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1. Supporting rotational grazing systems with virtual fencing: paddock transitions, beef heifer performance, and stress response

Author

N.A. Grinnell, D. Hamidi, M. Komainda, F. Riesch, J. Horn, I. Traulsen, R. Palme, and J. Isselstein

Subjects
Cattle welfare, Glucocorticoids, Grazing management, Precision grazing, Sustainable grazing, Animal culture, SF1-1100
Abstract

Animal welfare is integral to sustainable livestock production, and pasture access for cattle is known to enhance welfare. Despite positive welfare impacts, high labour requirements hinder the adoption of sustainable grazing practices such as rotational stocking management. Virtual fencing (VF) is an innovative technology for simplified, less laborious grazing management and remote animal monitoring, potentially facilitating the expansion of sustainable livestock production. VF uses Global Navigation Satellite System technology, wireless communication, and stimuli (auditory and electrical) to manage livestock movements and contain animals without physical barriers. Training animals to associate the auditory cue with the subsequent aversive stimulus enables effective livestock containment without physical barriers. While previous studies have largely dispelled concerns about adverse effects on cattle behaviour associated with the use of VF collars, there is limited knowledge regarding the impacts on animal physiology, particularly in rotational stocking systems. Addressing this knowledge gap, this study investigated differences in diet digestibility, livestock performance, and stress response of beef heifers on pastures using a VF compared to a physical electric fence. The study was conducted over 8 weeks, subdivided into two grazing cycles, with 32 heifers in four groups. Each experimental pasture was subdivided into four paddocks. The study monitored the interaction with the VF by analysing the temporal development of the ratio of auditory and electrical cues (success ratio and confidence ratio) emitted by the collars. Additionally, the grassland herbage quality, BW gain, and concentrations of faecal cortisol metabolites (FCMs) were assessed, as well as the time required for animals to cross into a new paddock. VF success ratios increased in the second grazing cycle, reflecting enhanced adaptation over time. Similarly, the reduction in time taken to cross into new paddocks in the VF groups indicated that animals learned to interact with the VF and rely on the auditory cues for directing movements. The absence of a significant effect of the fencing system on FCMs suggested that stress was unrelated to the VF technology. Further, animal performance was not affected as indicated by similar BW gains under both fencing systems. This study also attempts to establish a benchmark threshold for successful responses to the auditory cues, allowing comparative evaluation of VF systems. Overall, under rotational grazing, VF did not adversely impact animal welfare or performance compared to physical fencing, opening avenues for further exploration of VF technology in diverse grazing conditions.

Published
2025
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2. Old breeds, new solutions? Effects of two different traditional sire breeds on skin lesions, tail lesions, tail losses, performance and behaviour of rearing pigs

Author

A. Lange, M. Wutke, S. Ammer, A.K. Appel, H. Henne, A. Deermann, and I. Traulsen

Subjects
Activity, Aggressive behaviour, Average daily gain, Sire line, Tail-biting, Animal culture, SF1-1100
Abstract

Some studies indicated a relationship between modern, fast-growing, lean-meat-producing hybrid pigs and the occurrence of tail-biting, one of the major issues of conventional pig husbandry. Therefore, this study investigated the effects of different local, traditional sire breeds on the behaviour and performance of rearing pigs. Between December 2019 and November 2020, a total of 1 561 piglets were weaned from hybrid sows (Bundes Hybrid Zucht Programm (BHZP) Landrace × BHZP Large White) that were paired with either Swabian-Hall (SH), Bentheim Black Pied (BB) or BHZP-Piétrain (Pi) boars. Tails of the piglets were left intact (43.5%) or docked (56.5%), and male piglets were castrated. Piglets were conventionally reared on fully slatted plastic flooring in mixed-sex groups. Starting one day after weaning, skin lesions were scored once per pig, and tail lesions and losses were scored weekly until the end of rearing. The average daily gain was documented for the suckling and rearing period. The activity behaviour of eight focal pens was analysed using video recordings. Differences between modern and traditional breeds were found in this study for so-called aggressive and non-aggressive biting pronounced by skin and tail lesions and tail losses. Significantly fewer BB pigs had severe skin lesions on the front body than SH or Pi pigs (P 8.3 kg) weaning weight (P

Published
2023
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3. Development of a new grading system to assess the foster performance of lactating sows

Author

L.S. Trost, S. Zeidler, S. Ammer, S. Rosengart, M. Wendt, C. Visscher, J. Tetens, and I. Traulsen

Subjects
Animal welfare, Cross-fostering, Milk score, Performance analysis, Piglet mortality, Animal culture, SF1-1100
Abstract

Increasing litter size has created the need for more sophisticated, accurate, and welfare-oriented systems for assessing the foster performance of lactating sows. The estimation of milk yield alone is not sufficient for meeting these requirements. Therefore, the aim of the current study was to develop a grading system for assessing the foster performance of lactating sows that can be easily applied in commercial farm practice. Data were collected in two German conventional farrow-to-feeder farms with a total sample size of 639 sows (4.05 ± 2.86 parities) and 1 728 litters. Besides general performance data, the piglets were weighed individually within the first 24 hours after birth and at the peak of lactation (day 18.22 ± 2.48). Based on these data, we proposed a new score referring to the milk score (MS). This score was compared with the commonly used formula for estimating milk yield (est. MY), which solely involves litter weight gain and litter size. The improvement of the developed MS allowed us to distinguish between the birth and foster performances of the lactating sows through considering cross-fostering, litter size, individual piglet weights, and piglet mortality during lactation. Both scores showed a similar progression across parities. It was found that litter size had a significant impact on the performance of lactating sows. A high est. MY was found to be associated with a significantly higher number of piglets per litter (15.79 ± 2.20), lower weight gain per piglet, and increased piglet mortality during lactation compared with sows with high MS, which showed a smaller litter size (13.51 ± 2.18) (P

Published
2022
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4. Heifers don't care: no evidence of negative impact on animal welfare of growing heifers when using virtual fences compared to physical fences for grazing

Author

D. Hamidi, N.A. Grinnell, M. Komainda, F. Riesch, J. Horn, S. Ammer, I. Traulsen, R. Palme, M. Hamidi, and J. Isselstein

Subjects
Europe, Fleckvieh heifers, Precision livestock farming, Smart farming technology, Stress hormones, Animal culture, SF1-1100
Abstract

Virtual fencing (VF) represents a way to simplify traditional pasture management with its high labour and cost requirements for fencing and to make better use of the ‘beneficial’ agronomic and ecological effects of livestock grazing. In this study, the VF technology (® Nofence, AS, Batnfjordsøra Norway) was used with Fleckvieh heifers to investigate possible welfare impacts on the animals compared to conventionally fenced animals when they were trained to respond correctly to the system. The Nofence® collars (attached to the neck of the heifers) send acoustic signals as a warning when the animals approach the VF line, which was set up by GPS coordinates within the Nofence®-App, followed by an electric pulse when they do not stop or return. The heifers had no experience with VF prior to the study. Two treatments (VF versus physical fencing (PF)) were applied to six groups of four heifers each (three groups per treatment) over three 12-day time replicates. One VF line separated the pasture of the VF group into an accessible or non-accessible area. The control group had a PF line. Both groups were equipped with Nofence® collars (deactivated for the PF group). The trial took place on two adjacent paddocks of 1 000 m2 each following a 12-day schedule which was divided into three sections: visual support of the VF line by a physical barrier (first 2 days), only virtual border without visual support, moving the VF line (on day 8). Each time replicate followed the next successively on different paddocks with two new groups of heifers, which were grazed 5 h daily. During the whole experiment, the behaviour of each of the four animals per group was continuously observed; 2 h a.m., 2 h p.m. Exclusion by the VF line was effective in our trial. None of the heifers crossed the virtual boundary, i.e. the time spent in exclusion zone was zero. The heifers received 2.70 ± 2.63 acoustic signals and 0.30 ± 0.36 electric pulses (mean ± SD) per heifer and hour during all time replicates. Main cattle behaviour on pasture was not affected by the fencing system. Live weight gain, herbage consumption and faecal cortisol metabolites also revealed no significant differences. The duration until the heifers restarted grazing after an electric pulse from the Nofence® collar was significantly shorter than after an electric pulse from the physical fence. We can summarise that in our study, cattle well-being on pasture was not negatively affected by VF compared to PF.

Published
2022
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5. Development of a multi-criteria evaluation system to assess growing pig welfare

Author

P. Martín, I. Traulsen, C. Buxadé, and J. Krieter

Subjects
growing pigs, multi-criteria evaluation, Welfare Quality®, Animal culture, SF1-1100
Abstract

The aim of this paper was to present an alternative multi-criteria evaluation model to assess animal welfare on farms based on the Welfare Quality® (WQ) project, using an example of welfare assessment of growing pigs. The WQ assessment protocol follows a three-step aggregation process. Measures are aggregated into criteria, criteria into principles and principles into an overall assessment. This study focussed on the first step of the aggregation. Multi-attribute utility theory (MAUT) was used to produce a value of welfare for each criterion. The utility functions and the aggregation function were constructed in two separated steps. The Measuring Attractiveness by a Categorical Based Evaluation Technique (MACBETH) method was used for utility function determination and the Choquet Integral (CI) was used as an aggregation operator. The WQ decision-makers’ preferences were fitted in order to construct the utility functions and to determine the CI parameters. The methods were tested with generated data sets for farms of growing pigs. Using the MAUT, similar results were obtained to the ones obtained applying the WQ protocol aggregation methods. It can be concluded that due to the use of an interactive approach such as MACBETH, this alternative methodology is more transparent and more flexible than the methodology proposed by WQ, which allows the possibility to modify the model according, for instance, to new scientific knowledge.

Published
2017
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6. Detecting lameness in sows from ear tag-sampled acceleration data using wavelets

Author

C. Scheel, I. Traulsen, W. Auer, K. Müller, E. Stamer, and J. Krieter

Subjects
acceleration, wavelet, sow, lameness, detection, Animal culture, SF1-1100
Abstract

The objective of this study was to develop an automated monitoring system to detect lameness in group-housed sows early and reliably on the basis of acceleration data sampled from ear tags. To this end, acceleration data from ear tags were acquired from an experimental system deployed at the Futterkamp Agriculture Research Farm from May 2012 until November 2013. The developed method performs a wavelet transform for each individual sow’s time series of total acceleration. Feature series are then computed by locally estimating the energy, variation and variance in a small moving window. These feature series are then further decomposed into uniform level sets. From these series of level sets, the highest and lowest levels are monitored for lameness detection. To that end, they are split into a past record to serve as reference data representing a sow’s expected behaviour. The deviations between the reference and the remaining detection part of current data, termed feature activated, were then utilised to possibly indicate a lameness condition. The method was applied to a sample of 14 sows, seven of which were diagnosed as lame by a veterinarian on the last day of the sampling period of 14 days each. A prediction part of 3 days was set. Feature activated were clearly separable for the lame and healthy group with means of 8.8 and 0.8, respectively. The day-wise means were 1.93, 9.47 and 15.16 for the lame group and 0.02, 1.13 and 1.44 for the healthy group. A threshold could be set to completely avoid false positives while successfully classifying six lame sows on at least one of the 2 last days. The accuracy values for this threshold were 0.57, 0.71 and 0.78 when restricting to data from the particular day. A threshold that maximised the accuracy achieved values of 0.57, 0.79 and 0.93. Thus, the method presented seems powerful enough to suggest that an individual classification from ear tag-sampled acceleration data into lame and healthy is feasible without previous knowledge of the health status, but has to be validated by using a larger data set.

Published
2017
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7. Automatic detection of lameness in gestating group-housed sows using positioning and acceleration measurements

Author

I. Traulsen, S. Breitenberger, W. Auer, E. Stamer, K. Müller, and J. Krieter

Subjects
lameness, sow, sensor, positioning system, acceleration, Animal culture, SF1-1100
Abstract

Lameness is an important issue in group-housed sows. Automatic detection systems are a beneficial diagnostic tool to support management. The aim of the present study was to evaluate data of a positioning system including acceleration measurements to detect lameness in group-housed sows. Data were acquired at the Futterkamp research farm from May 2012 until April 2013. In the gestation unit, 212 group-housed sows were equipped with an ear sensor to sample position and acceleration per sow and second. Three activity indices were calculated per sow and day: path length walked by a sow during the day (Path), number of squares (25×25 cm) visited during the day (Square) and variance of the acceleration measurement during the day (Acc). In addition, data on lameness treatments of the sows and a weekly lameness score were used as reference systems. To determine the influence of a lameness event, all indices were analysed in a linear random regression model. Test day, parity class and day before treatment had a significant influence on all activity indices (P

Published
2016
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8. Comparative life cycle assessment (LCA) of pork using different protein sources in pig feed

Author

K. Reckmann, R. Blank, I. Traulsen, and J. Krieter

Subjects
Agriculture, Animal culture, SF1-1100, Science, Zoology, QL1-991
Abstract

Feed production is the main contributor to a subset of environmental impacts of pork production. In this context, this study is concerned with the substitution of soy products in pig diets in order to reduce these impacts. The aim of this study was to assess three alternative diets in gestating and lactating sows as well as growing and finishing pigs in order to reduce the amount of soy products used as ingredients. In the three alternative scenarios soy proteins were compensated for by either using a combination of different feedstuffs (e.g. rapeseed meal, fava beans, and synthetic amino acids) (LOW), maximising the use of legumes (mainly fava beans) (LEG) and increasing the amount of synthetic amino acids (AA). These alternative scenarios were compared with standard diets (ST) and formulated in order to reduce the crude-protein content of the diet while maintaining the same performance of the pigs. Each of the resulting 16 diets was then assessed with respect to global warming, eutrophication, acidification, and land use, both when accounting and not accounting for emissions due to land use change. The analysis per kilogram of feed showed that the ST diets performed best with regard to global warming, eutrophication, and acidification. When emissions from land use and land use change were added, ST and AA diets appeared to have the least impact. In contrast, the assessment of scenarios per kilogram of pork highlighted that the AA scenario contributed the least in all impact categories. In conclusion, it is possible to partly replace soybean products by using synthetic amino acids in order to minimise the environmental impacts of the pork supply chain.

Published
2016
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9. Probing the Accretion Processes in Soft X-Ray Selected Polars

Author

I. Traulsen, K. Reinsch, and A. D. Schwope

Subjects
Engineering (General). Civil engineering (General), TA1-2040
Abstract

High-energy data of accreting white dwarfs give access to the regime of the primary accretion-induced energy release and the different proposed accretion scenarios. We perform XMM-Newton observations of polars selected due to their ROSAT hardness ratios close to -1.0 and model the emission processes in accretion column and accretion region. Our models consider the multi-temperature structure of the emission regions and are mainly determined by mass-flow density, magnetic field strength, and white-dwarf mass. To describe the full spectral energy distribution from infrared to X-rays in a physically consistent way, we include the stellar contributions and establish composite models, which will also be of relevance for future X-ray missions. We confirm the X-ray soft nature of three polars.

