, F., Ripepi, V., Riva, A., Rivard, A., Rixon, G., Roegiers, T., Roelens, M., Romero-Gómez, M., Rowell, N., Royer, F., Ruiz-Dern, L., Sadowski, G., Sellés, T. Sagristà, Sahlmann, J., Salgado, J., Salguero, E., Sanna, N., Santana-Ros, T., Sarasso, M., Savietto, H., Schultheis, M., Sciacca, E., Segol, M., Segovia, J. C., Ségransan, D., Shih, I-C., Siltala, L., Silva, A. F., Smart, R. L., Smith, K. W., Solano, E., Solitro, F., Sordo, R., SoriaNieto, S., Souchay, J., Spagna, A., Spoto, F., Stampa, U., Steele, I. A., Steidelmüller, H., Stephenson, C. A., Stoev, H., Suess, F. F., Surdej, J., Szabados, L., Szegedi-Elek, E., Tapiador, D., Taris, F., Tauran, G., Taylor, M. B., Teixeira, R., Terrett, D., Teyssandier, P., Thuillot, W., Titarenko, A., TorraClotet, F., Turon, C., Ulla, A., Utrilla, E., Uzzi, S., Vaillant, M., Valentini, G., Valette, V., vanElteren, A., Van Hemelryck, E., Vaschetto, M., Vecchiato, A., Veljanoski, J., Viala, Y., Vicente, D., Vogt, S., vonEssen, C., Voss, H., Votruba, V., Voutsinas, S., Walmsley, G., Weiler, M., Wertz, O., Wevers, T., Wyrzykowski, Ł., Yoldas, A., Žerjal, M., Ziaeepour, H., Zorec, J., Zschocke, S., Zucker, S., Zurbach, C., and Zwitter, T.

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

We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples. We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects. The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics. Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies., Comment: Published in the A&A Gaia Data Release 2 special issue. Tables 2 and A.4 corrected. Tables available at http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/616/A10

Published
2018
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12. Operational experience of the Belle II pixel detector

Author

Wang, B., Abudinen, F., Ackermann, K., Ahlburg, P., Albalawi, M., Alonso, O., Andricek, L., Ayad, R., Babu, V., Baur, A., Bernlochner, F., Bilka, T., Bolz, A., Bozek, A., Camien, C., Caldwell, A., Cao, L., Chekelian, V., Dieguez, A., Dingfelder, J., Doležal, Z., Fras, M., Frey, A., Gabriel, M., Gadow, K., Gessler, T., Giakoustidis, G., Gioi, L., Greenwald, D., Heck, M., Hensel, M., Hoek, M., Huber, S., Kandra, J., Kapusta, P., Karl, R., Kehl, J., Kiesling, C., Kisielewski, B., Kittlinger, D., Klose, D., Kodyš, P., Koffmane, C., Konorov, I., Krivokuca, S., Kuhr, T., Kurz, S., Kvasnička, P., Lange, J.S., Lautenbach, K., Leis, U., Leitl, P., Levit, D., Liemann, G., Liu, Q., Liu, Z., Lück, T., Mariñas, C., Mccarney, S., Moser, H.G., Moya, D., Müller, F.J., Müller, F., Niebuhr, C., Ninkovic, J., Paschen, B., Paul, S., Peric, I., Pitzl, D., Rabusov, A., Reif, M., Reiter, S.P., Richter, R., Ritter, M., Ritzert, M., Sanchez, J.G., Scavino, B., Schaller, G., Schmitz, J., Schnecke, M., Schopper, F., Schreeck, H., Schwenker, B., Schwickardi, M., Sedlmeyer, R., Sfienti, C., Simon, F., Skambraks, S., Skorupa, J., Soloviev, Y., Spruck, B., Stefkova, S., Stever, R., Tafelmayer, E., Takahashi, M., Vila, I., Virto, A.L., Vogt, S., Wang, C., Wieduwilt, P., Windel, H., Ye, H., Zhao, J., and Žlebčík, R.

