Author: "Schwarz G." - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Schwarz G."' showing total 2,729 results

Start Over Author "Schwarz G."

2,729 results on '"Schwarz G."'

1. The Southern Photometrical Local Universe Survey (S-PLUS): searching for metal-poor dwarf galaxies

Author: Grossi, M., Gonçalves, D. R., Krabbe, A. C., Soto, L. A. Gutiérrez, Telles, E., Ribeiro, L. S., Gonçalves, T. Signorini, Lopes, A. R., Castelli, A. V. Smith, De Rossi, M. E., Lima-Dias, C., Limberg, G., Lopes, C. E. Ferreira, Hernandez-Jimenez, J. A., Humire, P. K., Santos, A. L. Chies, Lomelí-Nuñez, L., Torres-Flores, S., Herpich, F. R., Schwarz, G. B. Oliveira, Kanaan, A., de Oliveira, C. Mendes, Ribeiro, T., and Schoenell, W.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The metal content of a galaxy's interstellar medium reflects the interplay between different evolutionary processes such as feedback from massive stars and the accretion of gas from the intergalactic medium. Despite the expected abundance of low-luminosity galaxies, the low-mass and low-metallicity regime remains relatively understudied. Since the properties of their interstellar medium resemble those of early galaxies, identifying such objects in the Local Universe is crucial to understand the early stages of galaxy evolution. We used the DR3 catalog of the Southern Photometric Local Universe Survey (S-PLUS) to select low-metallicity dwarf galaxy candidates based on color selection criteria typical of metal-poor, star-forming, low-mass systems. The final sample contains approximately 50 candidates. Spectral energy distribution fitting of the 12 S-PLUS bands reveals that $\sim$ 90\% of the candidates are best fit by models with very low stellar metallicities. We obtained long-slit observations with the Gemini Multi-Object Spectrograph to follow-up a pilot sample and confirm whether these galaxies have low metallicities. We find oxygen abundances in the range $7.35<$ 12 + log(O/H) $< 7.93$ (5\% to 17\% of the solar value), confirming their metal-poor nature. Most targets are outliers in the mass-metallicity relation, i.e. they display a low metal content relative to their observed stellar masses. In some cases, perturbed optical morphologies might give evidence of dwarf-dwarf interactions or mergers. These results suggest that the low oxygen abundances may be associated with an external event causing the accretion of metal-poor gas, which dilutes the oxygen abundance in these systems., Comment: 23 pages, 13 figures, submitted to ApJ
Published: 2025

2. Stellar atmospheric parameters and chemical abundances of about 5 million stars from S-PLUS multi-band photometry

Author: Lopes, C. E. Ferreira, Gutiérrez-Soto, L. A., Alberice, V. S. Ferreira, Monsalves, N., Hazarika, D., Catelan, M., Placco, V. M., Limberg, G., Almeida-Fernandes, F., Perottoni, H. D., Castelli, A. V. Smith, Akras, S., Alonso-García, J., Cordeiro, V., Arancibia, M. Jaque, Daflon, S., Dias, B., Gonçalves, D. R., Machado-Pereira, E., Lopes, A. R., Bom, C. R., de Souza, R. C. Thom, de Isídio, N. G., Alvarez-Candal, A., De Rossi, M. E., Bonatto, C. J., Palma, B. Cubillos, Fernandes, M. Borges, Humire, P. K., Schwarz, G. B. Oliveira, Schoenell, W., Kanaan, A., and de Oliveira, C. Mendes
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Context. Spectroscopic surveys like APOGEE, GALAH, and LAMOST have significantly advanced our understanding of the Milky Way by providing extensive stellar parameters and chemical abundances. Complementing these, photometric surveys with narrow/medium-band filters, such as the Southern Photometric Local Universe Survey (S-PLUS), offer the potential to estimate stellar parameters and abundances for a much larger number of stars. Aims. This work develops methodologies to extract stellar atmospheric parameters and selected chemical abundances from S-PLUS photometric data, which spans ~3000 square degrees using seven narrowband and five broadband filters. Methods. Using 66 S-PLUS colors, we estimated parameters based on training samples from LAMOST, APOGEE, and GALAH, applying Cost-Sensitive Neural Networks (NN) and Random Forests (RF). We tested for spurious correlations by including abundances not covered by the S-PLUS filters and evaluated NN and RF performance, with NN consistently outperforming RF. Including Teff and log g as features improved accuracy by ~3%. We retained only parameters with a goodness-of-fit above 50%. Results. Our approach provides reliable estimates of fundamental parameters (Teff, log g, [Fe/H]) and abundance ratios such as [{\alpha}/Fe], [Al/Fe], [C/Fe], [Li/Fe], and [Mg/Fe] for ~5 million stars, with goodness-of-fit >60%. Additional ratios like [Cu/Fe], [O/Fe], and [Si/Fe] were derived but are less accurate. Validation using star clusters, TESS, and J-PLUS data confirmed the robustness of our methodology. Conclusions. By leveraging S-PLUS photometry and machine learning, we present a cost-effective alternative to high-resolution spectroscopy for deriving stellar parameters and abundances, enabling insights into Milky Way stellar populations and supporting future classification efforts., Comment: 23 pages, 14 Figures
Published: 2024
Full Text: View/download PDF

3. The Quasar Catalogue for S-PLUS DR4 (QuCatS) and the estimation of photometric redshifts

Author: Nakazono, L., Valença, R. R., Soares, G., Izbicki, R., Ivezić, Ž., Lima, E. V. R., Hirata, N. S. T., Sodré Jr., L., Overzier, R., Almeida-Fernandes, F., Schwarz, G. B. Oliveira, Schoenell, W., Kanaan, A., Ribeiro, T., and de Oliveira, C. Mendes
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The advent of massive broad-band photometric surveys enabled photometric redshift estimates for unprecedented numbers of galaxies and quasars. These estimates can be improved using better algorithms or by obtaining complementary data such as narrow-band photometry, and broad-band photometry over an extended wavelength range. We investigate the impact of both approaches on photometric redshifts for quasars using data from Southern Photometric Local Universe Survey (S-PLUS) DR4, Galaxy Evolution Explorer (GALEX) DR6/7, and the unWISE catalog for the Wide-field Infrared Survey Explorer (WISE) in three machine learning methods: Random Forest, Flexible Conditional Density Estimation (FlexCoDE), and Bayesian Mixture Density Network (BMDN). Including narrow-band photometry improves the root-mean-square error by 11% in comparison to a model trained with only broad-band photometry. Narrow-band information only provided an improvement of 3.8% when GALEX and WISE colours were included. Thus narrow bands play a more important role for objects that do not have GALEX or WISE counterparts, which respectively makes 92% and 25% of S-PLUS data considered here. Nevertheless, the inclusion of narrow-band information provided better estimates of the probability density functions obtained with FlexCoDE and BMDN. We publicly release a value-added catalogue of photometrically selected quasars with the photo-z predictions from all methods studied here. The catalogue provided with this work covers the S-PLUS DR4 area (~3000deg$^2$), containing 645 980, 244 912, 144 991 sources with the probability of being a quasar higher than, 80%, 90%, 95% up to r < 21.3 and good photometry quality in the detection image. More quasar candidates can be retrieved from the S-PLUS data base by considering less restrictive selection criteria.
Published: 2024
Full Text: View/download PDF

4. The S-PLUS Fornax Project (S+FP): A first 12-band glimpse of the Fornax galaxy cluster

Author: Castelli, A. V. Smith, Cortesi, A., Haack, R. F., Lopes, A. R., Thainá-Batista, J., Fernandes, R. Cid, Lomelí-Núñez, L., Ribeiro, U., de Bom, C. R., Cernic, V., Sodré Jr, L., Zenocratti, L., De Rossi, M. E., Calderón, J. P., Herpich, F., Telles, E., Saha, K., Lopes, P. A. A., Lopes-Silva, V. H., Gonçalves, T. S., Bambrila, D., Cardoso, N. M., Buzzo, M. L., Sotomayor, P. Astudillo, Demarco, R., Leigh, N., Sarzi, M., Menéndez-Delmestre, K., Faifer, F. R., Jiménez-Teja, Y., Grossi, M., Hernández-Jiménez, J. A., Krabbe, A. C., Soto, L. A. Gutiérrez, Brandão, D., Espinosa, L., Olave-Rojas, D. E., Schwarz, G. B. Oliveira, Almeida-Fernandes, F., Schoenell, W., Ribeiro, T., Kanaan, A., and de Oliveira, C. Mendes
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The Fornax galaxy cluster is the richest nearby (D ~ 20 Mpc) galaxy association in the southern sky. As such, it provides a wealth of oportunities to elucidate on the processes where environment holds a key role in transforming galaxies. Although it has been the focus of many studies, Fornax has never been explored with contiguous homogeneous wide-field imaging in 12 photometric narrow- and broad-bands like those provided by the Southern Photometric Local Universe Survey (S-PLUS). In this paper we present the S-PLUS Fornax Project (S+FP) that aims to comprehensively analyse the galaxy content of the Fornax cluster using S-PLUS. Our data set consists of 106 S-PLUS wide-field frames (FoV ~ 1.4 x 1.4 deg$^2$) observed in five SDSS-like ugriz broad-bands and seven narrow-bands covering specific spectroscopic features like [OII], CaII H+K, H$\delta$, G-band, Mg b triplet, H$\alpha$, and the CaII triplet. Based on S-PLUS specific automated photometry, aimed at correctly detecting Fornax galaxies and globular clusters in S-PLUS images, our dataset provides the community with catalogues containing homogeneous 12-band photometry for ~ 3 x 10$^6$ resolved and unresolved objects within a region extending over ~ 208 deg$^2$ (~ 5 Rvir in RA) around Fornax' central galaxy, NGC 1399. We further explore the EAGLE and IllustrisTNG cosmological simulations to identify 45 Fornax-like clusters and generate mock images on all 12 S-PLUS bands of these structures down to galaxies with M$\star \geq 10^8$ M$\odot$. The S+FP dataset we put forward in this first paper of a series will enable a variety of studies some of which are briefly presented., Comment: 25 pages, 30 figures, accepted for publication in MNRAS
Published: 2024

5. Morphological Classification of Galaxies in S-PLUS using an Ensemble of Convolutional Networks

Author: Cardoso, N. M., Schwarz, G. B. O., Dias, L. O., Bom, C. R., Sodré Jr., L., and de Oliveira, C. Mendes
Subjects: Astrophysics - Astrophysics of Galaxies, Computer Science - Computer Vision and Pattern Recognition, Computer Science - Machine Learning
Abstract: The universe is composed of galaxies that have diverse shapes. Once the structure of a galaxy is determined, it is possible to obtain important information about its formation and evolution. Morphologically classifying galaxies means cataloging them according to their visual appearance and the classification is linked to the physical properties of the galaxy. A morphological classification made through visual inspection is subject to biases introduced by subjective observations made by human volunteers. For this reason, systematic, objective and easily reproducible classification of galaxies has been gaining importance since the astronomer Edwin Hubble created his famous classification method. In this work, we combine accurate visual classifications of the Galaxy Zoo project with \emph {Deep Learning} methods. The goal is to find an efficient technique at human performance level classification, but in a systematic and automatic way, for classification of elliptical and spiral galaxies. For this, a neural network model was created through an Ensemble of four other convolutional models, allowing a greater accuracy in the classification than what would be obtained with any one individual. Details of the individual models and improvements made are also described. The present work is entirely based on the analysis of images (not parameter tables) from DR1 (www.datalab.noao.edu) of the Southern Photometric Local Universe Survey (S-PLUS). In terms of classification, we achieved, with the Ensemble, an accuracy of $\approx 99 \%$ in the test sample (using pre-trained networks)., Comment: 18 pages, 13 figures, codes and data available at https://natanael.net, text in portuguese
Published: 2021

6. The Fornax Cluster through S-PLUS

Author: Castelli, A. V. Smith, de Oliveira, C. Mendes, Herpich, F., Barbosa, C. E., Escudero, C., Grossi, M., Sodre, L., de Bom, C. R., Zenocratti, L., De Rossi, M. E., Cortesi, A., Fernandes, R. Cid, Lopes, A. R., Telles, E., Schwarz, G. B. Oliveira, Dantas, M. L. L., Faifer, F. R., Santos, A. Chies, Saponara, J., Reynaldi, V., Andruchow, I., Sesto, L., Mestre, M. F., de Amorim, A. L., de Lima, E. V. R., Abboud, J. C. R., Cernic, V., and Garcia, I. Souza de Almeida
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Southern Photometric Local Universe Survey (S-PLUS) aims to map $\approx$ 9300 deg$^2$ of the Southern sky using the Javalambre filter system of 12 optical bands, 5 Sloan-like filters and 7 narrow-band filters centered on several prominent stellar features ([OII], Ca H+K, D4000, H$_{\delta}$, Mgb, H$_{\alpha}$ and CaT). S-PLUS is carried out with the T80-South, a new robotic 0.826-m telescope located on CTIO, equipped with a wide FoV camera (2 deg$^2$). In this poster we introduce project #59 of the S-PLUS collaboration aimed at studying the Fornax galaxy cluster covering an sky area of $\approx$ 11 $\times$ 7 deg$^2$, and with homogeneous photometry in the 12 optical bands of S-PLUS (Coordinator: A. Smith Castelli)., Comment: 3 pages, 5 figures; accepted to be published in Bolet\'in de la Asociaci\'on Argentina de Astronom\'ia
Published: 2021

7. Data Release 2 of S-PLUS: accurate template-fitting based photometry covering $\sim$1000 square degrees in 12 optical filters

Author: Almeida-Fernandes, F., Sampedro, L., Herpich, F. R., Molino, A., Barbosa, C. E., Buzzo, M. L., Overzier, R. A., de Lima, E. V. R., Nakazono, L. M. I., Schwarz, G. B. Oliveira, Perottoni, H. D., Bolutavicius, G. F., Gutiérrez-Soto, L. A., Santos-Silva, T., Vitorelli, A. Z., Werle, A., Whitten, D. D., Duarte, M. V. Costa, Bom, C. R., Coelho, P., Sodré Jr., L., Placco, V. M., Teixeira, G. S. M., Alonso-García, J., Beers, T. C., Kanaan, A., Ribeiro, T., Schoenell, W., and de Oliveira, C. Mendes
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The Southern Photometric Local Universe Survey (S-PLUS) is an ongoing survey of $\sim$9300 deg$^2$ in the southern sky in a 12-band photometric system. This paper presents the second data release (DR2) of S-PLUS, consisting of 514 tiles covering an area of 950 deg$^2$. The data has been fully calibrated using a new photometric calibration technique suitable for the new generation of wide-field multi-filter surveys. This technique consists of a $\chi^2$ minimisation to fit synthetic stellar templates to already calibrated data from other surveys, eliminating the need for standard stars and reducing the survey duration by $\sim$15\%. We compare the template-predicted and S-PLUS instrumental magnitudes to derive the photometric zero-points (ZPs). We show that these ZPs can be further refined by fitting the stellar templates to the 12 S-PLUS magnitudes, which better constrain the models by adding the narrow-band information. We use the STRIPE82 region to estimate ZP errors, which are $\lesssim10$ mmags for filters J0410, J0430, $g$, J0515, $r$, J0660, $i$, J0861 and $z$; $\lesssim 15$ mmags for filter J0378; and $\lesssim 25$ mmags for filters $u$ and J0395. We describe the complete data flow of the S-PLUS/DR2 from observations to the final catalogues and present a brief characterisation of the data. We show that, for a minimum signal-to-noise threshold of 3, the photometric depths of the DR2 range from 19.9 mag to 21.3 mag (measured in Petrosian apertures), depending on the filter. The S-PLUS DR2 can be accessed from the website: https://splus.cloud}{https://splus.cloud., Comment: 29 pages, 26 figures, 7 tables
Published: 2021
Full Text: View/download PDF

8. Deep Learning Assessment of galaxy morphology in S-PLUS DataRelease 1

Author: Bom, C. R., Cortesi, A., Lucatelli, G., Dias, L. O., Schubert, P., Schwarz, G. B. Oliveira, Cardoso, N. M., Lima, E. V. R., de Oliveira, C. Mendes, Sodre Jr., L., Castelli, A. V. Smith, Ferrari, F., Damke, G., Overzier, R., Kanaan, A., Ribeiro, T., and Schoenell, W.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The morphological diversity of galaxies is a relevant probe of galaxy evolution and cosmological structure formation, but the classification of galaxies in large sky surveys is becoming a significant challenge. We use data from the Stripe-82 area observed by the Southern Photometric Local Universe Survey (S-PLUS) in twelve optical bands, and present a catalogue of the morphologies of galaxies brighter than $r=17$ mag determined both using a novel multi-band morphometric fitting technique and Convolutional Neural Networks (CNNs) for computer vision. Using the CNNs we find that, compared to our baseline results with 3 bands, the performance increases when using 5 broad and 3 narrow bands, but is poorer when using the full $12$ band S-PLUS image set. However, the best result is still achieved with just 3 optical bands when using pre-trained network weights from an ImageNet data set. These results demonstrate the importance of using prior knowledge about neural network weights based on training in unrelated, extensive data sets, when available. Our catalogue contains 3274 galaxies in Stripe-82 that are not present in Galaxy Zoo 1 (GZ1), and we also provide our classifications for 4686 galaxies that were considered ambiguous in GZ1. Finally, we present a prospect of a novel way to take advantage of $12$ band information for morphological classification using morphometric features, and we release a model that has been pre-trained on several bands that could be adapted for classifications using data from other surveys. The morphological catalogues are publicly available., Comment: accepted version for publication in MNRAS
Published: 2021
Full Text: View/download PDF

9. Whole-brain diffusion tensor imaging predicts 6-month functional outcome in acute intracerebral haemorrhage

Author: Schwarz, G., Kanber, B., Prados, F., Browning, S., Simister, R., Jäger, H. R., Ambler, G., Gandini Wheeler-Kingshott, C. A. M., and Werring, D. J.
Published: 2023
Full Text: View/download PDF

10. The January 2016 eruption of recurrent nova LMC 1968

Author: Kuin, N. P. M., Page, K. L., Mróz, P., Darnley, M. J., Shore, S. N., Osborne, J. P., Walter, F., Di Mille, F., Morrell, N., Munari, U., Bohlsen, T., Evans, A., Gehrz, R. D., Starrfield, S., Henze, M., Williams, S. C., Schwarz, G. J., Udalski, A., Szymański, M. K., Poleski, R., Soszyński, I., Ribeiro, V. A. R. M., Angeloni, R., Breeveld, A. A., Beardmore, A. P., and Skowron, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a comprehensive review of all observations of the eclipsing recurrent Nova LMC 1968 in the Large Magellanic Cloud which was previously observed in eruption in 1968, 1990, 2002, 2010, and most recently in 2016. We derive a probable recurrence time of $6.2 \pm 1.2$ years and provide the ephemerides of the eclipse. In the ultraviolet-optical-IR photometry the light curve shows high variability right from the first observation around two days after eruption. Therefore no colour changes can be substantiated. Outburst spectra from 2016 and 1990 are very similar and are dominated by H and He lines longward of 2000 Angstrom. Interstellar reddening is found to be E(B-V) = $0.07\pm0.01$. The super soft X-ray luminosity is lower than the Eddington luminosity and the X-ray spectra suggest the mass of the WD is larger than 1.3 M$_\odot$. Eclipses in the light curve suggest that the system is at high orbital inclination. On day four after the eruption a recombination wave was observed in Fe II ultraviolet absorption lines. Narrow line components are seen after day 6 and explained as being due to reionisation of ejecta from a previous eruption. The UV spectrum varies with orbital phase, in particular a component of the He II 1640 Angstrom emission line, which leads us to propose that early-on the inner WD Roche lobe might be filled with a bound opaque medium prior to the re-formation of an accretion disk. Both this medium and the ejecta can cause the delay in the appearance of the soft X-ray source., Comment: MNRAS accepted October 18, 2019
Published: 2019
Full Text: View/download PDF