Published
2015
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10. Comparison of different control strategies for classical swine fever using emergency vaccination and rapid PCR testing by using a Monte-Carlo simulation model

Author

J. Brosig, I. Traulsen, S. Blome, K. Depner, and J. Krieter

Subjects
Agriculture, Animal culture, SF1-1100, Science, Zoology, QL1-991
Abstract

Whenever an outbreak of classical swine fever has occurred in the European Union (EU), the basic control measures have usually been supplemented by preventive culling. This strategy has led to a great number of culled pigs and is discussed by general public and politics from both ethical and economic points of view. Emergency vaccination has been deemed to be an alternative control measure for some time now. PCR testing also provides a possible future strategy, since this method would allow a rapid and reliable testing of pigs in the vicinity of an outbreak farm. In this study, a spatial and temporal Monte-Carlo simulation model was used to compare alternative control strategies based upon these two measures (»Emergency Vaccination«, »Test To Slaughter«, »Test To Control« and »Vaccination in conjunction with Rapid Testing«) with the current control strategy. Two regions for investigation with different farm densities were used in the model. In a region with a low farm density, the basic EU control measures seemed to be sufficient to control an epidemic. In a region with a high farm density, additional measures would be necessary. »Emergency Vaccination« in a 3 km application zone and »Traditional Control« reached the same level of infected farms. Both »Test To Slaughter« and »Test To Control« combined with preventive culling led to a lower number of infected farms compared to the sole preventive culling strategy. The alternative control measures can reduce the number of culled farms significantly compared to »Traditional Control«.

Published
2013
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11. Comparison of growth performance and agonistic interaction in weaned piglets of different weight classes from farrowing systems with group or single housing

Author

A.-L. Bohnenkamp, I. Traulsen, C. Meyer, K. Müller, and J. Krieter

Subjects
agonistic behavior, group housing, growth performance, lesion score, weaning weight class, Animal culture, SF1-1100
Abstract

The present study was designed to analyze the growth performance, behavioral patterns and intensity of injuries of weaned pigs (26 days) during a rearing period of 6 weeks. The farrowing system (group housing (GH) v. single housing (SH)) and the post-weaning regrouping weight class (light, medium, heavy) were considered as the main factors. A number of 120 GH-pigs and 120 SH-pigs were kept in three batches (20 pens, 12 pigs each). The GH- and SH-pigs were divided by weight into three groups: light (5 to ⩽7 kg), medium (>7 to ⩽9 kg) and heavy (>9 to ⩽12 kg), with two pigs of six different litters in each pen. The pigs were weighed individually at weaning (week 1) and during rearing (weeks 2, 3 and 7). The feed conversion ratio (FCR) was calculated between weeks 1 and 7. The duration and number of fights (NF) per pen and hour were determined by continuous sampling (40 h after weaning). Lesions of the integument were scored into four classes (none, minor, medium, severe) and recorded at weaning and 48 h afterwards. The farrowing system had no effect on the weights in week 1 (GH: 7.8 kg v. SH: 7.7 kg; week as linear, quadratic regression nested within housing systems) or in week 7 (GH: 29.4 kg v. SH: 28.6 kg). The body weights were influenced significantly by the weaning weight class (light: 11.7 kg (s.e.m.: 0.30), medium: 14.8 kg (s.e.m.: 0.22), heavy: 17.3 kg (s.e.m.: 0.26)). The FCR of the GH-pigs was 1.64 (s.e.m.: 0.03) and 1.58 (s.e.m.: 0.03) for SH-pigs. A reduced agonistic behavior of the GH-pigs was observed with 2.1 fights per pen and hour (s.e.m.: 0.07) v. the SH-pigs with 4.6 fights per pen and hour (s.e.m.: 0.05). The fight duration of the GH-pigs with 10.3 s per pen and hour (s.e.m.: 1.07) was significantly lower in comparison to the SH-pigs with 18.8 s per pen and hour (s.e.m.: 1.06). The SH-pigs had more new skin lesions at the shoulders than the GH-pigs 48 h after weaning (P < 0.05). In conclusion, early mixing of unacquainted litters during lactation had no influence on their growth performance during rearing but reduced agonistic behavior and lesion score difference during the first 2 days after weaning. No significant interaction between the farrowing system and weaning weight class was detected with regard to growth performance and NF.

Published
2013
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12. XMM-Newton observations of eleven intermediate polars and possible candidates

Author

H. Worpel, A. D. Schwope, I. Traulsen, K Mukai, and S. Ok

Subjects
Astronomy
Abstract

We aim to identify new intermediate polars (IPs) in XMM-Newton observations from a list of promising candidates. By selecting targets not previously known to be X-ray bright we aim to uncover evidence for an X-ray underluminous IP subpopulation. We performed period searches on the XMM-Newton X-ray and optical data of our targets to seek both the spin and orbital periods, which differ in IPs. We also investigated the X-ray spectra to find the hot plasma emission shown by these objects. With archival Swift data we coarsely investigated the long-term X-ray variability, and with archival optical data from a variety of catalogues, we compared the optical to X-ray luminosity to identify X-ray faint objects. This paper presents the first XMM-Newton observation of the prototype IP, DQ Her. We find firm evidence for HZ Pup, V349 Aqr, and IGR J18151-1052 being IPs, with likely white dwarf spin periods of 1552, 390, and 390 s, respectively. The former two have luminosities typical of IPs, and the latter is strongly absorbed and with unknown distance. GI Mon and V1084 Her are apparently non-magnetic CVs with interesting short-term variability unrelated to WD spin. V533 Her is probably a magnetic CV and remains a good IP candidate, while V1039 Cen is possibly a polar. The remaining candidates were too faint to allow for any firm conclusions.

Published
2020
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13. An expanded ultraluminous X-ray source catalogue

Author

M. C. i Bernadich, K. Kovlakas, A. D. Schwope, A. Zezas, and I. Traulsen

Subjects
Ultraluminous X-ray source, Astrophysics::High Energy Astrophysical Phenomena, Population, black hole physics, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Luminosity, accretion, Astronomi, astrofysik och kosmologi, black holes [stars], Astronomy, Astrophysics and Cosmology, education, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Spiral galaxy, Star formation, accretion disks, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Accretion (astrophysics), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), binaries [X-rays], Astrophysics - High Energy Astrophysical Phenomena, catalogs
Abstract

Context. ULXs ($L_\textrm{X}>10^{39}$ erg s$^{-1}$) are excellent probes of accretion physics, star formation and IMBHs searches. As the sample size of X-ray data from modern observatories increases, producing extensive catalogues of ULXs and studying their collective properties is a possibility and a priority. Aims. We build a ULX catalogue based on one of the latest XMM-Newton releases, 4XMM-DR9, and the galaxy catalogue HECATE and study whether the properties of the expanded XMM-Newton ULX population are consistent with previous findings. Methods. We perform cross-matching between XMM-Newton sources and HECATE objects to identify host galaxies, and flag known interlopers in external catalogues and databases. Manual inspection of image data from PanSTARRS1 and the NASA/IPAC database is occasionally performed. We use distance and luminosity arguments to identify ULX candidates. Spectral, abundance and variability properties of the candidates are studied from 4XMM-DR9, HECATE and 4XMM-DR9s parameters. Results. We identify 779 ULX candidates. In spiral galaxies the number of ULX candidates per star forming rate is consistent with previous studies, and a significant ULX population in elliptical and lenticular is also found. Candidates hosted by late-type galaxies are more abundant, present harder spectra and undergo more and more extreme inter-observation variability than the early-type hosted ones. Around 30 candidates with $L_\textrm{X}>10^{41}$ erg s$^{-1}$ are also identified. Conclusions. Our results on the spectral and abundance properties of ULXs confirm the findings made by previous studies based on XMM-Newton and Chandra data, while our population-scale study on variability properties is unprecedented. Our study provides limited insight on the properties of the brightest ULX candidates due to the small sample size., Paper accepted for publication in A&A on 2021-10-13. 18 pages, 22 figures, 8 tables. Catalogue soon to be uploaded to the CDS - VizieR database

Published
2022

14. <scp>MACHO</scp> 311.37557.169: A <scp>VY</scp> Scl star

Author

H. Worpel, Michael J. I. Brown, Axel Schwope, and I. Traulsen

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Brightness, 010308 nuclear & particles physics, FOS: Physical sciences, Cataclysmic variable star, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Luminosity, Photometry (astronomy), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Emission spectrum, Variable star, Astrophysics - High Energy Astrophysical Phenomena, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Optical surveys, such as the MACHO project, often uncover variable stars whose classification requires followup observations by other instruments. We performed X-ray spectroscopy and photometry of the unusual variable star MACHO 311.37557.169 with \XMM\ in April 2018, supplemented by archival X-ray and optical spectrographic data. The star has a bolometric X-ray luminosity of about $1\times 10^{32}$ erg s$^{-1}$ cm$^{-2}$ and a heavily absorbed two-temperature plasma spectrum. The shape of its light curve, its overall brightness, its X-ray spectrum, and the emission lines in its optical spectrum suggest that it is most likely a VY~Scl cataclysmic variable., Comment: 7 pages, 5 figures

Published
2020
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15. Phase-resolved X-ray spectroscopy of PSR B0656+14 with SRG/eROSITA and XMM-Newton

Author

M. E. Ramos-Ceja, Adriana M. Pires, Georg Lamer, Valery F. Suleimanov, Andrea Santangelo, Alexander Y. Potekhin, Frank Haberl, Axel Schwope, Chandreyee Maitra, I. Traulsen, Werner Becker, Michael Freyberg, Konrad Dennerl, J. Kurpas, Victor Doroshenko, and Klaus Werner

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photon, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral line, Astrophysics - Solar and Stellar Astrophysics, Absorption edge, Pulsar, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Absorption (electromagnetic radiation), Spectroscopy, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

(abridged version) We present a detailed spectroscopic and timing analysis of X-ray observations of the bright radio-to-gamma-ray emitting pulsar PSR B0656+14, which were obtained simultaneously with eROSITA and XMM-Newton during the Calibration and Performance Verification phase of the Spektrum-Roentgen-Gamma mission (SRG) for 100 ks. Using XMM-Newton and NICER we firstly established an X-ray ephemeris for the time interval 2015 to 2020, which connects all X-ray observations in this period without cycle count alias and phase shifts. The mean eROSITA spectrum clearly reveals an absorption feature originating from the star at 570 eV with a Gaussian sigma of about 70 eV, tentatively identified earlier in a long XMM-Newton observation (Arumugasamy et al. 2018). A second absorption feature, described here as an absorption edge, occurs at 260-265 eV. It could be of atmospheric or of instrumental origin. These absorption features are superposed on various emission components, phenomenologically described as the sum of hot (120 eV) and cold (65 eV) blackbody components, both of photospheric origin, and a power-law with photon index Gamma=2. The phase-resolved spectroscopy reveals that the Gaussian absorption line at 570 eV is clearly present throughout ~60% of the spin cycle. The visibility of the line strength coincides in phase with the maximum flux of the hot blackbody. We also present three families of model atmospheres: a magnetised atmosphere, a condensed surface, and a mixed model, which were applied to the mean observed spectrum and whose continuum fit the observed data well. The atmosphere model, however, predicts too short distances. For the mixed model, the Gaussian absorption may be interpreted as proton cyclotron absorption in a field as high as 10^14 G, which is significantly higher than that derived from the moderate observed spin-down., Comment: Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission. 21 pages, 13 figures, 13 tables

Published
2021
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16. The various accretion modes of AM Herculis: Clues from multi-wavelength observations in high accretion states

Author

Hauke Worpel, I. Traulsen, Axel Schwope, and D. Sablowski

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, medicine.disease_cause, 01 natural sciences, 0103 physical sciences, medicine, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), AM Herculis, Scattering, White dwarf, Astronomy and Astrophysics, Light curve, Accretion (astrophysics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Polar, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Ultraviolet
Abstract

We report on XMM-Newton and NuSTAR X-ray observations of the prototypical polar, AM Herculis, supported by ground-based photometry and spectroscopy, all obtained in high accretion states. In 2005, AM Herculis was in its regular mode of accretion, showing a self-eclipse of the main accreting pole. X-ray emission during the self-eclipse was assigned to a second pole through its soft X-ray emission and not to scattering. In 2015, AM Herculis was in its reversed mode with strong soft blobby accretion at the far accretion region. The blobby acretion region was more luminous than the other, persistently accreting, therefore called main region. Hard X-rays from the main region did not show a self-eclipse indicating a pronounced migration of the accretion footpoint. Extended phases of soft X-ray extinction through absorption in interbinary matter were observed for the first time in AM Herculis. The spectral parameters of a large number of individual soft flares could be derived. Simultaneous NuSTAR observations in the reversed mode of accretion revealed clear evidence for Compton reflection of radiation from the main pole at the white dwarf surface. This picture is supported by the trace of the Fe resonance line at 6.4 keV through the whole orbit. Highly ionized oxygen lines observed with the Reflection Grating Spectrometer (RGS) were tentatively located at the bottom of the accretion column, although the implied densities are quite different from expectations. In the regular mode of accretion, the phase-dependent modulations in the ultraviolet (UV) are explained with projection effects of an accretion-heated spot at the prime pole. In the reversed mode projection effects cannot be recognized. The light curves reveal an extra source of UV radiation and extended UV absorbing dips. An Ha Doppler map obtained contemporaneously (abstract abridged), Accepted for publication in A&A, 21 pages, 21 figures

Published
2020

17. XMM-Newton observations of eleven intermediate polars and possible candidates

Author

Samet Ok, Koji Mukai, I. Traulsen, Hauke Worpel, Axel Schwope, and Ege Üniversitesi

Subjects
Service (systems architecture), 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Library science, Astrophysics, Virtual observatory, 01 natural sciences, X-rays: binaries, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Investment fund, white dwarfs, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Government, stars: magnetic field, Astronomy and Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Commonwealth, Survey data collection, Astrophysics - High Energy Astrophysical Phenomena, Research center
Abstract

Aims. We aim to identify new intermediate polars (IPs) in XMM-Newton observations from a list of promising candidates. By selecting targets not previously known to be X-ray bright, we aim to uncover evidence for an X-ray underluminous IP subpopulation.Methods. We performed period searches on the XMM-Newton X-ray and optical data of our targets to seek both the spin and orbital periods, which differ in IPs. We also investigated the X-ray spectra to find the hot plasma emission shown by these objects. With archival Swift data we coarsely investigated the long-term X-ray variability, and with archival optical data from a variety of catalogues, we compared the optical to X-ray luminosity to identify X-ray faint objects. This paper presents the first XMM-Newton observation of the prototype IP, DQ Her.Results. We find firm evidence for HZ Pup, V349 Aqr, and IGR J18151-1052 being IPs, with likely white dwarf spin periods of 1552, 390, and 390 s, respectively. the former two have luminosities typical of IPs, and the latter is strongly absorbed and with unknown distance. GI Mon and V1084 Her are apparently non-magnetic CVs with interesting short-term variability unrelated to WD spin. V533 Her is probably a magnetic CV and remains a good IP candidate, while V1039 Cen is possibly a polar. the remaining candidates were too faint to allow for any firm conclusions., German DLR [50 OR 1405, 50 OR 1711, 50 OR 1814]; TUBITAK 2214-A International Doctoral Research Fellowship ProgrammeTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK); TUBITAKTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK) [16BT100-1027]; Robert Martin Ayers Sciences Fund; ARC LIEF grant from the Australian Research Council,Australian Research Council [LE130100104]; Astronomy Australia Limited (AAL); Australian Government through the Commonwealth's Education Investment Fund (EIF); Australian Government through the National Collaborative Research Infrastructure Strategy (NCRIS)Australian GovernmentDepartment of Industry, Innovation and Science; National eResearch Collaboration Tools and Resources (NeCTAR); Australian National Data Service Projects (ANDS), This work was supported by the German DLR under contracts 50 OR 1405, 50 OR 1711, and 50 OR 1814. Samet Ok is supported by TUBITAK 2214-A International Doctoral Research Fellowship Programme. We thank TUBITAK for a partial support in using the T100 telescope with project number 16BT100-1027. We acknowledge with thanks the variable and comparison star observations from the AAVSO International Database contributed by observers worldwide and used in this research. Many of the AAVSO observations were the result of Centre for Backyard Astronomy (CBA) campaigns. This research has made use of the APASS database, located at the AAVSO web site. Funding for APASS has been provided by the Robert Martin Ayers Sciences Fund. This work has made use of Astropy (Astropy Collaboration 2013, 2018). This research has made use of data, software and/or web tools obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and of the Smithsonian Astrophysical Observatory's High Energy Astrophysics Division. the national facility capability for SkyMapper has been funded through ARC LIEF grant LE130100104 from the Australian Research Council, awarded to the University of Sydney, the Australian National University, Swinburne University of Technology, the University of Queensland, the University of Western Australia, the University of Melbourne, Curtin University of Technology, Monash University and the Australian Astronomical Observatory. SkyMapper is owned and operated by the Australian National University's Research School of Astronomy and Astrophysics. the survey data were processed and provided by the SkyMapper Team at ANU. the SkyMapper node of the All-Sky Virtual Observatory (ASVO) is hosted at the National Computational Infrastructure (NCI). Development and support the SkyMapper node of the ASVO has been funded in part by Astronomy Australia Limited (AAL) and the Australian Government through the Commonwealth's Education Investment Fund (EIF) and National Collaborative Research Infrastructure Strategy (NCRIS), particularly the National eResearch Collaboration Tools and Resources (NeCTAR) and the Australian National Data Service Projects (ANDS). We are grateful to the anonymous referee, whose comments led to large improvements in the clarity of the paper.