Published
2022
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13. Three planets around HD 27894. A close-in pair with a 2:1 period ratio and an eccentric Jovian planet at 5.4 AU

Author

Trifonov, T., Kürster, M., Zechmeister, M., Zakhozhay, O. V., Reffert, S., Lee, M. H., Rodler, F., Vogt, S. S., and Brems, S. S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Aims. Our new program with HARPS aims to detect mean motion resonant planetary systems around stars which were previously reported to have a single bona fide planet, often based only on sparse radial velocity data. Methods. Archival and new HARPS radial velocities for the K2V star HD 27894 were combined and fitted with a three-planet self-consistent dynamical model. The best-fit orbit was tested for long-term stability. Results. We find clear evidence that HD 27894 is hosting at least three massive planets. In addition to the already known Jovian planet with a period $P_{\rm b}$ $\approx$ 18 days we discover a Saturn-mass planet with $P_{\rm c}$ $\approx$ 36 days, likely in a 2:1 mean motion resonance with the first planet, and a cold massive planet ($\approx$ 5.3 $M_{\mathrm{Jup}}$) with a period $P_{\rm d}$ $\approx$ 5170 days on a moderately eccentric orbit ($e_{\rm d}$ = 0.39). Conclusions. HD 27894 is hosting a massive, eccentric giant planet orbiting around a tightly packed inner pair of massive planets likely involved in an asymmetric 2:1 mean motion resonance. HD 27894 may be an important milestone for probing planetary formation and evolution scenarios., Comment: 4 pages, 2 tables, 3 figures. Accepted for publication in A&A Letters to the Editor

Published
2017
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14. 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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15. 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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16. A Goldilocks principle for modeling radial velocity noise

Author

Feng, Fabo, Tuomi, M., Jones, H. R. A., Butler, R. P., and Vogt, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Statistics - Applications
Abstract

The doppler measurements of stars are diluted and distorted by stellar activity noise. Different choices of noise models and statistical methods have led to much controversy in the confirmation of exoplanet candidates obtained through analysing radial velocity data. To quantify the limitation of various models and methods, we compare different noise models and signal detection criteria for various simulated and real data sets in the Bayesian framework. According to our analyses, the white noise model tend to interpret noise as signal, leading to false positives. On the other hand, the red noise models are likely to interprete signal as noise, resulting in false negatives. We find that the Bayesian information criterion combined with a Bayes factor threshold of 150 can efficiently rule out false positives and confirm true detections. We further propose a Goldilocks principle aimed at modeling radial velocity noise to avoid too many false positives and too many false negatives. We propose that the noise model with RHK-dependent jitter is used in combination with the moving average model to detect planetary signals for M dwarfs. Our work may also shed light on the noise modeling for hotter stars, and provide a valid approach for finding similar principles in other disciplines., Comment: 14 pages, 6 figures, accepted for publication in MNRAS

Published
2016
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17. Time-Varying Sodium Absorption in the Type Ia Supernova 2013gh

Author

Ferretti, R., Amanullah, R., Goobar, A., Johansson, J., Vreeswijk, P. M., Butler, R. P., Cao, Y., Cenko, S. B., Doran, G., Filippenko, A. V., Freeland, E., Hosseinzadeh, G., Howell, D. A., Lundqvist, P., Mattila, S., Nordin, J., Nugent, P. E., Petrushevska, T., Valenti, S., Vogt, S., and Wozniak, P.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Temporal variability of narrow absorption lines in high-resolution spectra of Type Ia supernovae (SNe Ia) is studied to search for circumstellar matter. Time series which resolve the profiles of absorption lines such as Na I D or Ca II H&K are expected to reveal variations due to photoionisation and subsequent recombination of the gases. The presence, composition, and geometry of circumstellar matter may hint at the elusive progenitor system of SNe Ia and could also affect the observed reddening law. To date, there are few known cases of time-varying Na I D absorption in SNe Ia, all of which occurred during relatively late phases of the supernova evolution. Photoionisation, however, is predicted to occur during the early phases of SNe Ia, when the supernova peaks in the ultraviolet. We therefore attempt to observe early-time absorption-line variations by obtaining high-resolution spectra of SNe before maximum light. We have obtained photometry and high-resolution spectroscopy of SNe Ia 2013gh and iPTF 13dge, to search for absorption- line variations. Furthermore, we study interstellar absorption features in relation to the observed photometric colours of the SNe. Results. Both SNe display deep Na I D and Ca II H&K absorption features. Furthermore, small but significant variations are detected in a feature of the Na I D profile of SN 2013gh. The variations are consistent with either geometric effects of rapidly moving or patchy gas clouds or photoionisation of Na I gas at R \approx 1019 cm from the explosion. Our analysis indicates that it is necessary to focus on early phases to detect photoionisation effects of gases in the circumstellar medium of SNe Ia. Different absorbers such as Na I and Ca II can be used to probe for matter at different distances from the SNe., Comment: accepted for publication in A&A