11. Age-Related Physiology Changes: Cardiovascular Function in the Very Old Critically Ill Patient

Author: Skaar, E., Fanebust, H., Schwarz, G., Cecconi, Maurizio, Series Editor, De Backer, Daniel, Series Editor, Flaatten, Hans, editor, Guidet, Bertrand, editor, and Vallet, Hélène, editor
Published: 2022
Full Text: View/download PDF

12. Acute corticospinal tract diffusion tensor imaging predicts 6-month functional outcome after intracerebral haemorrhage

Author: Schwarz, G., Kanber, B., Prados, F., Browning, S., Simister, R., Jäger, R., Ambler, G., Wheeler-Kingshott, C. A. M. Gandini, and Werring, David J.
Published: 2022
Full Text: View/download PDF

13. The Temporal Development of Dust Formation and Destruction in Nova Sagittarii 2015#2 (V5668 Sgr): A Panchromatic Study

Author: Gehrz, R. D., Evans, A., Woodward, C. E., Helton, L. A., Banerjee, D. P. K., Srivastava, M. K., Ashok, N. M., Joshi, V., Eyres, S. P. S., Krautter, Joachim, Kuin, N. P. M., Page, K. L., Osborne, J. P., Schwarz, G. J., Shenoy, D. P., Shore, S. N., Starrfield, S. G., and Wagner, R. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present 5-28 micron SOFIA FORECAST spectroscopy complemented by panchromatic X-ray through infrared observations of the CO nova V5668 Sgr documenting the formation and destruction of dust during 500 days following outburst. Dust condensation commenced by 82 days after outburst at a temperature of 1090 K. The condensation temperature indicates that the condensate was amorphous carbon. There was a gradual decrease of the grain size and dust mass during the recovery phase. Absolute parameter values given here are for an assumed distance of 1.2 kpc. We conclude that the maximum mass of dust produced was 1.2 x 10-7 solar masses if the dust was amorphous carbon. The average grain radius grew to a maximum of 2.9 microns at a temperature of 720 K around day 113 when the shell visual optical depth was Tau = 5.4. Maximum grain growth was followed by followed by a period of grain destruction. X-rays were detected with Swift from day 95 to beyond day 500. The Swift X-ray count rate due to the hot white dwarf peaked around day 220, when its spectrum was that of a kT = 35 eV blackbody. The temperature, together with the super-soft X-ray turn-on and turn-off times, suggests a WD mass of 1.1 solar masses. We show that the X-ray fluence was sufficient to destroy the dust. Our data show that the post-dust event X-ray brightening is not due to dust destruction, which certainly occurred, as the dust is optically thin to X-rays., Comment: Accepted for publication in the Astrophysical Journal. This is the final version after correction of the proofs
Published: 2018
Full Text: View/download PDF

14. Strain-induced trace element mobility in a quartz-sulphide vein system: An example from the ONKALO™ spent nuclear fuel repository (Olkiluoto, SW Finland)

Author: Marchesini, B., Menegon, L., Schwarz, G., Neff, C., Keresztes Schmidt, P., Garofalo, P.S., Hattendorf, B., Günther, D., Mattila, J., and Viola, G.
Published: 2022
Full Text: View/download PDF

15. Is Gaining Affective Commitment the Missing Strategy for Successful Change Management in Healthcare?

Author: Harrison R, Chauhan A, Minbashian A, McMullan R, and Schwarz G
Subjects: change readiness, commitment to change, affective commitment, implementation, improvement, healthcare change, Public aspects of medicine, RA1-1270
Published: 2022

16. The panchromatic spectroscopic evolution of the classical CO nova V339 Del (Nova Del 2013) until X-ray turnoff

Author: Shore, S. N., Mason, E., Schwarz, G. J., Teyssier, F. M., Buil, C., Aquino, I. De Gennaro, Page, K. L., Osborne, J. P., Scaringi, S., Starrfield, S., van Winckel, H., Williams, R. E., and Woodward, C. E.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Classical novae are the product of thermonuclear runaway-initiated explosions occurring on accreting white dwarfs. V339 Del (Nova Delphinus 2013) was one of the brightest classical novae of the last hundred years. Spectroscopy and photometry are available from $\gamma$-rays through infrared at stages that have frequently not been well observed. The complete data set is intended to provide a benchmark for comparison with modeling and for understanding more sparsely monitored historical classical and recurrent novae. This paper is the first in the series of reports on the development of the nova. We report here on the early stages of the outburst, through the X-ray active stage. A time sequence of optical, flux calibrated high resolution spectra was obtained with the Nordic Optical Telescope (NOT) using FIES simultaneously, or contemporaneously, with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope during the early stages of the outburst. These were supplemented with MERCATOR/HERMES optical spectra. High resolution IUE ultraviolet spectra of OS And 1986, taken during the Fe curtain phase, served as a template for the distance determination. We used standard plasma diagnostics (e.g., [O III] and [N II] line ratios, and the H$\beta$ line flux) to constrain electron densities and temperatures of the ejecta. Using Monte Carlo modeling of the ejecta, we derived the structure, filling factor, and mass from comparisons of the optical and ultraviolet line profiles., Comment: 14 pages, 18 figures
Published: 2016
Full Text: View/download PDF

17. MRI-related anxiety can induce slow BOLD oscillations coupled with cardiac oscillations

Author: Pfurtscheller, G., Schwerdtfeger, A.R., Rassler, B., Andrade, A., and Schwarz, G.
Published: 2021
Full Text: View/download PDF

18. Pan-Chromatic observations of the Recurrent Nova LMC 2009a (LMC 1971b)

Author: Bode, M. F., Darnley, M. J., Beardmore, A. P., Osborne, J. P., Page, K. L., Walter, F. M., Krautter, J., Melandri, A., Ness, J. -U., O'Brien, T. J., Orio, M., Schwarz, G. J., Shara, M. M., and Starrfield, S.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Nova LMC 2009a is confirmed as a Recurrent Nova (RN) from positional coincidence with nova LMC 1971b. The observational data set is one of the most comprehensive for any Galactic or extragalactic RN: optical and near-IR photometry from outburst until over 6 years later; optical spectra for the first 6 months, and Swift satellite Ultraviolet and X-ray observations from 9 days to almost 1 year post-outburst. We find $M_V = -8.4\pm0.8_{\mathrm{r}}\pm0.7_{\mathrm{s}}$ and expansion velocities between 1000 and 4000 km s$^{-1}$. Coronal line emission before day 9 indicates shocks in the ejecta. Strengthening of He II $\lambda$4686 preceded the emergence of the Super-Soft Source (SSS) in X-rays at $\sim63-70$ days, which was initially very variable. Periodic modulations, $P=1.2$ days, most probably orbital in nature, were evident in the UV and optical from day 43. Subsequently, the SSS shows an oscillation with the same period but with a delay of 0.28P. The progenitor system has been identified; the secondary is most likely a sub-giant feeding a luminous accretion disk. Properties of the SSS infer a white dwarf (WD) mass $1.1 \mathrm{M}_\odot \lesssim M_{\rm WD} \lesssim 1.3 \mathrm{M}_\odot$. If the accretion occurs at constant rate, $\dot{\it{M}}_{\rm acc} \simeq 3.6^{+4.7}_{-2.5} \times 10^{-7} \mathrm{M}_\odot$ yr$^{-1}$ is needed, consistent with nova models for an inter-eruption interval of 38 years, low outburst amplitude, progenitor position in the color-magnitude diagram, and spectral energy distribution at quiescence. We note striking similarities between LMC 2009a and the Galactic nova KT Eri, suggesting that KT Eri is a candidate RN., Comment: 20 pages, 23 figures, accepted for publication in the Astrophysical Journal
Published: 2016
Full Text: View/download PDF

19. Swift detection of the super-swift switch-on of the super-soft phase in nova V745 Sco (2014)

Author: Page, K. L., Osborne, J. P., Kuin, N. P. M., Henze, M., Walter, F. M., Beardmore, A. P., Bode, M. F., Darnley, M. J., Delgado, L., Drake, J. J., Hernanz, M., Mukai, K., Nelson, T., Ness, J. -U., Schwarz, G. J., Shore, S. N., Starrfield, S., and Woodward, C. E.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: V745 Sco is a recurrent nova, with the most recent eruption occurring in February 2014. V745 Sco was first observed by Swift a mere 3.7 hr after the announcement of the optical discovery, with the super-soft X-ray emission being detected around four days later and lasting for only ~two days, making it both the fastest follow-up of a nova by Swift and the earliest switch-on of super-soft emission yet detected. Such an early switch-on time suggests a combination of a very high velocity outflow and low ejected mass and, together with the high effective temperature reached by the super-soft emission, a high mass white dwarf (>1.3 M_sun). The X-ray spectral evolution was followed from an early epoch where shocked emission was evident, through the entirety of the super-soft phase, showing evolving column density, emission lines, absorption edges and thermal continuum temperature. UV grism data were also obtained throughout the super-soft interval, with the spectra showing mainly emission lines from lower ionization transitions and the Balmer continuum in emission. V745 Sco is compared with both V2491 Cyg (another nova with a very short super-soft phase) and M31N 2008-12a (the most rapidly recurring nova yet discovered). The longer recurrence time compared to M31N 2008-12a could be due to a lower mass accretion rate, although inclination of the system may also play a part. Nova V745 Sco (2014) revealed the fastest evolving super-soft source phase yet discovered, providing a detailed and informative dataset for study., Comment: 14 pages, 11 figures (4 in colour), accepted for publication in MNRAS
Published: 2015
Full Text: View/download PDF

20. Age-Related Physiology Changes: Cardiovascular Function in the Very Old Critically Ill Patient

Author: Skaar, E., primary, Fanebust, H., additional, and Schwarz, G., additional
Published: 2022
Full Text: View/download PDF

21. Short-period X-ray oscillations in super-soft novae and persistent SSS

Author: Ness, J. -U., Beardmore, A. P., Osborne, J. P., Kuulkers, E., Henze, M., Piro, A. L., Drake, J. J., Dobrotka, A., Schwarz, G., Starrfield, S., Kretschmar, P., Hirsch, M., and Wilms, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: Transient short-period <100s oscillations have been found in the X-ray light curves of three novae during their SSS phase and in one persistent SSS. We pursue an observational approach to determine possible driving mechanisms and relations to fundamental system parameters such as the white dwarf mass. We performed a systematic search for short-period oscillations in all available XMM-Newton and Chandra X-ray light curves of persistent SSS and novae during their SSS phase. To study time evolution, we divided each light curve into short time segments and computed power spectra. We then constructed dynamic power spectra from which we identified transient periodic signals even when only present for a short time. From all time segments of each system, we computed fractions of time when periodic signals were detected. In addition to the previously known systems with short-period oscillations, RS Oph (35s), KT Eri (35s), V339 Del (54s), and Cal 83 (67s), we found one additional system, LMC 2009a (33s), and also confirm the 35s period from Chandra data of KT Eri. The amplitudes of oscillations are of order <15% of the respective count rates and vary without any clear dependence on the X-ray count rate. The fractions of the time when the respective periods were detected at 2-sigma significance (duty cycle) are 11.3%, 38.8%, 16.9%, 49.2%, and 18.7% for LMC 2009a, RS Oph, KT Eri, V339 Del, and Cal 83, respectively. The respective highest duty cycles found in a single observation are 38.1%, 74.5%, 61.4%, 67.8%, and 61.8%., Comment: accepted for publication in A&A
Published: 2015
Full Text: View/download PDF

22. A Methodology to Fulfill Environmental Requirements for Implementing Projects with Subsea Systems in Campos Basin Sensitive Regions

Author: dos Santos, A. B., additional, de Freitas, L. R., additional, Vigna, M. F., additional, and Schwarz, G. P., additional
Published: 2024
Full Text: View/download PDF

23. The Quasar Catalogue for S-PLUS DR4 (QuCatS) and the estimation of photometric redshifts

Author: Nakazono, L, primary, Valença, R R, additional, Soares, G, additional, Izbicki, R, additional, Ivezić, Ž, additional, Lima, E V R, additional, Hirata, N S T, additional, Sodré, L, additional, Overzier, R, additional, Almeida-Fernandes, F, additional, Schwarz, G B Oliveira, additional, Schoenell, W, additional, Kanaan, A, additional, Ribeiro, T, additional, and de Oliveira, C Mendes, additional
Published: 2024
Full Text: View/download PDF

24. CIP2A regulates MYC translation (via its 5′UTR) in colorectal cancer

Author: Denk, S., Schmidt, S., Schurr, Y., Schwarz, G., Schote, F., Diefenbacher, M., Armendariz, C., Dejure, F., Eilers, M., and Wiegering, Armin
Published: 2021
Full Text: View/download PDF

25. Managing Complex Healthcare Change: A Qualitative Exploration of Current Practice in New South Wales, Australia

Author: Le-Dao H, Chauhan A, Walpola R, Fischer S, Schwarz G, Minbashian A, Munro A, D'Arcy E, Allan J, and Harrison R
Subjects: transformation, leadership, capacity, capability, culture, change management, Public aspects of medicine, RA1-1270
Abstract: Huong Le-Dao,1 Ashfaq Chauhan,1 Ramesh Walpola,1 Sarah Fischer,2,3 Gavin Schwarz,4 Amirali Minbashian,4 Alice Munro,5 Ellie D’Arcy,5 Julaine Allan,6 Reema Harrison1 1School of Population Health, University of New South Wales, Sydney, New South Wales, 2052, Australia; 2Clinical Excellence Commission, New South Wales Health, Sydney, 2065, Australia; 3School of Psychology, Deakin University, Sydney, 3220, Australia; 4Business School, University of New South Wales, Sydney, New South Wales, 2052, Australia; 5Western New South Wales Local Health District, Bathurst, New South Wales 2795, Australia; 6School of Health and Society, University of Wollongong, Wollongong, New South Wales 2500, AustraliaCorrespondence: Reema Harrison Room 229, School of Population HealthUniversity of New South Wales, 2052, AustraliaTel +61 2 93853324Email reema.harrison@unsw.edu.auPurpose: As the cost of healthcare continues to rise, healthcare organizations internationally are seeking long-term solutions to eradicate inefficiency, achieve value-based healthcare, and minimize hospital inpatient services. This requires transformational change in healthcare organizations, and associated change management and leadership capability at multiple levels. Despite the critical need for effective change leadership and management in healthcare, limited evidence exists that this currently occurs in addition to the capability and capacity for managing change in health systems.Methods: Semi-structured interviews were undertaken with 16 healthcare managers and leaders at a range of levels in nine healthcare organizations across the public health system of one Australian state (New South Wales), including metropolitan, regional and rural geographical areas. Thematic content analysis was undertaken with the emergent data.Results: Four key themes emerged from the data: 1) lack of adoption of frameworks and methods for change management for any scope or scale of change, 2) inadequate resources for delivering, managing and leading change, 3) insufficient leadership, capacity and capability in managing change, and 4) the need for support and culture that supports change at all levels of the system.Conclusion: Ensuring dedicated resources for change and sufficient capacity and capability amongst health professionals and managers at every level in a health system are required for effective management of change. An enabling culture for change, supported by adequate education and training in change leadership and management are critical in order for the benefits of health service and system changes to be realised.Keywords: transformation, leadership, capacity, capability, culture, change management
Published: 2020

26. Concentration distribution of more than 100 drugs and metabolites in forensic hair samples

Author: Musshoff, F., Schwarz, G., Sachs, H., Skopp, G., and Franz, T.
Published: 2020
Full Text: View/download PDF

27. Obscuration effects in Super-Soft-Source X-ray spectra

Author: Ness, J. -U., Osborne, J. P., Henze, M., Dobrotka, A., Drake, J. J., Ribeiro, V. A. R. M., Starrfield, S., Kuulkers, E., Behar, E., Hernanz, M., Schwarz, G., Page, K. L., Beardmore, A., and Bode, M. F.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: Super-Soft-Source (SSS) X-ray spectra are blackbody-like spectra with effective temperatures ~3-7x10^5 K and luminosities of 10^{35-38} erg/s. SSS grating spectra display atmospheric absorption lines. Radiation transport atmosphere models can be used to derive physical parameters, but more sophisticated models are required. We bypass the complications of spectral models and concentrate on the data in a comparative, qualitative study. We inspect all available X-ray grating SSS spectra to determine systematic, model-independent trends. We use comparative plots of spectra of different systems to find common and different features. The results are interpreted in the context of system parameters obtained from the literature. We find two distinct types of SSS spectra which we name SSa and SSe. Their main observational characteristics are either clearly visible absorption lines or emission lines, respectively, while both types contain atmospheric continuum emission. SSe may be obscured SSa systems, which is supported by similarities between SSe and SSa with obscured and unobscured AGN, respectively. Further, we find all known or suspected high-inclination systems to emit permanently in an SSe state. Some sources are found to transition between SSa and SSe states, becoming SSe when fainter. SSS spectra are subject to various occultation processes. In Cal 87, the accretion disc blocks the central hot source when viewed edge on. In novae, the accretion disc may have been destroyed during the initial explosion but could have reformed by the time of the SSS phase. In addition, clumpy ejecta may lead to temporary obscuration events. The emission lines originate from reprocessed emission in the accretion disc, its wind or further out in clumpy ejecta while Thomson scattering allows continuum emission to be visible also during total obscuration of the central hot source., Comment: A&A in press, 16 pages, 10 figures, 2 tables
Published: 2013
Full Text: View/download PDF

28. The spectroscopic evolution of the $\gamma$-ray emitting classical nova Nova Mon 2012. I. Implications for the ONe subclass of classical novae

Author: Shore, S. N., Aquino, I. De Gennaro, Schwarz, G. J., Augusteijn, T., Cheung, C. C., Walter, F. M., and Starrfield, S.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Nova Mon 2012 was the first classical nova to be detected as a high energy $\gamma$-ray transient, by Fermi-LAT, before its optical discovery. We study a time sequence of high resolution optical echelle spectra (Nordic Optical Telescope) and contemporaneous NOT, STIS UV, and CHIRON echelle spectra (Nov 20/21/22). We use [O III] and H$\beta$ line fluxs to constrain the properties of the ejecta. We derive the structure from the optical and UV line profiles and compare our measured line fluxes for with predictions using Cloudy with abundances from other ONe novae. Mon 2012 is confirmed as an ONe nova. We find E(B-V)=0.85$\pm$0.05 and hydrogen column density $\approx 5\times 10^{21}$ cm$^{-2}$. The corrected continuum luminosity is nearly the same in the entire observed energy range as V1974 Cyg, V382 Mon, and Nova LMC 2000 at the same epoch after outburst. The distance, about 3.6 kpc, is quite similar to V1974 Cyg. The line profiles can be modeled using an axisymmetric bipolar geometry for the ejecta with various inclinations of the axis to the line of sight, 60 \le i \le 80 degrees, an opening angle of \approx$70 deg, inner radius $\Delta R/R(t)\approx 0.4$ for permitted lines and less filled for forbidden lines. The filling factor $f\approx 0.1-0.3$ implying M(ejecta) $\leq 6\times 10^{-5}$M$_\odot$. The ONe novae appear to comprise a single physical class with bipolar high mass ejecta, similarly enhanced abundances, and a common spectroscopic evolution within a narrow range of luminosities. The detected $\gamma$-ray emission may be a generic phenomenon, common to all ONe novae, possibly to all classical novae, and connected with acceleration and emission processes within the ejecta (abstract severely truncated)., Comment: Submitted to A&A 9/1/2013; Accepted 27/2/2013 (in press)
Published: 2013
Full Text: View/download PDF

29. The spectroscopic evolution of the recurrent nova T Pyxidis during its 2011 outburst. II.The optically thin phase and the structure of the ejecta in recurrent novae

