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1. Mid-range visual deficits after stroke: Prevalence and co-occurrence.

Author: Nikki A Lammers, Nils S Van den Berg, Selma Lugtmeijer, Anouk R Smits, Yair Pinto, Edward H F de Haan, and visual brain group
Subjects: Medicine, Science
Abstract: Visual deficits are common after stroke and are powerful predictors for the chronic functional outcome. However, while basic visual field and recognition deficits are relatively easy to assess with standardized methods, selective deficits in visual primitives, such as shape or motion, are harder to identify, as they often require a symmetrical bilateral posterior lesion in order to provoke full field deficits. Therefore, we do not know how often they occur. Nevertheless, they can have severe repercussions for daily-life functioning. We aimed to investigate the prevalence and co-occurrence of hemifield "mid-range" visual deficits (i.e. color, shape, location, orientation, correlated motion, contrast, texture and glossiness), using a novel experimental set-up with a gaze-contingent presentation of the stimuli. To this end, a prospective cohort of 220 ischemic (sub)cortical stroke patients and a healthy control group was assessed with this set-up. When comparing performance of patients with controls, the results showed that deficits in motion-perception were most prevalent (26%), followed by color (22%), texture (22%), location (21%), orientation (18%), contrast (14%), shape (14%) and glossiness (13%). 63% of the stroke patients showed one or more mid-range visual deficits. Overlap of deficits was small; they mostly occurred in isolation or co-occurred with only one or two other deficits. To conclude, it was found that deficits in "mid-range" visual functions were very prevalent. These deficits are likely to affect the chronic post-stroke condition. Since we found no strong patterns of co-occurrences, we suggest that an assessment of deficits at this level of visual processing requires screening the full range of visual functions.
Published: 2022
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2. A bright, high rotation-measure FRB that skewers the M33 halo

Author: L Connor, J van Leeuwen, L C Oostrum, E Petroff, Y Maan, E A K Adams, J J Attema, J E Bast, O M Boersma, H Dénes, D W Gardenier, J E Hargreaves, E Kooistra, I Pastor-Marazuela, R Schulz, A Sclocco, R Smits, S M Straal, D van der Schuur, D Vohl, B Adebahr, W J G de Blok, W A van Cappellen, A H W M Coolen, S Damstra, G N J van Diepen, B S Frank, K M Hess, B Hut, A Kutkin, G Marcel Loose, D M Lucero, Á Mika, V A Moss, H Mulder, T A Oosterloo, M Ruiter, H Vedantham, N J Vermaas, S J Wijnholds, and J Ziemke
Published: 2020
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3. Apercal - The Apertif calibration pipeline.

Author: Björn Adebahr, R. Schulz, Tammo Jan Dijkema, V. A. Moss, André R. Offringa, A. Kutkin, Jan M. van der Hülst, B. S. Frank, N. P. E. Vilchez, Joris Verstappen, Elizabeth A. K. Adams, W. J. G. de Blok, Helga Denes, Kelley M. Hess, D. Lucero, Raffaella Morganti, Tom Oosterloo, D.-J. Pisano, Marianna V. Ivashina, W. A. van Cappellen, L. D. Connor, A. H. W. M. Coolen, S. Damstra, G. Marcel Loose, Y. Maan, F. M. Maccagni, A. Mika, H. Mulder, Leon C. Oostrum, E. Orrú, R. Smits, D. van der Schuur, Joeri van Leeuwen, Dany Vohl, Stefan J. Wijnholds, and J. Ziemke
Published: 2022
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4. Tests of gravitational symmetries with pulsar binary J1713+0747

Author: W W Zhu, G Desvignes, N Wex, R N Caballero, D J Champion, P B Demorest, J A Ellis, G H Janssen, M Kramer, A Krieger, L Lentati, D J Nice, S M Ransom, I H Stairs, B W Stappers, J P W Verbiest, Z Arzoumanian, C G Bassa, M Burgay, I Cognard, K Crowter, T Dolch, R D Ferdman, E Fonseca, M E Gonzalez, E Graikou, L Guillemot, J W T Hessels, A Jessner, G Jones, M L Jones, C Jordan, R Karuppusamy, M T Lam, K Lazaridis, P Lazarus, K J Lee, L Levin, K Liu, A G Lyne, J W McKee, M A McLaughlin, S Osłowski, T Pennucci, D Perrodin, A Possenti, S Sanidas, G Shaifullah, R Smits, K Stovall, J Swiggum, G Theureau, and C Tiburzi
Published: 2018
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5. Characterising the Apertif primary beam response

Author: H. Dénes, K. M. Hess, E. A. K. Adams, A. Kutkin, R. Morganti, J. M. van der Hulst, T. A. Oosterloo, V. A. Moss, B. Adebahr, W. J. G. de Blok, M. V. Ivashina, A. H. W. M. Coolen, S. Damstra, B. Hut, G. M. Loose, D. M. Lucero, Y. Maan, Á. Mika, M. J. Norden, L. C. Oostrum, D. J. Pisano, R. Smits, W. A. van Cappellen, R. van den Brink, D. van der Schuur, G. N. J. van Diepen, J. van Leeuwen, D. Vohl, S. J. Wijnholds, J. Ziemke, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, German Research Foundation, Astronomy, and Kapteyn Astronomical Institute
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Methods: observational, Space and Planetary Science, Instrumentation: interferometers, Physics::Accelerator Physics, Instrumentation: detectors, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Telescopes
Abstract: Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. Phased array feeds (PAFs) are multi-element receivers in the focal plane of a telescope that make it possible to simultaneously form multiple beams on the sky by combining the complex gains of the individual antenna elements. Recently, the Westerbork Synthesis Radio Telescope (WSRT) was upgraded with PAF receivers to carry out several observing programs, including two imaging surveys and a time-domain survey. The Apertif imaging surveys use a configuration of 40 partially overlapping compound beams (CBs) simultaneously formed on the sky and arranged in an approximately rectangular shape. Aims. This work is aimed at characterising the response of the 40 Apertif CBs to create frequency-resolved I, XX, and YY polarization empirical beam shapes. The measured CB maps can be used for the image deconvolution, primary beam correction, and mosaicking processes of Apertif imaging data. Methods. We used drift scan measurements to measure the response of each of the 40 Apertif CBs. We derived beam maps for all individual beams in I, XX, and YY polarisation in 10 or 18 frequency bins over the same bandwidth as the Apertif imaging surveys. We sampled the main lobe of the beams and the side lobes up to a radius of 0.6 degrees from the beam centres. In addition, we derived beam maps for each individual WSRT dish. Results. We present the frequency and time dependence of the beam shapes and sizes. We compared the compound beam shapes derived with the drift scan method to beam shapes derived with an independent method using a Gaussian Process Regression comparison between the Apertif continuum images and the NRAO VLA Sky Survey (NVSS) catalogue. We find a good agreement between the beam shapes derived with the two independent methods. © H. Dénes et al. 2022., This work makes use of data from the Apertif system installed at the Westerbork Synthesis Radio Telescope owned by ASTRON. ASTRON, the Netherlands Institute for Radio Astronomy, is an institute of the Dutch Research Council (“De Nederlandse Organisatie voor Wetenschappelijk Onderzoek, NWO). K.M.H. acknowledges financial support from the State Agency for Research of the Spanish Ministry of Science, Innovation and universities through the “Center of Excellence Severo Ochoa” awarded to the Instituto de Astrofísica de Andalucía (SEV-2017-0709) from the coordination of the participation in SKA-SPAIN, funded by the Ministry of Science and innovation (MICIN). EAKA is supported by the WISE research programme, which is financed by the Netherlands Organization for Scientific Research (NWO). J.M.vd.H. and K.M.H. acknowledge funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. 291531 (‘HIStoryNU’). B.A. acknowledges funding from the German Science Foundation DFG, within the Collaborative Research Center SFB1491 “Cosmic Interacting Matters - From Source to Signal”. Y.M., L.C.O., and R.S. acknowledge funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. 617199. J.vL. acknowledges funding from Vici research programme ‘ARGO’ with project number 639.043.815, financed by the Dutch Research Council (NWO). D.V. acknowledges support from the Netherlands eScience Center (NLeSC) under grant ASDI.15.406. This research has made use of NUMPY (van der Walt et al. 2011), SCIPY (Virtanen et al. 2020), ASTROPY, a community-developed core PYTHON package for Astronomy (Astropy Collaboration 2013, 2018; http://www.astropy.org), and scikit-learn (Pedregosa et al. 2011). Data availability: The FITS format CB maps generated from the drift scan observations are available from zenodo as two data sets. Frequency setting 1130-1430 MHz DOI: https://doi.org/10.5281/zenodo.6615555, 1220–1520 MHz DOI: https://doi.org/10.5281/zenodo.6544109. The raw drift scan data are stored on the Apertif Long Term Storage and can be requested for further analysis trough the ASTRON helpdesk (https://support.astron.nl/sdchelpdesk). The observation taskIDs used for the individual drift scan beam maps are listed within aperPB (https://github.com/apertif/aperPB, https://doi.org/10.5281/zenodo.6544109) in the task_id_lists directory with the following file names: task_ids_{beamID}.txt. The GP CB maps are available within the Apertif DR1, trough the ASTRON Virtual Observatory (https://vo.astron.nl/; detailed documentation on the Apertif DR1 is available here: http://hdl.handle.net/21.12136/B014022C-978B-40F6-96C6-1A3B1F4A3DB0).
Published: 2022

6. First release of Apertif imaging survey data

Author: E. A. K. Adams, B. Adebahr, W. J. G. de Blok, H. Dénes, K. M. Hess, J. M. van der Hulst, A. Kutkin, D. M. Lucero, R. Morganti, V. A. Moss, T. A. Oosterloo, E. Orrú, R. Schulz, A. S. van Amesfoort, A. Berger, O. M. Boersma, M. Bouwhuis, R. van den Brink, W. A. van Cappellen, L. Connor, A. H. W. M. Coolen, S. Damstra, G. N. J. van Diepen, T. J. Dijkema, N. Ebbendorf, Y. G. Grange, R. de Goei, A. W. Gunst, H. A. Holties, B. Hut, M. V. Ivashina, G. I. G. Józsa, J. van Leeuwen, G. M. Loose, Y. Maan, M. Mancini, Á. Mika, H. Mulder, M. J. Norden, A. R. Offringa, L. C. Oostrum, I. Pastor-Marazuela, D. J. Pisano, A. A. Ponomareva, J. W. Romein, M. Ruiter, A. P. Schoenmakers, D. van der Schuur, J. J. Sluman, R. Smits, K. J. C. Stuurwold, J. Verstappen, N. P. E. Vilchez, D. Vohl, K. J. Wierenga, S. J. Wijnholds, E. E. M. Woestenburg, A. W. Zanting, J. Ziemke, Astronomy, Kapteyn Astronomical Institute, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, and German Research Foundation
Subjects: Galaxies: ISM, Radio lines: galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Polarization, FOS: Physical sciences, Astronomy and Astrophysics, Surveys, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Radio continuum: galaxies
Abstract: Full list of authors: Adams, E. A. K.; Adebahr, B.; de Blok, W. J. G.; Denes, H.; Hess, K. M.; van der Hulst, J. M.; Kutkin, A.; Lucero, D. M.; Morganti, R.; Moss, V. A.; Oosterloo, T. A.; Orru, E.; Schulz, R.; van Amesfoort, A. S.; Berger, A.; Boersma, O. M.; Bouwhuis, M.; van den Brink, R.; van Cappellen, W. A.; Connor, L.; Coolen, A. H. W. M.; Damstra, S.; van Diepen, G. N. J.; Dijkema, T. J.; Ebbendorf, N.; Grange, Y. G.; de Goei, R.; Gunst, A. W.; Holties, H. A.; Hut, B.; Ivashina, M., V; Jozsa, G. I. G.; van Leeuwen, J.; Loose, G. M.; Maan, Y.; Mancini, M.; Mika, A.; Mulder, H.; Norden, M. J.; Offringa, A. R.; Oostrum, L. C.; Pastor-Marazuela, I; Pisano, D. J.; Ponomareva, A. A.; Romein, J. W.; Ruiter, M.; Schoenmakers, A. P.; van der Schuur, D.; Sluman, J. J.; Smits, R.; Stuurwold, K. J. C.; Verstappen, J.; Vilchez, N. P. E.; Vohl, D.; Wierenga, K. J.; Wijnholds, S. J.; Woestenburg, E. E. M.; Zanting, A. W.; Ziemke, J.--Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. Apertif is a phased-array feed system for the Westerbork Synthesis Radio Telescope, providing forty instantaneous beams over 300 MHz of bandwidth. A dedicated survey program utilizing this upgrade started on 1 July 2019, with the last observations taken on 28 February 2022. The imaging survey component provides radio continuum, polarization, and spectral line data. Aims. Public release of data is critical for maximizing the legacy of a survey. Toward that end, we describe the release of data products from the first year of survey operations, through 30 June 2020. In particular, we focus on defining quality control metrics for the processed data products. Methods. The Apertif imaging pipeline, Apercal, automatically produces non-primary beam corrected continuum images, polarization images and cubes, and uncleaned spectral line and dirty beam cubes for each beam of an Apertif imaging observation. For this release, processed data products are considered on a beam-by-beam basis within an observation. We validate the continuum images by using metrics that identify deviations from Gaussian noise in the residual images. If the continuum image passes validation, we release all processed data products for a given beam. We apply further validation to the polarization and line data products and provide flags indicating the quality of those data products. Results. We release all raw observational data from the first year of survey observations, for a total of 221 observations of 160 independent target fields, covering approximately one thousand square degrees of sky. Images and cubes are released on a per beam basis, and 3374 beams (of 7640 considered) are released. The median noise in the continuum images is 41.4 uJy beam−1, with a slightly lower median noise of 36.9 uJy beam−1 in the Stokes V polarization image. The median angular resolution is 11.6″/sin δ. The median noise for all line cubes, with a spectral resolution of 36.6 kHz, is 1.6 mJy beam−1, corresponding to a 3-σ H I column density sensitivity of 1.8 × 1020 atoms cm−2 over 20 km s−1 (for a median angular resolution of 24″ × 15″). Line cubes at lower frequency have slightly higher noise values, consistent with the global RFI environment and overall Apertif system performance. We also provide primary beam images for each individual Apertif compound beam. The data are made accessible using a Virtual Observatory interface and can be queried using a variety of standard tools. © E. A. K. Adams et al. 2022., This work makes use of data from the Apertif system installed at the Westerbork Synthesis Radio Telescope owned by ASTRON. ASTRON, the Netherlands Institute for Radio Astronomy, is an institute of the Dutch Research Council (“De Nederlandse Organisatie voor Wetenschappelijk Onderzoek, NWO). Apertif was partly financed by the NWO Groot projects Apertif (175.010.2005.015) and Apropos (175.010.2009.012). This work was partly supported by funding from the European Research Council under the European Union’s Seventh Frame-work Programme (FP/2007-2013), through ERC Grant Agreement No. 291531 (‘HIStoryNU’, PI: JMvdH) and ERC Advanced Grant RADIOLIFE-320745 (PI: RM), in addition to funding from NWO via grant TOP1EW.14.105 (PI: TAO). E.A.K.A. is supported by the WISE research programme, which is financed by NWO. B.A. acknowledges funding from the German Science Foundation DFG, within the Collaborative Research Center SFB1491 “Cosmic Interacting Matters - From Source to Signal”. KMH acknowledges financial support from the State Agency for Research of the Spanish Ministry of Science, Innovation and Universities through the “Center of Excellence Severo Ochoa” awarded to the Instituto de Astrofísica de Andalucía (SEV-2017-0709), from the coordination of the participation in SKA-SPAIN, funded by the Ministry of Science and Innovation (MCIN). OMB and JvL acknowledge funding from NWO under the Vici research program “ARGO” with project number 639.043.815. Y.M., L.C.O., R.S. and J.vL. acknowledge funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. 617199 (“ALERT”). IPM acknowledges funding from the Netherlands Research School for Astronomy (grant no. NOVA5-NW3-10.3.5.14). A.A.P. acknowledges support of the STFC consolidated grant ST/S000488/1. DV acknowledges support from the Netherlands eScience Center (NLeSC) under grant ASDI.15.406. This research has made use of NASA’s Astrophysics Data System Bibliographic Services and Astropy, (http://www.astropy.org) a community-developed core Python package for Astronomy (Astropy Collaboration 2013, 2018).
Published: 2022