Published
2016
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18. Development of a strontium optical lattice clock for the SOC mission on the ISS

Author

Origlia, S., Schiller, S., Pramod, M. S., Smith, L., Singh, Y., He, W., Viswam, S., Świerad, D., Hughes, J., Bongs, K., Sterr, U., Lisdat, Ch., Vogt, S., Bize, S., Lodewyck, J., Targat, R. Le, Holleville, D., Venon, B., Gill, P., Barwood, G., Hill, I. R., Ovchinnikov, Y., Kulosa, A., Ertmer, W., Rasel, E. -M., Stuhler, J., Kaenders, W., and contributors, the SOC2 consortium

Subjects
Physics - Atomic Physics, Physics - Optics, Quantum Physics
Abstract

The ESA mission "Space Optical Clock" project aims at operating an optical lattice clock on the ISS in approximately 2023. The scientific goals of the mission are to perform tests of fundamental physics, to enable space-assisted relativistic geodesy and to intercompare optical clocks on the ground using microwave and optical links. The performance goal of the space clock is less than $1 \times 10^{-17}$ uncertainty and $1 \times 10^{-15} {\tau}^{-1/2}$ instability. Within an EU-FP7-funded project, a strontium optical lattice clock demonstrator has been developed. Goal performances are instability below $1 \times 10^{-15} {\tau}^{-1/2}$ and fractional inaccuracy $5 \times 10^{-17}$. For the design of the clock, techniques and approaches suitable for later space application are used, such as modular design, diode lasers, low power consumption subunits, and compact dimensions. The Sr clock apparatus is fully operational, and the clock transition in $^{88}$Sr was observed with linewidth as small as 9 Hz., Comment: 12 pages, 8 figures, SPIE Photonics Europe 2016

Published
2016
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19. Commissioning and performance of the Belle II pixel detector

Author

Ye, H., Abudinen, F., Ackermann, K., Ahlburg, P., Albalawi, M., Alonso, O., Andricek, L., Ayad, R., Babu, V., Bilka, T., Boronat, M., Bozek, A., Camien, C., Caldwell, A., Chekelian, V., Deschamps, B., Dieguez, A., Dingfelder, J., Doležal, Z., Esperante, D., Fras, M., Frey, A., Fuster, J., Gabriel, M., Gadow, K., Gebauer, U., Gessler, T., Giakoustidis, G., Gioi, L., Gomis, P., Greenwald, D., Heck, M., Hemperek, T., Hensel, M., Hoek, M., Huber, S., Kandra, J., Kapusta, P., Kiesling, C., Kisielewski, B., Kittlinger, D., Klose, D., Kodyš, P., Koffmane, C., Konorov, I., Krivokuca, S., Krüger, H., Kuhr, T., Kvasnička, P., Lacasta, C., Lange, J.S., Lautenbach, K., Leis, U., Leitl, P., Levit, D., Liemann, G., Liu, Q., Liu, Z., Lück, T., Lütticke, F., Macharski, L., Mariñas, C., Mccarney, S., Moser, H.G., Moya, D., Mueller, F.J., Müller, F., Niebuhr, C., Ninkovic, J., Paschen, B., Paul, S., Peric, I., Poblotzki, F., Rabusov, A., Reiter, S.P., Richter, R., Ritter, M., Ritzert, M., Sanchez, J.G., Scavino, B., Schaller, G., Schnecke, M., Schopper, F., Schreeck, H., Schwenker, B., Sedlmeyer, R., Sfienti, C., Simon, F., Skambraks, S., Soloviev, Y., Spruck, B., Stefkova, S., Stever, R., Stolzenberg, U., Tafelmayer, E., Takahashi, M., Vila, I., Virto, A.L., Vogt, S., Vos, M., Wang, C., Wermes, N., Wessel, C., Wieduwilt, P., Windel, H., and Zhao, J.