Author: Shore, S. N., Schwarz, G. J., Aquino, I. De Gennaro, Augusteijn, T., Walter, F. M., Starrfield, S., and Sion, E. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We continue our study of the physical properties of the recurrent nova T Pyx, focussing on the structure of the ejecta in the nebular stage of expansion during the 2011 outburst. The nova was observed contemporaneously with the Nordic Optical Telescope (NOT), at high resolution spectroscopic resolution (R ~ 65000) on 2011 Oct. 11 and 2012 Apr. 8 (without absolute flux calibration), and with the Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope, at high resolution (R ~ 30000) on 2011 Oct. 10 and 2012 Mar. 28 (absolute fluxes). We use standard plasma diagnostics (e.g. [O III] and [N II] line ratios and the H$\beta$ line fluxes) to constrain electron densities and temperatures. Using Monte Carlo modeling of the ejecta, we derive the structure and filling factor from comparisons to the optical and ultraviolet line profiles. The ejecta can be modeled using an axisymmetric conical -- bipolar -- geometry with a low inclination of the axis to the line of sight, i=15+/-5 degrees, compatible with published results from high angular resolution optical spectro-interferometry. The structure is similar to that observed in the other short orbital period recurrent novae during their nebular stages. We show that the electron density scales as $t^{-3}$ as expected from a ballistically ejected constant mass shell; there is no need to invoke a continuing mass outflow following the eruption. The derived mass for the ejecta with filling factor f ~ 3%, M_ej ~ 2E-6$M_sun is similar to that obtained for other recurrent nova ejecta but inconsistent with the previously reported extended optically thick epoch of the explosion. We suggest that the system underwent a common envelope phase following the explosion that produced the recombination event. Implications for the dynamics of the recurrent novae are discussed. (truncated), Comment: accepted for publication in A&A (10 Nov. 2012), 10 pgs, 16 figs
Published: 2012
Full Text: View/download PDF

30. Swift observations of the March 2011 outburst of the cataclysmic variable NSV 1436: a probable dwarf nova (Research Note)

Author: Osborne, J. P., Page, K. L., Henden, A. A., Ness, J. -U., Bode, M. F., Schwarz, G. J., Starrfield, S., Drake, J. J., Kuulkers, E., and Beardmore, A. P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The March 2011 outburst of the poorly-studied cataclysmic variable NSV 1436 offered an opportunity to decide between dwarf nova and recurrent nova classifications. We use seven daily observations in the X-ray and UV by the Swift satellite, together with AAVSO V photometry, to characterise the outburst and decline behaviour. The short optical outburst coincided with a faint and relatively soft X-ray state, whereas in decline to fainter optical magnitudes the X-ray source was harder and brighter. These attributes, and the modest optical outburst amplitude, indicate that this was a dwarf nova outburst and not a recurrent nova. The rapid optical fading suggests an orbital period below 2 hours., Comment: Accepted for publication in A&A
Published: 2011
Full Text: View/download PDF

31. A very luminous, highly extinguished, very fast nova - V1721 Aquilae

Author: Hounsell, R., Darnley, M. J., Bode, M. F., Harman, D. J., Helton, L. A., and Schwarz, G. J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: Fast novae are primarily located within the plane of the Galaxy, slow novae are found within its bulge. Because of high interstellar extinction along the line of sight many novae lying close to the plane are missed and only the brightest seen. One nova lying very close to the Galactic plane is V1721 Aquilae, discovered in outburst on 2008 September 22. Spectra obtained 2.69 days after outburst revealed very high expansion velocities (FWHM ~6450 km/s). In this paper we have used available pre- and post-outburst photometry and post-outburst spectroscopy to conclude that the object is a very fast, luminous, and highly extinguished A_V=11.6+/-0.2) nova system with an average ejection velocity of ~3400 km/s. Pre-outburst near-IR colours from 2MASS indicate that at quiescence the object is similar to many quiescent CNe and appears to have a main sequence/sub-giant secondary rather than a giant. Based on the speed of decline of the nova and its emission line profiles we hypothesise that the axis ratio of the nova ejecta is ~1.4 and that its inclination is such that the central binary accretion disc is face-on to the observer. The accretion disc's blue contribution to the system's near-IR quiescent colours may be significant. Simple models of the nova ejecta have been constructed using the morphological modelling code XS5, and the results support the above hypothesis. Spectral classification of this object has been difficult owing to low S/N levels and high extinction, which has eliminated all evidence of any He/N or FeII emission within the spectra. We suggest two possibilities for the nature of V1721 Aql: that it is a U Sco type RN with a sub-giant secondary or, less likely, that it is a highly energetic bright and fast classical nova with a main sequence secondary. Future monitoring of the object for possible RN episodes may be worthwhile, as would archival searches for previous outbursts., Comment: 9 pages 10 figures, accepted for publication in A&A. Abstract has been slightly shortened from published version
Published: 2011
Full Text: View/download PDF

32. XMM-Newton X-ray and UV observations of the fast nova V2491 Cyg during the supersoft source phase

Author: Ness, J. -U., Osborne, J. P., Dobrotka, A., Page, K. L., Drake, J. J., Pinto, C., Detmers, R. G., Schwarz, G., Bode, M. F., Beardmore, A. P., Starrfield, S., Hernanz, M., Sala, G., Krautter, J., and Woodward, C. E.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Two XMM observations of the fast classical nova V2491Cyg were carried out on days 39.93 and 49.62 after discovery, during the supersoft source (SSS) phase, yielding simultaneous X-ray and UV light curves and high-resolution X-ray spectra. The first X-ray light curve is highly variable with periodic oscillations (37.2 min) after an extended dip of factor of three lasting ~3 hours. The cause of the dip is currently unexplained and could have the same origin as similar events in V4743Sgr and RSOph, as it occurred on the same time scale. The 37-min period is not present during the dip and also not in the second observation. The UV light curves are variable but contain no dips and no period. High-resolution X-ray spectra are presented for 4 intervals of different intensity. All spectra are atmospheric continua with absorption lines and absorption edges. Interstellar lines of OI and NI are seen at their rest wavelengths, and a large number of high-ionization absorption lines are found at blue shifts indicating an expansion velocity of 3000-3400 km/s, which does not change significantly during the epochs of observation. Comparisons with the slower nova V4743Sgr and the symbiotic recurrent nova RSOph are presented. The SSS spectrum of V4743Sgr is much softer with broader and more complex photospheric absorption lines. Meanwhile, the absorption lines in RSOph are as narrow as in V2491Cyg, but they are less blue shifted. A remarkable similarity in the continua of V2491Cyg and RSOph is found. The only differences are smaller line shifts and additional emission lines in RSOph that are related to a dense stellar wind from the evolved companion. Three unidentified absorption lines are present in the X-ray spectra of all three novae, with rest wavelengths 26.05AA, 29.45AA, and 30.0AA. No satisfactory spectral model is currently available for the soft X-ray spectra of novae in outburst., Comment: accepted. 18 pages, 14 figures, 5 tables; Astrophysical Journals (ApJ) 2011
Published: 2011
Full Text: View/download PDF

33. The Super-Soft X-ray Phase of Nova RS Ophiuchi 2006

Author: Osborne, J. P., Page, K. L., Beardmore, A. P., Bode, M. F., Goad, M. R., O'Brien, T. J., Starrfield, S., Rauch, T., Ness, J. -U., Krautter, J., Schwarz, G., Burrows, D. N., Gehrels, N., Drake, J. J., Evans, A., and Eyres, S. P. S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Swift X-ray observations of the ~60 day super-soft phase of the recurrent nova RS Ophiuchi 2006 show the progress of nuclear burning on the white dwarf in exquisite detail. First seen 26 days after the optical outburst, this phase started with extreme variability likely due to variable absorption, although intrinsic white dwarf variations are not excluded. About 32 days later, a steady decline in count-rate set in. NLTE model atmosphere spectral fits during the super-soft phase show that the effective temperature of the white dwarf increases from ~65 eV to ~90 eV during the extreme variability phase, falling slowly after about day 60 and more rapidly after day 80. The bolometric luminosity is seen to be approximately constant and close to Eddington from day 45 up to day 60, the subsequent decline possibly signalling the end of extensive nuclear burning. Before the decline, a multiply-periodic, ~35 s modulation of the soft X-rays was present and may be the signature of a nuclear fusion driven instability. Our measurements are consistent with a white dwarf mass near the Chandrasekhar limit; combined with a deduced accumulation of mass transferred from its binary companion, this leads us to suggest RS Oph is a strong candidate for a future supernova explosion. The main uncertainty now is whether the WD is the CO type necessary for a SN Ia. This may be confirmed by detailed abundance analyses of spectroscopic data from the outbursts., Comment: Accepted for publication in ApJ
Published: 2010
Full Text: View/download PDF

34. X-ray and UV observations of nova V598 Puppis between 147 and 255 days after outburst

Author: Page, K. L., Osborne, J. P., Read, A. M., Evans, P. A., Ness, J. -U., Beardmore, A. P., Bode, M., Schwarz, G. J., and Starrfield, S.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Aims: The launch of Swift has allowed many more novae to be observed regularly over the X-ray band. Such X-ray observations of novae can reveal ejecta shocks and the nuclear burning white dwarf, allowing estimates to be made of the ejecta velocity. Methods: We analyse XMM-Newton and Swift X-ray and UV observations of the nova V598 Pup, which was initially discovered in the XMM-Newton slew survey. These data were obtained between 147 and 255 days after the nova outburst, and are compared with the earlier, brighter slew detection. Results: The X-ray spectrum consists of a super-soft source, with the soft emission becoming hotter and much fainter between days ~147 and ~172 after the outburst, and a more slowly declining optically thin component, formed by shocks with kT ~ 200-800 eV (corresponding to velocities of 400-800 km s^-1). The main super-soft phase had a duration of less than 130 days. The Reflection Grating Spectrometer data show evidence of emission lines consistent with optically thin emission of kT ~100 eV and place a limit on the density of the surrounding medium of log(n_e/cm^-3) < 10.4 at the 90 % level. The UV emission is variable over short timescales and fades by at least one magnitude (at lambda ~ 2246-2600 angstrom) between days 169 and 255., Comment: 6 pages, 5 figures, accepted for publication in A&A
Published: 2009
Full Text: View/download PDF

35. Swift observations of the X-ray and UV evolution of V2491 Cyg (Nova Cyg 2008 No. 2)

Author: Page, K. L., Osborne, J. P., Evans, P. A., Wynn, G. A., Beardmore, A. P., Starling, R. L. C., Bode, M. F., Ibarra, A., Kuulkers, E., Ness, J. -U., and Schwarz, G. J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present extensive, high-density Swift observations of V2491 Cyg (Nova Cyg 2008 No. 2). Observing the X-ray emission from only one day after the nova discovery, the source is followed through the initial brightening, the Super-Soft Source phase and back to the pre-outburst flux level. The evolution of the spectrum throughout the outburst is demonstrated. The UV and X-ray light-curves follow very different paths, although changes occur in them around the same times, indicating a link between the bands. Flickering in the late-time X-ray data indicates the resumption of accretion. We show that if the white dwarf is magnetic, it would be among the most magnetic known; the lack of a periodic signal in our later data argues against a magnetic white dwarf, however. We also discuss the possibility that V2491 Cyg is a recurrent nova, providing recurrence timescale estimates., Comment: 12 pages, 8 figure (2 in colour), accepted for publication in MNRAS
Published: 2009
Full Text: View/download PDF

36. Weaning from mechanical ventilation in intensive care units across 50 countries (WEAN SAFE): a multicentre, prospective, observational cohort study