Published
2020
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18. HILIGT, Upper Limit Servers II — Implementing the data servers

Author

O. König, R.D. Saxton, P. Kretschmar, L. Angelini, G. Belanger, P.A. Evans, M.J. Freyberg, V. Savchenko, I. Traulsen, and J. Wilms

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Computer Science Applications
Abstract

The High-Energy Lightcurve Generator (HILIGT) is a new web-based tool which allows the user to generate long-term lightcurves of X-ray sources. It provides historical data and calculates upper limits from image data in real-time. HILIGT utilizes data from twelve satellites, both modern missions such as XMM-Newton and Swift, and earlier facilities such as ROSAT, EXOSAT, Einstein or Ariel V. Together, this enables the user to query 50 years of X-ray data and, for instance, study outburst behavior of transient sources. In this paper we focus on the individual back-end servers for each satellite, detailing the software layout, database design, catalog calls, and image footprints. We compile all relevant calibration information of these missions and provide an in-depth summary of the details of X-ray astronomical instrumentation and data., Accepted for publication in Astronomy&Computing

Published
2022
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19. The XMM-Newton serendipitous survey. X: The second source catalogue from overlapping XMM-Newton observations and its long-term variable content

Author

Filippos Koliopanos, Christian Motch, J. Kurpas, Michael Freyberg, Axel Schwope, M. G. Watson, Jean Ballet, N. A. Webb, I. Traulsen, María Teresa Ceballos, Francisco J. Carrera, Georg Lamer, Mickael Coriat, Laurent Michel, M. J. Page, 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 de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, 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), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Brightness, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Context (language use), Astrophysics, astronomical databases: miscellaneous, X-rays: general, Computer Science::Digital Libraries, 01 natural sciences, surveys, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, 1. No poverty, Astronomy and Astrophysics, Light curve, Term (time), Variable (computer science), Space and Planetary Science, Feature (computer vision), Sky, Second source, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract

arXiv:2007.02932v1, [Context]: The XMM-Newton Survey Science Centre Consortium (SSC) develops software in close collaboration with the Science Operations Centre to perform a pipeline analysis of all XMM-Newton observations. In celebration of the twentieth anniversary of the XMM-Newton launch, the SSC has compiled the fourth generation of serendipitous source catalogues, 4XMM., [Aims]: The catalogue described here, 4XMM-DR9s, explores sky areas that were observed more than once by XMM-Newton. These observations are bundled in groups referred to as stacks. Stacking leads to a higher sensitivity, resulting in newly discovered sources and better constrained source parameters, and unveils long-term brightness variations., [Methods]: The 4XMM-DR9s catalogue was constructed from simultaneous source detection on overlapping observations. As a novel feature, positional rectification was applied beforehand. Observations with all filters and suitable camera settings were included. Exposures with a high background were discarded. The high-background thresholds were determined through a statistical analysis of all exposures in each instrument configuration. The X-ray background maps used in source detection were modelled via an adaptive smoothing procedure with newly determined parameters. Source fluxes were derived for all contributing observations, irrespective of whether the source would be detectable in an individual observation., [Results]: The new catalogue lists the X-ray sources detected in 1329 stacks with 6604 contributing observations over repeatedly covered 300 square degrees in the sky. Most stacks are composed of two observations, the largest one comprises 352 observations. We find 288 191 sources of which 218 283 were observed several times. The number of observations of a source ranges from 1 to 40. Auxiliary products, like X-ray full-band and false-colour images, long-term X-ray light curves, and optical finding charts, are published as well., [Conclusions]: 4XMM-DR9s contains new detections and is considered a prime resource to explore long-term variability of X-ray sources discovered by XMM-Newton. Regular incremental releases, including new public observations, are planned., FJC acknowledges financial support through grant AYA2015-64346-C2-1P (MINECO/FEDER). FJC and MTC acknowledges financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765.

Published
2020
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20. The XMM-Newton serendipitous survey: IX. The fourth XMM-Newton serendipitous source catalogue

Author

J. Ballet, J. V. Perea-Calderon, María Teresa Ceballos, Michael Freyberg, I. de la Calle, F. X. Pineau, Francisco J. Carrera, A. Zakardjian, N. A. Webb, Georg Lamer, D. Chuard, Filippos Koliopanos, Axel Schwope, M. Santos Lleo, M. Kolehmainen, R. D. Saxton, I. Traulsen, E. Colomo, P. Maggi, Simon Rosen, T. Garcia, Mickael Coriat, L. Tomas, Laurent Michel, M. J. Page, P. Rodriguez, Christian Motch, J. Authier, Clive G. Page, M. G. Watson, Dacheng Lin, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Bristol Robotics Laboratory (BRL), University of Bristol [Bristol], Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Cyclotron ARRONAX [Saint-Herblain], ARRONAX - (GIP) Groupement d'Intérêt Public [Saint-Herblain] (Institut de Recherche Public), Institut de Mathématiques de Bordeaux (IMB), Université Bordeaux Segalen - Bordeaux 2-Université Sciences et Technologies - Bordeaux 1-Université de Bordeaux (UB)-Institut Polytechnique de Bordeaux (Bordeaux INP)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Data products, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, astronomical databases: miscellaneous, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, surveys, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Cover (topology), Space and Planetary Science, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, catalogs
Abstract

[Context]: Sky surveys produce enormous quantities of data on extensive regions of the sky. The easiest way to access this information is through catalogues of standardised data products. XMM-Newton has been surveying the sky in the X-ray, ultra-violet, and optical bands for 20 years., [Aims]: The XMM-Newton Survey Science Centre has been producing standardised data products and catalogues to facilitate access to the serendipitous X-ray sky., [Methods]: Using improved calibration and enhanced software, we re-reduced all of the 14 041 XMM-Newton X-ray observations, of which 11 204 observations contained data with at least one detection and with these we created a new, high quality version of the XMM-Newton serendipitous source catalogue, 4XMM-DR9., [Results]: 4XMM-DR9 contains 810 795 detections down to a detection significance of 3σ, of which 550 124 are unique sources, which cover 1152 degrees2 (2.85%) of the sky. Filtering 4XMM-DR9 to retain only the cleanest sources with at least a 5σ detection significance leaves 433 612 detections. Of these detections, 99.6% have no pileup. Furthermore, 336 columns of information on each detection are provided, along with images. The quality of the source detection is shown to have improved significantly with respect to previous versions of the catalogues. Spectra and lightcurves are also made available for more than 288 000 of the brightest sources (36% of all detections)., FJC acknowledges financial support through grant AYA2015-64346-C2-1P (MINECO/FEDER). MTC and FJC acknowledge financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE) cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765.

Published
2020
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21. A giant X-ray dust scattering ring discovered with SRG/eROSITA around the black hole transient MAXI J1348–630

Author

Michael Freyberg, Axel Schwope, Joern Wilms, Georg Lamer, I. Traulsen, and Peter Predehl

Subjects
Physics, 010308 nuclear & particles physics, Scattering, Extinction (astronomy), Bolometer, Astronomy and Astrophysics, Astrophysics, Ring (chemistry), 01 natural sciences, Luminosity, law.invention, symbols.namesake, Space and Planetary Science, law, 0103 physical sciences, Eddington luminosity, symbols, Halo, Parallax, 010303 astronomy & astrophysics
Abstract

We report the discovery of a giant dust scattering ring around the Black Hole transient MAXI J1348−630 with SRG/eROSITA during its first X-ray all-sky survey. During the discovery observation in February 2020, the ring had an outer diameter of 1.3 deg, growing to 1.6 deg by the time of the second all-sky survey scan in August 2020. This makes the new dust ring by far the largest X-ray scattering ring observed so far. Dust scattering halos, in particular the rings found around transient sources, provide an opportunity to make precise distance measurements towards the original X-ray sources. We combine data from SRG/eROSITA, XMM-Newton, MAXI, and Gaia to measure the geometrical distance of MAXI J1348−630. The Gaia data place the scattering dust at a distance of 2050 pc. Based on the measured time lags and the geometry of the ring we find MAXI J1348−630 at a distance of 3390 pc with a statistical uncertainty of only 1.1% and a systematic uncertainty of 10% caused mainly by the parallax offset of Gaia. This result makes MAXI J1348−630 one of the black hole transients with the most accurately determined distances. The new distance leads to a revised mass estimate for the black hole of 11 ± 2 M⊙. The transition to the soft state during the outburst occurred when the bolometric luminosity of MAXI J1348−630 reached 1.7% of its Eddington luminosity.

Published
2021
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22. X-ray and ultraviolet observations of the eclipsing cataclysmic variables OV Bootis and SDSS J103533.02+055158.3 with degenerate donors

Author

I. Traulsen, Hauke Worpel, and Axel Schwope

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Cataclysmic variable star, White dwarf, Astronomy and Astrophysics, Astrophysics, Ephemeris, medicine.disease_cause, 01 natural sciences, Accretion (astrophysics), Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, medicine, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Dwarf nova, Solar and Stellar Astrophysics (astro-ph.SR), Ultraviolet, Eclipse
Abstract

The majority of cataclysmic variables are predicted to be post-period minimum systems with degenerate donor stars, the period bouncers. Owing to their intrinsic faintness, however, only a handful of these systems have so far been securely identified. We want to study the X-ray properties of two eclipsing period bouncers, OV Bootis and SDSS J103533.02+055158.3, that were selected for this study due to their proximity to Earth. We have obtained XMM-Newton phase-resolved X-ray and ultraviolet observations of the two objects for spectral and timing analysis. Owing to a recent dwarf nova outburst OV Boo was much brighter than SDSS J103533.02+055158.3 at X-ray and ultraviolet wavelengths and the eclipse could be studied in some detail. An updated eclipse ephemeris was derived. The X-rays were shown to originate close to the white dwarf, the boundary layer, with significant absorption affecting its spectrum. There was no absorption in SDSS J103533.02+055158.3, despite being observed at the same inclination indicating different shapes of the disk and the disk rim. The white-dwarf temperature was re-determined for both objects: the white dwarf in OV Boo was still hot (23,000 K) five months after a dwarf nova outburst, and the white dwarf in SDSS J103533.02+055158.3 hotter than assumed previously (Teff = 11,500 K). All three cataclysmic variables with degenerate donors studied so far in X-rays, including SDSS J121209.31+013627.7, were clearly discovered in X-rays and revealed mass accretion rates dot(M) >= 8 x 10^(-15) Msun/ yr. If their X-ray behavior is representative of the subpopulation of period bouncers, the all-sky X-ray surveys with eROSITA together with comprehensive follow-up will uncover new objects in sufficient number to address the remaining questions concerning late-stage cataclysmic variable evolution., 12 pages, 13 figures, accepted for publication in A&A

Published
2021
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23. The XMM-Newton serendipitous survey. VIII: The first XMM-Newton serendipitous source catalogue from overlapping observations

Author

Michael Freyberg, Jean Ballet, N. A. Webb, Filippos Koliopanos, Christian Motch, I. Traulsen, Georg Lamer, Francisco J. Carrera, Mickael Coriat, J. Kurpas, M. G. Watson, Simon Rosen, María Teresa Ceballos, Laurent Michel, M. J. Page, Axel Schwope, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Universidad de Cantabria

Subjects
Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, astronomical databases: miscellaneous, Surveys, EPIC, X-rays: general, 01 natural sciences, surveys, general [X-rays], 0103 physical sciences, Web page, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Member states, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Space and Planetary Science, Sky, miscellaneous [Astronomical databases], Catalogs, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs
Abstract

XMM-Newton has observed the X-ray sky since early 2000. The XMM-Newton Survey Science Centre Consortium has published catalogues of X-ray and ultraviolet sources found serendipitously in the individual observations. This series is now augmented by a catalogue dedicated to X-ray sources detected in spatially overlapping XMM-Newton observations. The aim of this catalogue is to explore repeatedly observed sky regions. It thus makes use of the long(er) effective exposure time per sky area and offers the opportunity to investigate long-term flux variability directly through the source detection process. A new standardised strategy for simultaneous source detection on multiple observations is introduced. It is coded as a new task within the XMM-Newton Science Analysis System and used to compile a catalogue of sources from 434 stacks comprising 1,789 overlapping XMM-Newton observations that entered the 3XMM-DR7 catalogue, have a low background and full-frame readout of all EPIC cameras. The first stacked catalogue is called 3XMM-DR7s. It contains 71,951 unique sources with positions and parameters such as fluxes, hardness ratios, quality estimates, and information on inter-observation variability. About 15% of the sources are new with respect to 3XMM-DR7. Through stacked source detection, the parameters of repeatedly observed sources can be determined with higher accuracy than in the individual observations. The method is more sensitive to faint sources and tends to produce fewer spurious detections. With this first stacked catalogue we demonstrate the feasibility and benefit of the approach. It supplements the large data base of XMM-Newton detections by additional, in particular faint, sources and adds variability information. In the future, the catalogue will be expanded to larger samples and continued within the series of serendipitous XMM-Newton source catalogues., Accepted for publication in A&A. 27 pages, ~4MB

Published
2019
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24. The XMM-Newton serendipitous survey. VII. The third XMM-Newton serendipitous source catalogue