Published
2021
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20. Development of a strontium optical lattice clock for the SOC mission on the ISS

Author

Bongs, K., Singh, Y., Smith, L., He, W., Kock, O., Swierad, D., Hughes, J., Schiller, S., Alighanbari, S., Origlia, S., Vogt, S., Sterr, U., Lisdat, Ch., Targat, R. Le, Lodewyck, J., Holleville, D., Venon, B., Bize, S., Barwood, G. P., Gill, P., Hill, I. R., Ovchinnikov, Y. B., Poli, N., Tino, G. M., Stuhler, J., Kaenders, W., and team, the SOC2

Subjects
Physics - Atomic Physics, Quantum Physics
Abstract

Ultra-precise optical clocks in space will allow new studies in fundamental physics and astronomy. Within an European Space Agency (ESA) program, the Space Optical Clocks (SOC) project aims to install and to operate an optical lattice clock on the International Space Station (ISS) towards the end of this decade. It would be a natural follow-on to the ACES mission, improving its performance by at least one order of magnitude. The payload is planned to include an optical lattice clock, as well as a frequency comb, a microwave link, and an optical link for comparisons of the ISS clock with ground clocks located in several countries and continents. Within the EU-FP7-SPACE-2010-1 project no. 263500, during the years 2011-2015 a compact, modular and robust strontium lattice optical clock demonstrator has been developed. Goal performance is a fractional frequency instability below 1x10^{-15}, tau^{-1/2} and a fractional inaccuracy below 5x10^{-17}. Here we describe the current status of the apparatus' development, including the laser subsystems. Robust preparation of cold {88}^Sr atoms in a second stage magneto-optical trap (MOT) is achieved., Comment: 27 Pages, 15 figures, Comptes Rendus Physique 2015

Published
2015
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22. Belle II pixel detector: Performance of final DEPFET modules

Author

Paschen, B., Abudinen, F., Ackermann, K., Ahlburg, P., Albalawi, M., Alonso, O., Andricek, L., Ayad, R., Babu, V., Bai, Y., Bilka, T., Blanco, R., Boronat, M., Bozek, A., Camien, C., Caldwell, A., Chekelian, V., Deschamps, B., Dieguez, A., Dingfelder, J., Doležal, Z., Esperante, D., Fras, M., Frey, A., Fuster, J., Gabriel, M., Gadow, K., Gebauer, U., Germic, L., Gessler, T., Getzkow, D., Gioi, L., Gomis, P., Heck, M., Hemperek, T., Hensel, M., Hoek, M., Huber, S., Kandra, J., Kapusta, P., Kiesling, C., Kisielewski, B., Kittlinger, D., Klose, D., Kodyš, P., Koffmane, C., Konorov, I., Krivokuca, S., Krüger, H., Kuhr, T., Kühn, W., Kvasnička, P., Lacasta, C., Lange, J.S., Lautenbach, K., Leis, U., Leitl, P., Levit, D., Liemann, G., Liu, Z., Lütticke, F., Macharski, L., Mariñas, C., Mccarney, S., Moser, H.G., Moya, D., Müller, F.J., Müller, F., Münchow, D., Niebuhr, C., Ninkovic, J., Packheiser, U., Paul, S., Peric, I., Poblotzki, F., Rabusov, A., Reiter, S.P., Richter, R., Ritter, M., Ritzert, M., Rummel, S., Sanchez, J.G., Scavino, B., Schaller, G., Schnecke, M., Schopper, F., Schreeck, H., Schwenker, B., Sedlmeyer, R., Sfienti, C., Simon, F., Skambraks, S., Soloviev, Y., Spruck, B., Stever, R., Stolzenberg, U., Takahashi, M., Tafelmayer, E., Vila, I., Virto, A.L., Vogt, S., Vos, M., Wang, C., Wermes, N., Wessel, C., Wieduwilt, P., Windel, H., Ye, H., and Zhao, J.

Published
2020
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23. Time-varying sodium absorption in the Type Ia supernova 2013gh⋆

Author

Ferretti, R, Amanullah, R, Goobar, A, Johansson, J, Vreeswijk, PM, Butler, RP, Cao, Y, Cenko, SB, Doran, G, Filippenko, AV, Freeland, E, Hosseinzadeh, G, Howell, DA, Lundqvist, P, Mattila, S, Nordin, J, Nugent, PE, Petrushevska, T, Valenti, S, Vogt, S, and Wozniak, P

Subjects
Astronomical Sciences, Physical Sciences, supernovae: general, supernovae: individual: SN 2013gh, dust, extinction, circumstellar matter, supernovae: individual: iPTF 13dge, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