Author: Pham, T, Heunks, L, Bellani, G, Madotto, F, Aragao, I, Beduneau, G, Goligher, E, Grasselli, G, Laake, J, Mancebo, J, Penuelas, O, Piquilloud, L, Pesenti, A, Wunsch, H, van Haren, F, Brochard, L, Laffey, J, Abrough, F, Acharya, S, Amin, P, Arabi, Y, Bauer, P, Beitler, J, Berkius, J, Bugedo, G, Camporota, L, Cerny, V, Cho, Y, Clarkson, K, Estenssoro, E, Gritsan, A, Hashemian, S, Hermans, G, Jovanovic, B, Kurahashi, K, Matamis, D, Moerer, O, Molnar, Z, Ozyilmaz, E, Panka, B, Papali, A, Perbet, S, Qiu, H, Razek, A, Rittayamai, N, Roldan, R, Serpa Neto, A, Szuldrzynski, K, Talmor, D, Tomescu, D, Villagomez, A, Zeggwagh, A, Abe, T, Aboshady, A, Acampo-de Jong, M, Adderley, J, Adiguzel, N, Agrawal, V, Aguilar, G, Aguirre, G, Aguirre-Bermeo, H, Ahlstrom, B, Akbas, T, Akker, M, Al Sadeh, G, Alamri, S, Algaba, A, Ali, M, Aliberti, A, Allegue, J, Alvarez, D, Amador, J, Andersen, F, Ansari, S, Apichatbutr, Y, Apostolopoulou, O, Arellano, D, Arica, M, Arikan, H, Arinaga, K, Arnal, J, Asano, K, Asin-Corrochano, M, Avalos Cabrera, J, Avila Fuentes, S, Aydemir, S, Aygencel, G, Azevedo, L, Bacakoglu, F, Badie, J, Baedorf Kassis, E, Bai, G, Balaraj, G, Ballico, B, Banner-Goodspeed, V, Banwarie, P, Barbieri, R, Baronia, A, Barrett, J, Barrot, L, Barrueco-Francioni, J, Barry, J, Bawangade, H, Beavis, S, Beck, E, Beehre, N, Belenguer Muncharaz, A, Belliato, M, Bellissima, A, Beltramelli, R, Ben Souissi, A, Benitez-Cano, A, Benlamin, M, Benslama, A, Bento, L, Benvenuti, D, Bernabe, L, Bersten, A, Berta, G, Bertini, P, Bertram-Ralph, E, Besbes, M, Bettini, L, Beuret, P, Bewley, J, Bezzi, M, Bhakhtiani, L, Bhandary, R, Bhowmick, K, Bihari, S, Bissett, B, Blythe, D, Bocher, S, Boedjawan, N, Bojanowski, C, Boni, E, Boraso, S, Borelli, M, Borello, S, Borislavova, M, Bosma, K, Bottiroli, M, Boyd, O, Bozbay, S, Briva, A, Bruel, C, Bruni, A, Buehner, U, Bulpa, P, Burt, K, Buscot, M, Buttera, S, Cabrera, J, Caccese, R, Caironi, P, Canchos Gutierrez, I, Canedo, N, Cani, A, Cappellini, I, Carazo, J, Cardonnet, L, Carpio, D, Carriedo, D, Carrillo, R, Carvalho, J, Caser, E, Castelli, A, Castillo Quintero, M, Castro, H, Catorze, N, Cengiz, M, Cereijo, E, Ceunen, H, Chaintoutis, C, Chang, Y, Chaparro, G, Chapman, C, Chau, S, Chavez, C, Chelazzi, C, Chelly, J, Chemouni, F, Chen, K, Chena, A, Chiarandini, P, Chilton, P, Chiumello, D, Chou-Lie, Y, Chudeau, N, Cinel, I, Cinnella, G, Clark, M, Clark, T, Clementi, S, Coaguila, L, Codecido, A, Collins, A, Colombo, R, Conde, J, Consales, G, Cook, T, Coppadoro, A, Cornejo, R, Cortegiani, A, Coxo, C, Cracchiolo, A, Crespo Ramirez, M, Crova, P, Cruz, J, Cubattoli, L, Cukurova, Z, Curto, F, Czempik, P, D'Andrea, R, da Silva Ramos, F, Dangers, L, Danguy des Deserts, M, Danin, P, Dantas, F, Daubin, C, Dawei, W, de Haro, C, de Jesus Montelongo, F, De Mendoza, D, de Pablo, R, De Pascale, G, De Rosa, S, Decavele, M, Declercq, P, Deicas, A, del Carmen Campos Moreno, M, Dellamonica, J, Delmas, B, Demirkiran, O, Demirkiran, H, Dendane, T, di Mussi, R, Diakaki, C, Diaz, A, Diaz, W, Dikmen, Y, Dimoula, A, Doble, P, Doha, N, Domingos, G, Dres, M, Dries, D, Duggal, A, Duke, G, Dunts, P, Dybwik, K, Dykyy, M, Eckert, P, Efe, S, Elatrous, S, Elay, G, Elmaryul, A, Elsaadany, M, Elsayed, H, Elsayed, S, Emery, M, Ena, S, Eng, K, Englert, J, Erdogan, E, Ergin Ozcan, P, Eroglu, E, Escobar, M, Esen, F, Esen Tekeli, A, Esquivel, A, Esquivel Gallegos, H, Ezzouine, H, Facchini, A, Faheem, M, Fanelli, V, Farina, M, Fartoukh, M, Fehrle, L, Feng, F, Feng, Y, Fernandez, I, Fernandez, B, Fernandez-Rodriguez, M, Ferrando, C, Ferreira da Silva, M, Ferreruela, M, Ferrier, J, Flamm Zamorano, M, Flood, L, Floris, L, Fluckiger, M, Forteza, C, Fortunato, A, Frans, E, Frattari, A, Fredes, S, Frenzel, T, Fumagalli, R, Furche, M, Fusari, M, Fysh, E, Galeas-Lopez, J, Galerneau, L, Garcia, A, Garcia, M, Garcia, E, Garcia Olivares, P, Garlicki, J, Garnero, A, Garofalo, E, Gautam, P, Gazenkampf, A, Gelinotte, S, Gelormini, D, Ghrenassia, E, Giacomucci, A, Giannoni, R, Gigante, A, Glober, N, Gnesin, P, Gollo, Y, Gomaa, D, Gomero Paredes, R, Gomes, R, Gomez, R, Gomez, O, Gomez, A, Gondim, L, Gonzalez, M, Gonzalez, I, Gonzalez-Castro, A, Gordillo Romero, O, Gordo, F, Gouin, P, Graf Santos, J, Grainne, R, Grando, M, Granov Grabovica, S, Grasso, S, Grasso, R, Grimmer, L, Grissom, C, Gu, Q, Guan, X, Guarracino, F, Guasch, N, Guatteri, L, Gueret, R, Guerin, C, Guerot, E, Guitard, P, Gul, F, Gumus, A, Gurjar, M, Gutierrez, P, Hachimi, A, Hadzibegovic, A, Hagan, S, Hammel, C, Han Song, J, Hanlon, G, Heines, S, Henriksson, J, Herbrecht, J, Heredia Orbegoso, G, Hermon, A, Hernandez, R, Hernandez, C, Herrera, L, Herrera-Gutierrez, M, Hidalgo, J, Hill, D, Holmquist, D, Homez, M, Hongtao, X, Hormis, A, Horner, D, Hornos, M, Hou, M, House, S, Housni, B, Hugill, K, Humphreys, S, Humbert, L, Hunter, S, Hwa Young, L, Iezzi, N, Ilutovich, S, Inal, V, Innes, R, Ioannides, P, Iotti, G, Ippolito, M, Irie, H, Iriyama, H, Itagaki, T, Izura, J, Izza, S, Jabeen, R, Jamaati, H, Jamadarkhana, S, Jamoussi, A, Jankowski, M, Jaramillo, L, Jeon, K, Jeong Lee, S, Jeswani, D, Jha, S, Jiang, L, Jing, C, Jochmans, S, Johnstad, B, Jongmin, L, Joret, A, Junhasavasdikul, D, Jurado, M, Kam, E, Kamohara, H, Kane, C, Kara, I, Karakurt, S, Karnjanarachata, C, Kataoka, J, Katayama, S, Kaushik, S, Kelebek Girgin, N, Kerr, K, Kerslake, I, Khairnar, P, Khalid, A, Khan, A, Khanna, A, Khorasanee, R, Kienhorst, D, Kirakli, C, Knafelj, R, Kol, M, Kongpolprom, N, Kopitko, C, Korkmaz Ekren, P, Kubisz-Pudelko, A, Kulcsar, Z, Kumasawa, J, Kuriyama, A, Kutchak, F, Labarca, E, Labat, F, Laborda, C, Laca Barrera, M, Lagache, L, Landaverde Lopez, A, Lanspa, M, Lascari, V, Le Meur, M, Lee, S, Lee, Y, Lee, J, Lee, W, Legernaes, T, Leiner, T, Lemiale, V, Leonor, T, Lepper, P, Li, D, Li, H, Li, O, Lima, A, Lind, D, Litton, E, Liu, N, Liu, L, Liu, J, Llitjos, J, Llorente, B, Lopez, R, Lopez, C, Lopez Nava, C, Lovazzano, P, Lu, M, Lucchese, F, Lugano, M, Lugo Goytia, G, Luo, H, Lynch, C, Macheda, S, Madrigal Robles, V, Maggiore, S, Magret Iglesias, M, Malaga, P, Mallapura Maheswarappa, H, Malpartida, G, Malyarchikov, A, Mansson, H, Manzano, A, Marey, I, Marin, N, Marin, M, Markman, E, Martin, F, Martin, A, Martin Dal Gesso, C, Martinez, F, Martinez-Fidalgo, C, Martin-Loeches, I, Mas, A, Masaaki, S, Maseda, E, Massa, E, Mattsson, A, Maugeri, J, Mccredie, V, Mccullough, J, Mcguinness, S, Mckown, A, Medve, L, Mei, C, Mellado Artigas, R, Mendes, V, Mervat, M, Michaux, I, Mikhaeil, M, Milagros, O, Milet, I, Millan, M, Minwei, Z, Mirabella, L, Mishra, S, Mistraletti, G, Mochizuki, K, Moghal, A, Mojoli, F, Molin, A, Montiel, R, Montini, L, Monza, G, Mora Aznar, M, Morakul, S, Morales, M, Moreno Torres, D, Morocho Tutillo, D, Motherway, C, Mouhssine, D, Mouloudi, E, Munoz, T, Munoz de Cabo, C, Mustafa, M, Muthuchellappan, R, Muthukrishnan, M, Muttini, S, Nagata, I, Nahar, D, Nakanishi, M, Nakayama, I, Namendys-Silva, S, Nanchal, R, Nandakumar, S, Nasi, A, Nasir, K, Navalesi, P, Naz Aslam, T, Nga Phan, T, Nichol, A, Niiyama, S, Nikolakopoulou, S, Nikolic, E, Nitta, K, Noc, M, Nonas, S, Nseir, S, Nur Soyturk, A, Obata, Y, Oeckler, R, Oguchi, M, Ohshimo, S, Oikonomou, M, Ojados, A, Oliveira, M, Oliveira Filho, W, Oliveri, C, Olmos, A, Omura, K, Orlandi, M, Orsenigo, F, Ortiz-Ruiz De Gordoa, L, Ota, K, Ovalle Olmos, R, Oveges, N, Oziemski, P, Ozkan Kuscu, O, Pachas Alvarado, F, Pagella, G, Palaniswamy, V, Palazon Sanchez, E, Palmese, S, Pan, G, Pan, W, Papanikolaou, M, Papavasilopoulou, T, Parekh, A, Parke, R, Parrilla, F, Parrilla, D, Pasha, T, Pasin, L, Patao, L, Patel, M, Patel, G, Pati, B, Patil, J, Pattnaik, S, Paul, D, Pavesi, M, Pavlotsky, V, Paz, G, Paz, E, Pecci, E, Pellegrini, C, Pena Padilla, A, Perchiazzi, G, Pereira, T, Pereira, V, Perez, M, Perez Calvo, C, Perez Cheng, M, Perez Maita, R, Perez-Araos, R, Perez-Teran, P, Perez-Torres, D, Perkins, G, Persona, P, Petnak, T, Petrova, M, Philippart, F, Picetti, E, Pierucci, E, Piervincenzi, E, Pinciroli, R, Pintado, M, Piraino, T, Piras, S, Piras, C, Pirompanich, P, Pisani, L, Platas, E, Plotnikow, G, Porras, W, Porta, V, Portilla, M, Portugal, J, Povoa, P, Prat, G, Pratto, R, Preda, G, Prieto, I, Prol-Silva, E, Pugh, R, Qi, Y, Qian, C, Qin, T, Qu, H, Quintana, T, Quispe Sierra, R, Quispe Soto, R, Rabbani, R, Rabee, M, Rabie, A, Rahe Pereira, M, Rai, A, Raj Ashok, S, Rajab, M, Ramdhani, N, Ramey, E, Ranieri, M, Rathod, D, Ray, B, Redwanul Huq, S, Regli, A, Reina, R, Resano Sarmiento, N, Reynaud, F, Rialp, G, Ricart, P, Rice, T, Richardson, A, Rieder, M, Rinket, M, Rios, F, Risso Vazquez, A, Riva, I, Rivette, M, Roca, O, Roche-Campo, F, Rodriguez, C, Rodriguez, G, Rodriguez Gonzalez, D, Rodriguez Tucto, X, Rogers, A, Romano, M, Rortveit, L, Rose, A, Roux, D, Rouze, A, Rubatto Birri, P, Ruilan, W, Ruiz Robledo, A, Ruiz-Aguilar, A, Sadahiro, T, Saez, I, Sagardia, J, Saha, R, Saiphoklang, N, Saito, S, Salem, M, Sales, G, Salgado, P, Samavedam, S, Sami Mebazaa, M, Samuelsson, L, San Juan Roman, N, Sanchez, P, Sanchez-Ballesteros, J, Sandoval, Y, Sani, E, Santos, M, Santos, C, Sanui, M, Saravanabavan, L, Sari, S, Sarkany, A, Sauneuf, B, Savioli, M, Sazak, H, Scano, R, Schneider, F, Schortgen, F, Schultz, M, Schwarz, G, Seckin Yucesoy, F, Seely, A, Seiler, F, Seker Tekdos, Y, Seok Chan, K, Serano, L, Serednicki, W, Setten, M, Shah, A, Shah, B, Shang, Y, Shanmugasundaram, P, Shapovalov, K, Shebl, E, Shiga, T, Shime, N, Shin, P, Short, J, Shuhua, C, Siddiqui, S, Silesky Jimenez, J, Silva, D, Silva Sales, B, Simons, K, Sjobo, B, Slessor, D, Smiechowicz, J, Smischney, N, Smith, P, Smith, T, Smith, M, Snape, S, Snyman, L, Soetens, F, Sook Hong, K, Sosa Medellin, M, Soto, G, Souloy, X, Sousa, E, Sovatzis, S, Sozutek, D, Spadaro, S, Spagnoli, M, Spangfors, M, Spittle, N, Spivey, M, Stapleton, A, Stefanovic, B, Stephenson, L, Stevenson, E, Strand, K, Strano, M, Straus, S, Sun, C, Sun, R, Sundaram, V, Sunpark, T, Surlemont, E, Sutherasan, Y, Szabo, Z, Tainter, C, Takaba, A, Tallott, M, Tamasato, T, Tang, Z, Tangsujaritvijit, V, Taniguchi, L, Taniguchi, D, Tarantino, F, Teerapuncharoen, K, Temprano, S, Terragni, P, Terzi, N, Thakur, A, Theerawit, P, Thille, A, Thomas, M, Thungtitigul, P, Thyrault, M, Tilouch, N, Timenetsky, K, Tirapu, J, Todeschini, M, Tomas, R, Tomaszewski, C, Tonetti, T, Tonnelier, A, Trinder, J, Trongtrakul, K, Truwit, J, Tsuei, B, Tulaimat, A, Turan, S, Turkoglu, M, Tyagi, S, Ubeda, A, Vagginelli, F, Valenti, M, Vallverdu, I, Van Axel, A, van den Hul, I, van der Hoeven, H, Van Der Meer, N, Vanhoof, M, Vargas-Ordonez, M, Vaschetto, R, Vascotto, E, Vatsik, M, Vaz, A, Vazquez-Sanchez, A, Ventura, S, Vermeijden, J, Vidal, A, Vieira, J, Vilela Costa Pinto, B, Villagra, A, Villegas Succar, C, Vinorum, O, Vitale, G, Vj, R, Vochin, A, Voiriot, G, Volta, C, von Seth, M, Wajdi, M, Walsh, D, Wang, S, Wardi, G, Ween-Velken, N, Wei, B, Weller, D, Welsh, D, Welters, I, Wert, M, Whiteley, S, Wilby, E, Williams, E, Williams, K, Wilson, A, Wojtas, J, Won Huh, J, Wrathall, D, Wright, C, Wu, J, Xi, G, Xing, Z, Xu, H, Yamamoto, K, Yan, J, Yanez, J, Yang, X, Yates, E, Yazicioglu Mocin, O, Ye, Z, Yildirim, F, Yoshida, N, Yoshido, H, Young Lee, B, Yu, R, Yu, G, Yu, T, Yuan, B, Yuangtrakul, N, Yumoto, T, Yun, X, Zakalik, G, Zaki, A, Zalba-Etayo, B, Zambon, M, Zang, B, Zani, G, Zarka, J, Zerbi, S, Zerman, A, Zetterquist, H, Zhang, J, Zhang, H, Zhang, W, Zhang, G, Zhao, H, Zheng, J, Zhu, B, Zumaran, R, Pham T., Heunks L., Bellani G., Madotto F., Aragao I., Beduneau G., Goligher E. C., Grasselli G., Laake J. H., Mancebo J., Penuelas O., Piquilloud L., Pesenti A., Wunsch H., van Haren F., Brochard L., Laffey J. G., Abrough F., Acharya S. P., Amin P., Arabi Y., Bauer P., Beitler J., Berkius J., Bugedo G., Camporota L., Cerny V., Cho Y. -J., Clarkson K., Estenssoro E., Goligher E., Gritsan A., Hashemian S. M., Hermans G., Heunks L. M., Jovanovic B., Kurahashi K., Matamis D., Moerer O., Molnar Z., Ozyilmaz E., Panka B., Papali A., Perbet S., Qiu H., Razek A. A., Rittayamai N., Roldan R., Serpa Neto A., Szuldrzynski K., Talmor D., Tomescu D., Villagomez A., Zeggwagh A. A., Abe T., Aboshady A., Acampo-de Jong M., Acharya S., Adderley J., Adiguzel N., Agrawal V. K., Aguilar G., Aguirre G., Aguirre-Bermeo H., Ahlstrom B., Akbas T., Akker M., Al Sadeh G., Alamri S., Algaba A., Ali M., Aliberti A., Allegue J. M., Alvarez D., Amador J., Andersen F. H., Ansari S., Apichatbutr Y., Apostolopoulou O., Arellano D., Arica M., Arikan H., Arinaga K., Arnal J. -M., Asano K., Asin-Corrochano M., Avalos Cabrera J. M., Avila Fuentes S., Aydemir S., Aygencel G., Azevedo L., Bacakoglu F., Badie J., Baedorf Kassis E., Bai G., Balaraj G., Ballico B., Banner-Goodspeed V., Banwarie P., Barbieri R., Baronia A., Barrett J., Barrot L., Barrueco-Francioni J. E., Barry J., Bawangade H., Beavis S., Beck E., Beehre N., Belenguer Muncharaz A., Belliato M., Bellissima A., Beltramelli R., Ben Souissi A., Benitez-Cano A., Benlamin M., Benslama A., Bento L., Benvenuti D., Bernabe L., Bersten A., Berta G., Bertini P., Bertram-Ralph E., Besbes M., Bettini L. R., Beuret P., Bewley J., Bezzi M., Bhakhtiani L., Bhandary R., Bhowmick K., Bihari S., Bissett B., Blythe D., Bocher S., Boedjawan N., Bojanowski C. M., Boni E., Boraso S., Borelli M., Borello S., Borislavova M., Bosma K. J., Bottiroli M., Boyd O., Bozbay S., Briva A., Bruel C., Bruni A., Buehner U., Bulpa P., Burt K., Buscot M., Buttera S., Cabrera J., Caccese R., Caironi P., Canchos Gutierrez I., Canedo N., Cani A., Cappellini I., Carazo J., Cardonnet L. P., Carpio D., Carriedo D., Carrillo R., Carvalho J., Caser E., Castelli A., Castillo Quintero M., Castro H., Catorze N., Cengiz M., Cereijo E., Ceunen H., Chaintoutis C., Chang Y., Chaparro G., Chapman C., Chau S., Chavez C. E., Chelazzi C., Chelly J., Chemouni F., Chen K., Chena A., Chiarandini P., Chilton P., Chiumello D., Chou-Lie Y., Chudeau N., Cinel I., Cinnella G., Clark M., Clark T., Clementi S., Coaguila L., Codecido A. J., Collins A., Colombo R., Conde J., Consales G., Cook T., Coppadoro A., Cornejo R., Cortegiani A., Coxo C., Cracchiolo A. N., Crespo Ramirez M., Crova P., Cruz J., Cubattoli L., Cukurova Z., Curto F., Czempik P., D'Andrea R., da Silva Ramos F., Dangers L., Danguy des Deserts M., Danin P. -E., Dantas F., Daubin C., Dawei W., de Haro C., de Jesus Montelongo F., De Mendoza D., de Pablo R., De Pascale G., De Rosa S., Decavele M., Declercq P. -L., Deicas A., del Carmen Campos Moreno M., Dellamonica J., Delmas B., Demirkiran O., Demirkiran H., Dendane T., di Mussi R., Diakaki C., Diaz A., Diaz W., Dikmen Y., Dimoula A., Doble P., Doha N., Domingos G., Dres M., Dries D., Duggal A., Duke G., Dunts P., Dybwik K., Dykyy M., Eckert P., Efe S., Elatrous S., Elay G., Elmaryul A. S., Elsaadany M., Elsayed H., Elsayed S., Emery M., Ena S., Eng K., Englert J. A., Erdogan E., Ergin Ozcan P., Eroglu E., Escobar M., Esen F., Esen Tekeli A., Esquivel A., Esquivel Gallegos H., Ezzouine H., Facchini A., Faheem M., Fanelli V., Farina M. F., Fartoukh M., Fehrle L., Feng F., Feng Y., Fernandez I., Fernandez B., Fernandez-Rodriguez M. L., Ferrando C., Ferreira da Silva M. J., Ferreruela M., Ferrier J., Flamm Zamorano M. J., Flood L., Floris L., Fluckiger M., Forteza C., Fortunato A., Frans E., Frattari A., Fredes S., Frenzel T., Fumagalli R., Furche M. A., Fusari M., Fysh E., Galeas-Lopez J. L., Galerneau L. -M., Garcia A., Garcia M. F., Garcia E., Garcia Olivares P., Garlicki J., Garnero A., Garofalo E., Gautam P., Gazenkampf A., Gelinotte S., Gelormini D., Ghrenassia E., Giacomucci A., Giannoni R., Gigante A., Glober N., Gnesin P., Gollo Y., Gomaa D., Gomero Paredes R., Gomes R., Gomez R. A., Gomez O., Gomez A., Gondim L., Gonzalez M., Gonzalez I., Gonzalez-Castro A., Gordillo Romero O., Gordo F., Gouin P., Graf Santos J., Grainne R., Grando M., Granov Grabovica S., Grasso S., Grasso R., Grimmer L., Grissom C., Gu Q., Guan X. -D., Guarracino F., Guasch N., Guatteri L., Gueret R., Guerin C., Guerot E., Guitard P. -G., Gul F., Gumus A., Gurjar M., Gutierrez P., Hachimi A., Hadzibegovic A., Hagan S., Hammel C., Han Song J., Hanlon G., Heines S., Henriksson