7. The Apertif science verification campaign

Author: B. Adebahr, A. Berger, E. A. K. Adams, K. M. Hess, W. J. G. de Blok, H. Dénes, V. A. Moss, R. Schulz, J. M. van der Hulst, L. Connor, S. Damstra, B. Hut, M. V. Ivashina, G. M. Loose, Y. Maan, A. Mika, H. Mulder, M. J. Norden, L. C. Oostrum, E. Orrú, M. Ruiter, R. Smits, W. A. van Cappellen, J. van Leeuwen, N. J. Vermaas, D. Voh, J. Ziemke, Astronomy, Kapteyn Astronomical Institute, High Energy Astrophys. & Astropart. Phys (API, FNWI), Ministerio de Ciencia e Innovación (España), European Research Council, and German Research Foundation
Subjects: polarization, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: active, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, methods: data analysis, Astrophysics - Astrophysics of Galaxies, surveys, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: magnetic fields, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Context. The characteristics of the polarised radio sky are a key ingredient in constraining evolutionary models of magnetic fields in the Universe and their role in feedback processes. The origin of the polarised emission and the characteristics of the intergalactic medium on the line of sight can be investigated using large samples of polarised sources. Ancillary infrared (IR) and optical data can be used to study the nature of the emitting objects. Aims. We analyse five early science datasets from the APERture Tile in Focus (Apertif) phased array feed system to verify the polarisation capabilities of Apertif in view of future larger data releases. We aim to characterise the source population of the polarised sky in the L-Band using polarised source information in combination with IR and optical data. Methods. We use automatic routines to generate full field-of-view Q- and U-cubes and perform rotation measure (RM)-Synthesis, source finding, and cross-matching with published radio, optical, and IR data to generate polarised source catalogues. All sources were inspected individually by eye for verification of their IR and optical counterparts. Spectral energy distribution (SED)-fitting routines were used to determine photometric redshifts, star-formation rates, and galaxy masses. IR colour information was used to classify sources as active galactic nuclei (AGN) or star-forming-dominated and early- or late-type. Results. We surveyed an area of 56 deg2 and detected 1357 polarised source components in 1170 sources. The fraction of polarised sources is 10.57% with a median fractional polarisation of 4.70 ± 0.14%. We confirmed the reliability of the Apertif measurements by comparing them with polarised cross-identified NVSS sources. Average RMs of the individual fields lie within the error of the best Milky Way foreground measurements. All of our polarised sources were found to be dominated by AGN activity in the radio regime with most of them being radio-loud (79%) and of the Fanaroff-Riley (FR)II class (87%). The host galaxies of our polarised source sample are dominated by intermediate disc and star-forming disc galaxies. The contribution of star formation to the radio emission is on the order of a few percent for ≈10% of the polarised sources while for ≈90% it is completely dominated by the AGN. We do not see any change in fractional polarisation for different star-formation rates of the AGN host galaxies. Conclusions. The Apertif system is suitable for large-area high-sensitivity polarised sky surveys. The data products of the polarisation analysis pipeline can be used to investigate the Milky Way magnetic field on projected scales of several arcminutes as well as the origin of the polarised emission in AGN and the properties of their host galaxies. © ESO 2022., This research made use of Montage. It is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration’s Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology. The Montage distribution includes an adaptation of the MOPEX algorithm developed at the Spitzer Science Center. BA and AB acknowledge funding from the German Science Foundation DFG, within the Collaborative Research Center SFB1491 “Cosmic Interacting Matters - From Source to Signal”. EAKA is supported by the WISE research programme, which is financed by the Dutch Research Council (NWO). K.M.H. acknowledges funding from the State Agency for Research of the Spanish Ministry of Science, Innovation and Universities through the “Center of Excellence Severo Ochoa” awarded to the Instituto de Astrofísica de Andalucía (SEV-2017-0709); from grant RTI2018-096228-B-C31 (Ministry of Science, Innovation and Universities/State Agency for Research/European Regional Development Funds, European Union); and from the coordination of the participation in SKA-SPAIN, funded by the Ministry of Science and innovation (MICIN). J.M.vdH. and K.M.H. acknowledge funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. 291531 (‘HIStoryNU’). J.vL. acknowledges funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007–2013)/ERC Grant Agreement no. 617199 (‘ALERT’), and from Vici research programme ‘ARGO’ with project number 639.043.815, financed by the Dutch Research Council (NWO). DV acknowledges support from the Netherlands eScience Center (NLeSC) under grant ASDI.15.406. RS acknowledges funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007–2013)/ERC Grant Agreement No. 617199. LCO acknowledges funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007–2013)/ERC Grant Agreement No. 617199.
Published: 2022
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8. Developmental differences in higher-order resting-state networks in Autism Spectrum Disorder

Author: Dienke J. Bos, Tamar R. van Raalten, Bob Oranje, Anouk R. Smits, Nieke A. Kobussen, Janna van Belle, Serge A.R.B. Rombouts, and Sarah Durston
Subjects: Autism, Development, Connectivity, Networks, Independent Component Analysis, Computer applications to medicine. Medical informatics, R858-859.7, Neurology. Diseases of the nervous system, RC346-429
Abstract: Objective: Autism Spectrum Disorder (ASD) has been associated with a complex pattern of increases and decreases in resting-state functional connectivity. The developmental disconnection hypothesis of ASD poses that shorter connections become overly well established with development in this disorder, at the cost of long-range connections. Here, we investigated resting-state connectivity in relatively young boys with ASD and typically developing children. We hypothesized that ASD would be associated with reduced connectivity between networks, and increased connectivity within networks, reflecting poorer integration and segregation of functional networks in ASD. Methods: We acquired resting-state fMRI from 27 boys with ASD and 29 age- and IQ-matched typically developing boys between 6 and 16 years of age. Functional connectivity networks were identified using Independent Component Analysis (ICA). Group comparisons were conducted using permutation testing, with and without voxel-wise correction for grey matter density. Results: We found no between-group differences in within-network connectivity. However, we did find reduced functional connectivity between two higher-order cognitive networks in ASD. Furthermore, we found an interaction effect with age in the DMN: insula connectivity increased with age in ASD, whereas it decreased in typically developing children. Conclusions: These results show subtle changes in between network connectivity in relatively young boys with ASD. However, the global architecture of resting-state networks appeared to be intact. This argues against recent suggestions that changes in connectivity in ASD may be the most prominent during development.
Published: 2014
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9. Oganesson: Ein Edelgas, das weder edel noch ein Gas ist

Author: Peter Schwerdtfeger, Odile R. Smits, Paul Jerabek, and Jan-Michael Mewes
Subjects: General Medicine
Published: 2020
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10. The periodic table and the physics that drives it

Author: Peter Schwerdtfeger, Odile R. Smits, and Pekka Pyykkö
Subjects: Physics, Period (periodic table), General Chemical Engineering, Transactinide element, General Chemistry, Electron, 010402 general chemistry, 7. Clean energy, 01 natural sciences, 0104 chemical sciences, Standard Model, Theoretical physics, symbols.namesake, Pauli exclusion principle, 13. Climate action, 0103 physical sciences, symbols, Electron configuration, Quantum field theory, 010306 general physics, Relativistic quantum chemistry
Abstract: Mendeleev’s introduction of the periodic table of elements is one of the most important milestones in the history of chemistry, as it brought order into the known chemical and physical behaviour of the elements. The periodic table can be seen as parallel to the Standard Model in particle physics, in which the elementary particles known today can be ordered according to their intrinsic properties. The underlying fundamental theory to describe the interactions between particles comes from quantum theory or, more specifically, from quantum field theory and its inherent symmetries. In the periodic table, the elements are placed into a certain period and group based on electronic configurations that originate from the Pauli and Aufbau principles for the electrons surrounding a positively charged nucleus. This order enables us to approximately predict the chemical and physical properties of elements. Apparent anomalies can arise from relativistic effects, partial-screening phenomena (of type lanthanide contraction) and the compact size of the first shell of every l-value. Further, ambiguities in electron configurations and the breakdown of assigning a dominant configuration, owing to configuration mixing and dense spectra for the heaviest elements in the periodic table. For the short-lived transactinides, the nuclear stability becomes an important factor in chemical studies. Nuclear stability, decay rates, spectra and reaction cross sections are also important for predicting the astrophysical origin of the elements, including the production of the heavy elements beyond iron in supernova explosions or neutron-star mergers. In this Perspective, we critically analyse the periodic table of elements and the current status of theoretical predictions and origins for the heaviest elements, which combine both quantum chemistry and physics. As the International Year of the Periodic Table came to an end in 2019, the authors reflect on the chemistry and physics that drive the periodic table of the elements. This includes aspects of periodic trends, relativistic electronic-structure theory, nuclear-structure theory and the astrophysical origin of the elements.
Published: 2020
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11. Dual-frequency single-pulse study of PSR B0950+08

Author: A. V. Bilous, J. M. Grießmeier, T. Pennucci, Z. Wu, L. Bondonneau, V. Kondratiev, J. van Leeuwen, Y. Maan, L. Connor, L. C. Oostrum, E. Petroff, J. P. W. Verbiest, D. Vohl, J. W. McKee, G. Shaifullah, G. Theureau, O. M. Ulyanov, B. Cecconi, A. H. Coolen, S. Corbel, S. Damstra, H. Dénes, J. N. Girard, B. Hut, M. Ivashina, O. O. Konovalenko, A. Kutkin, G. M. Loose, H. Mulder, M. Ruiter, R. Smits, P. L. Tokarsky, N. J. Vermaas, V. V. Zakharenko, P. Zarka, J. Ziemke, High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Bilous, A, Griessmeier, J, Pennucci, T, Wu, Z, Bondonneau, L, Kondratiev, V, van Leeuwen, J, Maan, Y, Connor, L, Oostrum, L, Petroff, E, Verbiest, J, Vohl, D, Mckee, J, Shaifullah, G, Theureau, G, Ulyanov, O, Cecconi, B, Coolen, A, Corbel, S, Damstra, S, Denes, H, Girard, J, Hut, B, Ivashina, M, Konovalenko, O, Kutkin, A, Loose, G, Mulder, H, Ruiter, M, Smits, R, Tokarsky, P, Vermaas, N, Zakharenko, V, Zarka, P, and Ziemke, J
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Population, Frequency drift, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Radio telescope, stars: neutron, Pulsar, 0103 physical sciences, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Scintillation, Line-of-sight, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Interstellar medium, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: PSR B0950+08 is a bright non-recycled pulsar whose single-pulse fluence variability is reportedly large. Based on observations at two widely separated frequencies, 55 MHz (NenuFAR) and 1.4 GHz (Westerbork Synthesis Radio Telescope), we review the properties of these single pulses. We conclude that they are more similar to ordinary pulses of radio emission than to a special kind of short and bright Giant Pulses, observed from only a handful of pulsars. We argue that temporal variation of properties of interstellar medium along the line of sight to this nearby pulsar, namely the fluctuating size of decorrelation bandwidth of diffractive scintillation makes important contribution to observed single-pulse fluence variability. We further present interesting structures in the low-frequency single-pulse spectra that resemble the "sad trombones" seen in Fast Radio Bursts (FRBs); although for PSR B0950+08 the upward frequency drift is also routinely present. We explain these spectral features with radius-to-frequency mapping, similar to the model developed by Wang et al. (2019) for FRBs. Finally, we speculate that microsecond-scale fluence variability of the general pulsar population remains poorly known, and that its further study may bring important clues about the nature of FRBs., Accepted by A&A. This version includes a number of minor corrections, including corrected FRB luminosities on the time-luminosity phase-space plot for radio pulses from neutron stars and repeating FRBs
Published: 2022
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12. Apertif: Phased array feeds for the Westerbork Synthesis Radio Telescope. System overview and performance characteristics

Author: W. A. van Cappellen, T. A. Oosterloo, M. A. W. Verheijen, E. A. K. Adams, B. Adebahr, R. Braun, K. M. Hess, H. Holties, J. M. van der Hulst, B. Hut, E. Kooistra, J. van Leeuwen, G. M. Loose, R. Morganti, V. A. Moss, E. Orrú, M. Ruiter, A. P. Schoenmakers, N. J. Vermaas, S. J. Wijnholds, A. S. van Amesfoort, M. J. Arts, J. J. Attema, L. Bakker, C. G. Bassa, J. E. Bast, P. Benthem, R. Beukema, R. Blaauw, W. J. G. de Blok, M. Bouwhuis, R. H. van den Brink, L. Connor, A. H. W. M. Coolen, S. Damstra, G. N. J. van Diepen, R. de Goei, H. Dénes, M. Drost, N. Ebbendorf, B. S. Frank, D. W. Gardenier, M. Gerbers, Y. G. Grange, T. Grit, A. W. Gunst, N. Gupta, M. V. Ivashina, G. I. G. Józsa, G. H. Janssen, A. Koster, G. H. Kruithof, S. J. Kuindersma, A. Kutkin, D. M. Lucero, Y. Maan, F. M. Maccagni, J. van der Marel, A. Mika, J. Morawietz, H. Mulder, E. Mulder, M. J. Norden, A. R. Offringa, L. C. Oostrum, R. E. Overeem, Z. Paragi, H. J. Pepping, E. Petroff, D. J. Pisano, A. G. Polatidis, P. Prasad, J. P. R. de Reijer, J. W. Romein, J. Schaap, G. W. Schoonderbeek, R. Schulz, D. van der Schuur, A. Sclocco, J. J. Sluman, R. Smits, B. W. Stappers, S. M. Straal, K. J. C. Stuurwold, J. Verstappen, D. Vohl, K. J. Wierenga, E. E. M. Woestenburg, A. W. Zanting, J. Ziemke, Astronomy, and Kapteyn Astronomical Institute
Subjects: Radio telescope, Physics, Space and Planetary Science, Phased array, Instrumentation: interferometers, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, Telescopes
Abstract: We describe the APERture Tile In Focus (Apertif) system, a phased array feed (PAF) upgrade of the Westerbork Synthesis Radio Telescope that transforms this telescope into a high-sensitivity, wide-field-of-view L-band imaging and transient survey instrument. Using novel PAF technology, up to 40 partially overlapping beams are formed on the sky simultaneously, significantly increasing the survey speed of the telescope. With this upgraded instrument, an imaging survey covering an area of 2300 deg2 is being performed that will deliver both continuum and spectral line datasets, of which the first data have been publicly released. In addition, a time domain transient and pulsar survey covering 15 000 deg2 is in progress. An overview of the Apertif science drivers, hardware, and software of the upgraded telescope is presented, along with its key performance characteristics.
Published: 2022