Author

Filippos Koliopanos, Manfred W. Pakull, I. Traulsen, Michael Freyberg, Natalie A. Webb, Simon Rosen, Masaaki Sakano, D. Law-Green, G. Denkinson, Axel Schwope, P. Esquej, A. E. Scott, Vladimir Yershov, Laurent Michel, M. J. Page, Jean Ballet, María Teresa Ceballos, Georg Lamer, R. D. Saxton, John P. Pye, Sean Farrell, R. Della Ceca, Valentina Braito, Francisco J. Carrera, Fabien Grisé, Mickael Coriat, Christian Motch, Didier Barret, P. Rodriguez, Dacheng Lin, K. L. Page, Clive G. Page, M. G. Watson, Richard Sturm, Patrick Guillout, A. M. Read, A. Nebot Gomez-Moran, L. Heil, Ivan Zolotukhin, R. Martino, Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), 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), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Observatoire astronomique de Strasbourg ( ObAS ), Université de Strasbourg ( UNISTRA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), and FRA

Subjects
media_common.quotation_subject, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, astronomical databases: miscellaneous, X-rays: general, 01 natural sciences, surveys, Observatory, 0103 physical sciences, Calibration, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Measure (data warehouse), Cross-correlation, 010308 nuclear & particles physics, Mode (statistics), Astronomy, Astronomy and Astrophysics, Space and Planetary Science, Sky, Data quality, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], catalogs, Data reduction
Abstract

Thanks to the large collecting area (3 x ~1500 cm$^2$ at 1.5 keV) and wide field of view (30' across in full field mode) of the X-ray cameras on board the European Space Agency X-ray observatory XMM-Newton, each individual pointing can result in the detection of hundreds of X-ray sources, most of which are newly discovered. Recently, many improvements in the XMM-Newton data reduction algorithms have been made. These include enhanced source characterisation and reduced spurious source detections, refined astrometric precision, greater net sensitivity and the extraction of spectra and time series for fainter sources, with better signal-to-noise. Further, almost 50\% more observations are in the public domain compared to 2XMMi-DR3, allowing the XMM-Newton Survey Science Centre (XMM-SSC) to produce a much larger and better quality X-ray source catalogue. The XMM-SSC has developed a pipeline to reduce the XMM-Newton data automatically and using improved calibration a new catalogue version has been produced from XMM-Newton data made public by 2013 Dec. 31 (13 years of data). Manual screening ensures the highest data quality. This catalogue is known as 3XMM. In the latest release, 3XMM-DR5, there are 565962 X-ray detections comprising 396910 unique X-ray sources. For the 133000 brightest sources, spectra and lightcurves are provided. For all detections, the positions on the sky, a measure of the quality of the detection, and an evaluation of the X-ray variability is provided, along with the fluxes and count rates in 7 X-ray energy bands, the total 0.2-12 keV band counts, and four hardness ratios. To identify the detections, a cross correlation with 228 catalogues is also provided for each X-ray detection. 3XMM-DR5 is the largest X-ray source catalogue ever produced. Thanks to the large array of data products, it is an excellent resource in which to find new and extreme objects., Comment: 23 pages, version accepted for publication in A&A

Published
2016
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25. X-ray and optical observations of four polars

Author

T. Granzer, K. Reinsch, Axel Schwope, R. Schwarz, I. Traulsen, and Hauke Worpel

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Infrared, Astrophysics::High Energy Astrophysical Phenomena, White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Astrophysics::Cosmology and Extragalactic Astrophysics, Ephemeris, 01 natural sciences, Accretion (astrophysics), Magnetic field, Space and Planetary Science, 0103 physical sciences, Polar, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

We aim to study the temporal and spectral behaviour of four polar CVs from the infrared to X-ray regimes, refine our knowledge of the physical parameters of these systems at different accretion rates, and to search for a possible excess of soft X-ray photons. We analysed four XMM X-ray observations of three of the sources, two of them discovered in SDSS, one in RASS. The X-ray data were complemented by optical photometry and spectroscopy and, for two sources, archival Swift observations. SDSSJ0328 was X-ray bright in two XMM and two Swift observations, and shows transitions from high and low accretion states over a few months. It has no strong soft excess. We measured the magnetic field strength at the main pole to be 39 MG, the inclination to be 45, Comment: 13 pages, 14 figures

Published
2016
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26. XMM-Newton observations of the low-luminosity cataclysmic variable V405 Pegasi

Author

Axel Schwope, V. Scipione, Adriana M. Pires, I. Traulsen, T. Granzer, R. Schwarz, and John R. Thorstensen

Subjects
Physics, education.field_of_study, Galactic ridge, Astrophysics::High Energy Astrophysical Phenomena, Population, Cataclysmic variable star, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Orbital period, Luminosity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, ROSAT, Spectral energy distribution, Astrophysics::Solar and Stellar Astrophysics, education, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

V405 Peg is a low-luminosity cataclysmic variable (CV) that was identified as the optical counterpart of the bright, high-latitude ROSAT all-sky survey source RBS1955. The system was suspected to belong to a largely undiscovered population of hibernating CVs. Despite intensive optical follow-up its subclass however remained undetermined. We want to further classify V405 Peg and understand its role in the CV zoo via its long-term behaviour, spectral properties, energy distribution and accretion luminosity. We perform a spectral and timing analysis of \textit{XMM-Newton} X-ray and ultra-violet data. Archival WISE, HST, and Swift observations are used to determine the spectral energy distribution and characterize the long-term variability. The X-ray spectrum is characterized by emission from a multi-temperature plasma. No evidence for a luminous soft X-ray component was found. Orbital phase-dependent X-ray photometric variability by $\sim50\%$ occurred without significant spectral changes. No further periodicity was significant in our X-ray data. The average X-ray luminosity during the XMM-Newton observations was L_X, bol simeq 5e30 erg/s but, based on the Swift observations, the corresponding luminosity varied between 5e29 erg/s and 2e31 erg/son timescales of years. The CV subclass of this object remains elusive. The spectral and timing properties show commonalities with both classes of magnetic and non-magnetic CVs. The accretion luminosity is far below than that expected for a standard accreting CV at the given orbital period. Objects like V405 Peg might represent the tip of an iceberg and thus may be important contributors to the Galactic Ridge X-ray Emission. If so they will be uncovered by future X-ray surveys, e.g. with eROSITA., Comment: A&A, in press

Published
2013
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27. XMM-Newton observations of the X-ray soft polar QS Telescopii

Author

Axel Schwope, R. Schwarz, Vadim Burwitz, F. M. Walter, I. Traulsen, K. Reinsch, and Stefan Dreizler

Subjects
Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Plasma, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, 01 natural sciences, 7. Clean energy, Accretion (astrophysics), Spectral line, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, ROSAT, fundamental parameters / stars: individual: QS Telescopii / X-rays: binaries / accretion, accretion disks [novae, cataclysmic variables / stars], Polar, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences
Abstract

Context. On the basis of XMM-Newton observations, we investigate the energy balance of selected magnetic cataclysmic variables, which have shown an extreme soft-to-hard X-ray flux ratio in the ROSAT All-Sky Survey. Aims. We intend to establish the X-ray properties of the system components, their flux contributions, and the accretion geometry of the X-ray soft polar QS Tel. In the context of high-resolution X-ray analyses of magnetic cataclysmic variables, this study will contribute to better understanding the accretion processes on magnetic white dwarfs. Methods. During an intermediate high state of accretion of QS Tel, we have obtained 20 ks of XMM-Newton data, corresponding to more than two orbital periods, accompanied by simultaneous optical photometry and phase-resolved spectroscopy. We analyze the multi-wavelength spectra and light curves and compare them to former high- and low-state observations. Results. Soft emission at energies below 2 keV dominates the X-ray light curves. The complex double-peaked maxima are disrupted by a sharp dip in the very soft energy range (0.1-0.5 keV), where the count rate abruptly drops to zero. The EPIC spectra are described by a minimally absorbed black body at 20 eV and two partially absorbed MEKAL plasma models with temperatures around 0.2 and 3 keV. The black-body-like component arises from one mainly active, soft X-ray bright accretion region nearly facing the mass donor. Parts of the plasma emission might be attributed to the second, virtually inactive pole. High soft-to-hard X-ray flux ratios and hardness ratios demonstrate that the high-energy emission of QS Tel is substantially dominated by its X-ray soft component., Comment: Accepted for publication in Astronomy and Astrophysics. 7 pages, 4 figures, 2 tables

Published
2011
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28. X-ray spectroscopy and photometry of the long-period polar AI Tri with XMM-Newton

Author

I. Traulsen, A. D. Schwope, K. Beuermann, Klaus Reinsch, Vadim Burwitz, R. Schwarz, and S. Dreizler

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Cataclysmic variable star, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Photometry (optics), 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, White dwarf, Astronomy and Astrophysics, Light curve, Accretion (astrophysics), Magnetic field, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Polar, Astrophysics::Earth and Planetary Astrophysics, novae, cataclysmic variables, stars, individual, AI Tri, X-rays, binaries, accretion, accretion disks
Abstract

Context. The energy balance of cataclysmic variables with strong magnetic fields is a central subject in understanding accretion processes on magnetic white dwarfs. With XMM-Newton, we perform a spectroscopic and photometric study of soft X-ray selected polars during their high states of accretion. Aims. On the basis of X-ray and optical observations of the magnetic cataclysmic variable AI Tri, we derive the properties of the spectral components, their flux contributions, and the physical structure of the accretion region in soft polars. Methods. We use multi-temperature approaches in our xspec modeling of the spectra to describe the physical conditions and the structures of the post-shock accretion flow and the accretion spot on the white-dwarf surface. In addition, we investigate the accretion geometry of the system by a timing analysis of the photometric data. Results. Flaring soft X-ray emission from the heated surface of the white dwarf dominates the X-ray flux during roughly 70% of the binary cycle. This component deviates from a single black body and can be described by a superimposition of mildly absorbed black bodies with a Gaussian temperature distribution. In addition, weaker hard X-ray emission is visible nearly all the time. The spectrum from the cooling post-shock accretion flow is most closely fitted by a combination of thermal plasma mekal models with temperature profiles adapted from prior stationary two-fluid hydrodynamic calculations. The soft X-ray light curves show a dip during the bright phase, which can be interpreted as self-absorption in the accretion stream. Phase-resolved spectral modeling supports the picture of one-pole accretion and self-eclipse. One of the optical light curves corresponds to an irregular mode of accretion. During a short XMM-Newton observation at the same epoch, the X-ray emission of the system is clearly dominated by the soft component., Comment: A&A, in press; 11 pages, 9 figures, 3 tables

Published
2010
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29. Towards a dynamical mass of a PG 1159 star: radial velocities and spectral analysis of SDSS J212531-010745

Author

Benjamin Beeck, Thorsten Nagel, Sonja Schuh, and I. Traulsen

Subjects
Physics, Stellar mass, Binary number, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Effective temperature, Star (graph theory), Light curve, Spectral line, Radial velocity, Stars, Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract

The evolutionary scenarios which are commonly accepted for PG 1159 stars are mainly based on numerical simulations, which have to be tested and calibrated with real objects with known stellar parameters. One of the most crucial but also quite uncertain parameters is the stellar mass. PG 1159 stars have masses between 0.5 and 0.8 M_sun, as derived from asteroseismic and spectroscopic determinations. Such mass determinations are, however, themselves model-dependent. Moreover, asteroseismically and spectroscopically determined masses deviate systematically for PG 1159 stars by up to 10%. SDSS J212531.92-010745.9 is the first known PG 1159 star in a close binary with a late-main-sequence companion allowing a dynamical mass determination. We have obtained 14 Calar Alto spectra of SDSS J212531.92-010745.9 covering the full orbital phase range. A radial velocity curve was extracted for both components. With co-added phase-corrected spectra the spectral analysis of the PG 1159 component was refined. The irradiation of the companion by the PG 1159 star is modelled with PHOENIX, yielding constraints on radii, effective temperature and separation of the system's components. The light curve of SDSS J212531.92-010745.9, obtained during three seasons of photometry with the Goettingen 50 cm and Tuebingen 80 cm telescopes, was modelled with both the NIGHTFALL and PHOEBE programs., 3 pages, JENAM 2008 proceedings, to be published in 'Communications in Asteroseismology', 159

Published
2009

30. A new period determination for the close PG1159 binary SDSSJ212531.92-010745.9

Author

Sonja Schuh, R. Lutz, Matthias R. Schreiber, Thorsten Nagel, E. Reiff, Derek Homeier, D.-J. Kusterer, H. Schwager, and I. Traulsen

Subjects
Physics, 010504 meteorology & atmospheric sciences, Astrophysics (astro-ph), Binary number, White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Ephemeris, 01 natural sciences, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Period (music), 0105 earth and related environmental sciences
Abstract

Methods to measure masses of PG1159 stars in order to test evolutionary scenarios are currently based on spectroscopic masses or asteroseismological mass determinations. One recently discovered PG1159 star in a close binary system may finally allow the first dynamical mass determination, which has so far been analysed on the basis of one SDSS spectrum and photometric monitoring. In order to be able to phase future radial velocity measurements of the system SDSSJ212531.92-010745.9, we follow up on the photometric monitoring of this system to provide a solid observational basis for an improved orbital ephemeris determination. New white-light time series of the brightness variation of SDSSJ212531.92-010745.9 with the Tuebingen 80cm and Goettingen 50cm telescopes extend the monitoring into a second season (2006), tripling the length of overall observational data available, and significantly increasing the time base covered. We give the ephemeris for the orbital motion of the system, based on a sine fit which now results in a period of 6.95573(5)h, and discuss the associated new amplitude determination in the context of the phased light curve variation profile. The accuracy of the ephemeris has been improved by more than one order of magnitude compared to that previously published for 2005 alone., Comment: 3 pages, 2 figures, accepted for publication in Astronomical Notes

Published
2007
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31. Light and heavy metal abundances in hot central stars of planetary nebulae

Author

Klaus Werner, I. Traulsen, Jeffrey W. Kruk, Agnes I. D. Hoffmann, E. Reiff, D. Jahn, Thomas Rauch, and Stefan Dreizler

Subjects
Physics, Very Large Telescope, Far ultraviolet, Astrophysics (astro-ph), chemistry.chemical_element, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Planetary nebula, Stars, Neon, chemistry, Hubble space telescope, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Spectroscopy, Astrophysics::Galaxy Astrophysics
Abstract

We present new results from our spectral analyses of very hot central stars achieved since the last IAU Symposium on planetary nebulae held in Canberra 2001. The analyses are mainly based on UV and far-UV spectroscopy performed with the Hubble Space Telescope and the Far Ultraviolet Spectroscopic Explorer but also on ground-based observations performed at the Very Large Telescope and other observatories. We report on temperature, gravity, and abundance determinations for the CNO elements of hydrogen-rich central stars. In many hydrogen-deficient central stars (spectral type PG1159) we discovered particular neon and fluorine lines, which are observed for the very first time in any astrophysical object. Their analysis strongly confirms the idea that these stars exhibit intershell matter as a consequence of a late helium-shell flash., Conf. proceedings, Gdansk 2005, Planetary Nebulae as astronomical tools, 4 pages, 4 figures

Published
2005

32. Phase-resolved X-ray spectroscopy and spectral energy distribution of the X-ray soft polar RS Caeli

Author

Axel Schwope, I. Traulsen, F. M. Walter, Vadim Burwitz, K. Reinsch, and R. Schwarz

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Stellar atmosphere, FOS: Physical sciences, Astronomy and Astrophysics, novae, cataclysmic variables, stars, fundamental parameters, individual, RS Caeli, X-rays, binaries, accretion, accretion disks, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Light curve, 01 natural sciences, Spectral line, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, ROSAT, Reflection (physics), Spectral energy distribution, Polar, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