J., Herbrecht J. -E., Heredia Orbegoso G. O., Hermon A., Hernandez R., Hernandez C., Herrera L., Herrera-Gutierrez M., Hidalgo J., Hill D., Holmquist D., Homez M., Hongtao X., Hormis A., Horner D., Hornos M. C., Hou M., House S., Housni B., Hugill K., Humphreys S., Humbert L., Hunter S., Hwa Young L., Iezzi N., Ilutovich S., Inal V., Innes R., Ioannides P., Iotti G. A., Ippolito M., Irie H., Iriyama H., Itagaki T., Izura J., Izza S., Jabeen R., Jamaati H., Jamadarkhana S., Jamoussi A., Jankowski M., Jaramillo L. A., Jeon K., Jeong Lee S., Jeswani D., Jha S., Jiang L., Jing C., Jochmans S., Johnstad B. A., Jongmin L., Joret A., Junhasavasdikul D., Jurado M. T., Kam E., Kamohara H., Kane C., Kara I., Karakurt S., Karnjanarachata C., Kataoka J., Katayama S., Kaushik S., Kelebek Girgin N., Kerr K., Kerslake I., Khairnar P., Khalid A., Khan A., Khanna A. K., Khorasanee R., Kienhorst D., Kirakli C., Knafelj R., Kol M. K., Kongpolprom N., Kopitko C., Korkmaz Ekren P., Kubisz-Pudelko A., Kulcsar Z., Kumasawa J., Kuriyama A., Kutchak F., Labarca E., Labat F., Laborda C., Laca Barrera M. A., Lagache L., Landaverde Lopez A., Lanspa M., Lascari V., Le Meur M., Lee S. H., Lee Y. J., Lee J., Lee W. -Y., Legernaes T., Leiner T., Lemiale V., Leonor T., Lepper P. M., Li D., Li H., Li O., Lima A. R., Lind D., Litton E., Liu N., Liu L., Liu J., Llitjos J. -F., Llorente B., Lopez R., Lopez C. E., Lopez Nava C., Lovazzano P., Lu M., Lucchese F., Lugano M., Lugo Goytia G., Luo H., Lynch C., Macheda S., Madrigal Robles V. H., Maggiore S. M., Magret Iglesias M., Malaga P., Mallapura Maheswarappa H., Malpartida G., Malyarchikov A., Mansson H., Manzano A., Marey I., Marin N., Marin M. D. C., Markman E., Martin F., Martin A., Martin Dal Gesso C., Martinez F., Martinez-Fidalgo C., Martin-Loeches I., Mas A., Masaaki S., Maseda E., Massa E., Mattsson A., Maugeri J., McCredie V., McCullough J., McGuinness S., McKown A., Medve L., Mei C., Mellado Artigas R., Mendes V., Mervat M. K. E., Michaux I., Mikhaeil M., Milagros O., Milet I., Millan M. T., Minwei Z., Mirabella L., Mishra S., Mistraletti G., Mochizuki K., Moghal A., Mojoli F., Molin A., Montiel R., Montini L., Monza G., Mora Aznar M., Morakul S., Morales M., Moreno Torres D., Morocho Tutillo D. R., Motherway C., Mouhssine D., Mouloudi E., Munoz T., Munoz de Cabo C., Mustafa M., Muthuchellappan R., Muthukrishnan M., Muttini S., Nagata I., Nahar D., Nakanishi M., Nakayama I., Namendys-Silva S. A., Nanchal R., Nandakumar S., Nasi A., Nasir K., Navalesi P., Naz Aslam T., Nga Phan T., Nichol A., Niiyama S., Nikolakopoulou S., Nikolic E., Nitta K., Noc M., Nonas S., Nseir S., Nur Soyturk A., Obata Y., Oeckler R., Oguchi M., Ohshimo S., Oikonomou M., Ojados A., Oliveira M. T., Oliveira Filho W., Oliveri C., Olmos A., Omura K., Orlandi M. C., Orsenigo F., Ortiz-Ruiz De Gordoa L., Ota K., Ovalle Olmos R., Oveges N., Oziemski P., Ozkan Kuscu O., Pachas Alvarado F., Pagella G., Palaniswamy V., Palazon Sanchez E. L., Palmese S., Pan G., Pan W., Papanikolaou M., Papavasilopoulou T., Parekh A., Parke R., Parrilla F. J., Parrilla D., Pasha T., Pasin L., Patao L., Patel M., Patel G., Pati B. K., Patil J., Pattnaik S., Paul D., Pavesi M., Pavlotsky V. A., Paz G., Paz E., Pecci E., Pellegrini C., Pena Padilla A. G., Perchiazzi G., Pereira T., Pereira V., Perez M., Perez Calvo C., Perez Cheng M., Perez Maita R., Perez-Araos R., Perez-Teran P., Perez-Torres D., Perkins G., Persona P., Petnak T., Petrova M., Philippart F., Picetti E., Pierucci E., Piervincenzi E., Pinciroli R., Pintado M. -C., Piraino T., Piras S., Piras C., Pirompanich P., Pisani L., Platas E., Plotnikow G., Porras W., Porta V., Portilla M., Portugal J., Povoa P., Prat G., Pratto R., Preda G., Prieto I., Prol-Silva E., Pugh R., Qi Y., Qian C., Qin T., Qu H., Quintana T., Quispe Sierra R., Quispe Soto R., Rabbani R., Rabee M., Rabie A., Rahe Pereira M. A., Rai A., Raj Ashok S., Rajab M., Ramdhani N., Ramey E., Ranieri M., Rathod D., Ray B., Redwanul Huq S. M., Regli A., Reina R., Resano Sarmiento N., Reynaud F., Rialp G., Ricart P., Rice T., Richardson A., Rieder M., Rinket M., Rios F., Risso Vazquez A., Riva I., Rivette M., Roca O., Roche-Campo F., Rodriguez C., Rodriguez G., Rodriguez Gonzalez D., Rodriguez Tucto X. Y., Rogers A., Romano M. E., Rortveit L., Rose A., Roux D., Rouze A., Rubatto Birri P. N., Ruilan W., Ruiz Robledo A., Ruiz-Aguilar A. L., Sadahiro T., Saez I., Sagardia J., Saha R., Saiphoklang N., Saito S., Salem M., Sales G., Salgado P., Samavedam S., Sami Mebazaa M., Samuelsson L., San Juan Roman N., Sanchez P., Sanchez-Ballesteros J., Sandoval Y., Sani E., Santos M., Santos C., Sanui M., Saravanabavan L., Sari S., Sarkany A., Sauneuf B., Savioli M., Sazak H., Scano R., Schneider F., Schortgen F., Schultz M. J., Schwarz G. L., Seckin Yucesoy F., Seely A., Seiler F., Seker Tekdos Y., Seok Chan K., Serano L., Serednicki W., Setten M., Shah A., Shah B., Shang Y., Shanmugasundaram P., Shapovalov K., Shebl E., Shiga T., Shime N., Shin P., Short J., Shuhua C., Siddiqui S., Silesky Jimenez J. I., Silva D., Silva Sales B., Simons K., Sjobo B. A., Slessor D., Smiechowicz J., Smischney N., Smith P., Smith T., Smith M., Snape S., Snyman L., Soetens F., Sook Hong K., Sosa Medellin M. A., Soto G., Souloy X., Sousa E., Sovatzis S., Sozutek D., Spadaro S., Spagnoli M., Spangfors M., Spittle N., Spivey M., Stapleton A., Stefanovic B., Stephenson L., Stevenson E., Strand K., Strano M. T., Straus S., Sun C., Sun R., Sundaram V., SunPark T., Surlemont E., Sutherasan Y., Szabo Z., Tainter C., Takaba A., Tallott M., Tamasato T., Tang Z., Tangsujaritvijit V., Taniguchi L., Taniguchi D., Tarantino F., Teerapuncharoen K., Temprano S., Terragni P., Terzi N., Thakur A., Theerawit P., Thille A. W., Thomas M., Thungtitigul P., Thyrault M., Tilouch N., Timenetsky K., Tirapu J., Todeschini M., Tomas R., Tomaszewski C., Tonetti T., Tonnelier A., Trinder J., Trongtrakul K., Truwit J., Tsuei B., Tulaimat A., Turan S., Turkoglu M., Tyagi S., Ubeda A., Vagginelli F., Valenti M. F., Vallverdu I., Van Axel A., van den Hul I., van der Hoeven H., Van Der Meer N., Vanhoof M., Vargas-Ordonez M., Vaschetto R., Vascotto E., Vatsik M., Vaz A., Vazquez-Sanchez A., Ventura S., Vermeijden J. W., Vidal A., Vieira J., Vilela Costa Pinto B., Villagra A., Villegas Succar C., Vinorum O. G., Vitale G., Vj R., Vochin A., Voiriot G., Volta C. A., von Seth M., Wajdi M., Walsh D., Wang S., Wardi G., Ween-Velken N. C., Wei B. -L., Weller D., Welsh D., Welters I., Wert M., Whiteley S., Wilby E., Williams E., Williams K., Wilson A., Wojtas J., Won Huh J., Wrathall D., Wright C., Wu J. -F., Xi G., Xing Z. -J., Xu H., Yamamoto K., Yan J., Yanez J., Yang X., Yates E., Yazicioglu Mocin O., Ye Z., Yildirim F., Yoshida N., Yoshido H. H. L., Young Lee B., Yu R., Yu G., Yu T., Yuan B., Yuangtrakul N., Yumoto T., Yun X., Zakalik G., Zaki A., Zalba-Etayo B., Zambon M., Zang B., Zani G., Zarka J., Zerbi S. M., Zerman A., Zetterquist H., Zhang J., Zhang H., Zhang W., Zhang G., Zhao H., Zheng J., Zhu B., Zumaran R., Pham, T, Heunks, L, Bellani, G, Madotto, F, Aragao, I, Beduneau, G, Goligher, E, Grasselli, G, Laake, J, Mancebo, J, Penuelas, O, Piquilloud, L, Pesenti, A, Wunsch, H, van Haren, F, Brochard, L, Laffey, J, Abrough, F, Acharya, S, Amin, P, Arabi, Y, Bauer, P, Beitler, J, Berkius, J, Bugedo, G, Camporota, L, Cerny, V, Cho, Y, Clarkson, K, Estenssoro, E, Gritsan, A, Hashemian, S, Hermans, G, Jovanovic, B, Kurahashi, K, Matamis, D, Moerer, O, Molnar, Z, Ozyilmaz, E, Panka, B, Papali, A, Perbet, S, Qiu, H, Razek, A, Rittayamai, N, Roldan, R, Serpa Neto, A, Szuldrzynski, K, Talmor, D, Tomescu, D, Villagomez, A, Zeggwagh, A, Abe, T, Aboshady, A, Acampo-de Jong, M, Adderley, J, Adiguzel, N, Agrawal, V, Aguilar, G, Aguirre, G, Aguirre-Bermeo, H, Ahlstrom, B, Akbas, T, Akker, M, Al Sadeh, G, Alamri, S, Algaba, A, Ali, M, Aliberti, A, Allegue, J, Alvarez, D, Amador, J, Andersen, F, Ansari, S, Apichatbutr, Y, Apostolopoulou, O, Arellano, D, Arica, M, Arikan, H, Arinaga, K, Arnal, J, Asano, K, Asin-Corrochano, M, Avalos Cabrera, J, Avila Fuentes, S, Aydemir, S, Aygencel, G, Azevedo, L, Bacakoglu, F, Badie, J, Baedorf Kassis, E, Bai, G, Balaraj, G, Ballico, B, Banner-Goodspeed, V, Banwarie, P, Barbieri, R, Baronia, A, Barrett, J, Barrot, L, Barrueco-Francioni, J, Barry, J, Bawangade, H, Beavis, S, Beck, E, Beehre, N, Belenguer Muncharaz, A, Belliato, M, Bellissima, A, Beltramelli, R, Ben Souissi, A, Benitez-Cano, A, Benlamin, M, Benslama, A, Bento, L, Benvenuti, D, Bernabe, L, Bersten, A, Berta, G, Bertini, P, Bertram-Ralph, E, Besbes, M, Bettini, L, Beuret, P, Bewley, J, Bezzi, M, Bhakhtiani, L, Bhandary, R, Bhowmick, K, Bihari, S, Bissett, B, Blythe, D, Bocher, S, Boedjawan, N, Bojanowski, C, Boni, E, Boraso, S, Borelli, M, Borello, S, Borislavova, M, Bosma, K, Bottiroli, M, Boyd, O, Bozbay, S, Briva, A, Bruel, C, Bruni, A, Buehner, U, Bulpa, P, Burt, K, Buscot, M, Buttera, S, Cabrera, J, Caccese, R, Caironi, P, Canchos Gutierrez, I, Canedo, N, Cani, A, Cappellini, I, Carazo, J, Cardonnet, L, Carpio, D, Carriedo, D, Carrillo, R, Carvalho, J, Caser, E, Castelli, A, Castillo Quintero, M, Castro, H, Catorze, N, Cengiz, M, Cereijo, E, Ceunen, H, Chaintoutis, C, Chang, Y, Chaparro, G, Chapman, C, Chau, S, Chavez, C, Chelazzi, C, Chelly, J, Chemouni, F, Chen, K, Chena, A, Chiarandini, P, Chilton, P, Chiumello, D, Chou-Lie, Y, Chudeau, N, Cinel, I, Cinnella, G, Clark, M, Clark, T, Clementi, S, Coaguila, L, Codecido, A, Collins, A, Colombo, R, Conde, J, Consales, G, Cook, T, Coppadoro, A, Cornejo, R, Cortegiani, A, Coxo, C, Cracchiolo, A, Crespo Ramirez, M, Crova, P, Cruz, J, Cubattoli, L, Cukurova, Z, Curto, F, Czempik, P, D'Andrea, R, da Silva Ramos, F, Dangers, L, Danguy des Deserts, M, Danin, P, Dantas, F, Daubin, C, Dawei, W, de Haro, C, de Jesus Montelongo, F, De Mendoza, D, de Pablo, R, De Pascale, G, De Rosa, S, Decavele, M, Declercq, P, Deicas, A, del Carmen Campos Moreno, M, Dellamonica, J, Delmas, B, Demirkiran, O, Demirkiran, H, Dendane, T, di Mussi, R, Diakaki, C, Diaz, A, Diaz, W, Dikmen, Y, Dimoula, A, Doble, P, Doha, N, Domingos, G, Dres, M, Dries, D, Duggal, A, Duke, G, Dunts, P, Dybwik, K, Dykyy, M, Eckert, P, Efe, S, Elatrous, S, Elay, G, Elmaryul, A, Elsaadany, M, Elsayed, H, Elsayed, S, Emery, M, Ena, S, Eng, K, Englert, J, Erdogan, E, Ergin Ozcan, P, Eroglu, E, Escobar, M, Esen, F, Esen Tekeli, A, Esquivel, A, Esquivel Gallegos, H, Ezzouine, H, Facchini, A, Faheem, M, Fanelli, V, Farina, M, Fartoukh, M, Fehrle, L, Feng, F, Feng, Y, Fernandez, I, Fernandez, B, Fernandez-Rodriguez, M, Ferrando, C, Ferreira da Silva, M, Ferreruela, M, Ferrier, J, Flamm Zamorano, M, Flood, L, Floris, L, Fluckiger, M, Forteza, C, Fortunato, A, Frans, E, Frattari, A, Fredes, S, Frenzel, T, Fumagalli, R, Furche, M, Fusari, M, Fysh, E, Galeas-Lopez, J, Galerneau, L, Garcia, A, Garcia, M, Garcia, E, Garcia Olivares, P, Garlicki, J, Garnero, A, Garofalo, E, Gautam, P, Gazenkampf, A, Gelinotte, S, Gelormini, D, Ghrenassia, E, Giacomucci, A, Giannoni, R, Gigante, A, Glober, N, Gnesin, P, Gollo, Y, Gomaa, D, Gomero Paredes, R, Gomes, R, Gomez, R, Gomez, O, Gomez, A, Gondim, L, Gonzalez, M, Gonzalez, I, Gonzalez-Castro, A, Gordillo Romero, O, Gordo, F, Gouin, P, Graf Santos, J, Grainne, R, Grando, M, Granov Grabovica, S, Grasso, S, Grasso, R, Grimmer, L, Grissom, C, Gu, Q, Guan, X, Guarracino, F, Guasch, N, Guatteri, L, Gueret, R, Guerin, C, Guerot, E, Guitard, P, Gul, F, Gumus, A, Gurjar, M, Gutierrez, P, Hachimi, A, Hadzibegovic, A, Hagan, S, Hammel, C, Han Song, J, Hanlon, G, Heines, S, Henriksson, J, Herbrecht, J, Heredia Orbegoso, G, Hermon, A, Hernandez, R, Hernandez, C, Herrera, L, Herrera-Gutierrez, M, Hidalgo, J, Hill, D, Holmquist, D, Homez, M, Hongtao, X, Hormis, A, Horner, D, Hornos, M, Hou, M, House, S, Housni, B, Hugill, K, Humphreys, S, Humbert, L, Hunter, S, Hwa Young, L, Iezzi, N, Ilutovich, S, Inal, V, Innes, R, Ioannides, P, Iotti, G, Ippolito, M, Irie, H, Iriyama, H, Itagaki, T, Izura, J, Izza, S, Jabeen, R, Jamaati, H, Jamadarkhana, S, Jamoussi, A, Jankowski, M, Jaramillo, L, Jeon, K, Jeong Lee, S, Jeswani, D, Jha, S, Jiang, L, Jing, C, Jochmans, S, Johnstad, B, Jongmin, L, Joret, A, Junhasavasdikul, D, Jurado, M, Kam, E, Kamohara, H, Kane, C, Kara, I, Karakurt, S, Karnjanarachata, C, Kataoka, J, Katayama, S, Kaushik, S, Kelebek Girgin, N, Kerr, K, Kerslake, I, Khairnar, P, Khalid, A, Khan, A, Khanna, A, Khorasanee, R, Kienhorst, D, Kirakli, C, Knafelj, R, Kol, M, Kongpolprom, N, Kopitko, C, Korkmaz Ekren, P, Kubisz-Pudelko, A, Kulcsar, Z, Kumasawa, J, Kuriyama, A, Kutchak, F, Labarca, E, Labat, F, Laborda, C, Laca Barrera, M, Lagache, L, Landaverde Lopez, A, Lanspa, M, Lascari, V, Le Meur, M, Lee, S, Lee, Y, Lee, J, Lee, W, Legernaes, T, Leiner, T, Lemiale, V, Leonor, T, Lepper, P, Li, D, Li, H, Li, O, Lima, A, Lind, D, Litton, E, Liu, N, Liu, L, Liu, J, Llitjos, J, Llorente, B, Lopez, R, Lopez, C, Lopez Nava, C, Lovazzano, P, Lu, M, Lucchese, F, Lugano, M, Lugo Goytia, G, Luo, H, Lynch, C, Macheda, S, Madrigal Robles, V, Maggiore, S, Magret Iglesias, M, Malaga, P, Mallapura Maheswarappa, H, Malpartida, G, Malyarchikov, A, Mansson, H, Manzano, A, Marey, I, Marin, N, Marin, M, Markman, E, Martin, F, Martin, A, Martin Dal Gesso, C, Martinez, F, Martinez-Fidalgo, C, Martin-Loeches, I, Mas, A, Masaaki, S, Maseda, E, Massa, E, Mattsson, A, Maugeri, J, Mccredie, V, Mccullough, J, Mcguinness, S, Mckown, A, Medve, L, Mei, C, Mellado Artigas, R, Mendes, V, Mervat, M, Michaux, I, Mikhaeil, M, Milagros, O, Milet, I, Millan, M, Minwei, Z, Mirabella, L, Mishra, S, Mistraletti, G, Mochizuki, K, Moghal, A, Mojoli, F, Molin, A, Montiel, R, Montini, L, Monza, G, Mora Aznar, M, Morakul, S, Morales, M, Moreno Torres, D, Morocho Tutillo, D, Motherway, C, Mouhssine, D, Mouloudi, E, Munoz, T, Munoz de Cabo, C, Mustafa, M, Muthuchellappan, R, Muthukrishnan, M, Muttini, S, Nagata, I, Nahar, D, Nakanishi, M, Nakayama, I, Namendys-Silva, S, Nanchal, R, Nandakumar, S, Nasi, A, Nasir, K, Navalesi, P, Naz Aslam, T, Nga Phan, T, Nichol, A, Niiyama, S, Nikolakopoulou, S, Nikolic, E, Nitta, K, Noc, M, Nonas, S, Nseir, S, Nur Soyturk, A, Obata, Y, Oeckler, R, Oguchi, M, Ohshimo, S, Oikonomou, M, Ojados, A, Oliveira, M, Oliveira Filho, W, Oliveri, C, Olmos, A, Omura, K, Orlandi, M, Orsenigo, F, Ortiz-Ruiz De Gordoa, L, Ota, K, Ovalle Olmos, R, Oveges, N, Oziemski, P, Ozkan Kuscu, O, Pachas Alvarado, F, Pagella, G, Palaniswamy, V, Palazon Sanchez, E, Palmese, S, Pan, G, Pan, W, Papanikolaou, M, Papavasilopoulou, T, Parekh, A, Parke, R, Parrilla, F, Parrilla, D, Pasha, T, Pasin, L, Patao, L, Patel, M, Patel, G, Pati, B, Patil, J, Pattnaik, S, Paul, D, Pavesi, M, Pavlotsky, V, Paz, G, Paz, E, Pecci, E, Pellegrini, C, Pena Padilla, A, Perchiazzi, G, Pereira, T, Pereira, V, Perez, M, Perez Calvo, C, Perez Cheng, M, Perez Maita, R, Perez-Araos, R, Perez-Teran, P, Perez-Torres, D, Perkins, G, Persona, P, Petnak, T, Petrova, M, Philippart, F, Picetti, E, Pierucci, E, Piervincenzi, E, Pinciroli, R, Pintado, M, Piraino, T, Piras, S, Piras, C, Pirompanich, P, Pisani, L, Platas, E, Plotnikow, G, Porras, W, Porta, V, Portilla, M, Portugal, J, Povoa, P, Prat, G, Pratto, R, Preda, G, Prieto, I, Prol-Silva, E, Pugh, R, Qi, Y, Qian, C, Qin, T, Qu, H, Quintana, T, Quispe Sierra, R, Quispe Soto, R, Rabbani, R, Rabee, M, Rabie, A, Rahe Pereira, M, Rai, A, Raj Ashok, S, Rajab, M, Ramdhani, N, Ramey, E, Ranieri, M, Rathod, D, Ray, B, Redwanul Huq, S, Regli, A, Reina, R, Resano Sarmiento, N, Reynaud, F, Rialp, G, Ricart, P, Rice, T, Richardson, A, Rieder, M, Rinket, M, Rios, F, Risso Vazquez, A, Riva, I, Rivette, M, Roca, O, Roche-Campo, F, Rodriguez, C, Rodriguez, G, Rodriguez Gonzalez, D, Rodriguez Tucto, X, Rogers, A, Romano, M, Rortveit, L, Rose, A, Roux, D, Rouze, A, Rubatto Birri, P, Ruilan, W, Ruiz Robledo, A, Ruiz-Aguilar, A, Sadahiro, T, Saez, I, Sagardia, J, Saha, R, Saiphoklang, N, Saito, S, Salem, M, Sales, G, Salgado, P, Samavedam, S, Sami Mebazaa, M, Samuelsson, L, San Juan