13. Removal and replacement of interference in tied-array radio pulsar observations using the spectral kurtosis estimator

Author: S. Sanidas, Kejia Lee, C. G. Bassa, Ramesh Karuppusamy, Ismaël Cognard, M. B. Purver, D. Perrodin, K. Liu, Michael Kramer, Gemma H. Janssen, J. W. McKee, Benjamin Stappers, R. Smits, ITA, GBR, FRA, DEU, CAN, NLD, and CHN
Subjects: Gaussian, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Interference (wave propagation), 01 natural sciences, law.invention, Telescope, 010104 statistics & probability, symbols.namesake, Pulsar, law, 0103 physical sciences, 0101 mathematics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Statistical hypothesis testing, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Estimator, Astronomy and Astrophysics, Computational physics, Amplitude, Space and Planetary Science, Kurtosis, symbols, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We describe how to implement the spectral kurtosis method of interference removal (zapping) on a digitized signal of averaged power values. Spectral kurtosis is a hypothesis test, analogous to the t-test, with a null hypothesis that the amplitudes from which power is formed belong to a `good' distribution -- typically Gaussian with zero mean -- where power values are zapped if the hypothesis is rejected at a specified confidence level. We derive signal-to-noise ratios (SNRs) as a function of amount of zapping for folded radio pulsar observations consisting of a sum of signals from multiple telescopes in independent radio-frequency interference (RFI) environments, comparing four methods to compensate for lost data with coherent (tied-array) and incoherent summation. For coherently summed amplitudes, scaling amplitudes from non-zapped telescopes achieves a higher SNR than replacing zapped amplitudes with artificial noise. For incoherently summed power values, the highest SNR is given by scaling power from non-zapped telescopes to maintain a constant mean. We use spectral kurtosis to clean a tied-array radio pulsar observation by the Large European Array for Pulsars (LEAP): the signal from one telescope is zapped with time and frequency resolutions of 6.25 $\mu$s and 0.16 MHz, removing interference along with 0.27 per cent of `good' data, giving an uncertainty of 0.25 $\mu$s in pulse time of arrival (TOA) for PSR J1022+1001. We use a single-telescope observation to demonstrate recovery of the pulse profile shape, with 0.6 per cent of data zapped and a reduction from 1.22 to 0.70 $\mu$s in TOA uncertainty., Comment: 16 pages, 9 figures
Published: 2022

14. Evaluation of divergent N-echelon (s, nQ)-policies under compound renewal demand.

Author: Gudrun P. Kiesmüller, Ton G. de Kok, Sanne R. Smits, and Peter J. M. van Laarhoven
Published: 2004
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15. Oganesson ist ein Halbleiter: Über die relativitische Bandlückenkontraktion in den schwersten Edelgasen

Author: Jan-Michael Mewes, Odile R. Smits, Peter Schwerdtfeger, and Paul Jerabek
Subjects: Physics, General Medicine
Published: 2019
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16. Solid Oganesson via a Many-Body Interaction Expansion Based on Relativistic Coupled-Cluster Theory and from Plane-Wave Relativistic Density Functional Theory

Author: Peter Schwerdtfeger, Kirk A. Peterson, Odile R. Smits, Jan-Michael Mewes, and Paul Jerabek
Subjects: 010304 chemical physics, Chemistry, Plane wave, Interaction model, 010402 general chemistry, 01 natural sciences, 0104 chemical sciences, law.invention, Pseudopotential, Dipole, Coupled cluster, Projector, law, Quantum electrodynamics, 0103 physical sciences, Density functional theory, Physical and Theoretical Chemistry, Dispersion (water waves)
Abstract: Many-body potentials up to fourth order are constructed using nonrelativistic, scalar-relativistic, and relativistic coupled-cluster theory to accurately describe the interaction between superheavy oganesson atoms. The obtained distance-dependent energy values were fitted to extended two-body Lennard-Jones and three-body Axilrod-Teller-Muto potentials, with the fourth-order term treated through a classical long-range Drude dipole interaction model. From these interaction potentials, spectroscopic constants for the oganesson dimer and solid-state properties were obtained. Furthermore, these high-level results are compared to scalar-relativistic and two-component plane-wave DFT calculations based on a tailor-made projector augmented wave pseudopotential (PAW-PP) and newly derived parameters for Grimme's dispersion correction. It is shown that the functionals PBE-D3(BJ), PBEsol, and in particular SCAN provide excellent agreement with the many-body reference for solid oganesson. Finally, the results for oganesson are compared and related to the lighter rare gas elements, and periodic trends are discussed.
Published: 2019
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17. P01.04.A Lesion-symptom mapping based on stroke or glioma: etiology matters!

Author: E E van Grinsven, A R Smits, E van Kessel, M Raemaekers, E H F de Haan, I M C Huenges-Wajer, V J Ruijters, M E P Philippens, J J C Verhoeff, N F Ramsey, P A J T Robe, T J Snijders, and M J E van Zandvoort
Subjects: Cancer Research, Oncology, Neurology (clinical)
Abstract: Background Lesion-symptom mapping is a key tool in understanding the relationship between brain structures and behavior. However, the behavioral consequences of lesions from different etiologies may vary as a result of how they affect brain tissue, and how they are distributed. The inclusion of different etiologies would increase the statistical power and improve generalizability of results, but has been critically debated. Findings from lesion studies are a resource for clinicians and used across different etiologies. This study directly compared lesion-symptom maps (LSM) between two populations (diffuse glioma versus ischemic stroke) in order to investigate if brain areas with adequate coverage in both groups, show topographical overlap in lesion-symptom associations. Material and Methods Data from two studies were combined. Both the glioma (N = 196, WHO grade 2-4) and stroke (N = 147) population underwent neuropsychological testing and an MRI, pre-operatively for the tumor population and within three months after stroke. For the purpose of this study, we selected two widely used cognitive tasks, the Rey Auditory Verbal Learning Test and the verbal fluency test. We used a state-of-the-art machine learning-based, multivariate voxel-wise approach to produce LSM for these cognitive tasks for both populations separately. Results For both tumor and stroke, our etiology-specific LSM largely followed the expected neuroanatomical pattern based on previous literature. Nevertheless, for both tasks substantial differences in LSM-results were present between the populations in brain areas with adequate coverage in both groups, though we did find similar white matter tracts involved in memory and semantic fluency performance across etiologies. Post-hoc analyses of these locations confirmed an interaction between lesion presence and etiology for a majority of these regions; damage by a tumor, but not a stroke, was related to worse cognitive performance for these regions. Conclusion This study provides the first direct comparison of LSM in a large cohort of patients. Differences in LSM were found between the glioma and stroke group, confirming that etiology matters when investigating the cognitive consequence of lesions. These differences could partly be explained by differences in lesion volume and topography. Nonetheless, the pattern shown by glioma patients on the group level is consistent with localizations found in earlier studies on both stroke and glioma patients using different techniques. While glioma series thus can be used to provide converging evidence about functional localization, we do suggest that findings from LSM studies in neuro-oncological populations should be considered as cause-specific. Findings from functional localization research from non-glioma populations should only be applied to a glioma population with caution.
Published: 2022
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18. Chromatic periodic activity down to 120 megahertz in a fast radio burst

Author: H. Dénes, S. M. Straal, Tom Oosterloo, Thijs van der Hulst, A. Kutkin, Joeri van Leeuwen, Dany Vohl, Henk Mulder, Jisk Attema, W. J. G. de Blok, M. J. Norden, Alessio Sclocco, Oliver M. Boersma, Á. Mika, S. Damstra, Sander ter Veen, Stefan J. Wijnholds, Kelley M. Hess, Emanuela Orrú, Daniel van der Schuur, Elizabeth A. K. Adams, E. Kooistra, Liam Connor, A. H. W. M. Coolen, Yogesh Maan, R. Smits, M. Ruiter, L. C. Oostrum, D. M. Lucero, Inés Pastor-Marazuela, B. Hut, Emily Petroff, V. Marianna Ivashina, A. V. Bilous, B. Adebahr, G. Marcel Loose, Vanessa A. Moss, High Energy Astrophys. & Astropart. Phys (API, FNWI), API Other Research (FNWI), Astronomy, and Kapteyn Astronomical Institute
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Brightness, Multidisciplinary, High-energy astronomy, Fast radio burst, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Radiation, Wavelength, Sky, Chromatic scale, Astrophysics - High Energy Astrophysical Phenomena, media_common, Time domain astronomy
Abstract: Fast radio bursts (FRBs) are extragalactic astrophysical transients whose brightness requires emitters that are highly energetic, yet compact enough to produce the short, millisecond-duration bursts. FRBs have thus far been detected between 300 MHz and 8 GHz, but lower-frequency emission has remained elusive. A subset of FRBs is known to repeat, and one of those sources, FRB 20180916B, does so with a 16.3 day activity period. Using simultaneous Apertif and LOFAR data, we show that FRB 20180916B emits down to 120 MHz, and that its activity window is both narrower and earlier at higher frequencies. Binary wind interaction models predict a narrower periodic activity window at lower frequencies, which is the opposite of our observations. Our detections establish that low-frequency FRB emission can escape the local medium. For bursts of the same fluence, FRB 20180916B is more active below 200 MHz than at 1.4 GHz. Combining our results with previous upper-limits on the all-sky FRB rate at 150 MHz, we find that there are 3-450 FRBs/sky/day above 50 Jy ms at 90% confidence. We are able to rule out the scenario in which companion winds cause FRB periodicity. We also demonstrate that some FRBs live in clean environments that do not absorb or scatter low-frequency radiation., Comment: 50 pages, 14 figures, 3 tables, submitted
Published: 2021

19. A search for radio emission from double-neutron star merger GW190425 using Apertif

Author: Dany Vohl, G. M. Loose, A. Kutkin, Kelley M. Hess, L. C. Oostrum, Á. Mika, H. Dénes, S. Damstra, Marianna Ivashina, M. Ruiter, R. H. S. van den Brink, B. Adebahr, D. van der Schuur, Liam Connor, N. J. Vermaas, V. A. Moss, Yogesh Maan, J. M. van der Hulst, Henk Mulder, W. J. G. de Blok, A. H. W. M. Coolen, Oliver M. Boersma, Tom Oosterloo, Elizabeth A. K. Adams, R. Smits, Joeri van Leeuwen, J. Ziemke, D. M. Lucero, B. Hut, High Energy Astrophys. & Astropart. Phys (API, FNWI), API Other Research (FNWI), and Astronomy
Subjects: Astrophysics and Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Radio telescope, stars: neutron, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Luminosity distance, Astrophysics::Galaxy Astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Epoch (reference date), Detector, Astronomy and Astrophysics, Galaxy, Afterglow, Neutron star, gravitational waves, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, radio continuum: stars
Abstract: Detection of the electromagnetic emission from coalescing binary neutron stars (BNS) is important for understanding the merger and afterglow. We present a search for a radio counterpart to the gravitational-wave source GW190425, a BNS merger, using Apertif on the Westerbork Synthesis Radio Telescope (WSRT). We observe a field of high probability in the associated localisation region for 3 epochs at 68, 90 and 109 days post merger. We identify all sources that exhibit flux variations consistent with the expected afterglow emission of GW190425. We also look for possible transients. These are sources which are only present in one epoch. In addition, we quantify our ability to search for radio afterglows in fourth and future observing runs of the gravitational-wave detector network using Monte Carlo simulations. We found 25 afterglow candidates based on their variability. None of these could be associated with a possible host galaxy at the luminosity distance of GW190425. We also found 55 transient afterglow candidates that were only detected in one epoch. All turned out to be image artefacts. In the fourth observing run, we predict that up to three afterglows will be detectable by Apertif. While we did not find a source related to the afterglow emission of GW190425, the search validates our methods for future searches of radio afterglows., 11 pages, 7 figures, accepted for publication
Published: 2021

20. Limits on Anisotropy in the Nanohertz Stochastic Gravitational Wave Background

Author: S. R. Taylor, C. M. F. Mingarelli, J. R. Gair, A. Sesana, G. Theureau, S. Babak, C. G. Bassa, P. Brem, M. Burgay, R. N. Caballero, D. J. Champion, I. Cognard, G. Desvignes, L. Guillemot, J. W. T. Hessels, G. H. Janssen, R. Karuppusamy, M. Kramer, A. Lassus, P. Lazarus, L. Lentati, K. Liu, S. Osłowski, D. Perrodin, A. Petiteau, A. Possenti, M. B. Purver, P. A. Rosado, S. A. Sanidas, R. Smits, B. Stappers, C. Tiburzi, R. van Haasteren, A. Vecchio, and J. P. W. Verbiest
Published: 2015
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21. Determination of instants of significant excitation in speech using group delay function.