RS Cae is the third target in our series of XMM-Newton observations of soft X-ray-dominated polars. Our observational campaign aims to better understand and describe the multiwavelength data, the physical properties of the system components, and the short- and long-term behavior of the component fluxes in RS Cae. We employ stellar atmosphere, stratified accretion-column, and widely used X-ray spectral models. We fit the XMM-Newton spectra, model the multiband light curves, and opt for a mostly consistent description of the spectral energy distribution. Results. Our XMM-Newton data of RS Cae are clearly dominated by soft X-ray emission. The X-ray light curves are shaped by emission from the main accretion region, which is visible over the whole orbital cycle, interrupted only by a stream eclipse. The optical light curves are formed by cyclotron and stream emission. The XMM-Newton X-ray spectra comprise a black-body-like and a plasma component at mean temperatures of 36eV and 7keV. The spectral fits give evidence of a partially absorbing and a reflection component. Multitemperature models, covering a broader temperature range in the X-ray emitting accretion regions, reproduce the spectra appropriately well. Including archival data, we describe the spectral energy distribution with a combination of models based on a consistent set of parameters and derive a lower limit estimate of the distance d > 750pc. Conclusions. The high bolometric soft-to-hard flux ratios and short-term variability of the (X-ray) light curves are characteristic of inhomogeneous accretion. RS Cae clearly belongs in the group of polars that show a very strong soft X-ray flux compared to their hard X-ray flux. The different black-body fluxes and similar hard X-ray and optical fluxes during the XMM-Newton and ROSAT observations show that soft and hard X-ray emission are not directly correlated., A&A, in press

Published
2014
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33. The LOFT mission concept: a status update

Author

Feroci, M, Bozzo, E, Brandt, S, Hernanz, M, Van Der Klis, M, Liu, L, Orleanski, P, Pohl, M, Santangelo, A, Schanne, S, Stella, L, Takahashi, T, Tamura, H, Watts, A, Wilms, J, Zane, S, Zhang, S, Bhattacharyya, S, Agudo, I, Ahangarianabhari, M, Albertus, C, Alford, M, Alpar, A, Altamirano, D, Alvarez, L, Amati, L, Amoros, C, Andersson, N, Antonelli, A, Argan, A, Artigue, R, Artigues, B, Atteia, J, Azzarello, P, Bakala, P, Ballantyne, Dr, Baldazzi, G, Baldo, M, Balman, S, Barbera, M, Van Baren, C, Barret, D, Baykal, A, Begelman, M, Behar, E, Behar, O, Belloni, T, Bellutti, P, Bernardini, F, Bertuccio, G, Bianchi, S, Bianchini, A, Binko, P, Blay, P, Bocchino, F, Bode, M, Bodin, P, Bombaci, I, Bonnet Bidaud, J, Borghi, G, Boutloukos, S, Bouyjou, F, Bradley, L, Braga, J, Briggs, Ms, Brown, E, Buballa, M, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jorgensen, C, Cackett, E, Cadoux, Fr, Cais, P, Caliandro, Ga, Campana, R, Campana, S, Cao, X, Capitanio, F, Casares, J, Casella, P, Castro-Tirado, Aj, Cavazzuti, E, Cavechi, Y, Celestin, S, Cerda-Duran, P, Chakrabarty, D, Chamel, N, Chateau, F, Chen, C, Chen, Y, Chenevez, J, Chernyakova, M, Coker, J, Cole, R, Collura, A, Coriat, M, Cornelisse, R, Costamante, L, Cros, A, Cui, W, Cumming, A, Cusumano, G, Czerny, B, D'Ai, A, D'Ammando, F, D'Elia, V, Dai, Z, Del Monte, E, De Luca, A, De Martino, D, Dercksen, Jpc, De Pasquale, M, De Rosa, A, Del Santo, M, Di Cosimo, S, Degenaar, N, Den Herder, Jw, Diebold, S, Di Salvo, T, Dong, Y, Donnarumma, I, Doroshenko, V, Doyle, G, Drake, Sa, Durant, M, Emmanoulopoulos, D, Enoto, T, Erkut, Mh, Esposito, P, Evangelista, Y, Fabian, A, Falanga, M, Favre, Y, Feldman, C, Fender, R, Feng, H, Ferrari, V, Ferrigno, C, Ficorella, F, Finger, M, Finger, Mh, Fraser, Gw, Frericks, M, Fullekrug, M, Fuschino, F, Gabler, M, Galloway, Dk, Galvez Sanchez, Jl, Gandhi, P, Gao, Z, Garcia-Berro, E, Gendre, B, Gevin, O, Gezari, S, Giles, Ab, Gilfanov, M, Giommi, P, Giovannini, G, Giroletti, M, Gogus, E, Goldwurm, A, Goluchova, K, Gotz, D, Gou, L, Gouiffes, C, Grandi, P, Grassi, M, Greiner, J, Grinberg, V, Groot, P, Gschwender, M, Gualtieri, L, Guedel, M, Guidorzi, C, Guy, L, Haas, D, Haensel, P, Hailey, M, Hamuguchi, K, Hansen, F, Hartmann, Dh, Haswell, Ca, Hebeler, K, Heger, A, Hempel, M, Hermsen, W, Homan, J, Hornstrup, A, Hudec, R, Huovelin, J, Huppenkothen, D, Inam, Sc, Ingram, A, In'Tzand, Jjm, Israel, G, Iwasawa, K, Izzo, L, Jacobs, Hm, Jetter, F, Johannsen, T, Jenke, Pa, Jonker, P, Jose, J, Kaaret, P, Kalamkar, M, Kalemci, E, Kanbach, G, Karas, V, Karelin, D, Kataria, D, Keek, L, Kennedy, T, Klochkov, D, Kluzniak, W, Koerding, E, Kokkotas, K, Komossa, S, Korpela, S, Kouveliotou, C, Kowalski, Af, Kreykenbohm, I, Kuiper, Lm, Kunneriath, D, Kurkela, A, Kuvvetli, I, La Franca, F, Labanti, C, Lai, D, Lamb, Fk, Lachaud, C, Laubert, Pp, Lebrun, F, Li, X, Liang, E, Limousin, O, Lin, D, Linares, M, Linder, D, Lodato, G, Longo, F, Lu, F, Lund, N, Maccarone, Tj, Macera, D, Maestre, S, Mahmoodifar, S, Maier, D, Malcovati, P, Malzac, J, Malone, C, Mandel, I, Mangano, V, Manousakis, A, Marelli, M, Margueron, J, Marisaldi, M, Markoff, Sb, Markowitz, A, Marinucci, A, Martindale, A, Martinez, G, Mchardy, Im, Medina-Tanco, G, Mehdipour, M, Melatos, A, Mendez, M, Mereghetti, S, Migliari, S, Mignani, R, Michalska, M, Mihara, T, Miller, Mc, Miller, Jm, Mineo, T, Miniutti, G, Morsink, S, Motch, C, Motta, S, Mouchet, M, Mouret, G, Mulacova, J, Muleri, F, Munoz-Darias, T, Negueruela, I, Neilsen, J, Neubert, T, Norton, Aj, Nowak, M, Nucita, A, O'Brien, P, Oertel, M, Olsen, Peh, Orienti, M, Orio, M, Orlandini, M, Osborne, Jp, Osten, R, Ozel, F, Pacciani, L, Paerels, F, Paltani, S, Paolillo, M, Papadakis, I, Papitto, A, Paragi, Z, Paredes, Jm, Patruno, A, Paul, B, Pederiva, F, Perinati, E, Pellizzoni, A, Penacchioni, Av, Peretz, U, Perez, Ma, Perez-Torres, M, Peterson, Bm, Petracek, V, Picciotto, A, Piemonte, C, Pittori, C, Pons, J, Portell, J, Possenti, A, Postnov, K, Poutanen, J, Prakash, M, Prandoni, I, Le Provost, H, Psaltis, D, Pye, J, Qu, J, Rambaud, D, Ramon, P, Ramsay, G, Rapisarda, M, Rachevski, A, Rashevskaya, I, Ray, Ps, Rea, N, Reddy, S, Reig, P, Reina Aranda, M, Remillard, R, Reynolds, C, Rezzolla, L, Ribo, M, De La Rie, R, Riggio, A, Rios, A, Rischke, Dh, Rodriguez-Gil, P, Rodriguez, J, Rohlfs, R, Romano, P, Rossi, Emr, Rozanska, A, Rousseau, A, Rudak, B, Russell, Dm, Ryde, F, Sabau-Graziati, L, Sakamoto, T, Sala, G, Salvaterra, R, Salvetti, D, Sanna, A, Sandberg, J, Savolainen, T, Scaringi, S, Schaffner-Bielich, J, Schatz, H, Schee, J, Schmid, C, Serino, M, Shakura, N, Shore, S, Schnittman, Jd, Schneider, R, Schwenk, A, Schwope, Ad, Sedrakian, A, Seyler, J, Shearer, A, Slowikowska, A, Sims, M, Smith, A, Smith, Dm, Smith, Pj, Sobolewska, M, Sochora, V, Soffitta, P, Soleri, P, Song, L, Spencer, A, Stamerra, A, Stappers, B, Staubert, R, Steiner, Aw, Stergioulas, N, Stevens, Al, Stratta, G, Strohmayer, Te, Stuchlik, Z, Suchy, S, Suleimanov, V, Tamburini, F, Tauris, T, Tavecchio, F, Tenzer, C, Thielemann, Fk, Tiengo, A, Tolos, L, Tombesi, F, Tomsick, J, Torok, G, Torrejon, Jm, Torres, Df, Torresi, E, Tramacere, A, Traulsen, I, Trois, A, Turolla, R, Turriziani, S, Typel, S, Uter, P, Uttley, P, Vacchi, A, Varniere, P, Vaughan, S, Vercellone, S, Vietri, M, Vincent, Fh, Vrba, V, Walton, D, Wang, J, Wang, Z, Watanabe, S, Wawrzaszek, R, Webb, N, Weinberg, N, Wende, H, Wheatley, P, Wijers, R, Wijnands, R, Wille, M, Wilson-Hodge, Ca, Winter, B, Walk, Sj, Wood, K, Woosley, Se, Wu, X, Xiao, L, Xu, R, Yu, W, Yuan, F, Yuan, W, Yuan, Y, Zampa, G, Zampa, N, Zampieri, L, Zdunik, L, Zdziarski, A, Zech, A, Zhang, B, Zhang, C, Zingale, M, Zorzi, N, Zwart, F, High Energy Astrophys. & Astropart. Phys (API, FNWI), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Icahn School of Medicine at Mount Sinai [New York] (MSSM), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, 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), Dipartimento di Scienze e Tecnologie Chimiche, Università degli Studi di Roma Tor Vergata [Roma], Graduate School of the Natural Science and Technology [Kanazawa], Kanazawa University (KU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Centre Interdisciplinaire de Nanoscience de Marseille (CINaM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Tampere University of Technology [Tampere] (TUT), University of Maryland [College Park], University of Maryland System, Department of Biological Sciences [Mississippi], University of Southern Mississippi (USM), School of Physics and Astronomy [Southampton], University of Southampton, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Università di Roma La Sapienza, Università di Roma Tor Vergata, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Swedish Institute of Space Physics [Uppsala] (IRF), INAF - Osservatorio Astronomico di Brera (OAB), Department of Computer Sciences [Scheffield], University of Sheffield [Sheffield], Colgate University, Bibliothèque nationale de France (BnF), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), ARC Centre of Excellence for Environmental Decisions (ARC CEED), The University of Western Australia (UWA)-Australian National University (ANU)-University of Queensland [Brisbane]-Royal Melbourne Institute of Technology University (RMIT University)-School of BioSciences [Melbourne], Faculty of Science [Melbourne], University of Melbourne-University of Melbourne-Faculty of Science [Melbourne], University of Melbourne-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies (CoralCoE), James Cook University (JCU), Lund University [Lund], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse (AMIS), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de synthèse organique (DCSO), École polytechnique (X)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Alabama at Birmingham [ Birmingham] (UAB), INAF - Osservatorio Astronomico di Cagliari (OAC), ELECTRONIQUE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), School of Geosciences, Monash University [Clayton], 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), Université libre de Bruxelles (ULB), National Oceanography Centre [Southampton] (NOC), Dublin Institute for Advanced Studies (DIAS), Dublin City University [Dublin] (DCU), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Institut Parisien de Chimie Moléculaire (IPCM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), China Information Technology Security Evaluation Center (CNITSEC), Department of Applied Mathematics and Computer Science [Lyngby] (DTU Compute), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), PCAS, Anton Pannekoek Institute for Astronomy, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), International Space Science Institute [Bern] (ISSI), Université Grenoble Alpes - UFR Médecine (UGA UFRM), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), CALVIN research group [Edinburgh], Institute of Perception, Action and Behaviour (IPAB), University of Edinburgh-University of Edinburgh, Department of Electronics and Electrical Engineering [Bath], University of Bath [Bath], United States Geological Survey [Reston] (USGS), Sr. PLM Consultant, 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, Dept Ind Engn & Informat Techonolgy, Università degli studi di Trieste = University of Trieste, Max-Planck-Institut für Extraterrestrische Physik (MPE), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Wisconsin Regional Primate Research Center, University of Wisconsin-Madison, SRON Netherlands Institute for Space Research (SRON), Opole University of Technology, University of Technology (Opole), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Radboud University [Nijmegen], NASA Goddard Space Flight Center (GSFC), Dept Fis Aplicada, Universidad de Granada = University of Granada (UGR), Victoria University [Melbourne], The Hong Kong Polytechnic University [Hong Kong] (POLYU), Chinese Academy of Sciences [Changchun Branch] (CAS), Department of Physics, Chemistry and Biology [Linköping] (IFM), Linköping University (LIU), Institut de Chimie des Substances Naturelles (ICSN), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Centre de recherche en Biologie cellulaire de Montpellier (CRBM), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Zielona Góra, Department of Electronics and Computer Systems, Takushoku University, Instituto Nacional de Pesquisas da Amazônia (INPA), Università degli studi di Catania = University of Catania (Unict), Centre d'Ecologie et des Sciences de la COnservation (CESCO), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ecologie Alpine (LECA ), 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]), Laboratoire de Physico-Chimie de l'Atmosphère (LPCA), Université du Littoral Côte d'Opale (ULCO)-Centre National de la Recherche Scientifique (CNRS), HEPL, Solar Physics, Stanford University, Institut des Sciences Moléculaires de Marseille (ISM2), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Columbia University [New York], Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Department of Anthropology [University of Arkansas], University of Arkansas [Fayetteville], Hu county ventre for disease control and prevention of Shaanxi province, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Istituto Nazionale di Fisica Nucleare (INFN), Institut Jean le Rond d'Alembert (DALEMBERT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Reading (UOR), Departamento de Matemática Aplicada, Universidade de Santiago de Compostela [Spain] (USC ), Osservatorio Astrofisico di Catania, Équipe Robotique et InteractionS (LAAS-RIS), Laboratoire d'analyse et d'architecture des systèmes (LAAS), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Centro Euro-Mediterraneo per i Cambiamenti Climatici [Bologna] (CMCC), Institut für Theoretische Physik, Universität Heidelberg [Heidelberg] = Heidelberg University, Augsburg Hospital, Leibniz-Institut für Astrophysik Potsdam (AIP), Daimler Chrysler AG (Daimler), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Montserrat Volcano Observatory (MVO), Institut Armand Frappier (INRS-IAF), Institut National de la Recherche Scientifique [Québec] (INRS)-Réseau International des Instituts Pasteur (RIIP), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], FICLIT, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Radioastronomie (MPIFR), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Christian-Albrechts-Universität zu Kiel (CAU), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), APC - Gravitation (APC-Gravitation), 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, Cahill Center for Astronomy and Astrophysics, California Institute of Technology (CALTECH), Xinjiang Astronomical Observatory, Mitsubishi Electric Research Laboratories (MERL), Mitsubishi Research Institute, Inc., School of Urban and Regional Planning, University of Southern California (USC), National University of Defense Technology [China], Princeton University, Department of Microtechnology and Nanoscience (MC2), Chalmers University of Technology [Gothenburg, Sweden], Feroci, M., Bozzo, E., Brandt, S., Hernanz, M., van der Klis, M., Liu, L., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Zhang, S., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, E., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M., Brown, E., Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Cais, P., Caliandro, G., Campana, R., Campana, S., Cao, X., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, C., Chen, Y., Chenevez, J., Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Z., Del Monte, E., De Luca, A., De Martino, D., Dercksen, J., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J., Diebold, S., DI SALVO, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, H., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D., Gálvez Sanchez, J., Gandhi, P., Gao, Z., Garcia Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jenke, P., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A., Kreykenbohm, I., Kuiper, L., Kunneriath, D., Kurkela, A., Kuvvetli, I., La Franca, F., Labanti, C., Lai, D., Lamb, F., Lachaud, C., Laubert, P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., Mchardy, I., Medina Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Neubert, T., Norton, A., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A., Peretz, U., Perez, M., Perez Torres, M., Peterson, B., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, J., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Rudak, B., Russell, D., Ryde, F., Sabau Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J., Schneider, R., Schwenk, A., Schwope, A., Sedrakian, A., Seyler, J., Shearer, A., Slowikowska, A., Sims, M., Smith, A., Smith, D., Smith, P., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A., Stergioulas, N., Stevens, A., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Torresi, E., Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F., Vrba, V., Walton, D., Wang, J., Wang, Z., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Walk, S., Wood, K., Woosley, S., Wu, X., Xu, R., Yu, W., Yuan, F., Yuan, W., Yuan, Y., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, B., Zhang, C., Zingale, M., Zwart, F., University of Geneva [Switzerland], Eberhard Karls Universität Tübingen, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Graduate School of the Natural Science and Technology, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), School of BioSciences [Melbourne], University of Melbourne-University of Melbourne-Royal Melbourne Institute of Technology University (RMIT University)-University of Queensland [Brisbane]-Australian National University (ANU)-The University of Western Australia (UWA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), 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 Libre de Bruxelles [Bruxelles] (ULB), Dublin City University, Dublin 9, Ireland, Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), China Information Technology Security Evaluation Center, Technical University of Denmark [Lyngby] (DTU), Université Grenoble Alpes (UGA), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-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), University of Trieste, Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie Intégrative de la Cellule (I2BC), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Università degli Studi di Roma 'La Sapienza' [Rome], Radboud university [Nijmegen]-Radboud university [Nijmegen], Radboud university [Nijmegen], Universidad de Granada (UGR), Centre National de la Recherche Scientifique (CNRS), Centre de recherche en Biologie Cellulaire (CRBM), Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Catania [Catania], Laboratoire d'Ecologie Alpine (LECA), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Université du Littoral Côte d'Opale, Stanford University [Stanford], Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Università degli studi di Napoli Federico II, IFP Energies nouvelles (IFPEN), National Institute for Nuclear Physics (INFN), Institut Jean Le Rond d'Alembert (DALEMBERT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J), Ingénierie des Matériaux Polymères (IMP), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Centro Euro-Mediterraneo per i Cambiamenti Climatici (CMCC), Universität Heidelberg [Heidelberg], Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP)-Institut National de la Recherche Scientifique [Québec] (INRS), Università di Bologna [Bologna] (UNIBO), University of California [Berkeley], University of California-University of California, Universita degli Studi di Padova, 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), Chalmers University of Technology [Göteborg], Astronomy, Jan-Willem A. den Herder, Shouleh Nikzad, Kazuhiro Nakazawa, Van Der Klis, M., Liu, L. -P., Zhang, S. -N., Atteia, J. -L., Ballantyne, D. R., Van Baren, C., Bellutti, P., Bonnet Bidaud, J. -M., Borghi, G., Briggs, M. S., Budtz-Jorgensen, C., Cadoux, F. R., Caliandro, G. A., Castro-Tirado, A. J., Cerda-Duran, P., Chateau, F., D'Ai, A., Dercksen, J. P. C., Den Herder, J. W., Di Salvo, T., Drake, S. A., Erkut, M. H., Ficorella, F., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Garcia-Berro, E., Giles, A. B., Goluchova, K., Gotz, D., Hartmann, D. H., Haswell, C. A., Inam, S. C., In'Tzand, J. J. M., Jacobs, H. M., Jenke, P. A., Jose, J., Kalamkar, M., Kowalski, A. F., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Markoff, S. B., Martinez, G., Mchardy, I. M., Medina-Tanco, G., Miller, M. C., Miller, J. M., Mulacova, J., Munoz-Darias, T., Norton, A. J., Olsen, P. E. H., Osborne, J. P., Paredes, J. M., Penacchioni, A. V., Perez, M. A., Perez-Torres, M., Peterson, B. M., Picciotto, A., Piemonte, C., Rachevski, A., Ray, P. S., De La Rie, R., Rischke, D. H., Rodriguez-Gil, P., Rossi, E. M. R., Russell, D. M., Sabau-Graziati, L., Schaffner-Bielich, J., Schnittman, J. D., Schwope, A. D., Seyler, J. -Y., Smith, D. M., Smith, P. J., Steiner, A. W., Stevens, A. L., Strohmayer, T. E., Thielemann, F. K., Torrejon, J. M., Torres, D. F., Vincent, F. H., Wilson-Hodge, C. A., Walk, S. J., Woosley, S. E., Xiao, L., Zorzi, N., 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), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - Sciences et Techniques (UM2)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Université Montpellier 1 (UM1), Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, 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), Department of Psychiatry (Icahn School of Medicine at Mount Sinai) ( ISMMS ), Rutgers, The State University of New Jersey [New Brunswick] ( RUTGERS ), Institut fur Astronomie und Astrophysik, Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Kanazawa University ( KU ), Department of Earth Sciences, University of Oxford [Oxford], Centre Interdisciplinaire de Nanoscience de Marseille ( CINaM ), Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Tampere University of Technology [Tampere] ( TUT ), University of Southern Mississippi ( USM ), University of Southampton [Southampton], Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), Istituto Nazionale di Astrofisica ( INAF ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Osservatorio Astronomico di Brera ( INAF ), Bibliothèque nationale de France ( BnF ), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo ( IASF-Pa ), ARC Centre of Excellence for Environmental Decisions ( ARC CEED ), The University of Western Australia ( UWA ) -Australian National University ( ANU ) -University of Queensland [Brisbane]-RMIT University [Melbourne]-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies ( CoralCoE ), James Cook University ( JCU ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse ( AMIS ), PRES Université de Toulouse-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de synthèse organique ( DCSO ), École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Pathology, University of Alabama at Birmingham, University of Alabama at Birmingham Comprehensive Cancer Center, Birmingham, Alabama, INAF-Osservatorio di Cagliari, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique et Modèles Statistiques ( LPTMS ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Université Libre de Bruxelles [Bruxelles] ( ULB ), Ocean and Earth Sciences, National Oceanography Centre Southampton, Dublin Institute for advanced studies, 31 Fitzwilliam Place, Dublin 2, Ireland, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Institut Parisien de Chimie Moléculaire ( IPCM ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Chinese Academy of Sciences [Beijing] ( CAS ), 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 ), Department of Applied Mathematics and Computer Science [Lyngby] ( DTU Compute ), Technical University of Denmark [Lyngby] ( DTU ), Institut für Astronomie und Astrophysik ( IAAT ), Anton Pannekoek Institute for Astronomy, University of Amsterdam, University of Cambridge [UK] ( CAM ), International Space Science Institute ( ISSI ), Université Grenoble Alpes - UFR Médecine ( UGA UFRM ), Université Grenoble Alpes ( UGA ), Institute of Perception, Action and Behaviour ( IPAB ), United States Geological Survey [Reston] ( USGS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Max-Planck-Institut für Extraterrestrische Physik ( MPE ), Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology ( MIT ), Institut de Physique du Globe de Paris ( IPGP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie Intégrative de la Cellule ( I2BC ), Université Paris-Sud - Paris 11 ( UP11 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Matériaux, ingénierie et science [Villeurbanne] ( MATEIS ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ) -Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ), University of Wisconsin-Madison [Madison], SRON Netherlands Institute for Space Research ( SRON ), University of Technology ( Opole ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Grp Fis Atmosfera, Ctr Andaluz Medio Ambiente CEAMA, Universidad de Granada ( UGR ), The Hong Kong Polytechnic University [Hong Kong] ( POLYU ), Chinese Academy of Sciences [Changchun Branch] ( CAS ), Department of Physics, Chemistry and Biology, Linköping University ( LIU ), Institut de Chimie des Substances Naturelles ( ICSN ), Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique Nucléaire de Lyon ( IPNL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astronomical Institute Anton Pannekoek ( AI PANNEKOEK ), University of Amsterdam [Amsterdam] ( UvA ), Erlangen Centre for Astroparticle Physics ( ECAP ), Friedrich-Alexander Universität Erlangen-Nürnberg ( FAU ), Centre de recherches de biochimie macromoléculaire ( CRBM ), Université Montpellier 1 ( UM1 ) -Université Montpellier 2 - 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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, California Institute of Technology ( CALTECH ), Mitsubishi Electric Research Laboratories ( MERL ), Mitsubishi Electric Research Laboratories, Institute for Astronomy, University of Amsterdam, The Netherland, University of Southern California ( USC ), National University of Defense Technology [Changsha], Department of Microtechnology and Nanoscience ( MC2 ), Université Chalmers, 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), Université Nice Sophia Antipolis (UNS), Université Paris-Sud - 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P., Zhang, S. N., Atteia, J. L., Bonnet Bidaud, J. M., Castro Tirado, A. J., D'Aı, A., den Herder, J. W., Gálvez Sanchez, J. L., In't Zand, J. J. M., Nucita, Achille, Seyler, J. Y., Wilson Hodge, C. A., Baldazzi, Giuseppe, Fuschino, Fabio, Bianchi, Stefano, Casella, Piergiorgio, DE ROSA, Alessandra, Giovannini, Gabriele, LA FRANCA, Fabio, Marinucci, Andrea, Paredes, M. J., Schneider, Raffaella, Vietri, Mario, 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)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), 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), M., Feroci, E., Bozzo, S., Brandt, M., Hernanz, M., van der Kli, L. P., Liu, P., Orleanski, M., Pohl, A., Santangelo, S., Schanne, L., Stella, T., Takahashi, H., Tamura, A., Watt, J., Wilm, S., Zane, S. N., Zhang, S., Bhattacharyya, I., Agudo, M., Ahangarianabhari, C., Albertu, M., Alford, A., Alpar, D., Altamirano, L., Alvarez, L., Amati, C., Amoro, N., Andersson, A., Antonelli, A., Argan, R., Artigue, B., Artigue, J. L., Atteia, P., Azzarello, P., Bakala, D., Ballantyne, G., Baldazzi, M., Baldo, S., Balman, M., Barbera, C., van Baren, D., Barret, A., Baykal, M., Begelman, E., Behar, O., Behar, T., Belloni, F., Bernardini, G., Bertuccio, S., Bianchi, A., Bianchini, P., Binko, P., Blay, F., Bocchino, M., Bode, P., Bodin, I., Bombaci, J. M., Bonnet Bidaud, S., Boutlouko, F., Bouyjou, L., Bradley, J., Braga, M. S., Brigg, E., Brown, M., Buballa, N., Bucciantini, L., Burderi, M., Burgay, M., Bursa, C., Budtz Jørgensen, E., Cackett, F., Cadoux, P., Cai, G. A., Caliandro, R., Campana, S., Campana, X., Cao, F., Capitanio, J., Casare, P., Casella, A. J., Castro Tirado, E., Cavazzuti, Y., Cavechi, S., Celestin, P., Cerda Duran, D., Chakrabarty, N., Chamel, F., Château, C., Chen, Y., Chen, J., Chenevez, M., Chernyakova, J., Coker, R., Cole, A., Collura, M., Coriat, R., Cornelisse, L., Costamante, A., Cro, W., Cui, A., Cumming, G., Cusumano, B., Czerny, A., D'Aì, F., D'Ammando, V., D'Elia, Z., Dai, E., Del Monte, A., De Luca, D., De Martino, J. P. C., Dercksen, M., De Pasquale, A., De Rosa, M., Del Santo, S., Di Cosimo, N., Degenaar, J. W., den Herder, S., Diebold, T., Di Salvo, Y., Dong, I., Donnarumma, V., Doroshenko, G., Doyle, S. A., Drake, M., Durant, D., Emmanoulopoulo, T., Enoto, M. H., Erkut, P., Esposito, Y., Evangelista, A., Fabian, M., Falanga, Y., Favre, C., Feldman, R., Fender, H., Feng, V., Ferrari, C., Ferrigno, M., Finger, M. H., Finger, G. W., Fraser, M., Frerick, M., Fullekrug, F., Fuschino, M., Gabler, D. K., Galloway, J. L., Gálvez Sanchez, P., Gandhi, Z., Gao, E., Garcia Berro, B., Gendre, O., Gevin, S., Gezari, A. B., Gile, M., Gilfanov, P., Giommi, G., Giovannini, M., Giroletti, E., Gogu, A., Goldwurm, K., Goluchová, D., Götz, L., Gou, C., Gouiffe, P., Grandi, M., Grassi, J., Greiner, V., Grinberg, P., Groot, M., Gschwender, L., Gualtieri, M., Guedel, C., Guidorzi, L., Guy, D., Haa, P., Haensel, M., Hailey, K., Hamuguchi, F., Hansen, D. H., Hartmann, C. A., Haswell, K., Hebeler, A., Heger, M., Hempel, W., Hermsen, J., Homan, A., Hornstrup, R., Hudec, J., Huovelin, D., Huppenkothen, S. C., Inam, A., Ingram, J. J. M., In't Zand, G., Israel, K., Iwasawa, L., Izzo, H. M., Jacob, F., Jetter, T., Johannsen, P. A., Jenke, P., Jonker, J., Josè, P., Kaaret, K., Kalamkar, E., Kalemci, G., Kanbach, V., Kara, D., Karelin, D., Kataria, L., Keek, T., Kennedy, D., Klochkov, W., Kluzniak, E., Koerding, K., Kokkota, S., Komossa, S., Korpela, C., Kouveliotou, A. F., Kowalski, I., Kreykenbohm, L. M., Kuiper, D., Kunneriath, A., Kurkela, I., Kuvvetli, F., La Franca, C., Labanti, D., Lai, F. K., Lamb, C., Lachaud, P. P., Laubert, F., Lebrun, X., Li, E., Liang, O., Limousin, D., Lin, M., Linare, D., Linder, G., Lodato, F., Longo, F., Lu, N., Lund, T. J., Maccarone, D., Macera, S., Maestre, S., Mahmoodifar, D., Maier, P., Malcovati, J., Malzac, C., Malone, I., Mandel, V., Mangano, A., Manousaki, M., Marelli, J., Margueron, M., Marisaldi, S. B., Markoff, A., Markowitz, A., Marinucci, A., Martindale, G., Martínez, I. M., Mchardy, G., Medina Tanco, M., Mehdipour, A., Melato, M., Mendez, S., Mereghetti, S., Migliari, R., Mignani, M., Michalska, T., Mihara, M. C., Miller, J. M., Miller, T., Mineo, G., Miniutti, S., Morsink, C., Motch, S., Motta, M., Mouchet, G., Mouret, J., Mulačová, F., Muleri, T., Muñoz Daria, I., Negueruela, J., Neilsen, T., Neubert, A. J., Norton, M., Nowak, A., Nucita, P., O'Brien, M., Oertel, P. E. H., Olsen, M., Orienti, M., Orio, M., Orlandini, J. P., Osborne, R., Osten, F., Ozel, L., Pacciani, F., Paerel, S., Paltani, Paolillo, Maurizio, I., Papadaki, A., Papitto, Z., Paragi, J. M., Parede, A., Patruno, B., Paul, F., Pederiva, E., Perinati, A., Pellizzoni, A. V., Penacchioni, U., Peretz, M. A., Perez, M., Perez Torre, B. M., Peterson, V., Petracek, C., Pittori, J., Pon, J., Portell, A., Possenti, K., Postnov, J., Poutanen, M., Prakash, I., Prandoni, H., Le Provost, D., Psalti, J., Pye, J., Qu, D., Rambaud, P., Ramon, G., Ramsay, M., Rapisarda, A., Rashevski, I., Rashevskaya, P. S., Ray, N., Rea, S., Reddy, P., Reig, M., Reina Aranda, R., Remillard, C., Reynold, L., Rezzolla, M., Ribo, R., de la Rie, A., Riggio, A., Rio, D. H., Rischke, P., Rodríguez Gil, J., Rodriguez, R., Rohlf, P., Romano, E. M. R., Rossi, A., Rozanska, A., Rousseau, B., Rudak, D. M., Russell, F., Ryde, L., Sabau Graziati, T., Sakamoto, G., Sala, R., Salvaterra, D., Salvetti, A., Sanna, J., Sandberg, T., Savolainen, S., Scaringi, J., Schaffner Bielich, H., Schatz, J., Schee, C., Schmid, M., Serino, N., Shakura, S., Shore, J. D., Schnittman, R., Schneider, A., Schwenk, A. D., Schwope, A., Sedrakian, J. Y., Seyler, A., Shearer, A., Slowikowska, M., Sim, A., Smith, D. M., Smith, P. J., Smith, M., Sobolewska, V., Sochora, P., Soffitta, P., Soleri, L., Song, A., Spencer, A., Stamerra, B., Stapper, R., Staubert, A. W., Steiner, N., Stergioula, A. L., Steven, G., Stratta, T. E., Strohmayer, Z., Stuchlik, S., Suchy, V., Suleimanov, F., Tamburini, T., Tauri, F., Tavecchio, C., Tenzer, F. K., Thielemann, A., Tiengo, L., Tolo, F., Tombesi, J., Tomsick, G., Torok, J. M., Torrejon, D. F., Torre, E., Torresi, A., Tramacere, I., Traulsen, A., Troi, R., Turolla, S., Turriziani, S., Typel, P., Uter, P., Uttley, A., Vacchi, P., Varniere, S., Vaughan, S., Vercellone, M., Vietri, F. H., Vincent, V., Vrba, D., Walton, J., Wang, Z., Wang, S., Watanabe, R., Wawrzaszek, N., Webb, N., Weinberg, H., Wende, P., Wheatley, R., Wijer, R., Wijnand, M., Wille, C. A., Wilson Hodge, B., Winter, S. J., Walk, K., Wood, S. E., Woosley, X., Wu, R., Xu, W., Yu, F., Yuan, W., Yuan, Y., Yuan, G., Zampa, N., Zampa, L., Zampieri, L., Zdunik, A., Zdziarski, A., Zech, B., Zhang, C., Zhang, S., Zhang, M., Zingale, and F., Zwart

Subjects
X-ray timing, [ SDU.ASTR.GA ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Field of view, Astrophysics, 01 natural sciences, law.invention, law, Observatory, timing, 010303 astronomy & astrophysics, QB, Physics, microchannel plates. PROPORTIONAL COUNTER ARRAY, CALIBRATION, X-ray astronomy, Electronic, Optical and Magnetic Material, Applied Mathematics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, X-ray detectors, Condensed Matter Physics, compact objects, X-ray spectroscopy, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], spectroscopy, Cosmic Vision, [ INFO ] Computer Science [cs], Silicon detector, Astrophysics::High Energy Astrophysical Phenomena, Condensed Matter Physic, Telescope, X-ray, Silicon detectors, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Electronic, [INFO]Computer Science [cs], Optical and Magnetic Materials, Spectral resolution, DETECTOR, ta115, X-ray astronomy, Silicon detectors, timing, spectroscopy, 010308 nuclear & particles physics, X-ray imaging, Applied Mathematic, Neutron star, QB460-466 Astrophysics, Large Observatory For x-ray Timing (LOFT), Large Area Detector (LAD), Wide Field Monitor (WFM), Large Area Silicon Drift Detectors (SDD), Gamma-ray burst
Abstract

The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, >8m2 effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g., GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the current technical and programmatic status of the mission. © (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.

Published
2016
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34. Use of organic material provided by an automatic enrichment device by weaner pigs and its influence on tail lesions.

Author

Heseker P, Probst J, Ammer S, Hartmann U, Hasler M, Kemper N, and Traulsen I

Subjects
Animals, Swine, Behavior, Animal, Animal Husbandry methods, Animal Husbandry instrumentation, Weaning, Animal Welfare, Weight Gain, Exploratory Behavior, Tail
Abstract

Providing pigs with organic enrichment material is important for satisfying pigs' natural explorative behavior to prevent injurious tail biting and thus increase animal welfare in general. The aim of this study was to investigate the effects of automatically supplied enrichment material of three different types (alfalfa pellets, oat bran pellets, or a mixture of both) and different enrichment frequencies (2, 4, or 6 supplies/day) on the behavior, the occurrence of tail biting, and daily weight gains of weaner pigs. The results showed significant effects and interactions of enrichment material, frequency and the time of day on the exploratory behavior, the occurrence of tail biting, and daily weight gains. Higher probabilities for pigs using the enrichment material were observed for groups provided with only two supplies/day or receiving oat bran pellets. Additionally, more pigs explored the material when supplied in the afternoon compared to the morning. Tail lesions began to increase in week 4 of the rearing period. Higher probabilities of having a tail lesion were recorded in groups provided with two supplies/day compared to four or six supplies per day. Furthermore, the highest probabilities for pigs having a tail length loss at the end of the rearing period were shown by groups receiving two supplies/day, with 0.170 for alfalfa pellets, 0.342 for mixture, and 0.486 for oat bran pellets. For daily weight gains, only alfalfa groups differed significantly from mixture groups in the case of two supplies/day. No differences were observed for the other factor combinations. These results showed the potential of an automatic enrichment device supporting pigs in performing their natural exploratory behavior in a conventional housing system. Higher numbers of daily enrichment supplies show beneficial effects to reduce the occurrence of tail biting and tail length losses., Competing Interests: The authors have declared that no competing interests exist., (Copyright: © 2024 Heseker et al. This is an open access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited.)

Published
2024
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35. Towards automatic farrowing monitoring-A Noisy Student approach for improving detection performance of newborn piglets.

Author

Wutke M, Lensches C, Hartmann U, and Traulsen I

Subjects
Animals, Swine, Video Recording, Animal Husbandry methods, Algorithms, Female, Deep Learning, Behavior, Animal, Animal Welfare, Animals, Newborn
Abstract

Nowadays, video monitoring of farrowing and automatic video evaluation using Deep Learning have become increasingly important in farm animal science research and open up new possibilities for addressing specific research questions like the determination of husbandry relevant indicators. A robust detection performance of newborn piglets is essential for reliably monitoring the farrowing process and to access important information about the welfare status of the sow and piglets. Although object detection algorithms are increasingly being used in various scenarios in the field of livestock farming, their usability for detecting newborn piglets has so far been limited. Challenges such as frequent animal occlusions, high overlapping rates or strong heterogeneous animal postures increase the complexity and place new demands on the detection model. Typically, new data is manually annotated to improve model performance, but the annotation effort is expensive and time-consuming. To address this problem, we propose a Noisy Student approach to automatically generate annotation information and train an improved piglet detection model. By using a teacher-student model relationship we transform the image structure and generate pseudo-labels for the object classes piglet and tail. As a result, we improve the initial detection performance of the teacher model from 0.561, 0.838, 0.672 to 0.901, 0.944, 0.922 for the performance metrics Recall, Precision and F1-score, respectively. The results of this study can be used in two ways. Firstly, the results contribute directly to the improvement of piglet detection in the context of birth monitoring systems and the evaluation of the farrowing progress. Secondly, the approach presented can be transferred to other research questions and species, thereby reducing the problem of cost-intensive annotation processes and increase training efficiency. In addition, we provide a unique dataset for the detection and evaluation of newborn piglets and sow body parts to support researchers in the task of monitoring the farrowing process., Competing Interests: The authors have declared that no competing interests exist., (Copyright: © 2024 Wutke et al. This is an open access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited.)

Published
2024
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36. Detecting tail biters by monitoring pig screams in weaning pigs.

Author

Heseker P, Bergmann T, Scheumann M, Traulsen I, Kemper N, and Probst J

Subjects
Humans, Swine, Animals, Tail injuries, Weaning, Animal Welfare, Vocalization, Animal, Behavior, Animal, Bites and Stings
Abstract

Early identification of tail biting and intervention are necessary to reduce tail lesions and their impact on animal health and welfare. Removal of biters has become an effective intervention strategy, but finding them can be difficult and time-consuming. The aim of this study was to investigate whether tail biting and, in particular, individual biters could be identified by detecting pig screams in audio recordings. The study included 288 undocked weaner pigs housed in six pens in two batches. Once a tail biter (n = 7) was identified by visual inspection in the stable and removed by the farm staff, the previous days of video and audio recordings were analyzed for pig screams (sudden increase in loudness with frequencies above 1 kHz) and tail biting events until no biting before the removal was observed anymore. In total, 2893 screams were detected in four pens where tail biting occurred. Of these screams, 52.9% were caused by tail biting in the observed pen, 25.6% originated from other pens, 8.8% were not assignable, and 12.7% occurred due to other reasons. In case of a tail biting event, screams were assigned individually to biter and victim pigs. Based on the audio analysis, biters were identified between one and nine days prior to their removal from the pen after visual inspection. Screams were detected earlier than the increase in hanging tails and could therefore be favored as an early warning indicator. Analyzing animal vocalization has potential for monitoring and early detection of tail biting events. In combination with individual marks and automatic analysis algorithms, biters could be identified and tail biting efficiently reduced. In this way, biters can be removed earlier to increase animal health and welfare., (© 2024. The Author(s).)

Published
2024
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37. Characteristics of thermal images of the mammary gland and of performance in sows differing in health status and parity.

Author

Rosengart S, Chuppava B, Trost LS, Henne H, Tetens J, Traulsen I, Deermann A, Wendt M, and Visscher C

Abstract

Precision livestock farming can combine sensors and complex data to provide a simple score of meaningful productivity, pig welfare, and farm sustainability, which are the main drivers of modern pig production. Examples include using infrared thermography to monitor the temperature of sows to detect the early stages of the disease. To take account of these drivers, we assigned 697 hybrid (BHZP db. Viktoria) sows to four parity groups. In addition, by pooling clinical findings from every sow and their piglets, sows were classified into three groups for the annotation: healthy, clinically suspicious, and diseased. Besides, the udder was thermographed, and performance data were documented. Results showed that the piglets of diseased sows with eighth or higher parity had the lowest daily weight gain [healthy; 192 g ± 31.2, clinically suspicious; 191 g ± 31.3, diseased; 148 g ± 50.3 ( p < 0.05)] and the highest number of stillborn piglets (healthy; 2.2 ± 2.39, clinically suspicious; 2.0 ± 1.62, diseased; 3.91 ± 4.93). Moreover, all diseased sows showed higher maximal skin temperatures by infrared thermography of the udder ( p < 0.05). Thus, thermography coupled with Artificial Intelligence (AI) systems can help identify and orient the diagnosis of symptomatic animals to prompt adequate reaction at the earliest time., Competing Interests: Author AD was employed by EVH Select GmbH, Meppen, Germany. Author HH was employed by BHZP GmbH, Dahlenburg-Ellringen, Germany. The remaining authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest., (Copyright © 2022 Rosengart, Chuppava, Trost, Henne, Tetens, Traulsen, Deermann, Wendt and Visscher.)

Published
2022
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38. An Information-Theoretic Approach to Detect the Associations of GPS-Tracked Heifers in Pasture.

Author

Meckbach C, Elsholz S, Siede C, and Traulsen I

Subjects
Animals, Cattle, Female, Phylogeny, Geographic Information Systems
Abstract

Sensor technologies, such as the Global Navigation Satellite System (GNSS), produce huge amounts of data by tracking animal locations with high temporal resolution. Due to this high resolution, all animals show at least some co-occurrences, and the pure presence or absence of co-occurrences is not satisfactory for social network construction. Further, tracked animal contacts contain noise due to measurement errors or random co-occurrences. To identify significant associations, null models are commonly used, but the determination of an appropriate null model for GNSS data by maintaining the autocorrelation of tracks is challenging, and the construction is time and memory consuming. Bioinformaticians encounter phylogenetic background and random noise on sequencing data. They estimate this noise directly on the data by using the average product correction procedure, a method applied to information-theoretic measures. Using Global Positioning System (GPS) data of heifers in a pasture, we performed a proof of concept that this approach can be transferred to animal science for social network construction. The approach outputs stable results for up to 30% missing data points, and the predicted associations were in line with those of the null models. The effect of different distance thresholds for contact definition was marginal, but animal activity strongly affected the network structure.

Published
2021
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39. Detecting Animal Contacts-A Deep Learning-Based Pig Detection and Tracking Approach for the Quantification of Social Contacts.

Author

Wutke M, Heinrich F, Das PP, Lange A, Gentz M, Traulsen I, Warns FK, Schmitt AO, and Gültas M

Subjects
Algorithms, Animal Welfare, Animals, Movement, Neural Networks, Computer, Swine, Deep Learning
Abstract

The identification of social interactions is of fundamental importance for animal behavioral studies, addressing numerous problems like investigating the influence of social hierarchical structures or the drivers of agonistic behavioral disorders. However, the majority of previous studies often rely on manual determination of the number and types of social encounters by direct observation which requires a large amount of personnel and economical efforts. To overcome this limitation and increase research efficiency and, thus, contribute to animal welfare in the long term, we propose in this study a framework for the automated identification of social contacts. In this framework, we apply a convolutional neural network (CNN) to detect the location and orientation of pigs within a video and track their movement trajectories over a period of time using a Kalman filter (KF) algorithm. Based on the tracking information, we automatically identify social contacts in the form of head-head and head-tail contacts. Moreover, by using the individual animal IDs, we construct a network of social contacts as the final output. We evaluated the performance of our framework based on two distinct test sets for pig detection and tracking. Consequently, we achieved a Sensitivity, Precision, and F1-score of 94.2%, 95.4%, and 95.1%, respectively, and a MOTA score of 94.4%. The findings of this study demonstrate the effectiveness of our keypoint-based tracking-by-detection strategy and can be applied to enhance animal monitoring systems.

Published
2021
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40. Effects of Different Housing Systems during Suckling and Rearing Period on Skin and Tail Lesions, Tail Losses and Performance of Growing and Finishing Pigs.

Author

Lange A, Hahne M, Lambertz C, Gauly M, Wendt M, Janssen H, and Traulsen I

Abstract

Feasible alternatives to stressful weaning and tail-docking are needed to inhibit tail biting. Therefore, we investigated the effects of housing systems for 1106 pigs that were weaned from: (1) conventional farrowing crates (FC), (2) free-farrowing pens (FF), or (3) group housing of lactating sows (GH) into (1) conventional rearing pens (Conv) or (2) piglets remained in their farrowing pens for rearing (Reaf). Tails were docked or left undocked batchwise. All pigs were regrouped for the fattening period. Pigs were scored for skin lesions, tail lesions and losses. After weaning, Conv-GH pigs had significantly less skin lesions than Conv-FC and Conv-FF pigs. After regrouping for fattening, Reaf-GH pigs had significantly less skin lesions than Conv pigs, Reaf-FC and Reaf-FF. The frequency of tail lesions of undocked Conv pigs peaked in week 4 (66.8%). Two weeks later, Reaf undocked pigs reached their maximum (36.2%). At the end of fattening, 99.3% of undocked Conv pigs and 43.1% of undocked Reaf pigs lost parts of their tail. In conclusion, the co-mingling of piglets during suckling reduced the incidence of skin lesions. Rearing in the farrowing pen significantly reduced the incidence of tail lesions and losses for undocked pigs. No housing system negatively affected the performance.

Published
2021
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41. Body size in relation to cubicle dimensions affects lying behavior and joint lesions in dairy cows.

Author

Dirksen N, Gygax L, Traulsen I, Wechsler B, and Burla JB

Subjects
Animals, Behavior, Animal, Body Size, Cattle, Female, Joint Diseases, Cattle Diseases etiology, Dairying methods, Housing, Animal
Abstract

Adequate cubicle dimensions are important for dairy cows to allow for species-appropriate lying behavior. Even though cow body size has increased in the last 2 decades, the cubicle dimensions of housing systems built many years ago have not been adjusted on most farms. Therefore, cows may be impaired in their lying behaviors, and thus the present study aimed to determine the influence of the ratio of body size to cubicle dimension on lying behavior and joint lesions. We investigated the lying behavior of 144 cows with withers heights of 140 to 163 cm on 8 Swiss dairy farms. Among the farms, the cubicle bed length varied from 187 to 200 cm and lunge space length varied from 47 to 202 cm. Specific behaviors of lying down and standing up movements, as well as lying positions, were observed on 3 d per farm. As outcome variables, the occurrences of these behaviors were calculated as proportions in relation to the respective total number of observations per cow. In addition, the presence of joint lesions was scored once. Data of the individual cows were analyzed in relation to the given cubicle dimensions on the farms by mixed-effects models. The bed length ratio [bed length (cm) on the farm/withers height (cm) of the observed cow] and the lunge space ratio [lunge space length (cm) on the farm/withers height (cm) of the observed cow] were used as explanatory variables. An increase in the bed length ratio was associated with decreased proportions of lying down movements with (1) repeated head pendulum movements, (2) repeated stepping with front legs, and (3) hitting against cubicle elements; decreased proportions of standing up movements with (1) shifting backward, (2) hesitant head lunge movements, and (3) hitting against cubicle elements; and an increased proportion of lying positions without physical contact with cubicle elements. An increase in the lunge space ratio was associated with a decreased proportion of standing up movements with sideways directed head lunge movements. Furthermore, an increase in the bed length ratio decreased the proportion of cows with tarsal joint lesions. To summarize, the lying behavior of large-framed cows was clearly modified given the cubicle dimensions in use on the study farms. In view of the consistency of the obtained results, we recommend adjusting the dimensions of cubicles so that they are suitable for cows whose body size meets the breeding goals of the farm., (The Authors. Published by Elsevier Inc. and Fass Inc. on behalf of the American Dairy Science Association®. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licenses/by-nc-nd/4.0/).)

Published
2020
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42. Panoptic Segmentation of Individual Pigs for Posture Recognition.

Author

Brünger J, Gentz M, Traulsen I, and Koch R

Subjects
Animals, Image Processing, Computer-Assisted, Neural Networks, Computer, Posture, Swine
Abstract

Behavioural research of pigs can be greatly simplified if automatic recognition systems are used. Systems based on computer vision in particular have the advantage that they allow an evaluation without affecting the normal behaviour of the animals. In recent years, methods based on deep learning have been introduced and have shown excellent results. Object and keypoint detector have frequently been used to detect individual animals. Despite promising results, bounding boxes and sparse keypoints do not trace the contours of the animals, resulting in a lot of information being lost. Therefore, this paper follows the relatively new approach of panoptic segmentation and aims at the pixel accurate segmentation of individual pigs. A framework consisting of a neural network for semantic segmentation as well as different network heads and postprocessing methods will be discussed. The method was tested on a data set of 1000 hand-labeled images created specifically for this experiment and achieves detection rates of around 95% (F1 score) despite disturbances such as occlusions and dirty lenses.

Published
2020
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43. Classification of Pigs with Tail Lesions from Different Farrowing and Rearing Systems during Rearing and Fattening Period.

Author

Gentz M, Lange A, Zeidler S, and Traulsen I

Abstract

The aim of the present study was to classify and characterise pigs with tail lesions using a combined parameter based on the frequency and duration of tail lesions and to find out whether biologically relevant groups could be separated by cluster analysis. Pigs (n = 677, 50% docked, 50% undocked) from three farrowing systems, as follows: (1) Conventional farrowing crate (FC), (2) free farrowing (FF), and (3) a group housing lactating sows (GH), were divided into two rearing systems as follows: (1) A conventional system (CONV) and (2) a wean-to-finish (W-F) system. Within 18 assessment weeks, starting after weaning, animal tail lesions were recorded individually. The animals were characterised into five lesion groups, as follows: (I) No lesions to (V) many long lasting lesions. The separability of the predefined lesion groups was checked by an animal individual lesion parameter. By using a k-means cluster analysis, it was shown that the docking status was the mainly affected parameter on the tail lesions. The separation of the groups only succeeded for the most distinct groups, I and V. The high impact of the docking status and the reduction of tail lesions by more space allowance was shown. More characterising information for the individual pigs would improve the separability of the lesion groups.

Published
2019
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44. Using Acceleration Data to Automatically Detect the Onset of Farrowing in Sows.

Author

Traulsen I, Scheel C, Auer W, Burfeind O, and Krieter J

Subjects
Animals, Behavior, Animal, Female, Swine, Acceleration
Abstract

The aim of the present study was to automatically predict the onset of farrowing in crate-confined sows. (1) Background: Automatic tools are appropriate to support animal surveillance under practical farming conditions. (2) Methods: In three batches, sows in one farrowing compartment of the Futterkamp research farm were equipped with an ear sensor to sample acceleration. As a reference video, recordings of the sows were used. A classical CUSUM chart using different acceleration indices of various distribution characteristics with several scenarios were compared. (3) Results: The increase of activity mainly due to nest building behavior before the onset of farrowing could be detected with the sow individual CUSUM chart. The best performance required a statistical distribution characteristic that represented fluctuations in the signal (for example, 1st variation) combined with a transformation of this parameter by cumulating differences in the signal within certain time periods from one day to another. With this transformed signal, farrowing sows could reliably be detected. For 100% or 85% of the sows, an alarm was given within 48 or 12 h before the onset of farrowing. (4) Conclusions: Acceleration measurements in the ear of a sow are suitable for detecting the onset of farrowing in individually housed sows in commercial farrowing crates., Competing Interests: The authors declare no conflict of interest.

Published
2018
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45. Providing supplementary, artificial milk for large litters during lactation: effects on performance and health of sows and piglets: a case study.

Author

Pustal J, Traulsen I, Preißler R, Müller K, Beilage TG, Börries U, and Kemper N

Abstract

Background: One possible way to support raising large litter sizes in pigs is to offer supplementary, artificial milk ad libitum in the farrowing pen in addition to the sow's milk. In order to evaluate the potential use of this method and its effects on performance and health, supplemented ( n  = 60) and control sows ( n  = 60) with their litters were tested over 15 batches in one herd during one year. In the supplemented group (SG), piglets had access to supplementary milk in addition to sow's milk from their 2 nd day of life until weaning (day 27). The litters of SG sows were adjusted to contain as many piglets as the sow had functional teats, whereas in the control group (CG), piglets were set to the number of functional teats minus one, due to animal welfare reasons., Case Presentation: With supplementary milk provision, the weaning of large litters was achieved without any negative impacts on performance and health. On average, 13.5 and 12.4 piglets were weaned in SG and CG, respectively ( P  < 0.05). While average weaning weights (SG: 7.8 kg v . CG: 7.8 kg; P  > 0.05) and average daily weight gain of the piglets (SG: 0.25 kg v . CG: 0.25 kg; P  > 0.05) did not differ, total litter weight was consequently higher in SG than in CG (104.9 kg v . 96.7 kg; P  < 0.001). The average milk replacer intakes were 1.1 kg milk powder per day and batch, and varied significantly between the "warm" and "cold" seasons (1.5 v . 0.9 kg milk powder per batch and day; P  < 0.001). No significant differences in the mortality rate or the occurrence of diarrhoea were detected in the piglets of both SG and CG ( P  > 0.05). With regard to documented medical treatments, facial lesions were treated less frequently in piglets of SG (46 v . 32 treatments; P  < 0.05). There was no effect of supplementary milk on the loss of body weight, backfat thickness and body condition score of the sows ( P  > 0.05)., Conclusions: To summarise, in the presented case offering ad libitum supplementary, artificial milk supported the sow in raising large litters by compensating possible negative impacts of high piglet numbers on the weight gain of piglets and the body condition of the sows.

Published
2015
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46. Efficient interruption of infection chains by targeted removal of central holdings in an animal trade network.

Author

Büttner K, Krieter J, Traulsen A, and Traulsen I

Subjects
Animals, Humans, Time Factors, Communicable Diseases transmission, Models, Theoretical, Transportation
Abstract

Centrality parameters in animal trade networks typically have right-skewed distributions, implying that these networks are highly resistant against the random removal of holdings, but vulnerable to the targeted removal of the most central holdings. In the present study, we analysed the structural changes of an animal trade network topology based on the targeted removal of holdings using specific centrality parameters in comparison to the random removal of holdings. Three different time periods were analysed: the three-year network, the yearly and the monthly networks. The aim of this study was to identify appropriate measures for the targeted removal, which lead to a rapid fragmentation of the network. Furthermore, the optimal combination of the removal of three holdings regardless of their centrality was identified. The results showed that centrality parameters based on ingoing trade contacts, e.g. in-degree, ingoing infection chain and ingoing closeness, were not suitable for a rapid fragmentation in all three time periods. More efficient was the removal based on parameters considering the outgoing trade contacts. In all networks, a maximum percentage of 7.0% (on average 5.2%) of the holdings had to be removed to reduce the size of the largest component by more than 75%. The smallest difference from the optimal combination for all three time periods was obtained by the removal based on out-degree with on average 1.4% removed holdings, followed by outgoing infection chain and outgoing closeness. The targeted removal using the betweenness centrality differed the most from the optimal combination in comparison to the other parameters which consider the outgoing trade contacts. Due to the pyramidal structure and the directed nature of the pork supply chain the most efficient interruption of the infection chain for all three time periods was obtained by using the targeted removal based on out-degree.

Published
2013
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47. Implementation of multivariate cumulative sum control charts in mastitis and lameness monitoring.

Author

Miekley B, Stamer E, Traulsen I, and Krieter J

Subjects
Animals, Cattle, Cattle Diseases epidemiology, Dairying methods, Female, Lameness, Animal epidemiology, Mastitis, Bovine epidemiology, Multivariate Analysis, Cattle Diseases diagnosis, Lameness, Animal diagnosis, Mastitis, Bovine diagnosis, Records veterinary
Abstract

This study analyzed the methodology and applicability of multivariate cumulative sum (MCUSUM) charts for early mastitis and lameness detection. Data used were recorded on the Karkendamm dairy research farm, Germany, between August 2008 and December 2010. Data of 328 and 315 cows in their first 200 d in milk were analyzed for mastitis and lameness detection, respectively. Mastitis as well as lameness was specified according to veterinary treatments. Both diseases were defined as disease blocks. Different disease definitions for mastitis and lameness (2 for mastitis and 3 for lameness) varied solely in the sequence length of the blocks. Only the days before the treatment were included in the disease blocks. Milk electrical conductivity, milk yield, and feeding patterns (feed intake, number of trough visits, and feeding time) were used for the recognition of mastitis. Pedometer activity and feeding patterns were used for lameness detection. To exclude biological trends and obtain independent observations, the values of each input variable were either preprocessed by wavelet filters or a multivariate vector autoregressive model. The residuals generated between the observed and filtered or observed and forecast values, respectively, were then transferred to a classic or self-starting MCUSUM chart. The combination of the 2 preprocessing methods with each of the 2 MCUSUM sum charts resulted in 4 combined monitoring systems. For mastitis as well as lameness detection requiring a block sensitivity of at least 70%, all 4 of the combined monitoring systems used revealed similar results within each of the disease definitions. Specificities of 73 to 80% and error rates of 99.6% were achieved for mastitis. The results for lameness showed that the definitions used obtained specificities of up to 81% and error rates of 99.1%. The results indicate that the monitoring systems with these study characteristics have appealing features for mastitis and lameness detection. However, they are not yet directly applicable for practical implementations., (Copyright © 2013 American Dairy Science Association. Published by Elsevier Inc. All rights reserved.)

Published
2013
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48. Environmental Impact Assessment--methodology with special emphasis on European pork production.

Author

Reckmann K, Traulsen I, and Krieter J

Subjects
Animals, Swine, Environment, Meat
Abstract

One of the most discussed topics worldwide is climate change, upon which livestock production is known to have a great environmental impact. There are different methods to measure these environmental impacts, some of which are mentioned in this review. It especially focuses on the method of Life Cycle Assessment (LCA), because it is widely used, of high relevance and good quality. This review highlights a sample of the few published European LCA studies on pork production. These assessments result in an average global warming potential of 3.6 kg CO(2)- eq per kg pork, ranging from 2.6 to 6.3 kg CO(2)- eq per kg pork. Additionally, it illustrates the main limitations of the methodology itself (e.g. data intensiveness, different allocation techniques) and its application in pork production (e.g. limited data availability, use of multiple functional units, varying system boundaries). The missing comparability of various studies arising from a vague standard still represents the main problem in LCA. Therefore, a new standardisation and the development of a more exhaustive database would generate a future trend., (Copyright © 2012 Elsevier Ltd. All rights reserved.)

Published
2012
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