Roman, N, Sanchez, P, Sanchez-Ballesteros, J, Sandoval, Y, Sani, E, Santos, M, Santos, C, Sanui, M, Saravanabavan, L, Sari, S, Sarkany, A, Sauneuf, B, Savioli, M, Sazak, H, Scano, R, Schneider, F, Schortgen, F, Schultz, M, Schwarz, G, Seckin Yucesoy, F, Seely, A, Seiler, F, Seker Tekdos, Y, Seok Chan, K, Serano, L, Serednicki, W, Setten, M, Shah, A, Shah, B, Shang, Y, Shanmugasundaram, P, Shapovalov, K, Shebl, E, Shiga, T, Shime, N, Shin, P, Short, J, Shuhua, C, Siddiqui, S, Silesky Jimenez, J, Silva, D, Silva Sales, B, Simons, K, Sjobo, B, Slessor, D, Smiechowicz, J, Smischney, N, Smith, P, Smith, T, Smith, M, Snape, S, Snyman, L, Soetens, F, Sook Hong, K, Sosa Medellin, M, Soto, G, Souloy, X, Sousa, E, Sovatzis, S, Sozutek, D, Spadaro, S, Spagnoli, M, Spangfors, M, Spittle, N, Spivey, M, Stapleton, A, Stefanovic, B, Stephenson, L, Stevenson, E, Strand, K, Strano, M, Straus, S, Sun, C, Sun, R, Sundaram, V, Sunpark, T, Surlemont, E, Sutherasan, Y, Szabo, Z, Tainter, C, Takaba, A, Tallott, M, Tamasato, T, Tang, Z, Tangsujaritvijit, V, Taniguchi, L, Taniguchi, D, Tarantino, F, Teerapuncharoen, K, Temprano, S, Terragni, P, Terzi, N, Thakur, A, Theerawit, P, Thille, A, Thomas, M, Thungtitigul, P, Thyrault, M, Tilouch, N, Timenetsky, K, Tirapu, J, Todeschini, M, Tomas, R, Tomaszewski, C, Tonetti, T, Tonnelier, A, Trinder, J, Trongtrakul, K, Truwit, J, Tsuei, B, Tulaimat, A, Turan, S, Turkoglu, M, Tyagi, S, Ubeda, A, Vagginelli, F, Valenti, M, Vallverdu, I, Van Axel, A, van den Hul, I, van der Hoeven, H, Van Der Meer, N, Vanhoof, M, Vargas-Ordonez, M, Vaschetto, R, Vascotto, E, Vatsik, M, Vaz, A, Vazquez-Sanchez, A, Ventura, S, Vermeijden, J, Vidal, A, Vieira, J, Vilela Costa Pinto, B, Villagra, A, Villegas Succar, C, Vinorum, O, Vitale, G, Vj, R, Vochin, A, Voiriot, G, Volta, C, von Seth, M, Wajdi, M, Walsh, D, Wang, S, Wardi, G, Ween-Velken, N, Wei, B, Weller, D, Welsh, D, Welters, I, Wert, M, Whiteley, S, Wilby, E, Williams, E, Williams, K, Wilson, A, Wojtas, J, Won Huh, J, Wrathall, D, Wright, C, Wu, J, Xi, G, Xing, Z, Xu, H, Yamamoto, K, Yan, J, Yanez, J, Yang, X, Yates, E, Yazicioglu Mocin, O, Ye, Z, Yildirim, F, Yoshida, N, Yoshido, H, Young Lee, B, Yu, R, Yu, G, Yu, T, Yuan, B, Yuangtrakul, N, Yumoto, T, Yun, X, Zakalik, G, Zaki, A, Zalba-Etayo, B, Zambon, M, Zang, B, Zani, G, Zarka, J, Zerbi, S, Zerman, A, Zetterquist, H, Zhang, J, Zhang, H, Zhang, W, Zhang, G, Zhao, H, Zheng, J, Zhu, B, Zumaran, R, Pham T., Heunks L., Bellani G., Madotto F., Aragao I., Beduneau G., Goligher E. C., Grasselli G., Laake J. H., Mancebo J., Penuelas O., Piquilloud L., Pesenti A., Wunsch H., van Haren F., Brochard L., Laffey J. G., Abrough F., Acharya S. P., Amin P., Arabi Y., Bauer P., Beitler J., Berkius J., Bugedo G., Camporota L., Cerny V., Cho Y. -J., Clarkson K., Estenssoro E., Goligher E., Gritsan A., Hashemian S. M., Hermans G., Heunks L. M., Jovanovic B., Kurahashi K., Matamis D., Moerer O., Molnar Z., Ozyilmaz E., Panka B., Papali A., Perbet S., Qiu H., Razek A. A., Rittayamai N., Roldan R., Serpa Neto A., Szuldrzynski K., Talmor D., Tomescu D., Villagomez A., Zeggwagh A. A., Abe T., Aboshady A., Acampo-de Jong M., Acharya S., Adderley J., Adiguzel N., Agrawal V. K., Aguilar G., Aguirre G., Aguirre-Bermeo H., Ahlstrom B., Akbas T., Akker M., Al Sadeh G., Alamri S., Algaba A., Ali M., Aliberti A., Allegue J. M., Alvarez D., Amador J., Andersen F. H., Ansari S., Apichatbutr Y., Apostolopoulou O., Arellano D., Arica M., Arikan H., Arinaga K., Arnal J. -M., Asano K., Asin-Corrochano M., Avalos Cabrera J. M., Avila Fuentes S., Aydemir S., Aygencel G., Azevedo L., Bacakoglu F., Badie J., Baedorf Kassis E., Bai G., Balaraj G., Ballico B., Banner-Goodspeed V., Banwarie P., Barbieri R., Baronia A., Barrett J., Barrot L., Barrueco-Francioni J. E., Barry J., Bawangade H., Beavis S., Beck E., Beehre N., Belenguer Muncharaz A., Belliato M., Bellissima A., Beltramelli R., Ben Souissi A., Benitez-Cano A., Benlamin M., Benslama A., Bento L., Benvenuti D., Bernabe L., Bersten A., Berta G., Bertini P., Bertram-Ralph E., Besbes M., Bettini L. R., Beuret P., Bewley J., Bezzi M., Bhakhtiani L., Bhandary R., Bhowmick K., Bihari S., Bissett B., Blythe D., Bocher S., Boedjawan N., Bojanowski C. M., Boni E., Boraso S., Borelli M., Borello S., Borislavova M., Bosma K. J., Bottiroli M., Boyd O., Bozbay S., Briva A., Bruel C., Bruni A., Buehner U., Bulpa P., Burt K., Buscot M., Buttera S., Cabrera J., Caccese R., Caironi P., Canchos Gutierrez I., Canedo N., Cani A., Cappellini I., Carazo J., Cardonnet L. P., Carpio D., Carriedo D., Carrillo R., Carvalho J., Caser E., Castelli A., Castillo Quintero M., Castro H., Catorze N., Cengiz M., Cereijo E., Ceunen H., Chaintoutis C., Chang Y., Chaparro G., Chapman C., Chau S., Chavez C. E., Chelazzi C., Chelly J., Chemouni F., Chen K., Chena A., Chiarandini P., Chilton P., Chiumello D., Chou-Lie Y., Chudeau N., Cinel I., Cinnella G., Clark M., Clark T., Clementi S., Coaguila L., Codecido A. J., Collins A., Colombo R., Conde J., Consales G., Cook T., Coppadoro A., Cornejo R., Cortegiani A., Coxo C., Cracchiolo A. N., Crespo Ramirez M., Crova P., Cruz J., Cubattoli L., Cukurova Z., Curto F., Czempik P., D'Andrea R., da Silva Ramos F., Dangers L., Danguy des Deserts M., Danin P. -E., Dantas F., Daubin C., Dawei W., de Haro C., de Jesus Montelongo F., De Mendoza D., de Pablo R., De Pascale G., De Rosa S., Decavele M., Declercq P. -L., Deicas A., del Carmen Campos Moreno M., Dellamonica J., Delmas B., Demirkiran O., Demirkiran H., Dendane T., di Mussi R., Diakaki C., Diaz A., Diaz W., Dikmen Y., Dimoula A., Doble P., Doha N., Domingos G., Dres M., Dries D., Duggal A., Duke G., Dunts P., Dybwik K., Dykyy M., Eckert P., Efe S., Elatrous S., Elay G., Elmaryul A. S., Elsaadany M., Elsayed H., Elsayed S., Emery M., Ena S., Eng K., Englert J. A., Erdogan E., Ergin Ozcan P., Eroglu E., Escobar M., Esen F., Esen Tekeli A., Esquivel A., Esquivel Gallegos H., Ezzouine H., Facchini A., Faheem M., Fanelli V., Farina M. F., Fartoukh M., Fehrle L., Feng F., Feng Y., Fernandez I., Fernandez B., Fernandez-Rodriguez M. L., Ferrando C., Ferreira da Silva M. J., Ferreruela M., Ferrier J., Flamm Zamorano M. J., Flood L., Floris L., Fluckiger M., Forteza C., Fortunato A., Frans E., Frattari A., Fredes S., Frenzel T., Fumagalli R., Furche M. A., Fusari M., Fysh E., Galeas-Lopez J. L., Galerneau L. -M., Garcia A., Garcia M. F., Garcia E., Garcia Olivares P., Garlicki J., Garnero A., Garofalo E., Gautam P., Gazenkampf A., Gelinotte S., Gelormini D., Ghrenassia E., Giacomucci A., Giannoni R., Gigante A., Glober N., Gnesin P., Gollo Y., Gomaa D., Gomero Paredes R., Gomes R., Gomez R. A., Gomez O., Gomez A., Gondim L., Gonzalez M., Gonzalez I., Gonzalez-Castro A., Gordillo Romero O., Gordo F., Gouin P., Graf Santos J., Grainne R., Grando M., Granov Grabovica S., Grasso S., Grasso R., Grimmer L., Grissom C., Gu Q., Guan X. -D., Guarracino F., Guasch N., Guatteri L., Gueret R., Guerin C., Guerot E., Guitard P. -G., Gul F., Gumus A., Gurjar M., Gutierrez P., Hachimi A., Hadzibegovic A., Hagan S., Hammel C., Han Song J., Hanlon G., Heines S., Henriksson J., Herbrecht J. -E., Heredia Orbegoso G. O., Hermon A., Hernandez R., Hernandez C., Herrera L., Herrera-Gutierrez M., Hidalgo J., Hill D., Holmquist D., Homez M., Hongtao X., Hormis A., Horner D., Hornos M. C., Hou M., House S., Housni B., Hugill K., Humphreys S., Humbert L., Hunter S., Hwa Young L., Iezzi N., Ilutovich S., Inal V., Innes R., Ioannides P., Iotti G. A., Ippolito M., Irie H., Iriyama H., Itagaki T., Izura J., Izza S., Jabeen R., Jamaati H., Jamadarkhana S., Jamoussi A., Jankowski M., Jaramillo L. A., Jeon K., Jeong Lee S., Jeswani D., Jha S., Jiang L., Jing C., Jochmans S., Johnstad B. A., Jongmin L., Joret A., Junhasavasdikul D., Jurado M. T., Kam E., Kamohara H., Kane C., Kara I., Karakurt S., Karnjanarachata C., Kataoka J., Katayama S., Kaushik S., Kelebek Girgin N., Kerr K., Kerslake I., Khairnar P., Khalid A., Khan A., Khanna A. K., Khorasanee R., Kienhorst D., Kirakli C., Knafelj R., Kol M. K., Kongpolprom N., Kopitko C., Korkmaz Ekren P., Kubisz-Pudelko A., Kulcsar Z., Kumasawa J., Kuriyama A., Kutchak F., Labarca E., Labat F., Laborda C., Laca Barrera M. A., Lagache L., Landaverde Lopez A., Lanspa M., Lascari V., Le Meur M., Lee S. H., Lee Y. J., Lee J., Lee W. -Y., Legernaes T., Leiner T., Lemiale V., Leonor T., Lepper P. M., Li D., Li H., Li O., Lima A. R., Lind D., Litton E., Liu N., Liu L., Liu J., Llitjos J. -F., Llorente B., Lopez R., Lopez C. E., Lopez Nava C., Lovazzano P., Lu M., Lucchese F., Lugano M., Lugo Goytia G., Luo H., Lynch C., Macheda S., Madrigal Robles V. H., Maggiore S. M., Magret Iglesias M., Malaga P., Mallapura Maheswarappa H., Malpartida G., Malyarchikov A., Mansson H., Manzano A., Marey I., Marin N., Marin M. D. C., Markman E., Martin F., Martin A., Martin Dal Gesso C., Martinez F., Martinez-Fidalgo C., Martin-Loeches I., Mas A., Masaaki S., Maseda E., Massa E., Mattsson A., Maugeri J., McCredie V., McCullough J., McGuinness S., McKown A., Medve L., Mei C., Mellado Artigas R., Mendes V., Mervat M. K. E., Michaux I., Mikhaeil M., Milagros O., Milet I., Millan M. T., Minwei Z., Mirabella L., Mishra S., Mistraletti G., Mochizuki K., Moghal A., Mojoli F., Molin A., Montiel R., Montini L., Monza G., Mora Aznar M., Morakul S., Morales M., Moreno Torres D., Morocho Tutillo D. R., Motherway C., Mouhssine D., Mouloudi E., Munoz T., Munoz de Cabo C., Mustafa M., Muthuchellappan R., Muthukrishnan M., Muttini S., Nagata I., Nahar D., Nakanishi M., Nakayama I., Namendys-Silva S. A., Nanchal R., Nandakumar S., Nasi A., Nasir K., Navalesi P., Naz Aslam T., Nga Phan T., Nichol A., Niiyama S., Nikolakopoulou S., Nikolic E., Nitta K., Noc M., Nonas S., Nseir S., Nur Soyturk A., Obata Y., Oeckler R., Oguchi M., Ohshimo S., Oikonomou M., Ojados A., Oliveira M. T., Oliveira Filho W., Oliveri C., Olmos A., Omura K., Orlandi M. C., Orsenigo F., Ortiz-Ruiz De Gordoa L., Ota K., Ovalle Olmos R., Oveges N., Oziemski P., Ozkan Kuscu O., Pachas Alvarado F., Pagella G., Palaniswamy V., Palazon Sanchez E. L., Palmese S., Pan G., Pan W., Papanikolaou M., Papavasilopoulou T., Parekh A., Parke R., Parrilla F. J., Parrilla D., Pasha T., Pasin L., Patao L., Patel M., Patel G., Pati B. K., Patil J., Pattnaik S., Paul D., Pavesi M., Pavlotsky V. A., Paz G., Paz E., Pecci E., Pellegrini C., Pena Padilla A. G., Perchiazzi G., Pereira T., Pereira V., Perez M., Perez Calvo C., Perez Cheng M., Perez Maita R., Perez-Araos R., Perez-Teran P., Perez-Torres D., Perkins G., Persona P., Petnak T., Petrova M., Philippart F., Picetti E., Pierucci E., Piervincenzi E., Pinciroli R., Pintado M. -C., Piraino T., Piras S., Piras C., Pirompanich P., Pisani L., Platas E., Plotnikow G., Porras W., Porta V., Portilla M., Portugal J., Povoa P., Prat G., Pratto R., Preda G., Prieto I., Prol-Silva E., Pugh R., Qi Y., Qian C., Qin T., Qu H., Quintana T., Quispe Sierra R., Quispe Soto R., Rabbani R., Rabee M., Rabie A., Rahe Pereira M. A., Rai A., Raj Ashok S., Rajab M., Ramdhani N., Ramey E., Ranieri M., Rathod D., Ray B., Redwanul Huq S. M., Regli A., Reina R., Resano Sarmiento N., Reynaud F., Rialp G., Ricart P., Rice T., Richardson A., Rieder M., Rinket M., Rios F., Risso Vazquez A., Riva I., Rivette M., Roca O., Roche-Campo F., Rodriguez C., Rodriguez G., Rodriguez Gonzalez D., Rodriguez Tucto X. Y., Rogers A., Romano M. E., Rortveit L., Rose A., Roux D., Rouze A., Rubatto Birri P. N., Ruilan W., Ruiz Robledo A., Ruiz-Aguilar A. L., Sadahiro T., Saez I., Sagardia J., Saha R., Saiphoklang N., Saito S., Salem M., Sales G., Salgado P., Samavedam S., Sami Mebazaa M., Samuelsson L., San Juan Roman N., Sanchez P., Sanchez-Ballesteros J., Sandoval Y., Sani E., Santos M., Santos C., Sanui M., Saravanabavan L., Sari S., Sarkany A., Sauneuf B., Savioli M., Sazak H., Scano R., Schneider F., Schortgen F., Schultz M. J., Schwarz G. L., Seckin Yucesoy F., Seely A., Seiler F., Seker Tekdos Y., Seok Chan K., Serano L., Serednicki W., Setten M., Shah A., Shah B., Shang Y., Shanmugasundaram P., Shapovalov K., Shebl E., Shiga T., Shime N., Shin P., Short J., Shuhua C., Siddiqui S., Silesky Jimenez J. I., Silva D., Silva Sales B., Simons K., Sjobo B. A., Slessor D., Smiechowicz J., Smischney N., Smith P., Smith T., Smith M., Snape S., Snyman L., Soetens F., Sook Hong K., Sosa Medellin M. A., Soto G., Souloy X., Sousa E., Sovatzis S., Sozutek D., Spadaro S., Spagnoli M., Spangfors M., Spittle N., Spivey M., Stapleton A., Stefanovic B., Stephenson L., Stevenson E., Strand K., Strano M. T., Straus S., Sun C., Sun R., Sundaram V., SunPark T., Surlemont E., Sutherasan Y., Szabo Z., Tainter C., Takaba A., Tallott M., Tamasato T., Tang Z., Tangsujaritvijit V., Taniguchi L., Taniguchi D., Tarantino F., Teerapuncharoen K., Temprano S., Terragni P., Terzi N., Thakur A., Theerawit P., Thille A. W., Thomas M., Thungtitigul P., Thyrault M., Tilouch N., Timenetsky K., Tirapu J., Todeschini M., Tomas R., Tomaszewski C., Tonetti T., Tonnelier A., Trinder J., Trongtrakul K., Truwit J., Tsuei B., Tulaimat A., Turan S., Turkoglu M., Tyagi S., Ubeda A., Vagginelli F., Valenti M. F., Vallverdu I., Van Axel A., van den Hul I., van der Hoeven H., Van Der Meer N., Vanhoof M., Vargas-Ordonez M., Vaschetto R., Vascotto E., Vatsik M., Vaz A., Vazquez-Sanchez A., Ventura S., Vermeijden J. W., Vidal A., Vieira J., Vilela Costa Pinto B., Villagra A., Villegas Succar C., Vinorum O. G., Vitale G., Vj R., Vochin A., Voiriot G., Volta C. A., von Seth M., Wajdi M., Walsh D., Wang S., Wardi G., Ween-Velken N. C., Wei B. -L., Weller D., Welsh D., Welters I., Wert M., Whiteley S., Wilby E., Williams E., Williams K., Wilson A., Wojtas J., Won Huh J., Wrathall D., Wright C., Wu J. -F., Xi G., Xing Z. -J., Xu H., Yamamoto K., Yan J., Yanez J., Yang X., Yates E., Yazicioglu Mocin O., Ye Z., Yildirim F., Yoshida N., Yoshido H. H. L., Young Lee B., Yu R., Yu G., Yu T., Yuan B., Yuangtrakul N., Yumoto T., Yun X., Zakalik G., Zaki A., Zalba-Etayo B., Zambon M., Zang B., Zani G., Zarka J., Zerbi S. M., Zerman A., Zetterquist H., Zhang J., Zhang H., Zhang W., Zhang G., Zhao H., Zheng J., Zhu B., and Zumaran R.
Abstract: Background: Current management practices and outcomes in weaning from invasive mechanical ventilation are poorly understood. We aimed to describe the epidemiology, management, timings, risk for failure, and outcomes of weaning in patients requiring at least 2 days of invasive mechanical ventilation. Methods: WEAN SAFE was an international, multicentre, prospective, observational cohort study done in 481 intensive care units in 50 countries. Eligible participants were older than 16 years, admitted to a participating intensive care unit, and receiving mechanical ventilation for 2 calendar days or longer. We defined weaning initiation as the first attempt to separate a patient from the ventilator, successful weaning as no reintubation or death within 7 days of extubation, and weaning eligibility criteria based on positive end-expiratory pressure, fractional concentration of oxygen in inspired air, and vasopressors. The primary outcome was the proportion of patients successfully weaned at 90 days. Key secondary outcomes included weaning duration, timing of weaning events, factors associated with weaning delay and weaning failure, and hospital outcomes. This study is registered with ClinicalTrials.gov, NCT03255109. Findings: Between Oct 4, 2017, and June 25, 2018, 10 232 patients were screened for eligibility, of whom 5869 were enrolled. 4523 (77·1%) patients underwent at least one separation attempt and 3817 (65·0%) patients were successfully weaned from ventilation at day 90. 237 (4·0%) patients were transferred before any separation attempt, 153 (2·6%) were transferred after at least one separation attempt and not successfully weaned, and 1662 (28·3%) died while invasively ventilated. The median time from fulfilling weaning eligibility criteria to first separation attempt was 1 day (IQR 0–4), and 1013 (22·4%) patients had a delay in initiating first separation of 5 or more days. Of the 4523 (77·1%) patients with separation attempts, 2927 (64·7%) had a short wean (≤1 d
Published: 2023