Author: R. Smits and B. Yegnanarayana 0001
Published: 1995
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22. The Lennard Jones Potential Revisited -- Analytical Expressions for Vibrational Effects in Cubic and Hexagonal Close-Packed Lattices

Author: Antony Burrows, Odile R. Smits, and Peter Schwerdtfeger
Subjects: Condensed Matter - Materials Science, 010304 chemical physics, Condensed matter physics, Vibrational energy, Analytical expressions, Chemistry, Anharmonicity, Close-packing of equal spheres, Materials Science (cond-mat.mtrl-sci), FOS: Physical sciences, Grüneisen parameter, 010402 general chemistry, 01 natural sciences, 0104 chemical sciences, symbols.namesake, Lennard-Jones potential, 0103 physical sciences, symbols, Physics::Chemical Physics, Physical and Theoretical Chemistry, Einstein, Cohesive energy
Abstract: Analytical formulae are derived for the zero-point vibrational energy and anharmonicity corrections of the cohesive energy and the mode Gr\"{u}neisen parameter within the Einstein model for the cubic lattices (sc, bcc and fcc) and for the hexagonal close-packed structure. This extends the work done by Lennard Jones and Ingham in 1924, Corner in 1939 and Wallace in 1965. The formulae are based on the description of two-body energy contributions by an inverse power expansion (extended Lennard-Jones potential). These make use of three-dimensional lattice sums, which can be transformed to fast converging series and accurately determined by various expansion techniques. We apply these new lattice sum expressions to the rare gas solids and discuss associated critical points. The derived formulae give qualitative but nevertheless deep insight into vibrational effects in solids from the lightest (helium) to the heaviest rare gas element (oganesson), both presenting special cases because of strong quantum effects for the former and strong relativistic effects for the latter., Comment: 63 pages, 26 figures
Published: 2020

23. Accurate elemental boiling points from first principles

Author: Odile R. Smits and Jan-Michael Mewes
Subjects: Physics, 010405 organic chemistry, Extrapolation, General Physics and Astronomy, Thermodynamics, Thermodynamic integration, 010402 general chemistry, 01 natural sciences, 0104 chemical sciences, Gibbs free energy, Absolute deviation, symbols.namesake, Boiling point, symbols, Physical and Theoretical Chemistry, Hamiltonian (quantum mechanics), Ambient pressure
Abstract: The normal boiling point (NBP) is a fundamental property of liquids and marks the intersection of the Gibbs energies of the liquid and the gas-phase at ambient pressure. This work provides the first comprehensive demonstration of the calculation of boiling points of atomic liquids through first-principles molecular-dynamics simulations. To this end, thermodynamic integration (TDI) and perturbation theory (TPT) are combined with a density-functional theory (DFT) Hamiltonian, which provides absolute Gibbs energies, internal energies, and entropies of atomic liquids with an accuracy of a few meV/atom. Linear extrapolation to the intersection with the Gibbs energy of a non-interacting gas-phase eventually pins-down the NBPs. While these direct results can already be quite accurate, they are susceptible to a systematic over or underbinding of the employed density functional. It is shown how this dependency can be strongly reduced and the robustness of the method increased through a simple linear correction termed λ-scaling. Eventually, by carefully tuning of the technical parameters of the approach, the walltime per element is reduced from weeks to about a day (10–20k core-hours), enabling extensive testing for B, Al, Na, K, Ca, Sr, Ba, Mn, Cu, Xe, and Hg. This comprehensive benchmark demonstrates the excellent performance and robustness of the approach with a mean absolute deviation (MAD) of less than 2% from experimental NBPs and very similar accuracy for liquid entropies (MAD 2.3 J (mol K)−1, 2% relative). In some cases, the uncertainties in the predictions are several times smaller than the variation between literature values, allowing us to clear out long-standing ambiguities in the NBPs of B and Ba.
Published: 2020

24. Oganesson: A Noble Gas Element That Is Neither Noble Nor a Gas

Author: Paul Jerabek, Jan-Michael Mewes, Odile R. Smits, and Peter Schwerdtfeger
Subjects: Physics, Phase transition, Period (periodic table), 010405 organic chemistry, Communication, Noble gas, Thermodynamics, Thermodynamic integration, free energy calculations, melting and boiling processes, General Chemistry, 010402 general chemistry, 01 natural sciences, Catalysis, Communications, 0104 chemical sciences, Monte Carlo simulations, Boiling point, Melting point, Oganesson, Density functional theory, Relativistic quantum chemistry, ddc:620.11, density functional theory
Abstract: Oganesson (Og) is the last entry into the Periodic Table completing the seventh period of elements and group 18 of the noble gases. Only five atoms of Og have been successfully produced in nuclear collision experiments, with an estimate half‐life for 294118 Og of 0.69+0.64-0.22 ms.[1] With such a short lifetime, chemical and physical properties inevitably have to come from accurate relativistic quantum theory. Here, we employ two complementary computational approaches, namely parallel tempering Monte‐Carlo (PTMC) simulations and first‐principles thermodynamic integration (TI), both calibrated against a highly accurate coupled‐cluster reference to pin‐down the melting and boiling points of this super‐heavy element. In excellent agreement, these approaches show Og to be a solid at ambient conditions with a melting point of ≈325 K. In contrast, calculations in the nonrelativistic limit reveal a melting point for Og of 220 K, suggesting a gaseous state as expected for a typical noble gas element. Accordingly, relativistic effects shift the solid‐to‐liquid phase transition by about 100 K., Is the latest addition to the periodic table an actual or a formal noble gas? Two complementary state‐of‐the‐art approaches reveal in unison that Og is a solid at ambient conditions. And with predicted melting and boiling points of 325±15 K and 450±10 K, not even particularly volatile.
Published: 2020
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25. Repeating fast radio bursts with WSRT/Apertif

Author: Alessio Sclocco, J. M. van der Hulst, G. van Diepen, Jisk Attema, W. J. G. de Blok, R. H. van den Brink, D. W. Gardenier, N. J. Vermaas, S. ter Veen, Tom Oosterloo, Stefan J. Wijnholds, M. J. Norden, Henk Mulder, Liam Connor, B. Adebahr, G. M. Loose, D. M. Lucero, B. Hut, Emily Petroff, W. A. van Cappellen, J.-P. de Reijer, J. Ziemke, L. C. Oostrum, S. Damstra, Elizabeth A. K. Adams, Dany Vohl, A. H. W. M. Coolen, R. Smits, D. van der Schuur, Emanuela Orru, Á. Mika, Yogesh Maan, J. E. Bast, M. Ruiter, Vanessa A. Moss, J. van Leeuwen, B. S. Frank, Kelley M. Hess, R. Morganti, Marianna Ivashina, E. Kooistra, Samayra Straal, J. E. Hargreaves, Astronomy, Kapteyn Astronomical Institute, High Energy Astrophys. & Astropart. Phys (API, FNWI), and API Other Research (FNWI)
Subjects: stars, DEEP, media_common.quotation_subject, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, radio continuum, Radio telescope, SEARCHES, neutron, Pulsar, GIANT PULSES, 0103 physical sciences, REPETITION, 010306 general physics, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Spectral index, Astronomy and Astrophysics, Position angle, Stars, Space and Planetary Science, Sky, general, pulsars, Astrophysics - High Energy Astrophysical Phenomena, EMISSION, Energy (signal processing)
Abstract: Repeating fast radio bursts (FRBs) present excellent opportunities to identify FRB progenitors and host environments, as well as decipher the underlying emission mechanism. Detailed studies of repeating FRBs might also hold clues to the origin of FRBs as a population. We aim to detect the first two repeating FRBs: FRB 121102 (R1) and FRB 180814.J0422+73 (R2), and characterise their repeat statistics. We also want to significantly improve the sky localisation of R2. We use the Westerbork Synthesis Radio Telescope to conduct extensive follow-up of these two repeating FRBs. The new phased-array feed system, Apertif, allows covering the entire sky position uncertainty of R2 with fine spatial resolution in one pointing. We characterise the energy distribution and the clustering of detected R1 bursts. We detected 30 bursts from R1. Our measurements indicate a dispersion measure of 563.5(2) pc cm$^{-3}$, suggesting a significant increase in DM over the past few years. We place an upper limit of 8% on the linear polarisation fraction of the brightest burst. We did not detect any bursts from R2. A single power-law might not fit the R1 burst energy distribution across the full energy range or widely separated detections. Our observations provide improved constraints on the clustering of R1 bursts. Our stringent upper limits on the linear polarisation fraction imply a significant depolarisation, either intrinsic to the emission mechanism or caused by the intervening medium, at 1400 MHz that is not observed at higher frequencies. The non-detection of any bursts from R2 implies either a highly clustered nature of the bursts, a steep spectral index, or a combination of both. Alternatively, R2 has turned off completely, either permanently or for an extended period of time., 11 pages, 7 figures, submitted to A&A
Published: 2020

26. Statewide Treatment Center Referral Patterns for Adolescent and Young Adult Patients with Cancer in Utah

Author: Rochelle R. Smits-Seeman, Hongyan Li, Anne C. Kirchhoff, and Holly Spraker-Perlman
Subjects: Adult, medicine.medical_specialty, Adolescent, Referral, Cancer therapy, Cancer Care Facilities, Health Services Accessibility, Young Adult, 03 medical and health sciences, 0302 clinical medicine, Neoplasms, Utah, medicine, Humans, 030212 general & internal medicine, Young adult, Referral and Consultation, Academic Medical Centers, business.industry, Age Factors, Cancer, Facility type, medicine.disease, humanities, Treatment center, Oncology, 030220 oncology & carcinogenesis, Family medicine, Pediatrics, Perinatology and Child Health, business
Abstract: Cancer therapy is selected by individual oncology providers. For adolescent and young adults (AYAs), the type of provider, adult or pediatric, and medical facility type, non- or academic, influence regimens offered. We evaluated the proportions of 15-29-year-old cancer patients in Utah seen at pediatric and adult academic centers between 1994 and 2013 and examined factors that influence treatment location. Of all AYA patients, 31.6% were treated in academic centers and those with sarcomas, central nervous system tumors, and leukemias were more likely to be treated at academic centers. Further determinants of AYA healthcare access and cooperation between adult and pediatric providers are needed.
Published: 2018
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27. Ein hundert Jahre altes Experiment auf dem Prüfstand: hochgenaue Ab-Initio-Monte-Carlo-Schmelzsimulationen von Radon

Author: Paul Jerabek, Odile R. Smits, Peter Schwerdtfeger, and Elke Pahl
Subjects: Physics, 010405 organic chemistry, General Medicine, 010402 general chemistry, 01 natural sciences, 0104 chemical sciences
Published: 2018
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28. A Hundred-Year-Old Experiment Re-evaluated: Accurate Ab Initio Monte Carlo Simulations of the Melting of Radon

Author: Odile R. Smits, Paul Jerabek, Peter Schwerdtfeger, and Elke Pahl
Subjects: Phase transition, Materials science, 010405 organic chemistry, Direct sampling, Monte Carlo method, Extrapolation, Ab initio, chemistry.chemical_element, Radon, General Chemistry, 010402 general chemistry, 01 natural sciences, Catalysis, 0104 chemical sciences, Computational physics, chemistry, Cluster (physics), Parallel tempering
Abstract: State-of-the-art relativistic coupled-cluster theory is used to construct many-body potentials for the noble-gas element radon to determine its bulk properties including the solid-to-liquid phase transition from parallel tempering Monte Carlo simulations through either direct sampling of the bulk or from a finite cluster approach. The calculated melting temperature are 200(3) K and 200(6) K from bulk simulations and from extrapolation of finite cluster values, respectively. This is in excellent agreement with the often debated (but widely cited) and only available value of 202 K, dating back to measurements by Gray and Ramsay in 1909.
Published: 2018
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29. Exploratory study of the course of posttraumatic stress disorder after aneurysmal subarachnoid hemorrhage

Author: Gabriel J.E. Rinkel, Martine J. E. van Zandvoort, Irene M.C. Huenges Wajer, Anouk R. Smits, Johanna M A Visser-Meily, and Leoniek Wijngaards-de Meij
Subjects: Adult, Male, 050103 clinical psychology, Subarachnoid hemorrhage, Exploratory research, behavioral disciplines and activities, Stress Disorders, Post-Traumatic, 03 medical and health sciences, 0302 clinical medicine, mental disorders, medicine, Humans, 0501 psychology and cognitive sciences, Prospective Studies, Cognitive skill, Prospective cohort study, Group level, Aged, business.industry, Multilevel modelling, 05 social sciences, Intracranial Aneurysm, Middle Aged, Subarachnoid Hemorrhage, medicine.disease, Neuroticism, Psychiatry and Mental health, Posttraumatic stress, Disease Progression, Female, business, 030217 neurology & neurosurgery, Clinical psychology
Abstract: Objective Posttraumatic stress disorder (PTSD) occurs often in aneurysmal subarachnoid hemorrhage (aSAH) survivors, but how PTSD develops over time post-aSAH is still unclear. We examined the course of PTSD symptoms during the first year after aSAH. Method In this prospective cohort study, the Impact of Event Scale (IES) was applied in 128 patients 3, 6 and 12 months after aSAH. Multilevel modelling was used to assess changes in levels of PTSD symptoms over time and to explore if demographic characteristics, aSAH characteristics, level of education, cognitive functioning and neuroticism are associated to the course of PTSD symptoms. Results Multilevel analyses showed at group level no differences in the average level of PTSD symptoms between 3, 6 of 12 months post-aSAH (p = 0.22). At individual level, changes in PTSD symptoms over time were present (X2 (121) = 149.73 p = 0.04). None of the factors could explain the variance in change of PTSD symptoms over time. Conclusions The course of PTSD appears to differ between individuals after aSAH. We found no factors that explain these differences. There is not one optimal moment in time to assess PTSD. Therefore, it is important to assess PTSD at several time points after aSAH.
Published: 2018
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30. Follow-Up Care Provider Preferences of Adolescent and Young Adult Cancer Survivors

Author: Eduardo R. Zamora, Sapna Kaul, Rochelle R. Smits-Seemann, Joemy M. Ramsay, Anne C. Kirchhoff, and Karely Mann
Subjects: Adult, Male, medicine.medical_specialty, Adolescent, Health Personnel, Aftercare, Survivorship, Patient Care Planning, Young Adult, 03 medical and health sciences, 0302 clinical medicine, Cancer Survivors, Neoplasms, Survivorship curve, Humans, Medicine, 030212 general & internal medicine, Young adult, business.industry, Cancer, Transitional Care, Original Articles, Prognosis, medicine.disease, humanities, Follow up care, Oncology, 030220 oncology & carcinogenesis, Family medicine, Pediatrics, Perinatology and Child Health, Female, business, Delivery of Health Care, Healthcare providers, Follow-Up Studies
Abstract: Purpose: To explore the experiences and perspectives of adolescent and young adult (AYA) cancer survivors regarding patient–provider relationships and their preferences surrounding type of healthcare provider for follow-up care. Methods: We recruited AYA cancer survivors who were diagnosed between the ages of 15 and 39 using the Utah Cancer Registry. Twenty-eight survivors participated in six focus groups held between March and May of 2015 in Salt Lake City and St. George, Utah. This analysis focuses on how survivors' preferences about type of healthcare provider may influence their transition into, and utilization of, follow-up care. Results: On average, survivors were 6.3 (standard deviation = 1.7) years from their cancer diagnosis. A majority of survivors expressed a desire not to transition to a new provider and preferred continuing to see their oncologist for follow-up care. For these survivors, this was due to already having a close relationship with their oncologist and because they trusted their provider's knowledge about cancer and how to handle late effects. However, survivors placed emphasis on being comfortable with their healthcare provider, regardless of provider type. Conclusions: Our findings demonstrate the importance of formalizing provider transitions and roles after cancer therapy to improve patient comfort with new providers. By understanding the complexities of the transition from active cancer treatment to follow-up care for AYA survivors, these findings can inform programs undertaking post-care educational activities to ensure a seamless transition into survivorship care. Survivorship care plans can facilitate these transitions and improve patient confidence in follow-up care.
Published: 2018
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31. Mid-range visual functions in relation to higher-order visual functions after stroke