Context. Temporal variability of narrow absorption lines in high-resolution spectra of Type Ia supernovae (SNe Ia) is studied to search for circumstellar matter. Time series which resolve the profiles of absorption lines such as Na I D or Ca II H&K are expected to reveal variations due to photoionisation and subsequent recombination of the gases. The presence, composition, and geometry of circumstellar matter may hint at the elusive progenitor system of SNe Ia and could also affect the observed reddening law. Aims. To date, there are few known cases of time-varying Na I D absorption in SNe Ia, all of which occurred during relatively late phases of the supernova (SN) evolution. Photoionisation, however, is predicted to occur during the early phases of SNe Ia, when the supernovae peak in the ultraviolet. We attempt, therefore, to observe early-time absorption-line variations by obtaining high-resolution spectra of SNe before maximum light. Methods. We have obtained photometry and high-resolution spectroscopy of SNe Ia 2013gh and iPTF 13dge, to search for absorption-line variations. Furthermore, we study interstellar absorption features in relation to the observed photometric colours of the SNe. Results. Both SNe display deep Na I D and Ca II H&K absorption features. Furthermore, small but significant variations are detected in a feature of the Na I D profile of SN 2013gh. The variations are consistent with either geometric effects of rapidly moving or patchy gas clouds or photoionisation of Na I gas at R ≈ 1019 cm from the explosion. Conclusions. Our analysis indicates that it is necessary to focus on early phases to detect photoionisation effects of gases in the circumstellar medium of SNe Ia. Different absorbers such as Na I and Ca II can be used to probe for matter at different distances from the SNe. The nondetection of variations during early phases makes it possible to put limits on the abundance of the species at those distances.

Published
2016

30. Arthrose

Author

Schuh, R., Hofstätter, S., Trnka, H.-J., Schmitt, A., Vogt, S., Imhoff, Andreas B., editor, and Feucht, Matthias J., editor

Published
2017
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31. Sehnen

Author

Plath, J., Vogt, S., Reuter, S., Lenich, A., Imhoff, Andreas B., editor, and Feucht, Matthias J., editor

Published
2017
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32. Osteochondrale Läsion

Author

Plath, J., Schmitt, A., Lenich, A., Vogt, S., Reuter, S., Imhoff, Andreas B., editor, and Feucht, Matthias J., editor

Published
2017
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36. Deformable 3D-2D Registration of Known Components for Image Guidance in Spine Surgery

Author

Uneri, A., Goerres, J., De Silva, T., Jacobson, M. W., Ketcha, M. D., Reaungamornrat, S., Kleinszig, G., Vogt, S., Khanna, A. J., Wolinsky, J.-P., Siewerdsen, J. H., Hutchison, David, Editorial Board Member, Kanade, Takeo, Editorial Board Member, Kittler, Josef, Editorial Board Member, Kleinberg, Jon M., Editorial Board Member, Mattern, Friedemann, Editorial Board Member, Mitchell, John C., Editorial Board Member, Naor, Moni, Editorial Board Member, Pandu Rangan, C., Editorial Board Member, Terzopoulos, Demetri, Editorial Board Member, Tygar, Doug, Editorial Board Member, Weikum, Gerhard, Series Editor, Goos, Gerhard, Founding Editor, Hartmanis, Juris, Founding Editor, Bertino, Elisa, Editorial Board Member, Gao, Wen, Editorial Board Member, Steffen, Bernhard, Editorial Board Member, Yung, Moti, Editorial Board Member, Woeginger, Gerhard, Editorial Board Member, Ourselin, Sebastien, editor, Joskowicz, Leo, editor, Sabuncu, Mert R., editor, Unal, Gozde, editor, and Wells, William, editor

Published
2016
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43. Correction to: Risdiplam in Patients Previously Treated with Other Therapies for Spinal Muscular Atrophy: An Interim Analysis from the JEWELFISH Study (Neurology and Therapy, (2023), 12, 2, (543-557), 10.1007/s40120-023-00444-1)

Author

Chiriboga, C. A., Bruno, C., Duong, T., Fischer, D., Mercuri, Eugenio Maria, Kirschner, J., Kostera-Pruszczyk, A., Jaber, B., Gorni, K., Kletzl, H., Carruthers, I., Martin, Craig, Warren, F., Scalco, R. S., Wagner, K. R., Muntoni, F., Deconinck, N., Balikova, I., Joniau, I., Tahon, V., Wittevrongel, S., Goemans, N., Cassiman, C., Prove, L., Vancampenhout, L., van den Hauwe, M., Van Impe, A., Cances, C., Soler, V., De La Morandais, L. M., Vovan, D., Cintas, P., Auriol, F., Mus, M., Alphonsa, G., Bellio, V., Gil Mato, O., Flamein, F., Evrard, C., Ziouche, A., Bouacha-Allou, I., Debruyne, P., Derlyn, G., Defoort, S., Leroy, F., Danjoux, L., Desguerre, I., Bremond-Gignac, D., Rateuax, M., Deladriere, E., Vuillerot, C., Veillerot, Q., Sibille-Dabadi, B., Barriere, A., Tinat, M., Saidi, M., Fontaine, S., De Montferrand, C., Le-Goff, L., Portefaix, A., Louvier, U. W., Duval, P. -A., Caradec, P., Touati, S., Herranz, A. Z., Bollig, J., Molnar, F., Vogt, S., Pechmann, A., Schorling, D., Wider, S., Kolbel, H., Schara, U., Braun, F., Gangfuss, A., Hagenacker, T., Eckstein, A., Dekowski, D., Oeverhaus, M., Stoehr, M., Andres, B., Smuda, K., Bertini, Enrico Silvio, D'Amico, A., Petroni, S., Valente, Paola, Bonetti, A. M., Carlesi, A., Mizzoni, I., Pedemonte, M., Brolatti, N., Priolo, E., Rao, G., Sposetti, L., Morando, S., Comi, G., Osnaghi, S., Minorini, V., Abbati, F., Fassini, F., Foa, M., Lopopolo, M. A., Magri, F., Govoni, A., Meneri, M., Parente, V., Antonaci, Laura, Pera, Maria Carmela, Pane, Marika, Amorelli, Giulia Maria, Barresi, C., D'Amico, Guglielmo, Orazi, Lorenzo, Coratti, Giorgia, De Sanctis, Roberto, Vita, G., Sframeli, M., Vita, G. L., Aragona, P., Inferrera, L., Postorino, E. I., Montanini, D., Di Bella, V., Donato, C., Cala, E., Van der Pol, L., Aalbers, J., de Boer, J., Imhof, S., Cooijmans, P., Ruyten, T., Van Der Woude, D., Klimaszewska, B., Romanczak, D., Gierlak-Wojcicka, Z., Kepa, M., Sikorski, A., Sobieraj, M., Lusakowska, A., Kierdaszuk, B., Czeczko, K., Henzi, B., Gugleta, K., Kusnyerik, A., Siems, P., Akos, S., Frei, N., Seppi, C., Haschke, C. W., Guglieri, M., Straub, V., Bell, R., Nassar, M., Page, S., Clarke, M. P., Regan, A., Mayhew, A., Lofra, R. M., Parasuraman, D., Bruschi, Sara, Ghauri, A. -J., Castle, A., Naqvi, S., Patt, N., Scoto, M., Trucco, F., Henderson, R. H., Kukadia, R., Moore, W., Milev, E., Rye, C., Selby, V., Wolfe, A., Darras, B., Baglieri, A. M., Fulton, A., Lucken, C., Maczek, E., Pasternak, A., Kane, S., Bautista, M. E. M., Frommer, E., Pensec, N., Salazar, R., Yochai, C., Rodrigues-Torres, R., Chawla, M., Day, J., Beres, S., Gee, R., Young, S. D., Finkel, R., Nazario, A. N., Fasiuddin, A., Wells, J. A., Wilson, J., Berry, D., Rizzo, V., Duke, J., Monduy, M., Collado, J., Mercuri E. (ORCID:0000-0002-9851-5365), Martin C., Bertini E., Valente P., Antonaci L., Pera M. C. (ORCID:0000-0001-6777-1721), Pane M. (ORCID:0000-0002-4851-6124), Amorelli G. M., D'Amico G., Orazi L., Coratti G. (ORCID:0000-0001-6666-5628), De Sanctis R., Bruschi S., Chiriboga, C. A., Bruno, C., Duong, T., Fischer, D., Mercuri, Eugenio Maria, Kirschner, J., Kostera-Pruszczyk, A., Jaber, B., Gorni, K., Kletzl, H., Carruthers, I., Martin, Craig, Warren, F., Scalco, R. S., Wagner, K. R., Muntoni, F., Deconinck, N., Balikova, I., Joniau, I., Tahon, V., Wittevrongel, S., Goemans, N., Cassiman, C., Prove, L., Vancampenhout, L., van den Hauwe, M., Van Impe, A., Cances, C., Soler, V., De La Morandais, L. M., Vovan, D., Cintas, P., Auriol, F., Mus, M., Alphonsa, G., Bellio, V., Gil Mato, O., Flamein, F., Evrard, C., Ziouche, A., Bouacha-Allou, I., Debruyne, P., Derlyn, G., Defoort, S., Leroy, F., Danjoux, L., Desguerre, I., Bremond-Gignac, D., Rateuax, M., Deladriere, E., Vuillerot, C., Veillerot, Q., Sibille-Dabadi, B., Barriere, A., Tinat, M., Saidi, M., Fontaine, S., De Montferrand, C., Le-Goff, L., Portefaix, A., Louvier, U. W., Duval, P. -A., Caradec, P., Touati, S., Herranz, A. Z., Bollig, J., Molnar, F., Vogt, S., Pechmann, A., Schorling, D., Wider, S., Kolbel, H., Schara, U., Braun, F., Gangfuss, A., Hagenacker, T., Eckstein, A., Dekowski, D., Oeverhaus, M., Stoehr, M., Andres, B., Smuda, K., Bertini, Enrico Silvio, D'Amico, A., Petroni, S., Valente, Paola, Bonetti, A. M., Carlesi, A., Mizzoni, I., Pedemonte, M., Brolatti, N., Priolo, E., Rao, G., Sposetti, L., Morando, S., Comi, G., Osnaghi, S., Minorini, V., Abbati, F., Fassini, F., Foa, M., Lopopolo, M. A., Magri, F., Govoni, A., Meneri, M., Parente, V., Antonaci, Laura, Pera, Maria Carmela, Pane, Marika, Amorelli, Giulia Maria, Barresi, C., D'Amico, Guglielmo, Orazi, Lorenzo, Coratti, Giorgia, De Sanctis, Roberto, Vita, G., Sframeli, M., Vita, G. L., Aragona, P., Inferrera, L., Postorino, E. I., Montanini, D., Di Bella, V., Donato, C., Cala, E., Van der Pol, L., Aalbers, J., de Boer, J., Imhof, S., Cooijmans, P., Ruyten, T., Van Der Woude, D., Klimaszewska, B., Romanczak, D., Gierlak-Wojcicka, Z., Kepa, M., Sikorski, A., Sobieraj, M., Lusakowska, A., Kierdaszuk, B., Czeczko, K., Henzi, B., Gugleta, K., Kusnyerik, A., Siems, P., Akos, S., Frei, N., Seppi, C., Haschke, C. W., Guglieri, M., Straub, V., Bell, R., Nassar, M., Page, S., Clarke, M. P., Regan, A., Mayhew, A., Lofra, R. M., Parasuraman, D., Bruschi, Sara, Ghauri, A. -J., Castle, A., Naqvi, S., Patt, N., Scoto, M., Trucco, F., Henderson, R. H., Kukadia, R., Moore, W., Milev, E., Rye, C., Selby, V., Wolfe, A., Darras, B., Baglieri, A. M., Fulton, A., Lucken, C., Maczek, E., Pasternak, A., Kane, S., Bautista, M. E. M., Frommer, E., Pensec, N., Salazar, R., Yochai, C., Rodrigues-Torres, R., Chawla, M., Day, J., Beres, S., Gee, R., Young, S. D., Finkel, R., Nazario, A. N., Fasiuddin, A., Wells, J. A., Wilson, J., Berry, D., Rizzo, V., Duke, J., Monduy, M., Collado, J., Mercuri E. (ORCID:0000-0002-9851-5365), Martin C., Bertini E., Valente P., Antonaci L., Pera M. C. (ORCID:0000-0001-6777-1721), Pane M. (ORCID:0000-0002-4851-6124), Amorelli G. M., D'Amico G., Orazi L., Coratti G. (ORCID:0000-0001-6666-5628), De Sanctis R., and Bruschi S.

Abstract

In this article the JEWELFISH Study Group members were missing in the Acknowledgements. The collaborator names are corrected in the supplementary material and the complete list is given below. In Table 1, footnote symbol ‘g’ was incorrectly written as ‘f’ in the entries Non-sitters—2 (14)g and Sitters-12 (86)g under column Onasemnogene abeparvovec of section Motor function, n (%)f. The original article has been corrected.

Published
2023

47. Surgical navigation for guidewire placement from intraoperative fluoroscopy in orthopaedic surgery.

Author

Mekki, L, Sheth, N M, Vijayan, R C, Rohleder, M, Sisniega, A, Kleinszig, G, Vogt, S, Kunze, H, Osgood, G M, Siewerdsen, J H, and Uneri, A

Subjects
ORTHOPEDIC surgery, FLUOROSCOPY, GEOMETRIC modeling, NAVIGATION, RADIATION doses, MEDICAL cadavers
Abstract

Objective. Surgical guidewires are commonly used in placing fixation implants to stabilize fractures. Accurate positioning of these instruments is challenged by difficulties in 3D reckoning from 2D fluoroscopy. This work aims to enhance the accuracy and reduce exposure times by providing 3D navigation for guidewire placement from as little as two fluoroscopic images. Approach. Our approach combines machine learning-based segmentation with the geometric model of the imager to determine the 3D poses of guidewires. Instrument tips are encoded as individual keypoints, and the segmentation masks are processed to estimate the trajectory. Correspondence between detections in multiple views is established using the pre-calibrated system geometry, and the corresponding features are backprojected to obtain the 3D pose. Guidewire 3D directions were computed using both an analytical and an optimization-based method. The complete approach was evaluated in cadaveric specimens with respect to potential confounding effects from the imaging geometry and radiographic scene clutter due to other instruments. Main results. The detection network identified the guidewire tips within 2.2 mm and guidewire directions within 1.1°, in 2D detector coordinates. Feature correspondence rejected false detections, particularly in images with other instruments, to achieve 83% precision and 90% recall. Estimating the 3D direction via numerical optimization showed added robustness to guidewires aligned with the gantry rotation plane. Guidewire tips and directions were localized in 3D world coordinates with a median accuracy of 1.8 mm and 2.7°, respectively. Significance. The paper reports a new method for automatic 2D detection and 3D localization of guidewires from pairs of fluoroscopic images. Localized guidewires can be virtually overlaid on the patient's pre-operative 3D scan during the intervention. Accurate pose determination for multiple guidewires from two images offers to reduce radiation dose by minimizing the need for repeated imaging and provides quantitative feedback prior to implant placement. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
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48. An investigation of pathways for rebuilding Australia's sheep flock.

Author

Brien, F. D., Pitchford, R. L., Vogt, S. P., and Koopman, D. J.

Abstract

Context: A significant opportunity remains to further increase the supply of premium sheepmeat products to Australia's customers, which requires a more rapid rebuilding of the national sheep flock. To help meet this challenge, developing relevant information for sheep producers to assist them to achieve a profitable flock-rebuilding outcome is viewed as highly desirable. Aims: (1) Develop flock-rebuild scenarios that track inventory, cashflow, profit and loss, and the overall balance sheet over a 5-year projection. (2) Model the impact on flock-rebuilding pathways of exposure to variation in supplementary-feed costs, purchase of stock and price received for sale animals and flock structure. (3) Model variation in benefits and costs for a range of production zones, enterprise types and flock-age profiles. Methods: Fourteen flock-rebuilding pathways were assessed for up to nine flock types, using a spreadsheet model that tracked inventory, cashflow, profit and loss, and the overall balance sheet over 5 years. Key results: The top four pathways for profitability and capacity to rapidly rebuild flock numbers include retention of more older ewes, purchasing young ewes, purchasing older ewes (mostly 5–6-year olds) in Merino and Merino-cross flock types only and joining ewe lambs in Maternal and Cleanskin flock types only. These pathways were not sensitive to variation in the cost of supplementary feed, stock prices or flock structure, although joining Merino ewe lambs became one of the top four pathways when feed costs were lower. Conclusions and implications: The well established practices of retaining ewes for longer and purchasing ewes, especially young ewes, have the most potential to both rapidly and profitably rebuild flock numbers. However, joining ewe lambs, particularly in Maternal and Cleanskin flocks, can also profitably contribute to rapid flock rebuilding. While reducing reproductive wastage or increasing reproductive potential were mostly profitable, they could not rapidly rebuild flock numbers. In contrast, accelerated lambing systems can rapidly rebuild flock numbers, but are only marginally profitable. The outlook for Australia's sheepmeat industry is very positive, with a significant opportunity available to further increase the supply of premium sheepmeat products to customers, by more rapidly rebuilding the national flock. This paper presents the findings of a study focussed on providing the confidence and material to sheep producers to choose optimal pathways to rebuild their flocks. At least 6 of the 14 alternatives investigated were deemed suitable for commercial use and not sensitive to variations in supplementary-feed costs, stock-purchasing and -sale prices. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
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