37. Safety and Outcome of Revascularization Treatment in Patients With Acute Ischemic Stroke and COVID-19

Author: Marto, J, Strambo, D, Ntaios, G, Nguyen, T, Herzig, R, Czlonkowska, A, Demeestere, J, Mansour, O, Salerno, A, Wegener, S, Baumgartner, P, Cereda, C, Bianco, G, Beyeler, M, Arnold, M, Carrera, E, Machi, P, Altersberger, V, Bonati, L, Gensicke, H, Bolognese, M, Peters, N, Wetzel, S, Magrico, M, Ramos, J, Sargento-Freitas, J, Machado, R, Maia, C, Machado, E, Nunes, A, Ferreira, P, Pinho E Melo, T, Dias, M, Paula, A, Correia, M, Castro, P, Azevedo, E, Albuquerque, L, Alves, J, Ferreira-Pinto, J, Meira, T, Pereira, L, Rodrigues, M, Araujo, A, Rocha, M, Pereira-Fonseca, A, Ribeiro, L, Varela, R, Malheiro, S, Cappellari, M, Zivelonghi, C, Sajeva, G, Zini, A, Gentile, M, Forlivesi, S, Migliaccio, L, Sessa, M, La Gioia, S, Pezzini, A, Sangalli, D, Zedde, M, Pascarella, R, Ferrarese, C, Beretta, S, Diamanti, S, Schwarz, G, Frisullo, G, Marcheselli, S, Seners, P, Sabben, C, Escalard, S, Piotin, M, Maier, B, Charbonnier, G, Vuillier, F, Legris, L, Cuisenier, P, Vodret, F, Marnat, G, Liegey, J, Sibon, I, Flottmann, F, Broocks, G, Gloyer, N, Bohmann, F, Schaefer, J, Nolte, C, Audebert, H, Siebert, E, Sykora, M, Lang, W, Ferrari, J, Mayer-Suess, L, Knoflach, M, Gizewski, E, Stolp, J, Stolze, L, Coutinho, J, Nederkoorn, P, Van Den Wijngaard, I, De Meris, J, Lemmens, R, De Raedt, S, Vandervorst, F, Rutgers, M, Guilmot, A, Dusart, A, Bellante, F, Calleja-Castano, P, Ostos, F, Gonzalez-Ortega, G, Martin-Jimenez, P, Garcia-Madrona, S, Cruz-Culebras, A, Vera, R, Matute, M, Fuentes, B, Alonso-De-Lecinana, M, Rigual, R, Diez-Tejedor, E, Perez-Sanchez, S, Montaner, J, Diaz-Otero, F, Perez-De-La-Ossa, N, Flores-Pina, B, Munoz-Narbona, L, Chamorro, A, Rodriguez-Vazquez, A, Renu, A, Ayo-Martin, O, Hernandez-Fernandez, F, Segura, T, Tejada-Meza, H, Sagarra-Mur, D, Serrano-Ponz, M, Hlaing, T, See, I, Simister, R, Werring, D, Kristoffersen, E, Nordanstig, A, Jood, K, Rentzos, A, Simunek, L, Krajickova, D, Krajina, A, Mikulik, R, Cvikova, M, Vinklarek, J, Skoloudik, D, Roubec, M, Hurtikova, E, Hruby, R, Ostry, S, Skoda, O, Pernicka, M, Jurak, L, Eichlova, Z, Jira, M, Kovar, M, Pansky, M, Mencl, P, Palouskova, H, Tomek, A, Jansky, P, Olserova, A, Sramek, M, Havlicek, R, Maly, P, Trakal, L, Fiksa, J, Slovak, M, Karlinski, M, Nowak, M, Sienkiewicz-Jarosz, H, Bochynska, A, Wrona, P, Homa, T, Sawczynska, K, Slowik, A, Wlodarczyk, E, Wiacek, M, Tomaszewska-Lampart, I, Sieczkowski, B, Bartosik-Psujek, H, Bilik, M, Bandzarewicz, A, Dorobek, M, Zielinska-Turek, J, Nowakowska-Kotas, M, Obara, K, Urbanowski, P, Budrewicz, S, Guzinski, M, Switonska, M, Rutkowska, I, Sobieszak-Skura, P, Labuz-Roszak, B, Debiec, A, Staszewski, J, Stepien, A, Zwiernik, J, Wasilewski, G, Tiu, C, Terecoasa, E, Radu, R, Negrila, A, Dorobat, B, Panea, C, Tiu, V, Petrescu, S, Ozdemir, A, Mahmoud, M, El-Samahy, H, Abdelkhalek, H, Al-Hashel, J, Ismail, I, Salmeen, A, Ghoreishi, A, Sabetay, S, Gross, H, Klein, P, Abdalkader, M, Jabbour, P, El Naamani, K, Tjoumakaris, S, Abbas, R, Mohamed, G, Chebl, A, Min, J, Hovingh, M, Tsai, J, Khan, M, Nalleballe, K, Onteddu, S, Masoud, H, Michael, M, Kaur, N, Maali, L, Abraham, M, Khandelwal, P, Bach, I, Ong, M, Babici, D, Khawaja, A, Hakemi, M, Rajamani, K, Cano-Nigenda, V, Arauz, A, Amaya, P, Llanos, N, Arango, A, Vences, M, Barrientos Guerra, J, Caetano, R, Martins, R, Scollo, S, Yalung, P, Nagendra, S, Gaikwad, A, Seo, K, Georgiopoulos, G, Nogueira, R, Michel, P, Marto J. P., Strambo D., Ntaios G., Nguyen T. N., Herzig R., Czlonkowska A., Demeestere J., Mansour O. Y., Salerno A., Wegener S., Baumgartner P., Cereda C. W., Bianco G., Beyeler M., Arnold M., Carrera E., Machi P., Altersberger V., Bonati L., Gensicke H., Bolognese M., Peters N., Wetzel S., Magrico M., Ramos J. N., Sargento-Freitas J., Machado R., Maia C., Machado E., Nunes A. P., Ferreira P., Pinho E Melo T., Dias M. C., Paula A., Correia M. A., Castro P., Azevedo E., Albuquerque L., Alves J. N., Ferreira-Pinto J., Meira T., Pereira L., Rodrigues M., Araujo A. P., Rocha M., Pereira-Fonseca A., Ribeiro L., Varela R., Malheiro S., Cappellari M., Zivelonghi C., Sajeva G., Zini A., Gentile M., Forlivesi S., Migliaccio L., Sessa M., La Gioia S., Pezzini A., Sangalli D., Zedde M., Pascarella R., Ferrarese C., Beretta S., Diamanti S., Schwarz G., Frisullo G., Marcheselli S., Seners P., Sabben C., Escalard S., Piotin M., Maier B., Charbonnier G., Vuillier F., Legris L., Cuisenier P., Vodret F. R., Marnat G., Liegey J. -S., Sibon I., Flottmann F., Broocks G., Gloyer N. -O., Bohmann F. O., Schaefer J. H., Nolte C., Audebert H. J., Siebert E., Sykora M., Lang W., Ferrari J., Mayer-Suess L., Knoflach M., Gizewski E. R., Stolp J., Stolze L. J., Coutinho J. M., Nederkoorn P., Van Den Wijngaard I., De Meris J., Lemmens R., De Raedt S., Vandervorst F., Rutgers M. P., Guilmot A., Dusart A., Bellante F., Calleja-Castano P., Ostos F., Gonzalez-Ortega G., Martin-Jimenez P., Garcia-Madrona S., Cruz-Culebras A., Vera R., Matute M. C., Fuentes B., Alonso-De-Lecinana M., Rigual R., Diez-Tejedor E., Perez-Sanchez S., Montaner J., Diaz-Otero F., Perez-De-La-Ossa N., Flores-Pina B., Munoz-Narbona L., Chamorro A., Rodriguez-Vazquez A., Renu A., Ayo-Martin O., Hernandez-Fernandez F., Segura T., Tejada-Meza H., Sagarra-Mur D., Serrano-Ponz M., Hlaing T., See I., Simister R., Werring D., Kristoffersen E. S., Nordanstig A., Jood K., Rentzos A., Simunek L., Krajickova D., Krajina A., Mikulik R., Cvikova M., Vinklarek J., Skoloudik D., Roubec M., Hurtikova E., Hruby R., Ostry S., Skoda O., Pernicka M., Jurak L., Eichlova Z., Jira M., Kovar M., Pansky M., Mencl P., Palouskova H., Tomek A., Jansky P., Olserova A., Sramek M., Havlicek R., Maly P., Trakal L., Fiksa J., Slovak M., Karlinski M. A., Nowak M., Sienkiewicz-Jarosz H., Bochynska A., Wrona P., Homa T., Sawczynska K., Slowik A., Wlodarczyk E., Wiacek M., Tomaszewska-Lampart I., Sieczkowski B., Bartosik-Psujek H., Bilik M., Bandzarewicz A., Dorobek M., Zielinska-Turek J., Nowakowska-Kotas M., Obara K., Urbanowski P., Budrewicz S., Guzinski M., Switonska M., Rutkowska I., Sobieszak-Skura P., Labuz-Roszak B. M., Debiec A., Staszewski J., Stepien A., Zwiernik J., Wasilewski G., Tiu C., Terecoasa E. O., Radu R. A., Negrila A., Dorobat B., Panea C., Tiu V., Petrescu S., Ozdemir A., Mahmoud M., El-Samahy H., Abdelkhalek H., Al-Hashel J., Ismail I. I., Salmeen A., Ghoreishi A., Sabetay S. I., Gross H., Klein P., Abdalkader M., Jabbour P., El Naamani K., Tjoumakaris S., Abbas R., Mohamed G. A., Chebl A., Min J., Hovingh M., Tsai J. P., Khan M., Nalleballe K., Onteddu S., Masoud H., Michael M., Kaur N., Maali L., Abraham M. G., Khandelwal P., Bach I., Ong M., Babici D., Khawaja A. M., Hakemi M., Rajamani K., Cano-Nigenda V., Arauz A., Amaya P., Llanos N., Arango A., Vences M. A., Barrientos Guerra J. D., Caetano R., Martins R. T., Scollo S. D., Yalung P. M., Nagendra S., Gaikwad A., Seo K. -D., Georgiopoulos G., Nogueira R. G., Michel P., Marto, J, Strambo, D, Ntaios, G, Nguyen, T, Herzig, R, Czlonkowska, A, Demeestere, J, Mansour, O, Salerno, A, Wegener, S, Baumgartner, P, Cereda, C, Bianco, G, Beyeler, M, Arnold, M, Carrera, E, Machi, P, Altersberger, V, Bonati, L, Gensicke, H, Bolognese, M, Peters, N, Wetzel, S, Magrico, M, Ramos, J, Sargento-Freitas, J, Machado, R, Maia, C, Machado, E, Nunes, A, Ferreira, P, Pinho E Melo, T, Dias, M, Paula, A, Correia, M, Castro, P, Azevedo, E, Albuquerque, L, Alves, J, Ferreira-Pinto, J, Meira, T, Pereira, L, Rodrigues, M, Araujo, A, Rocha, M, Pereira-Fonseca, A, Ribeiro, L, Varela, R, Malheiro, S, Cappellari, M, Zivelonghi, C, Sajeva, G, Zini, A, Gentile, M, Forlivesi, S, Migliaccio, L, Sessa, M, La Gioia, S, Pezzini, A, Sangalli, D, Zedde, M, Pascarella, R, Ferrarese, C, Beretta, S, Diamanti, S, Schwarz, G, Frisullo, G, Marcheselli, S, Seners, P, Sabben, C, Escalard, S, Piotin, M, Maier, B, Charbonnier, G, Vuillier, F, Legris, L, Cuisenier, P, Vodret, F, Marnat, G, Liegey, J, Sibon, I, Flottmann, F, Broocks, G, Gloyer, N, Bohmann, F, Schaefer, J, Nolte, C, Audebert, H, Siebert, E, Sykora, M, Lang, W, Ferrari, J, Mayer-Suess, L, Knoflach, M, Gizewski, E, Stolp, J, Stolze, L, Coutinho, J, Nederkoorn, P, Van Den Wijngaard, I, De Meris, J, Lemmens, R, De Raedt, S, Vandervorst, F, Rutgers, M, Guilmot, A, Dusart, A, Bellante, F, Calleja-Castano, P, Ostos, F, Gonzalez-Ortega, G, Martin-Jimenez, P, Garcia-Madrona, S, Cruz-Culebras, A, Vera, R, Matute, M, Fuentes, B, Alonso-De-Lecinana, M, Rigual, R, Diez-Tejedor, E, Perez-Sanchez, S, Montaner, J, Diaz-Otero, F, Perez-De-La-Ossa, N, Flores-Pina, B, Munoz-Narbona, L, Chamorro, A, Rodriguez-Vazquez, A, Renu, A, Ayo-Martin, O, Hernandez-Fernandez, F, Segura, T, Tejada-Meza, H, Sagarra-Mur, D, Serrano-Ponz, M, Hlaing, T, See, I, Simister, R, Werring, D, Kristoffersen, E, Nordanstig, A, Jood, K, Rentzos, A, Simunek, L, Krajickova, D, Krajina, A, Mikulik, R, Cvikova, M, Vinklarek, J, Skoloudik, D, Roubec, M, Hurtikova, E, Hruby, R, Ostry, S, Skoda, O, Pernicka, M, Jurak, L, Eichlova, Z, Jira, M, Kovar, M, Pansky, M, Mencl, P, Palouskova, H, Tomek, A, Jansky, P, Olserova, A, Sramek, M, Havlicek, R, Maly, P, Trakal, L, Fiksa, J, Slovak, M, Karlinski, M, Nowak, M, Sienkiewicz-Jarosz, H, Bochynska, A, Wrona, P, Homa, T, Sawczynska, K, Slowik, A, Wlodarczyk, E, Wiacek, M, Tomaszewska-Lampart, I, Sieczkowski, B, Bartosik-Psujek, H, Bilik, M, Bandzarewicz, A, Dorobek, M, Zielinska-Turek, J, Nowakowska-Kotas, M, Obara, K, Urbanowski, P, Budrewicz, S, Guzinski, M, Switonska, M, Rutkowska, I, Sobieszak-Skura, P, Labuz-Roszak, B, Debiec, A, Staszewski, J, Stepien, A, Zwiernik, J, Wasilewski, G, Tiu, C, Terecoasa, E, Radu, R, Negrila, A, Dorobat, B, Panea, C, Tiu, V, Petrescu, S, Ozdemir, A, Mahmoud, M, El-Samahy, H, Abdelkhalek, H, Al-Hashel, J, Ismail, I, Salmeen, A, Ghoreishi, A, Sabetay, S, Gross, H, Klein, P, Abdalkader, M, Jabbour, P, El Naamani, K, Tjoumakaris, S, Abbas, R, Mohamed, G, Chebl, A, Min, J, Hovingh, M, Tsai, J, Khan, M, Nalleballe, K, Onteddu, S, Masoud, H, Michael, M, Kaur, N, Maali, L, Abraham, M, Khandelwal, P, Bach, I, Ong, M, Babici, D, Khawaja, A, Hakemi, M, Rajamani, K, Cano-Nigenda, V, Arauz, A, Amaya, P, Llanos, N, Arango, A, Vences, M, Barrientos Guerra, J, Caetano, R, Martins, R, Scollo, S, Yalung, P, Nagendra, S, Gaikwad, A, Seo, K, Georgiopoulos, G, Nogueira, R, Michel, P, Marto J. P., Strambo D., Ntaios G., Nguyen T. N., Herzig R., Czlonkowska A., Demeestere J., Mansour O. Y., Salerno A., Wegener S., Baumgartner P., Cereda C. W., Bianco G., Beyeler M., Arnold M., Carrera E., Machi P., Altersberger V., Bonati L., Gensicke H., Bolognese M., Peters N., Wetzel S., Magrico M., Ramos J. N., Sargento-Freitas J., Machado R., Maia C., Machado E., Nunes A. P., Ferreira P., Pinho E Melo T., Dias M. C., Paula A., Correia M. A., Castro P., Azevedo E., Albuquerque L., Alves J. N., Ferreira-Pinto J., Meira T., Pereira L., Rodrigues M., Araujo A. P., Rocha M., Pereira-Fonseca A., Ribeiro L., Varela R., Malheiro S., Cappellari M., Zivelonghi C., Sajeva G., Zini A., Gentile M., Forlivesi S., Migliaccio L., Sessa M., La Gioia S., Pezzini A., Sangalli D., Zedde M., Pascarella R., Ferrarese C., Beretta S., Diamanti S., Schwarz G., Frisullo G., Marcheselli S., Seners P., Sabben C., Escalard S., Piotin M., Maier B., Charbonnier G., Vuillier F., Legris L., Cuisenier P., Vodret F. R., Marnat G., Liegey J. -S., Sibon I., Flottmann F., Broocks G., Gloyer N. -O., Bohmann F. O., Schaefer J. H., Nolte C., Audebert H. J., Siebert E., Sykora M., Lang W., Ferrari J., Mayer-Suess L., Knoflach M., Gizewski E. R., Stolp J., Stolze L. J., Coutinho J. M., Nederkoorn P., Van Den Wijngaard I., De Meris J., Lemmens R., De Raedt S., Vandervorst F., Rutgers M. P., Guilmot A., Dusart A., Bellante F., Calleja-Castano P., Ostos F., Gonzalez-Ortega G., Martin-Jimenez P., Garcia-Madrona S., Cruz-Culebras A., Vera R., Matute M. C., Fuentes B., Alonso-De-Lecinana M., Rigual R., Diez-Tejedor E., Perez-Sanchez S., Montaner J., Diaz-Otero F., Perez-De-La-Ossa N., Flores-Pina B., Munoz-Narbona L., Chamorro A., Rodriguez-Vazquez A., Renu A., Ayo-Martin O., Hernandez-Fernandez F., Segura T., Tejada-Meza H., Sagarra-Mur D., Serrano-Ponz M., Hlaing T., See I., Simister R., Werring D., Kristoffersen E. S., Nordanstig A., Jood K., Rentzos A., Simunek L., Krajickova D., Krajina A., Mikulik R., Cvikova M., Vinklarek J., Skoloudik D., Roubec M., Hurtikova E., Hruby R., Ostry S., Skoda O., Pernicka M., Jurak L., Eichlova Z., Jira M., Kovar M., Pansky M., Mencl P., Palouskova H., Tomek A., Jansky P., Olserova A., Sramek M., Havlicek R., Maly P., Trakal L., Fiksa J., Slovak M., Karlinski M. A., Nowak M., Sienkiewicz-Jarosz H., Bochynska A., Wrona P., Homa T., Sawczynska K., Slowik A., Wlodarczyk E., Wiacek M., Tomaszewska-Lampart I., Sieczkowski B., Bartosik-Psujek H., Bilik M., Bandzarewicz A., Dorobek M., Zielinska-Turek J., Nowakowska-Kotas M., Obara K., Urbanowski P., Budrewicz S., Guzinski M., Switonska M., Rutkowska I., Sobieszak-Skura P., Labuz-Roszak B. M., Debiec A., Staszewski J., Stepien A., Zwiernik J., Wasilewski G., Tiu C., Terecoasa E. O., Radu R. A., Negrila A., Dorobat B., Panea C., Tiu V., Petrescu S., Ozdemir A., Mahmoud M., El-Samahy H., Abdelkhalek H., Al-Hashel J., Ismail I. I., Salmeen A., Ghoreishi A., Sabetay S. I., Gross H., Klein P., Abdalkader M., Jabbour P., El Naamani K., Tjoumakaris S., Abbas R., Mohamed G. A., Chebl A., Min J., Hovingh M., Tsai J. P., Khan M., Nalleballe K., Onteddu S., Masoud H., Michael M., Kaur N., Maali L., Abraham M. G., Khandelwal P., Bach I., Ong M., Babici D., Khawaja A. M., Hakemi M., Rajamani K., Cano-Nigenda V., Arauz A., Amaya P., Llanos N., Arango A., Vences M. A., Barrientos Guerra J. D., Caetano R., Martins R. T., Scollo S. D., Yalung P. M., Nagendra S., Gaikwad A., Seo K. -D., Georgiopoulos G., Nogueira R. G., and Michel P.
Abstract: Background and Objectives COVID-19–related inflammation, endothelial dysfunction, and coagulopathy may increase the bleeding risk and lower the efficacy of revascularization treatments in patients with acute ischemic stroke (AIS). We aimed to evaluate the safety and outcomes of revascularization treatments in patients with AIS and COVID-19. Methods This was a retrospective multicenter cohort study of consecutive patients with AIS receiving intravenous thrombolysis (IVT) and/or endovascular treatment (EVT) between March 2020 and June 2021 tested for severe acute respiratory syndrome coronavirus 2 infection. With a doubly robust model combining propensity score weighting and multivariate regression, we studied the association of COVID-19 with intracranial bleeding complications and clinical outcomes. Subgroup analyses were performed according to treatment groups (IVT-only and EVT). Results Of a total of 15,128 included patients from 105 centers, 853 (5.6%) were diagnosed with COVID-19; of those, 5,848 (38.7%) patients received IVT-only and 9,280 (61.3%) EVT (with or without IVT). Patients with COVID-19 had a higher rate of symptomatic intracerebral hemorrhage (SICH) (adjusted OR 1.53; 95% CI 1.16–2.01), symptomatic subarachnoid hemorrhage (SSAH) (OR 1.80; 95% CI 1.20–2.69), SICH and/or SSAH combined (OR 1.56; 95% CI 1.23–1.99), 24-hour mortality (OR 2.47; 95% CI 1.58–3.86), and 3-month mortality (OR 1.88; 95% CI 1.52–2.33). Patients with COVID-19 also had an unfavorable shift in the distribution of the modified Rankin score at 3 months (OR 1.42; 95% CI 1.26–1.60). Discussion Patients with AIS and COVID-19 showed higher rates of intracranial bleeding complications and worse clinical outcomes after revascularization treatments than contemporaneous non–COVID-19 patients receiving treatment. Current available data do not allow direct conclusions to be drawn on the effectiveness of revascularization treatments in patients with COVID-19 or to establish different treatment r
Published: 2023