Author: Nils S. van den Berg, Nikki A. Lammers, Anouk R. Smits, Selma Lugtmeijer, Yair Pinto, Edward H.F. De Haan, Psychology Other Research (FMG), and Brein en Cognitie (Psychologie, FMG)
Subjects: higher-order cognitive functions, mid-range visual functions, Emotions, Brain, Cognitive artificial intelligence, patchwork model, stroke, Clinical Psychology, Cognition, Neuropsychology and Physiological Psychology, Neurology, Memory, Visual functions, Humans, Two-visual pathway model, Neurology (clinical)
Abstract: Contains fulltext : 285111.pdf (Publisher’s version ) (Open Access) Introduction: We aimed to investigate whether associations between deficits in "mid-range" visual functions and deficits in higher-order visual cognitive functions in stroke patients are more in line with a hierarchical, two-pathway model of the visual brain, or with a patchwork model, which assumes a parallel organization with many processing routes and cross-talk. Methods: A group of 182 ischemic stroke patients was assessed with a new diagnostic set-up for the investigation of a comprehensive range of visuosensory mid-range functions: color, shape, location, orientation, correlated motion, contrast and texture. With logistic regression analyses we investigated the predictive value of these mid-range functions for deficits in visuoconstruction (Copy of the Rey-Complex Figure Test), visual emotion recognition (Ekman 60 Faces Test of the FEEST) and visual memory (computerized Doors-test). Results: Results showed that performance on most mid-range visual tasks could not predict performance on higher-order visual cognitive tasks. Correlations were low to weak. Impaired visuoconstruction and visual memory were only modestly predicted by a worse location perception. Impaired emotion perception was modestly predicted by a worse orientation perception. In addition, double dissociations were found: there were patients with selective deficits in mid-range visual functions without higher-order visual deficits and vice versa. Conclusions: Our findings are not in line with the hierarchical, two-pathway model. Instead, the findings are more in line with alternative "patchwork" models, arguing for a parallel organization with many processing routes and cross-talk. However, future studies are needed to test these alternative models. 12 p.
Published: 2022
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32. A method for backward calculation of debris in a post blast scene

Author: J. Weerheijm, E. K. Verolme, K.W. Kang, M.M. van der Voort, R. Smits, and Y.H. Koh
Subjects: Quantitative method, Engineering, Forensic investigation, Strengths based, Explosive material, Ballistic properties, General Chemical Engineering, Defence Research, Explosions, Energy Engineering and Power Technology, Explosive safety, Terrain, Defence, Safety and Security, 02 engineering and technology, Management Science and Operations Research, Industrial and Manufacturing Engineering, 020401 chemical engineering, Accident investigation, 0502 economics and business, Accidental explosion, Accurate prediction, EBP - Explosions, Ballistics & Protection, 050207 economics, 0204 chemical engineering, High order, Safety, Risk, Reliability and Quality, Debris analysis, TS - Technical Sciences, Blast overpressure, business.industry, 05 social sciences, Structural engineering, Observation, Weapon & Protection Systems, Debris, Overpressure, Control and Systems Engineering, Accidents, Explosives, Terrorism, Stage (hydrology), business, Food Science, Marine engineering
Abstract: There is limited knowledge on deriving the strength of an explosion based on the observed explosion effects. Existing methods are based primarily on the effects of blast overpressure on surrounding structures. Window breakage and structural damage are well studied and are widely used to derive most probable explosion strengths. Other explosive effects such as debris throw are usually left out of such forensic analyses. In this paper, a quantitative method is presented that can be used to obtain the explosion strength based on debris throw. When the method is applied together with analysis of other evidence at a post blast scene, more accurate predictions of the original amount of explosive can be obtained. An overview of the required information that has to be collected from a post-blast scene is outlined, which will aid in the backward calculations that will be carried out in the next stage. This calculation method is applied to two case studies, which illustrate that it is applicable to events involving both low and high order accidental explosion events. Besides accidents, the method is also applicable to intentional explosion scenarios such as terrorist attacks. It is shown that the added value of such a method to forensic investigation depends on the precision of the data collected. Therefore, it is recommended that first responders not only register the impact locations but also attempt to identify the part of the donor installation from which the debris originated. Furthermore, estimates should be made of the launch height and ballistic properties of the debris and information should be recorded on obstructions and terrain properties in the vicinity. In this way, the quality of the backward calculations can be optimized. © 2017 Elsevier Ltd
Published: 2018
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33. A relativistic coupled-cluster interaction potential and rovibrational constants for the xenon dimer

Author: Odile R. Smits, Peter Schwerdtfeger, Paul Jerabek, and Elke Pahl
Subjects: 010304 chemical physics, Biophysics, chemistry.chemical_element, Rotational–vibrational spectroscopy, 010402 general chemistry, Condensed Matter Physics, 01 natural sciences, Potential energy, 0104 chemical sciences, Schrödinger equation, symbols.namesake, Superposition principle, Coupled cluster, Xenon, Lattice constant, chemistry, 0103 physical sciences, Physics::Atomic and Molecular Clusters, symbols, Physical and Theoretical Chemistry, Atomic physics, Molecular Biology, Basis set
Abstract: An accurate potential energy curve has been derived for the xenon dimer using state-of-the-art relativistic coupled-cluster theory up to quadruple excitations accounting for both basis set superposition and incompleteness errors. The data obtained is fitted to a computationally efficient extended Lennard-Jones potential form and to a modified Tang–Toennies potential function treating the short- and long-range part separately. The vibrational spectrum of Xe2 obtained from a numerical solution of the rovibrational Schrodinger equation and subsequently derived spectroscopic constants are in excellent agreement with experimental values. We further present solid-state calculations for xenon using a static many-body expansion up to fourth-order in the xenon interaction potential including dynamic effects within the Einstein approximation. Again we find very good agreement with the experimental (face-centred cubic) lattice constant and cohesive energy.
Published: 2017
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34. Risk of hospitalization among survivors of childhood and adolescent acute lymphoblastic leukemia compared to siblings and a general population sample

Author: Carol Sweeney, Sapna Kaul, Anne C. Kirchhoff, Rochelle R. Smits-Seemann, Judy Y. Ou, and Mark Fluchel
Subjects: Adult, Male, Cancer Research, Pediatrics, medicine.medical_specialty, Adolescent, Population sample, Epidemiology, Lymphoblastic Leukemia, Population, Article, Young Adult, 03 medical and health sciences, 0302 clinical medicine, Cancer Survivors, Risk Factors, Utah, Population Database, Humans, Medicine, 030212 general & internal medicine, education, Survival rate, Generalized estimating equation, Proportional Hazards Models, education.field_of_study, business.industry, Proportional hazards model, Siblings, Hazard ratio, Middle Aged, Precursor Cell Lymphoblastic Leukemia-Lymphoma, Hospitalization, Survival Rate, Oncology, 030220 oncology & carcinogenesis, Female, business
Abstract: Background Acute Lymphoblastic Leukemia (ALL) has a high survival rate, but cancer-related late effects in the early post-treatment years need documentation. Hospitalizations are an indicator of the burden of late effects. We identify rates and risk factors for hospitalization from five to ten years after diagnosis for childhood and adolescent ALL survivors compared to siblings and a matched population sample. Methods 176 ALL survivors were diagnosed at ≤22 years between 1998 and 2008 and treated at an Intermountain Healthcare facility. The Utah Population Database identified siblings, an age- and sex-matched sample of the Utah population, and statewide inpatient hospital discharges. Sex- and birth year-adjusted Poisson models with Generalized Estimating Equations and robust standard errors calculated rates and rate ratios. Cox proportional hazards models identified demographic and clinical risk factors for hospitalizations among survivors. Results Hospitalization rates for survivors (Rate:3.76, 95% CI = 2.22–6.36) were higher than siblings (Rate:2.69, 95% CI = 1.01–7.18) and the population sample (Rate:1.87, 95% CI = 1.13–3.09). Compared to siblings and population comparisons, rate ratios (RR) were significantly higher for survivors diagnosed between age 6 and 22 years (RR:2.87, 95% CI = 1.03–7.97 vs siblings; RR:2.66, 95% CI = 1.17–6.04 vs population comparisons). Rate ratios for diagnosis between 2004 and 2008 were significantly higher compared to the population sample (RR:4.29, 95% CI = 1.49, 12.32), but not siblings (RR:2.73, 95% CI = 0.54, 13.68). Survivors originally diagnosed with high-risk ALL did not have a significantly higher risk than siblings or population comparators. However, high-risk ALL survivors (Hazard ratio [HR]:3.36, 95% CI = 1.33–8.45) and survivors diagnosed from 2004 to 2008 (HR:9.48, 95% CI = 1.93–46.59) had the highest risk compared to their survivor counterparts. Conclusions Five to ten years after diagnosis is a sensitive time period for hospitalizations in the ALL population. Survivors of childhood ALL require better long-term surveillance.
Published: 2017
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35. Adolescent and Young Adult Cancer Survivors' Valuation of Post-Treatment Recommended Care

Author: Sapna Kaul, Rochelle R. Smits-Seemann, Eduardo R. Zamora, Holly Spraker-Perlman, Kevin J. Boyle, and Anne C. Kirchhoff
Subjects: Adult, Male, medicine.medical_specialty, Adolescent, media_common.quotation_subject, Aftercare, Young Adult, 03 medical and health sciences, 0302 clinical medicine, Qualitative analysis, Cancer Survivors, Willingness to pay, Humans, Medicine, 030212 general & internal medicine, Young adult, media_common, Valuation (finance), business.industry, Original Articles, Focus Groups, Payment, Focus group, Cancer registry, Oncology, 030220 oncology & carcinogenesis, Family medicine, Pediatrics, Perinatology and Child Health, Female, Health Expenditures, Post treatment, business, Social psychology
Abstract: Purpose: Examine whether survivors of adolescent and young adult (AYA) cancer value recommended post-treatment care using focus groups and a willingness to pay (WTP) survey. WTP, a measure of value, indicates the dollar amount individuals are willing to pay to use a service. Methods: Participants were recruited through the Utah Cancer Registry. N = 28 survivors diagnosed with cancer at ages 15–39 and currently aged ≥18 participated in focus groups, and N = 4 in phone interviews (participation rate = 50%). All participants responded to a demographic survey and WTP questions based on one-time and monthly payments for annual visits. Focus group participants responded to an open-ended question on the value of follow-up care. Interval regressions identified factors associated with WTP. Qualitative analysis summarized themes for the open-ended question. Results: Focus group participants reported valuing follow-up care as it brings peace of mind and helps them manage their health. Yet, 38% reported not having a cancer-related visit in the previous year. Only 27% and 43% of survivors agreed to pay any one-time and monthly payments, respectively. The monthly payment mean WTP was $41 (95% confidence interval [CI]: 31–84), equating to $494 annually, which is greater than the mean WTP for one-time payment ($362, 95% CI: 293–432, p
Published: 2017
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36. Abaelard: Epistolae

Author: Edmé R. Smits and Thomas Haye
Published: 2020
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37. Abaelard: Theologia christiana

Author: Marc-Aeilko Aris and Edmé R. Smits
Subjects: Philosophy
Published: 2020
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38. Correction to 'Solid Oganesson via a Many-Body Interaction Expansion Based on Relativistic Coupled-Cluster Theory and from Plane-Wave Relativistic Density Functional Theory'

Author: Paul Jerabek, Odile R. Smits, Jan-Michael Mewes, Kirk A. Peterson, and Peter Schwerdtfeger
Subjects: Physical and Theoretical Chemistry
Published: 2019

39. ESRA19-0668 Paravertebral block versus erector spinae plane block in patients undergoing breast cancer surgery: a feasibility study

Author: G.J. van Geffen, R Smits, M Fenten, and G Filippini-de Moor
Subjects: medicine.medical_specialty, business.industry, medicine.medical_treatment, Chronic pain, medicine.disease, Piritramide, Surgery, Regimen, Breast cancer, medicine, Paravertebral Block, business, Prospective cohort study, Oxycodone, Mastectomy, medicine.drug
Abstract: Background and aims Breast cancer patients have a very high incidence of chronic pain after mastectomy. a risk factor for chronification of pain is severe postoperative pain. the novel erector spinae plane block (ESPB) is considered to be a safer technique than the paravertebral block (PVB) for postoperative thoracic pain. Methods 20 patients were prospectively included: 10 patients received a PVB and 10 patients received a ESPB. Induction and maintenance of anesthesia, PONV prophylaxis and a complementary multimodal postoperative pain regimen was standardized for all patients. When the numeric rating scale of pain was >3, rescue medication was administered. Study parameters were opioid use in the first 24h; piritramide in the recovery room and oxycodone on the ward. Furthermore, discomfort experienced during placement of the block and overall postoperative patient satisfaction were scored using a numeric rating scale from 0 to 10. Results Patients received on average 8 mg (PVB) and 4,5 mg (ESPB) piritramide in the recovery room. In the first 24 hours postoperatively, patients received an additional 5,65 mg (PVB) and 1 mg (ESPB) oxycodone. Discomfort was rated as 3 in the PVB group and 1,7 in the ESPB group, satisfaction as 6,75 versus 8,6 respectively. Conclusions This prospective study was performed to demonstrate the feasibility of the ESPB. Although the study is underpowered for statistical comparisons, the results consistently suggest a better profile in favor of the ESPB. Randomized and adequately powered studies are necessary to confirm this hypothesis.
Published: 2019
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40. Oganesson Is a Semiconductor: On the Relativistic Band-Gap Narrowing in the Heaviest Noble-Gas Solids

Author: Jan-Michael Mewes, Odile R. Smits, Peter Schwerdtfeger, and Paul Jerabek
Subjects: Band gap, Electronic structure, 010402 general chemistry, 01 natural sciences, Catalysis, band gap, Perturbation theory, Electronic band structure, Physics, 010405 organic chemistry, business.industry, Communication, Noble gas, radon, General Chemistry, Communications, Superheavy Elements | Hot Paper, 0104 chemical sciences, superheavy elements, Semiconductor, noble gases, Density functional theory, oganesson, Atomic physics, Relativistic quantum chemistry, business
Abstract: Oganesson (Og) is the most recent addition to Group 18. Investigations of its atomic electronic structure have unraveled a tremendous impact of relativistic effects, raising the question whether the heaviest noble gas lives up to its position in the periodic table. To address the issue, we explore the electronic structure of bulk Og by means of relativistic Kohn–Sham density functional theory and many‐body perturbation theory in the form of the GW method. Calculating the band structure of the noble‐gas solids from Ne to Og, we demonstrate excellent agreement for the band gaps of the experimentally known solids from Ne to Xe and provide values of 7.1 eV and 1.5 eV for the unknown solids of Rn and Og. While this is in line with periodic trends for Rn, the band gap of Og completely breaks with these trends. The surprisingly small band gap of Og moreover means that, in stark contrast to all other noble‐gas solids, the solid form of Og is a semiconductor., Breaking rank: The electronic structure of the noble‐gas solids of neon to oganesson was investigated by means of relativistic density functional theory and many‐body perturbation theory. This revealed band gaps of 7.1 eV and 1.5 eV for the unknown solids of Rn and Og, which means that, in stark contrast to all other noble gases, solid Og is a (short‐lived) semiconductor.
Published: 2019

41. The domain effect in delay discounting: The roles of fungibility and perishability

Author: Andrew M. Tiry, Rochelle R. Smits-Seemann, Daniel D. Holt, and Kathryn Glodowski
Subjects: Adult, Discounting, Delay discounting, 05 social sciences, Commodity, General Medicine, Fungibility, Outcome (game theory), Young Adult, 03 medical and health sciences, Behavioral Neuroscience, 0302 clinical medicine, Delay Discounting, Reward, Value (economics), Economics, Econometrics, Perishability, Humans, 0501 psychology and cognitive sciences, Animal Science and Zoology, 050102 behavioral science & comparative psychology, Temporal discounting, health care economics and organizations, 030217 neurology & neurosurgery
Abstract: There is a growing body of literature demonstrating domain effects where the rate of temporal discounting depends, in part, on the commodity being evaluated. The commodity of money, for example, is typically discounted much less steeply than commodities of entertainment or food. There are several plausible explanations for domain effects: differences in conditioned reinforcer status, degree of fungibility, and differences in metabolic function. While money can be thought of as a conditioned reinforcer exchangeable for a number of different outcomes (highly fungible), comparing money to food (non-fungible) does not separate whether the difference in rates of discounting are due to food having metabolic importance, being perishable, being less fungible, or all of the above. We systematically manipulated the degree of fungibility and perishability of various outcomes and found that while food outcomes tend to be discounted most steeply, the rate of discounting for these outcomes can be moderated by reducing perishability and by increasing fungibility. Important here is that we have identified two independent means of moderating the effect of delay on the value of the outcome.
Published: 2016
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42. High-precision timing of 42 millisecond pulsars with the European Pulsar Timing Array

Author: P. Lazarus, R. van Haasteren, Christine Jordan, Pablo Rosado, Jason W. T. Hessels, S. Babak, Alberto Sesana, Joris P. W. Verbiest, Chiara M. F. Mingarelli, Benjamin Stappers, A. Jessner, D. J. Champion, J. W. McKee, J. R. Gair, Lucas Guillemot, Delphine Perrodin, Antoine Petiteau, P. Brem, Michael Kramer, Ramesh Karuppusamy, Andrew Lyne, Ismaël Cognard, Gregory Desvignes, Gilles Theureau, Kejia Lee, G. Shaifullah, E. Graikou, M. Burgay, Stefan Oslowski, M. B. Purver, Caterina Tiburzi, R. Smits, K. Lazaridis, Stephen Taylor, R. N. Caballero, Kang Liu, C. G. Bassa, A. Lassus, Gemma H. Janssen, Alberto Vecchio, S. Sanidas, L. Lentati, A. Possenti, Desvignes, G, Caballero, R, Lentati, L, Verbiest, J, Champion, D, Stappers, B, Janssen, G, Lazarus, P, Osłowski, S, Babak, S, Bassa, C, Brem, P, Burgay, M, Cognard, I, Gair, J, Graikou, E, Guillemot, L, Hessels, J, Jessner, A, Jordan, C, Karuppusamy, R, Kramer, M, Lassus, A, Lazaridis, K, Lee, K, Liu, K, Lyne, A, Mckee, J, Mingarelli, C, Perrodin, D, Petiteau, A, Possenti, A, Purver, M, Rosado, P, Sanidas, S, Sesana, A, Shaifullah, G, Smits, R, Taylor, S, Theureau, G, Tiburzi, C, van Haasteren, R, Vecchio, A, Max-Planck-Institut für Radioastronomie (MPIFR), Cavendish Laboratory, University of Cambridge [UK] (CAM), Universität Bielefeld, Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Netherlands Institute for Radio Astronomy ( ASTRON ), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), University of Amsterdam [Amsterdam] (UvA), Kavli Institute for Astronomy and Astrophysics [Beijing] (KIAA-PKU), Peking University [Beijing], APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Theoretical Astrophysics [Pasadena] (TAPIR), California Institute of Technology (CALTECH), Birmingham City University (BCU), National Natural Science Foundation of China (Grant No.11373011)., European Project: 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET(2014), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Division of Physics, Mathematics and Astronomy [Pasadena], California Institute of Technology (CALTECH)-California Institute of Technology (CALTECH), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: astro-ph.SR, FOS: Physical sciences, Proper motion, Astrophysics, Magnetar, 01 natural sciences, Radio spectrum, Radio telescope, Pulsar timing array, proper motions, Pulsar, Millisecond pulsar, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Stars: Distance, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Pulsars: General, Astronomy, Astronomy and Astrophysics, pulsars:general, European Pulsar Timing Array, Neutron star, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, stars: distances, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, stars:distances, astro-ph.IM
Abstract: We report on the high-precision timing of 42 radio millisecond pulsars (MSPs) observed by the European Pulsar Timing Array (EPTA). This EPTA Data Release 1.0 extends up to mid-2014 and baselines range from 7-18 years. It forms the basis for the stochastic gravitational-wave background, anisotropic background, and continuous-wave limits recently presented by the EPTA elsewhere. The Bayesian timing analysis performed with TempoNest yields the detection of several new parameters: seven parallaxes, nine proper motions and, in the case of six binary pulsars, an apparent change of the semi-major axis. We find the NE2001 Galactic electron density model to be a better match to our parallax distances (after correction from the Lutz-Kelker bias) than the M2 and M3 models by Schnitzeler (2012). However, we measure an average uncertainty of 80\% (fractional) for NE2001, three times larger than what is typically assumed in the literature. We revisit the transverse velocity distribution for a set of 19 isolated and 57 binary MSPs and find no statistical difference between these two populations. We detect Shapiro delay in the timing residuals of PSRs J1600$-$3053 and J1918$-$0642, implying pulsar and companion masses $m_p=1.22_{-0.35}^{+0.5} \text{M}_{\odot}$, $m_c = 0.21_{-0.04}^{+0.06} \text{M}_{\odot }$ and $m_p=1.25_{-0.4}^{+0.6} \text{M}_{\odot}$, $m_c = 0.23_{-0.05}^{+0.07} \text{M}_{\odot }$, respectively. Finally, we use the measurement of the orbital period derivative to set a stringent constraint on the distance to PSRs J1012$+$5307 and J1909$-$3744, and set limits on the longitude of ascending node through the search of the annual-orbital parallax for PSRs J1600$-$3053 and J1909$-$3744., Comment: 42 pages, 11 figures. Accepted for publication in MNRAS
Published: 2016
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43. Statistics of VHE gamma-Rays in Temporal Association with Radio Giant Pulses from the Crab Pulsar

Author: J. Palacio, J. M. Paredes, Antonio Stamerra, L. Maraschi, Elina Lindfors, Daniel Mazin, Chiara Righi, Wlodek Bednarek, Alessandro Carosi, P. Temnikov, Pratik Majumdar, N. Torres-Albà, M. V. Fonseca, S. N. Shore, Martin Will, Jose Miguel Miranda, E. Colombo, E. Prandini, Aaron Dominguez, Kari Nilsson, L. O. Takalo, Francesco Longo, Juan Abel Barrio, Masahiro Teshima, Nikola Godinovic, U. Menzel, L. A. Antonelli, Mosè Mariotti, D. Hadasch, J. E. Ward, Alba Fernández-Barral, M. Engelkemeier, Stefano Covino, Martin Makariev, Alexander Hahn, P. Colin, Saverio Lombardi, Andrea Rugliancich, Sidika Merve Colak, Oscar Blanch, Arka Chatterjee, Adrian Biland, Christian Fruck, Tomoki Saito, M. Doert, T. Surić, Shimpei Tsujimoto, M. Garczarczyk, Ana Babić, D. Fidalgo, M. Peresano, Camilla Maggio, J. Rico, S. Schroeder, Ivica Puljak, Ievgen Vovk, M. Vazquez Acosta, D. Dominis Prester, Tarek M. Hassan, B. Biasuzzi, Victoria Moreno, Fabrizio Tavecchio, L. Nogués, E. Moretti, D. Kuveždić, Jose Luis Contreras, Abelardo Moralejo, F. Di Pierro, Yusuke Konno, Juan Cortina, T. Schweizer, J. R. Garcia, Giacomo Bonnoli, A. De Angelis, A. Treves, Vitaly Neustroev, V. Fallah Ramazani, Max Ludwig Ahnen, Wrijupan Bhattacharyya, T. Nagayoshi, Daniela Dorner, Dariusz Gora, Gaia Vanzo, G. Maneva, Junko Kushida, P. Da Vela, Kyoshi Nishijima, U. Barres de Almeida, M. Minev, I. Reichardt, P. Giammaria, A. Niedzwiecki, R. Smits, M. Gaug, Damir Lelas, D. Elsaesser, I. Snidaric, Dorota Sobczyńska, J. Herrera, B. De Lotto, Julian Sitarek, Koji Noda, J. Hose, Elisa Bernardini, Stefano Ansoldi, David Paneque, M. I. Martínez, Riccardo Paoletti, D. Guberman, Marina Manganaro, Sabrina Einecke, D. Galindo, P. Cumani, Konstancja Satalecka, Michele Doro, Dario Hrupec, M. A. Lopez, S. Paiano, Karl Mannheim, P. G. Prada Moroni, Tomislav Terzić, Francesco Dazzi, J. Becerra González, Alessio Berti, Natalia Lewandowska, L. Perri, D. Eisenacher Glawion, Cosimo Nigro, M. Nievas Rosillo, B. Banerjee, C. Arcaro, Lluis Font, Marcel Strzys, R. J. García López, G. Pedaletti, Massimo Persic, Wolfgang Rhode, D. Ninci, M. Hayashida, D. Zarić, Marc Ribó, P. Bangale, Hidetoshi Kubo, R. Mirzoyan, Kazuma Ishio, Rodolfo Carosi, German Research Foundation, Istituto Nazionale di Fisica Nucleare, Istituto Nazionale di Astrofisica, Swiss National Science Foundation, Ministerio de Economía y Competitividad (España), Japan Society for the Promotion of Science, Ministry of Education, Culture, Sports, Science and Technology (Japan), Universidad de Barcelona, Croatian Science Foundation, University of Rijeka, Foundation for Polish Science, Ministério da Ciência, Tecnologia e Inovação (Brasil), Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babic, A., Banerjee, B., Bangale, P., Barres De Almeida, U., Barrio, J. A., Becerra Gonzalez, J., Bednarek, W., Bernardini, E., Berti, A., Bhattacharyya, W., Biasuzzi, B., Biland, A., Blanch, O., Bonnoli, G., Carosi, R., Carosi, A., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Di Pierro, F., Doert, M., Dominguez, A., Dominis Prester, D., Dorner, D., Doro, M., Einecke, S., Eisenacher Glawion, D., Elsaesser, D., Engelkemeier, M., Fallah Ramazani, V., Fernandez-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Fruck, C., Galindo, D., Garcia Lopez, R. J., Garczarczyk, M., Gaug, M., Giammaria, P., Godinovic, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Kuvez Dic, D., Lelas, D., Lewandowska, N., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Mazin, D., Menzel, U., Minev, M., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Nievas Rosillo, M., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Prada Moroni, P. G., Prandini, E., Puljak, I., Garcia, J. R., Reichardt, I., Rhode, W., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Satalecka, K., Schroeder, S., Schweizer, T., Shore, S. N., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Strzys, M., Suric, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Treves, A., Tsujimoto, S., Vanzo, G., Vazquez Acosta, M., Vovk, I., Ward, J. E., Will, M., Zaric, D., and Smits, R.
Subjects: Photon, Radiation mechanisms: non-thermal, Radio continuum: stars, VHE [gamma ray], Astrophysics, 01 natural sciences, Cherenkov, individual, 010303 astronomy & astrophysics, Pulsars: individual: Crab pulsar, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), photon, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, pulsed, Gamma rays: stars, pulsars: individual: Crab pulsar - gamma-rays: stars - radio continuum: stars - radiation mechanics: non-thermal, detector [radio wave], statistics, Crab pulsar, Global Positioning System, stars [Radio continuum], Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, stars, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, pulsars, gamma rays, radio continuum, radiation mechanisms, non-thermal, Astrophysics::Cosmology and Extragalactic Astrophysics, Radio telescope, star [Gamma rays], Pulsar, emission [gamma ray], 0103 physical sciences, 010306 general physics, enhancement, Astrophysics::Galaxy Astrophysics, Cherenkov radiation, non-thermal [Radiation mechanisms], business.industry, Crab Pulsar, stars [Gamma rays], Astronomy and Astrophysics, individual: Crab pulsar [Pulsars], MAGIC, flux, Stars, Space and Planetary Science, correlation, ddc:520, business, statistical
Abstract: [Aims] The aim of this study is to search for evidence of a common emission engine between radio giant pulses (GPs) and very-high-energy (VHE, E > 100 GeV) γ-rays from the Crab pulsar., [Methods] We performed 16 h of simultaneous observations of the Crab pulsar at 1.4 GHz with the Effelsberg radio telescope and the Westerbork Synthesis Radio Telescope (WSRT), and at energies above 60 GeV we used the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes. We searched for a statistical correlation between the radio and VHE γ-ray emission with search windows of different lengths and different time lags to the arrival times of a radio GP. A dedicated search for an enhancement in the number of VHE γ-rays correlated with the occurrence of radio GPs was carried out separately for the P1 and P2 phase ranges, respectively., [Results] In the radio data sample, 99444 radio GPs were detected. We find no significant correlation between the GPs and VHE photons in any of the search windows. Depending on phase cuts and the chosen search windows, we find upper limits at a 95% confidence level on an increase in VHE γ-ray events correlated with radio GPs between 7% and 61% of the average Crab pulsar VHE flux for the P1 and P2 phase ranges, respectively. This puts upper limits on the flux increase during a radio GP between 12% and 2900% of the pulsed VHE flux, depending on the search window duration and phase cuts. This is the most stringent upper limit on a correlation between γ-ray emission and radio GPs reported so far., The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ.
Published: 2019
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44. Tests of gravitational symmetries with pulsar binary J1713+0747

Author: Michael Kramer, Kang Liu, Robert D. Ferdman, Lina Levin, P. Lazarus, Marjorie Gonzalez, Michael T. Lam, Gemma H. Janssen, Kejia Lee, Timothy Dolch, Norbert Wex, Scott M. Ransom, Kathryn Crowter, A. Jessner, Ramesh Karuppusamy, J. K. Swiggum, Andrew Lyne, K. Lazaridis, M. L. Jones, Gregory Desvignes, J. W. McKee, Gilles Theureau, Ismaël Cognard, R. Smits, Maura McLaughlin, A. Krieger, Weiwei Zhu, M. Burgay, D. J. Champion, Timothy T. Pennucci, Delphine Perrodin, Caterina Tiburzi, L. Lentati, Kevin Stovall, Joris P. W. Verbiest, A. Possenti, Christine Jordan, Glenn Jones, G. Shaifullah, E. Graikou, J. A. Ellis, David J. Nice, R. N. Caballero, Ingrid H. Stairs, Stefan Oslowski, Jason W. T. Hessels, C. G. Bassa, Emmanuel Fonseca, Benjamin Stappers, S. A. Sanidas, Zaven Arzoumanian, Lucas Guillemot, Paul Demorest, High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Zhu, W, Desvignes, G, Wex, N, Caballero, R, Champion, D, Demorest, P, Ellis, J, Janssen, G, Kramer, M, Krieger, A, Lentati, L, Nice, D, Ransom, S, Stairs, I, Stappers, B, Verbiest, J, Arzoumanian, Z, Bassa, C, Burgay, M, Cognard, I, Crowter, K, Dolch, T, Ferdman, R, Fonseca, E, Gonzalez, M, Graikou, E, Guillemot, L, Hessels, J, Jessner, A, Jones, G, Jones, M, Jordan, C, Karuppusamy, R, Lam, M, Lazaridis, K, Lazarus, P, Lee, K, Levin, L, Liu, K, Lyne, A, Mckee, J, Mclaughlin, M, Osłowski, S, Pennucci, T, Perrodin, D, Possenti, A, Sanidas, S, Shaifullah, G, Smits, R, Stovall, K, Swiggum, J, Theureau, G, Tiburzi, C, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: General relativity, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, FOS: Physical sciences, Astrophysics, Lorentz covariance, 01 natural sciences, Binary pulsar, Gravitation, stars: neutron, General Relativity and Quantum Cosmology, Pulsar, Gravitational field, 0103 physical sciences, pulsars: individual (PSR J1713+0747), 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Gravitational constant, European Pulsar Timing Array, binaries: general, Space and Planetary Science, [SDU]Sciences of the Universe [physics], gravitation, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Symmetries play an important role in modern theories of gravity. The strong equivalence principle (SEP) constitutes a collection of gravitational symmetries which are all implemented by general relativity. Alternative theories, however, are generally expected to violate some aspects of SEP. We test three aspects of SEP using observed change rates in the orbital period and eccentricity of binary pulsar J1713+0747: 1. the gravitational constant's constancy as part of locational invariance of gravitation; 2. the post-Newtonian parameter $\hat{\alpha}_3$ in gravitational Lorentz invariance; 3. the universality of free fall (UFF) for strongly self-gravitating bodies. Based on the pulsar timing result of the combined dataset from the North American Nanohertz Gravitational Observatory (NANOGrav) and the European Pulsar Timing Array (EPTA), we find $\dot{G}/G = (-0.1 \pm 0.9) \times 10^{-12}\,{\rm yr}^{-1}$, which is weaker than Solar system limits, but applies for strongly self-gravitating objects. Furthermore, we obtain the constraints $|\Delta|< 0.002$ for the UFF test and $-3\times10^{-20} < \hat{\alpha}_3 < 4\times10^{-20}$ at 95% confidence. These are the first direct UFF and $\hat{\alpha}_3$ tests based on pulsar binaries, and they overcome various limitations of previous tests., Comment: 11 pages, 6 figures, and 1 table; submitted to MNRAS
Published: 2019
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45. A detailed study of giant pulses from PSR B1937+21 using the Large European Array for Pulsars

Author: Si Chen, Michael Kramer, J. W. McKee, Delphine Perrodin, Benjamin Stappers, M. Gaikwad, Gemma H. Janssen, Weiwei Zhu, C. G. Bassa, Kejia Lee, Long Wang, Kang Liu, S. A. Sanidas, Ramesh Karuppusamy, Ismaël Cognard, R. Smits, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), ITA, GBR, FRA, DEU, NLD, and CHN
Subjects: FOS: Physical sciences, Astrophysics, 01 natural sciences, Power law, stars: neutron, Time of arrival, Pulsar, Millisecond pulsar, stars: rotation, pulsars: general, 0103 physical sciences, structure, 010303 astronomy & astrophysics, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, polarization, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, radiation mechanisms: non-thermal, Polarization (waves), Fractional polarization, Interstellar medium, modulation, pulsars: individual (PSR J1939+2134), Space and Planetary Science, [SDU]Sciences of the Universe [physics], correlation, fractional, Global Positioning System, pulsars: individual (PSR B1937+21), Astrophysics - High Energy Astrophysical Phenomena, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We have studied 4265 giant pulses (GPs) from the millisecond pulsar B1937+21; the largest-ever sample gathered for this pulsar, in observations made with the Large European Array for Pulsars. The pulse energy distribution of GPs associated with the interpulse are well-described by a power law, with index $\alpha = -3.99 \pm 0.04$, while those associated with the main pulse are best-described by a broken power law, with the break occurring at $\sim7$ Jy $\mu$s, with power law indices $\alpha_{\text{low}} = -3.48 \pm 0.04$ and $\alpha_{\text{high}} = -2.10 \pm 0.09$. The modulation indices of the GP emission are measured, which are found to vary by $\sim0.5$ at pulse phases close to the centre of the GP phase distributions. We find the frequency-resolved structure of GPs to vary significantly, and in a manner that cannot be attributed to the interstellar medium influence on the observed pulses. We examine the distribution of polarisation fractions of the GPs and find no correlation between GP emission phase and fractional polarisation. We use the GPs to time PSR B1937+21 and although the achievable time of arrival precision of the GPs is approximately a factor of two greater than that of the average pulse profile, there is a negligible difference in the precision of the overall timing solution when using the GPs., Comment: 20 pages, 21 figures, 3 tables, accepted for publication in MNRAS
Published: 2019
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46. Pain sensitivity study in the Dutch population: relationship with current pain, gender and sports

Author: R. van Boekel, Monique A H Steegers, R. Smits, T. Bouw, E.N. Blaney Davidson, K. Stolzenbach, S. E. I. Van Der Wal, Hans Timmerman, and M. van Nieuwland
Subjects: Rheumatology, business.industry, Dutch Population, Biomedical Engineering, Medicine, Orthopedics and Sports Medicine, Sensitivity (control systems), Current (fluid), business, Clinical psychology
Published: 2019
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47. From spin noise to systematics: stochastic processes in the first International Pulsar Timing Array data release

Author: R. van Haasteren, Scott M. Ransom, S. Babak, Antoine Petiteau, Paul Demorest, L. Toomey, Gemma H. Janssen, Alberto Sesana, Marjorie Gonzalez, Sourav Chatterjee, A. Lassus, Ryan Shannon, Justin A. Ellis, Glenn Jones, E. Graikou, J. W. McKee, Kang Liu, Kejia Lee, Matthew Kerr, Sarah Burke-Spolaor, William A. Coles, Maura McLaughlin, G. Shaifullah, Stephen Taylor, Weiwei Zhu, P. Lazarus, S. A. Sanidas, D. J. Champion, Delphine Perrodin, R. N. Caballero, Kevin Stovall, Joris P. W. Verbiest, Benetge Perera, Richard N. Manchester, C. G. Bassa, Emmanuel Fonseca, Jonathan R. Gair, George Hobbs, D. R. Madison, R. Smits, Alberto Vecchio, Daniel R. Stinebring, Michael T. Lam, Daniel J. Reardon, X. P. You, Zaven Arzoumanian, Paul D. Lasky, Yue-Fei Wang, Lucas Guillemot, R. S. Lynch, Pablo Rosado, Lina Levin, Xing-Jiang Zhu, Chiara M. F. Mingarelli, L. Lentati, Benjamin Stappers, A. Possenti, T. J. W. Lazio, Robert D. Ferdman, Stefan Oslowski, J. K. Swiggum, X. Siemens, Gregory Desvignes, Gilles Theureau, Ramesh Karuppusamy, Ismaël Cognard, M. Burgay, Timothy T. Pennucci, Michele Vallisneri, J. B. Wang, James M. Cordes, Sean T. McWilliams, David J. Nice, P. Brem, W. van Straten, Caterina Tiburzi, N. D. R. Bhat, Shi Dai, Jason W. T. Hessels, Ingrid H. Stairs, Timothy Dolch, Michael Kramer, Michael Keith, Lentati, L, Shannon, R, Coles, W, Verbiest, J, van Haasteren, R, Ellis, J, Caballero, R, Manchester, R, Arzoumanian, Z, Babak, S, Bassa, C, Bhat, N, Brem, P, Burgay, M, Burke-Spolaor, S, Champion, D, Chatterjee, S, Cognard, I, Cordes, J, Dai, S, Demorest, P, Desvignes, G, Dolch, T, Ferdman, R, Fonseca, E, Gair, J, Gonzalez, M, Graikou, E, Guillemot, L, Hessels, J, Hobbs, G, Janssen, G, Jones, G, Karuppusamy, R, Keith, M, Kerr, M, Kramer, M, Lam, M, Lasky, P, Lassus, A, Lazarus, P, Lazio, T, Lee, K, Levin, L, Liu, K, Lynch, R, Madison, D, Mckee, J, Mclaughlin, M, Mcwilliams, S, Mingarelli, C, Nice, D, Osłowski, S, Pennucci, T, Perera, B, Perrodin, D, Petiteau, A, Possenti, A, Ransom, S, Reardon, D, Rosado, P, Sanidas, S, Sesana, A, Shaifullah, G, Siemens, X, Smits, R, Stairs, I, Stappers, B, Stinebring, D, Stovall, K, Swiggum, J, Taylor, S, Theureau, G, Tiburzi, C, Toomey, L, Vallisneri, M, van Straten, W, Vecchio, A, Wang, J, Wang, Y, You, X, Zhu, W, Zhu, X, High Energy Astrophys. & Astropart. Phys (API, FNWI), Cavendish Laboratory, University of Cambridge [UK] (CAM), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), University of California, University of California (UC), Max-Planck-Institut für Radioastronomie (MPIFR), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), NASA Goddard Space Flight Center (GSFC), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, Netherlands Institute for Radio Astronomy (ASTRON), Curtin University [Perth], Planning and Transport Research Centre (PATREC), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), National Radio Astronomy Observatory (NRAO), Center for Radiophysics and Space Research [Ithaca] (CRSR), Cornell University [New York], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Department of Astronomy [Ithaca], Department of Physics, Hillsdale College, Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), University of British Columbia (UBC), Vancouver Coastal Health, Department of Nuclear Medicine, Netherlands Institute for Radio Astronomy ( ASTRON ), ARC Centre of Excellence for Coral Reef Studies (CoralCoE), James Cook University (JCU), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Vrije Universiteit Medical Centre (VUMC), Vrije Universiteit Amsterdam [Amsterdam] (VU), Kavli Institute for Astronomy and Astrophysics [Beijing] (KIAA-PKU), Peking University [Beijing], National Radio Astronomy Observatory [Green Bank] (NRAO), Jodrell Bank Centre for Astrophysics (JBCA), Department of Physics, West Virginia University, West Virginia University, Theoretical Astrophysics [Pasadena] (TAPIR), California Institute of Technology (CALTECH), Physics Department, Lafayette College, Lafayette College [Easton], Department of Astronomy [Charlottesville], University of Virginia, APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de glaciologie et géophysique de l'environnement (LGGE), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), University of Wisconsin - Milwaukee, Department of Physics and Astronomy, University of British Columbia, Department of Physics and Astronomy [Oberlin], Oberlin College, Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Department of Physics and Astronomy, West Virginia University, West Virginia University [Morgantown], Birmingham City University (BCU), Xinjiang Astronomical Observatory, Chinese Academy of Sciences [Beijing] (CAS), Huazhong University of Science and Technology [Wuhan] (HUST), School of Physical Science and Technology, Southwest University [Chongqing], Australian Research Council Discovery Project DP140102578NASA through Einstein Fellowship grant PF3-140116West Light Foundation of CAS XBBS201322 and NSFC project no.11403086National Science Fundation of China (NSFC) award number 11503007NNSF of China (U1231120) and FRFCU (XDJK2015B012), European Project: 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET(2014), European Project: 227947,EC:FP7:ERC,ERC-2008-AdG,LEAP(2009), European Project: 610058,EC:FP7:ERC,ERC-2013-SyG,BLACKHOLECAM(2014), Cornell University, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Division of Physics, Mathematics and Astronomy [Pasadena], California Institute of Technology (CALTECH)-California Institute of Technology (CALTECH), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), California Institute of Technology (CALTECH)-NASA, Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), University of Virginia [Charlottesville], Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, data analysis, pulsars: general [methods], FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Methods: Data analysi, Astrophysics, Astronomy & Astrophysics, general [pulsars], 01 natural sciences, General Relativity and Quantum Cosmology, pulsars:individual, Binary pulsar, Pulsar, 0103 physical sciences, data analysis [methods], Coherence (signal processing), Sensitivity (control systems), Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Stochastic process, Noise (signal processing), Model selection, Pulsars: General, Astronomy and Astrophysics, methods: data analysis, LIGO, Computational physics, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astronomical and Space Sciences
Abstract: We analyse the stochastic properties of the 49 pulsars that comprise the first International Pulsar Timing Array (IPTA) data release. We use Bayesian methodology, performing model selection to determine the optimal description of the stochastic signals present in each pulsar. In addition to spin-noise and dispersion-measure (DM) variations, these models can include timing noise unique to a single observing system, or frequency band. We show the improved radio-frequency coverage and presence of overlapping data from different observing systems in the IPTA data set enables us to separate both system and band-dependent effects with much greater efficacy than in the individual PTA data sets. For example, we show that PSR J1643$-$1224 has, in addition to DM variations, significant band-dependent noise that is coherent between PTAs which we interpret as coming from time-variable scattering or refraction in the ionised interstellar medium. Failing to model these different contributions appropriately can dramatically alter the astrophysical interpretation of the stochastic signals observed in the residuals. In some cases, the spectral exponent of the spin noise signal can vary from 1.6 to 4 depending upon the model, which has direct implications for the long-term sensitivity of the pulsar to a stochastic gravitational-wave (GW) background. By using a more appropriate model, however, we can greatly improve a pulsar's sensitivity to GWs. For example, including system and band-dependent signals in the PSR J0437$-$4715 data set improves the upper limit on a fiducial GW background by $\sim 60\%$ compared to a model that includes DM variations and spin-noise only., Comment: 29 pages. 16 figures. Accepted for publication in MNRAS
Published: 2016
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48. The International Pulsar Timing Array: First data release

Author: Lucas Guillemot, Sourav Chatterjee, N. Garver-Daniels, D. R. Madison, Scott M. Ransom, J. K. Swiggum, Daniel R. Stinebring, Delphine Perrodin, Ingrid H. Stairs, Alberto Vecchio, Timothy Dolch, X. Siemens, Gregory Desvignes, Antoine Petiteau, Gilles Theureau, W. van Straten, J. B. Wang, X. P. You, Jason W. T. Hessels, Renée Spiewak, R. N. Caballero, Alberto Sesana, Stefan Oslowski, R. S. Lynch, Xing-Jiang Zhu, C. G. Bassa, Emmanuel Fonseca, Daniel J. Reardon, Yue-Fei Wang, Chiara M. F. Mingarelli, Benjamin Stappers, Kejia Lee, Stanislav Babak, Benetge Perera, Pablo Rosado, Zaven Arzoumanian, Richard N. Manchester, Paul Demorest, A. Brazier, Jonathan R. Gair, R. van Haasteren, Nipuni Palliyaguru, Lina Levin, R. Smits, Joseph Simon, P. Brem, Michele Vallisneri, Michael Kramer, James M. Cordes, Andrew Lyne, L. Lentati, Weiwei Zhu, Matthew Kerr, Peter A. Gentile, Michael Keith, A. Possenti, D. J. Champion, Caterina Tiburzi, T. J. W. Lazio, N. D. R. Bhat, A. Lassus, Stephen Taylor, Linqing Wen, Ryan Shannon, Glenn Jones, Shi Dai, E. Graikou, Gemma H. Janssen, S. J. Chamberlin, Kevin Stovall, Kang Liu, P. Lazarus, Ramesh Karuppusamy, S. A. Sanidas, Ismaël Cognard, George Hobbs, Robert D. Ferdman, Timothy T. Pennucci, M. Burgay, Sean T. McWilliams, David J. Nice, B. Christy, G. Shaifullah, L. Toomey, Justin A. Ellis, J. W. McKee, Maura McLaughlin, Paul D. Lasky, Michael T. Lam, Sarah Burke-Spolaor, Joris P. W. Verbiest, Marjorie Gonzalez, High Energy Astrophys. & Astropart. Phys (API, FNWI), Verbiest, J, Lentati, L, Hobbs, G, van Haasteren, R, Demorest, P, Janssen, G, Wang, J, Desvignes, G, Caballero, R, Keith, M, Champion, D, Arzoumanian, Z, Babak, S, Bassa, C, Bhat, N, Brazier, A, Brem, P, Burgay, M, Burke-Spolaor, S, Chamberlin, S, Chatterjee, S, Christy, B, Cognard, I, Cordes, J, Dai, S, Dolch, T, Ellis, J, Ferdman, R, Fonseca, E, Gair, J, Garver-Daniels, N, Gentile, P, Gonzalez, M, Graikou, E, Guillemot, L, Hessels, J, Jones, G, Karuppusamy, R, Kerr, M, Kramer, M, Lam, M, Lasky, P, Lassus, A, Lazarus, P, Lazio, T, Lee, K, Levin, L, Liu, K, Lynch, R, Lyne, A, Mckee, J, Mclaughlin, M, Mcwilliams, S, Madison, D, Manchester, R, Mingarelli, C, Nice, D, Osłowski, S, Palliyaguru, N, Pennucci, T, Perera, B, Perrodin, D, Possenti, A, Petiteau, A, Ransom, S, Reardon, D, Rosado, P, Sanidas, S, Sesana, A, Shaifullah, G, Shannon, R, Siemens, X, Simon, J, Smits, R, Spiewak, R, Stairs, I, Stappers, B, Stinebring, D, Stovall, K, Swiggum, J, Taylor, S, Theureau, G, Tiburzi, C, Toomey, L, Vallisneri, M, van Straten, W, Vecchio, A, Wang, Y, Wen, L, You, X, Zhu, W, Zhu, X, Max-Planck-Institut für Radioastronomie (MPIFR), Cavendish Laboratory, University of Cambridge [UK] (CAM), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), National Radio Astronomy Observatory [Socorro] (NRAO), National Radio Astronomy Observatory (NRAO), Netherlands Institute for Radio Astronomy (ASTRON), Xinjiang Astronomical Observatory, Chinese Academy of Sciences [Beijing] (CAS), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], NASA Goddard Space Flight Center (GSFC), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, Curtin University [Perth], Planning and Transport Research Centre (PATREC), Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University [New York], INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Pennsylvania State University (Penn State), Penn State System, Center for Radiophysics and Space Research [Ithaca] (CRSR), University of Maryland [College Park], University of Maryland System, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Department of Astronomy [Ithaca], Department of Physics, Hillsdale College, University of British Columbia (UBC), University of Edinburgh, Department of Physics and Astronomy, West Virginia University, West Virginia University [Morgantown], Vancouver Coastal Health, Department of Nuclear Medicine, Department of Physics, Columbia University, Columbia University [New York], Monash Centre for Astrophysics (MoCA), Monash University [Clayton], Kavli Institute for Astronomy and Astrophysics [Beijing] (KIAA-PKU), Peking University [Beijing], National Radio Astronomy Observatory [Green Bank] (NRAO), Theoretical Astrophysics [Pasadena] (TAPIR), Division of Physics, Mathematics and Astronomy [Pasadena], California Institute of Technology (CALTECH)-California Institute of Technology (CALTECH), Physics Department, Lafayette College, Lafayette College [Easton], Physics Department, Texas Tech University, Texas Tech University [Lubbock] (TTU), Department of Astronomy [Charlottesville], University of Virginia [Charlottesville], APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Centre for Astrophysics and Supercomputing [Swinburne] (CAS), Swinburne University of Technology [Melbourne], Anton Pannekoek Institute for Astronomy, University of Amsterdam [Amsterdam] (UvA), University of Wisconsin - Milwaukee, Center for Gravitation, Cosmology and Astrophysics, Netherlands Institute for Radio Astronomy ( ASTRON ), Department of Physics and Astronomy, University of British Columbia, Department of Physics and Astronomy [Oberlin], Oberlin College, Department of Physics and Astronomy [Albuquerque], The University of New Mexico [Albuquerque], Birmingham City University (BCU), School of Physics [HUST], Huazhong University of Science and Technology [Wuhan] (HUST), School of Physics (University of Western Australia), Université, School of Physical Science and Technology, Southwest University [Chongqing], European Project: 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET(2014), Max-Planck-Institut für Radioastronomie, Cavendish Laboratory - University of Cambridge, University of Cambridge [UK] ( CAM ), CSIRO Astronomy and Space Science, PO BOX 76, NSW 1710, Australia, Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), National Radio Astronomy Observatory [Socorro] ( NRAO ), National Radio Astronomy Observatory ( NRAO ), Netherlands Institute for Radio Astronomy, Chinese Academy of Sciences [Beijing] ( CAS ), NASA Goddard Space Flight Center ( GSFC ), Albert Einstein Institute, Max-Planck-Institut für Gravitationsphysik, Curtin University, Perth, Australia, Cornell Center for Astrophysics and Planetary Science ( CCAPS ), Cornell University, MPI for Gravitational Physics (Albert Einstein Institute), INAF-Osservatorio di Cagliari, PennState University [Pennsylvania] ( PSU ), Center for Radiophysics and Space Research [Ithaca] ( CRSR ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), University of British Columbia ( UBC ), University of Edimburgh, Kavli Institute for Astronomy and Astrophysics, National Radio Astronomy Observatory [Green Bank] ( NRAO ), Commonwealth Scientific and Industrial Research Organisation [Canberra] ( CSIRO ), TAPIR (Theoretical Astrophysics), California Institute of Technology, Texas Tech University [Lubbock] ( TTU ), Osservatorio Astronomico di Cagliari, Ist Nazl Astrofis, Osservatorio Astronomico di Cagliari, APC - Gravitation ( APC-Gravitation ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Centre for Astrophysics and Supercomputing [Swinburne] ( CAS ), Anton Pannekoek Institute for Astronomy, University of Amsterdam, Max Planck Institut für Gravitationsphysik, Albert Einstein Institut, Physics and Astronomy Department [Oberlin], Center for Gravitational Wave Astronomy, The University of Texas at Brownsville and Texas Southmost College, Birmingham City University ( BCU ), School of Physics, Huazhong University of Science and Technology, Huazhong University of Science and Technology, School of Physics ( University of Western Australia ), European Project : 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET ( 2014 ), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), University of Virginia, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)
Subjects: data analysis, data analysis, pulsars: general [methods], FOS: Physical sciences, Methods: Data analysi, general [pulsars], 01 natural sciences, 7. Clean energy, Set (abstract data type), Pulsar timing array, Pulsar, 0103 physical sciences, data analysis [methods], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, instrumentation, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Pulsars: General, Astronomy, Astronomy and Astrophysics, methods: data analysis, Data set, European Pulsar Timing Array, Neutron star, gravitational waves, Space and Planetary Science, pulsars, Measurement uncertainty, Astrophysics - Instrumentation and Methods for Astrophysics, [ SDU.ASTR.SR ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Algorithm, astro-ph.IM
Abstract: The highly stable spin of neutron stars can be exploited for a variety of (astro-)physical investigations. In particular arrays of pulsars with rotational periods of the order of milliseconds can be used to detect correlated signals such as those caused by gravitational waves. Three such "Pulsar Timing Arrays" (PTAs) have been set up around the world over the past decades and collectively form the "International" PTA (IPTA). In this paper, we describe the first joint analysis of the data from the three regional PTAs, i.e. of the first IPTA data set. We describe the available PTA data, the approach presently followed for its combination and suggest improvements for future PTA research. Particular attention is paid to subtle details (such as underestimation of measurement uncertainty and long-period noise) that have often been ignored but which become important in this unprecedentedly large and inhomogeneous data set. We identify and describe in detail several factors that complicate IPTA research and provide recommendations for future pulsar timing efforts. The first IPTA data release presented here (and available online) is used to demonstrate the IPTA's potential of improving upon gravitational-wave limits placed by individual PTAs by a factor of ~2 and provides a 2-sigma limit on the dimensionless amplitude of a stochastic GWB of 1.7x10^{-15} at a frequency of 1 yr^{-1}. This is 1.7 times less constraining than the limit placed by (Shannon et al. 2015), due mostly to the more recent, high-quality data they used., 25 pages, 6 tables, 5 figures. Accepted for publication in MNRAS
Published: 2016
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49. A retrospective analysis of treatment‐related hospitalization costs of pediatric, adolescent, and young adult acute lymphoblastic leukemia

Author: E K Korgenski, Sapna Kaul, Rochelle R. Smits-Seemann, Elizabeth A. Raetz, Seth Andrews, Jian Ying, Richard E. Nelson, Anne C. Kirchhoff, Mark Fluchel, Richard S. Lemons, and Christi F. Ng
Subjects: Adult, Male, Cancer Research, Pediatrics, medicine.medical_specialty, Adolescent, Lymphoblastic Leukemia, hospital costs, Psychological intervention, Pharmacy, Acute lymphoblastic leukemia, Neutropenia, Young Adult, 03 medical and health sciences, 0302 clinical medicine, Outcome Assessment, Health Care, Humans, Medicine, Radiology, Nuclear Medicine and imaging, Young adult, Child, Original Research, Retrospective Studies, business.industry, pediatric/adolescent/young adult, Age Factors, Clinical Cancer Research, Infant, Retrospective cohort study, Health Care Costs, Precursor Cell Lymphoblastic Leukemia-Lymphoma, medicine.disease, 3. Good health, Cancer registry, Hospitalization, Identified patient, Oncology, Child, Preschool, 030220 oncology & carcinogenesis, Female, business, 030215 immunology
Abstract: This retrospective study examined the longitudinal hospital outcomes (costs adjusted for inflation, hospital days, and admissions) associated with the treatment of pediatric, adolescent, and young adult acute lymphoblastic leukemia (ALL). Patients between one and 26 years of age with newly diagnosed ALL, who were treated at Primary Children's Hospital (PCH) in Salt Lake City, Utah were included. Treatment and hospitalization data were retrieved from system‐wide cancer registry and enterprise data warehouse. PCH is a member of the Children's Oncology Group (COG) and patients were treated on, or according to, active COG protocols. Treatment‐related hospital costs of ALL were examined by computing the average annual growth rates (AAGR). Longitudinal regressions identified patient characteristics associated with costs. A total of 505 patients (46.9% female) were included. The majority of patients had B‐cell lineage ALL, 6.7% had T‐ALL, and the median age at diagnosis was 4 years. Per‐patient, first‐year ALL hospitalization costs at PCH rose from $24,197 in 1998 to $37,924 in 2012. The AAGRs were 6.1, 13.0, and 7.6% for total, pharmacy, and room and care costs, respectively. Average days (AAGR = 5.2%) and admissions (AAGR = 3.8%) also demonstrated an increasing trend. High‐risk patients had 47% higher costs per 6‐month period in the first 5 years from diagnosis than standard‐risk patients (P
Published: 2015
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50. European Pulsar Timing Array limits on an isotropic stochastic gravitational-wave background

Author: Pablo Rosado, Chiara M. F. Mingarelli, Lucas Guillemot, Rutger van Haasteren, S. Sanidas, P. Brem, A. Lassus, M. B. Purver, Stanislav Babak, Cees Bassa, Jason W. T. Hessels, R. Smits, Antoine Petiteau, Alberto Vecchio, Ramesh Karuppusamy, D. J. Champion, Ismaël Cognard, Kejia Lee, Caterina Tiburzi, Andrea Possenti, Marta Burgay, P. Lazarus, Alberto Sesana, Lindley Lentati, Stefan Oslowski, Gemma H. Janssen, Stephen Taylor, Gregory Desvignes, Gilles Theureau, Joris P. W. Verbiest, Ben Stappers, Michael Kramer, R. Nicolas Caballero, Kuo Liu, Delphine Perrodin, Jonathan R. Gair, Cavendish Laboratory, University of Cambridge [UK] (CAM), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft, Birmingham City University (BCU), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Max-Planck-Institut für Radioastronomie (MPIFR), Kavli Institute for Astronomy and Astrophysics [Beijing] (KIAA-PKU), Peking University [Beijing], INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Netherlands Institute for Radio Astronomy (ASTRON), University of Amsterdam [Amsterdam] (UvA), Columbia Astrophysics Laboratory (CAL), Columbia University [New York], AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universität Bielefeld, Centre for Astrophysics and Supercomputing, Swinburne University of Technology [Melbourne], Netherlands Institute for Radio Astronomy ( ASTRON ), 'Programme National de Cosmologie and Galaxies' (PNCG) of CNRS/INSU, France, European Project: 337062,EC:FP7:ERC,ERC-2013-StG,DRAGNET(2014), European Project: 610058,EC:FP7:ERC,ERC-2013-SyG,BLACKHOLECAM(2014), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Lentati, L, Taylor, S, Mingarelli, C, Sesana, A, Sanidas, S, Vecchio, A, Caballero, R, Lee, K, van Haasteren, R, Babak, S, Bassa, C, Brem, P, Burgay, M, Champion, D, Cognard, I, Desvignes, G, Gair, J, Guillemot, L, Hessels, J, Janssen, G, Karuppusamy, R, Kramer, M, Lassus, A, Lazarus, P, Liu, K, Oslowski, S, Perrodin, D, Petiteau, A, Possenti, A, Purver, M, Rosado, P, Smits, R, Stappers, B, Theureau, G, Tiburzi, C, Verbiest, J, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), High Energy Astrophys. & Astropart. Phys (API, FNWI), and API (FNWI)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gravitational wave background, Pulsar timing array, gravitational waves methods: data analysis pulsars: general, Pulsar, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Spectral index, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Gravitational wave, Spectral density, Astronomy and Astrophysics, Pulsars: general, Space and Planetary Science, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Methods: data analysi, astro-ph.IM
Abstract: We present new limits on an isotropic stochastic gravitational-wave background (GWB) using a six pulsar dataset spanning 18 yr of observations from the 2015 European Pulsar Timing Array data release. Performing a Bayesian analysis, we fit simultaneously for the intrinsic noise parameters for each pulsar, along with common correlated signals including clock, and Solar System ephemeris errors, obtaining a robust 95$\%$ upper limit on the dimensionless strain amplitude $A$ of the background of $A, 24 pages, 5 tables, 17 figures
Published: 2015
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