38. Swift X-ray and UV monitoring of the Classical Nova V458 Vul (Nova Vul 2007)

Author: Ness, J. -U., Drake, J. J., Beardmore, A. P., Boyd, D., Bode, M. F., Brady, S., Evans, P. A., Gaensicke, B. T., Kitamoto, S., Knigge, C., Miller, I., Osborne, J. P., Page, K. L., Rodriguez-Gil, P., Schwarz, G., Staels, B., Steeghs, D., Takei, D., Tsujimoto, M., Wesson, R., and Zijlstra, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Galaxy Astrophysics
Abstract: We describe the highly variable X-ray and UV emission of V458 Vul (Nova Vul 2007), observed by Swift between 1 and 422 days after outburst. Initially bright only in the UV, V458 Vul became a variable hard X-ray source due to optically thin thermal emission at kT=0.64 keV with an X-ray band unabsorbed luminosity of 2.3x10^{34} erg s^{-1} during days 71-140. The X-ray spectrum at this time requires a low Fe abundance (0.2^{+0.3}_{-0.1} solar), consistent with a Suzaku measurement around the same time. On day 315 we find a new X-ray spectral component which can be described by a blackbody with temperature of kT=23^{+9}_{-5} eV, while the previous hard X-ray component has declined by a factor of 3.8. The spectrum of this soft X-ray component resembles those typically seen in the class of supersoft sources (SSS) which suggests that the nova ejecta were starting to clear and/or that the WD photosphere is shrinking to the point at which its thermal emission reaches into the X-ray band. We find a high degree of variability in the soft component with a flare rising by an order of magnitude in count rate in 0.2 days. In the following observations on days 342.4-383.6, the soft component was not seen, only to emerge again on day 397. The hard component continued to evolve, and we found an anticorrelation between the hard X-ray emission and the UV emission, yielding a Spearman rank probability of 97%. After day 397, the hard component was still present, was variable, and continued to fade at an extremely slow rate but could not be analysed owing to pile up contamination from the bright SSS component., Comment: 10 pages, 6 figures; accepted for AJ
Published: 2009
Full Text: View/download PDF

39. Swift Observations of Shock Evolution in RS Ophiuchi

Author: Bode, M. F., Osborne, J. P., Page, K. L., Beardmore, A. P., O'Brien, T. J., Ness, J. -U., Starrfield, S., Skinner, G. K., Darnley, M. J., Drake, J. J., Evans, A., Eyres, S. P. S., Krautter, J., and Schwarz, G.
Subjects: Astrophysics
Abstract: Our \textit{Swift} observations of RS Oph form an unprecedented X-ray dataset to undertake investigations of both the central source and the interaction of the outburst ejecta with the circumstellar environment. Over the first month, the XRT data are dominated by emission from rapidly evolving shocks. We discuss the differences in derived parameters from those found for \textit{RXTE} at early times and the evolution of the X-ray emission to much later times. It is apparent that at late times several emission components are present. We find no strong evidence of the proposed shock break-out in our data., Comment: 5 pages, 3 figures, to appear in ASP conference proceedings Volume 401 "RS Ophiuchi (2006) and the recurrent nova phenomenon"
Published: 2008

40. V723 Cassiopeia still on in X-rays: A bright Super Soft Source 12 years after outburst

Author: Ness, J. U-., Schwarz, G., Starrfield, S., Osborne, J. P., Page, K. L., Beardmore, A. P., Wagner, R. M., and Woodward, C. E.
Subjects: Astrophysics
Abstract: We find that the classical nova V723 Cas (1995) is still an active X-ray source more than 12 years after outburst and analyze seven X-ray observations carried out with Swift between 2006 January 31 and 2007 December 3. The average count rate is 0.022+/-0.01 cts s^-1 but the source is variable within a factor of two of the mean and does not show any signs of turning off. We present supporting optical observations which show that between 2001 and 2006 an underlying hot source was present with steadily increasing temperature. In order to confirm that the X-ray emission is from V723 Cas, we extract a ROSAT observation taken in 1990 and find that there was no X-ray source at the position of the nova. The Swift XRT spectra resemble those of the Super Soft X-ray binary Sources (SSS) which is confirmed by RXTE survey data which show no X-ray emission above 2 keV between 1996 and 2007. Using blackbody fits we constrain the effective temperature to between T_eff=(2.8-3.8)x10^5 K and a bolometric luminosity >5x10^36 erg s^-1 and caution that luminosities from blackbodies are generally overestimated and temperatures underestimated. We discuss a number of possible explanations for the continuing X-ray activity, including the intriguing possibility of steady hydrogen burning due to renewed accretion., Comment: Accepted by AJ; 7 pages, 5 figures, 2 tables
Published: 2008

41. Silicate dust in the environment of RS Ophiuchi following the 2006 eruption

Author: Evans, A., Woodward, C. E., Helton, L. A., van Loon, J. Th., Barry, R. K., Bode, M. F., Davis, R. J., Drake, J. J., Eyres, S. P. S., Geballe, T. R., Gehrz, R. D., Kerr, T., Krautter, J., Lynch, D. K., Ness, J. -U., O'Brien, T. J., Osborne, J. P., Page, K. L., Rudy, R. J., Russell, R. W., Schwarz, G., Starrfield, S., and Tyne, V. H.
Subjects: Astrophysics
Abstract: We present further Spitzer Space Telescope observations of the recurrent nova RS Ophiuchi, obtained over the period 208-430 days after the 2006 eruption. The later Spitzer IRS data show that the line emission and free-free continuum emission reported earlier is declining, revealing incontrovertible evidence for the presence of silicate emission features at 9.7 and 18microns. We conclude that the silicate dust survives the hard radiation impulse and shock blast wave from the eruption. The existence of the extant dust may have significant implications for understanding the propagation of shocks through the red giant wind and likely wind geometry., Comment: 12 pages, 4 figures, accepted for publication in ApJ (Letters)
Published: 2007
Full Text: View/download PDF

42. The Neon Abundance in the Ejecta of QU Vul From Late-Epoch IR Spectra

Author: Gehrz, Robert D., Woodward, Charles E., Helton, L. Andrew, Polomski, Elisha F., Hayward, Thomas L., Houck, James R., Evans, A., Krautter, Joachim, Shore, Steven N., Starrfield, Sumner, Truran, James, Schwarz, G. J., and Wagner, R. Mark
Subjects: Astrophysics
Abstract: We present ground-based SpectroCam-10 mid-infrared, MMT optical, and Spitzer Space Telescope IRS mid-infrared spectra taken 7.62, 18.75, and 19.38 years respectively after the outburst of the old classical nova QU Vulpeculae (Nova Vul 1984 #2). The spectra of the ejecta are dominated by forbidden line emission from neon and oxygen. Our analysis shows that neon was, at the first and last epochs respectively, more than 76 and 168 times overabundant by number with respect to hydrogen compared to the solar value. These high lower limits to the neon abundance confirm that QU Vul involved a thermonuclear runaway on an ONeMg white dwarf and approach the yields predicted by models of the nucleosynthesis in such events., Comment: ApJ 2007 accepted, 18 pages, including 5 figures, 1 table
Published: 2007
Full Text: View/download PDF

43. Spitzer and ground-based infrared observations of the 2006 eruption of RS Ophiuchi

Author: Evans, A., Woodward, C. E., Helton, L. A., Gehrz, R. D., Lynch, D. K., Rudy, R. J., Russell, R. W., Kerr, T., Bode, M. F., Darnley, M. J., Eyres, S. P. S., Geballe, T. R., O'Brien, T. J., Davis, R. J., Starrfield, S., Ness, J. -U., Drake, J., Osborne, J. P., Page, K. L., Schwarz, G., and Krautter, J.
Subjects: Astrophysics
Abstract: We present Spitzer Space Telescope and complementary ground-based infrared observations of the recurrent nova RS Ophiuchi, obtained over the period 64-111 days after the 2006 eruption. The Spitzer IRS data show a rich emission line spectrum superimposed on a free-free continuum. The presence of fine structure and coronal infrared lines lead us to deduce that there are at least two temperatures (1.5e5K and 9e5K) in the ejecta/wind environment, and that the electron density in the `cooler' region is 2.2e5 cm-3. The determination of elemental abundances is not straightforward but on the assumption that the Ne and O fine structure lines arise in the same volume of the ejecta, the O/Ne ratio is >~0.6 by number., Comment: 13 pages, 4 figures, accepted for publication in ApJ Letters
Published: 2007
Full Text: View/download PDF

44. The Early Spectrophotometric Evolution of V1186 Scorpii (Nova Scorpii 2004 #1)

Author: Schwarz, G. J., Woodward, C. E., Bode, M. F., Evans, A., Eyres, S. P., Geballe, T. R., Gehrz, R. D., Greenhouse, M. A., Hauschildt, P. H., Helton, L. A., Lynch, D. K., Lyke, J. E., O'Brien, T. J., Russell, R. W., Rudy, R. J., Shore, S. N., Starrfield, S. G., Temim, T., Truran, J. W., Venturini, C. C., Williams, R. E., and Zamanov, R.
Subjects: Astrophysics
Abstract: We report optical photometry and optical through mid-infrared spectroscopy of the classical nova V1186 Sco. This slowly developing nova had an complex light curve with multiple secondary peaks similar to those seen in PW Vul. The time to decline 2 magnitudes, t$_2$, was 20 days but the erratic nature of the light curve makes determination of intrinsic properties based on the decline time (e.g., luminosity) problematic, and the often cited MMRD relationship of Della Valle and Livio (1995) fails to yield a plausible distance. Spectra covering 0.35 to 35 $\mu$m were obtained in two separate epochs during the first year of outburst. The first set of spectra, taken about 2 months after visible maximum, are typical of a CO-type nova with narrow line emission from \ion{H}{1}, \ion{Fe}{2}, \ion{O}{1} and \ion{He}{1}. Later data, obtained between 260 and 380 days after maximum, reveal an emerging nebular spectrum. \textit{Spitzer} spectra show weakening hydrogen recombination emission with the emergence of [\ion{Ne}{2}] (12.81 $\mu$m) as the strongest line. Strong emission from [\ion{Ne}{3}] (15.56 $\mu$m) is also detected. Photoionization models with low effective temperature sources and only marginal neon enhancement (Ne $\sim$ 1.3 Ne$_{\odot}$) are consistent with these IR fine-structure neon lines indicating that V1186 Sco did not occur on a ONeMg white dwarf. In contrast, the slow and erratic light curve evolution, spectral development, and photoionization analysis of the ejecta imply the outburst occurred on a low mass CO white dwarf. We note that this is the first time strong [\ion{Ne}{2}] lines have been detected so early in the outburst of a CO nova and suggests that the presence of mid-infrared neon lines is not directly indicative of a ONeMg nova event., Comment: 7 figures, 37 pages. Astronimocal Journal accepted
Published: 2007
Full Text: View/download PDF

45. Swift X-ray Observations of Classical Novae

Author: Ness, J. -U., Schwarz, G. J., Retter, A., Starrfield, S., Schmitt, J. H. M. M., Gehrels, N., Burrows, D., and Osborne, J. P.
Subjects: Astrophysics
Abstract: The new gamma-ray burst mission Swift has obtained pointed observations of several classical novae in outburst. We analyzed all the observations of classical novae from the Swift archive up to 30 June, 2006. We analyzed usable observations of 12 classical novae and found 4 non-detections, 3 weak sources and 5 strong sources. This includes detections of 2 novae exhibiting spectra resembling those of Super Soft X-ray binary Source spectra (SSS) implying ongoing nuclear burning on the white dwarf surface. With these new Swift data, we add to the growing statistics of the X-ray duration and characteristics of classical novae., Comment: Accepted for ApJ; this version contains additional material: 18 pages, 16 figures
Published: 2007
Full Text: View/download PDF

46. Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase

Author: Evans, A., Kerr, T., Yang, Bin, Matsuoka, Y., Tsuzuki, Y., Bode, M. F., Eyres, S. P. S., Geballe, T. R., Woodward, C. E., Gehrz, R. D., Lynch, D. K., Rudy, R. J., Russell, R. W., O'Brien, T. J., Starrfield, S. G., Davis, R. J., Ness, Jan-Uwe, Drake, J., Osborne, J. P., Page, K. L., Adamson, A., Schwarz, G., and Krautter, J.
Subjects: Astrophysics
Abstract: We present infrared spectroscopy of the recurrent nova RS Ophiuchi, obtained 11.81, 20.75 and 55.71 days following its 2006 eruption. The spectra are dominated by hydrogen recombination lines, together with HeI, OI and OII lines; the electron temperature of ~10^4 K implied by the recombination spectrum suggests that we are seeing primarily the wind of the red giant, ionized by the ultraviolet flash when RS Oph erupted. However, strong coronal emission lines (i.e. emission from fine structure transitions in ions having high ionization potential) are present in the last spectrum. These imply a temperature of 930000K for the coronal gas; this is in line with x-ray observations of the 2006 eruption. The emission line widths decrease with time in a way that is consistent with the shock model for the x-ray emission., Comment: 5 pages, 4 figures, 3 tables. Accepted for publication in MNRAS
Published: 2006
Full Text: View/download PDF

47. Swift observations of the 2006 outburst of the recurrent nova RS Ophiuchi: I. Early X-ray emission from the shocked ejecta and red giant wind

Author: Bode, M. F., O'Brien, T. J., Osborne, J. P., Page, K. L., Senziani, F., Skinner, G. K., Starrfield, S., Ness, J-U., Drake, J. J., Schwarz, G., Beardmore, A. P., Darnley, M. J., Eyres, S. P. S., Evans, A., Gehrels, N., Goad, M. R., Jean, P., Krautter, J., and Novara, G.
Subjects: Astrophysics
Abstract: RS Ophiuchi began its latest outburst on 2006 February 12. Previous outbursts have indicated that high velocity ejecta interact with a pre-existing red giant wind, setting up shock systems analogous to those seen in Supernova Remnants. However, in the previous outburst in 1985, X-ray observations did not commence until 55 days after the initial explosion. Here we report on Swift observations covering the first month of the 2006 outburst with the Burst Alert (BAT) and X-ray Telescope (XRT) instruments. RS Oph was clearly detected in the BAT 14-25 keV band from t=0 to $t\sim6$ days. XRT observationsfrom 0.3-10 keV, started at 3.17 days after outburst. The rapidly evolving XRT spectra clearly show the presence of both line and continuum emission which can be fitted by thermal emission from hot gas whose characteristic temperature, overlying absorbing column, $[N_H]_W$, and resulting unabsorbed total flux decline monotonically after the first few days. Derived shock velocities are in good agreement with those found from observations at other wavelengths. Similarly, $[N_H]_W$ is in accord with that expected from the red giant wind ahead of the forward shock. We confirm the basic models of the 1985 outburst and conclude that standard Phase I remnant evolution terminated by $t\sim10$ days and the remnant then rapidly evolved to display behaviour characteristic of Phase III. Around t=26 days however, a new, luminous and highly variable soft X-ray source began to appear whose origin will be explored in a subsequent paper., Comment: 20 pages, 4 figures (2 updated), accepted by ApJ
Published: 2006
Full Text: View/download PDF

48. Cartan decomposition of the moment map

Author: Heinzner, P. and Schwarz, G. W.
Subjects: Mathematics - Complex Variables, Mathematics - Representation Theory, Mathematics - Symplectic Geometry, 32M05
Abstract: We investigate a class of actions of real Lie groups on complex spaces. Using moment map techniques we establish the existence of a quotient and a version of Luna's slice theorem as well as a version of the Hilbert-Mumford criterion. A global slice theorem is proved for proper actions. We give new proofs of results of Mostow on decompositions of groups and homogeneous spaces., Comment: 27 pages
Published: 2005

49. New Elemental Abundances for V1974 Cygni

Author: Vanlandingham, K. M., Schwarz, G. J., Shore, S. N., Starrfield, S., and Wagner, R. M.
Subjects: Astrophysics
Abstract: We present a new analysis of existing optical and ultraviolet spectra of the ONeMg nova V1974 Cygni 1992. Using these data and the photoionization code Cloudy, we have determined the physical parameters and elemental abundances for this nova. Many of the previous studies of this nova have made use of incorrect analyses and hence a new study was required. Our results show that the ejecta are enhanced, relative to solar, in helium, nitrogen, oxygen, neon, magnesium and iron. Carbon was found to be subsolar. We find an ejected mass of ~2x10e-4 solar masses. Our model results fit well with observations taken at IR, radio, sub-millimeter and X-ray wavelengths., Comment: 18 pages, 4 figures, accepted for publication in ApJ
Published: 2005
Full Text: View/download PDF

50. The Early Ultraviolet Evolution of the ONeMg Nova V382 Velorum 1999

Author: Shore, S. N., Schwarz, G., Bond, H. E., Downes, R. A., Starrfield, S., Evans, A., Gehrz, R. D., Hauschildt, P. H., Krautter, J., and Woodward, C. E.
Subjects: Astrophysics
Abstract: We present a multiwavelength study of the ONeMg Galactic nova V382 Velorum 1999 using HST/STIS and FUSE ultraviolet spectra and comparisons with published groundbased optical spectra. We find a close match to the basic phenomenology of another well-studied ONeMg nova, V1974 Cygni (Nova Cygni 1992), in particular to the spectral development through the start of the nebular phase. Following an ``iron curtain'' phase, the nova proceeded through a stage of P Cygni line profiles on all important resonance lines, as in many ONeMg novae and unlike the CO class. Emergent emission lines displayed considerable structure, as seen in V1974 Cyg, indicating fragmentation of the ejecta at the earliest stages of the outburst. Analysis and modeling of our ultraviolet spectra suggest that 4 - 5 $\times$ 10$^{-4}$M$_{\odot}$ of material was ejected and that the distance to the nova is $\simeq 2.5$ kpc. Relative to solar values, we find the following abundances: He = 1.0, C = 0.6$\pm$0.3, N = 17$\pm$4, O = 3.4$\pm$0.3, Ne = 17$\pm$3, Mg = 2.6$\pm$0.1, Al = 21$\pm$2, and Si = 0.5$\pm$0.3. Finally, we briefly draw comparisons with Nova LMC 2000, another ONeMg nova, for which similar data were obtained with HST and FUSE., Comment: 12 pages, 15 figures, accepted for publication in AJ, vol. 125, 2003 Mar
Published: 2003
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Region

Database

Publisher

2,729 results on '"Schwarz G."'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources