dataesr/scientific-paragraphs-categorization huggingface dataset:
Conclusion The calculation chain presented in this work is designed to simulate early DNA damage and is the first simulation tool based on Geant4-DNA that is able to fully simulate the physical, physicochemical and chemical stages of irradiation damage at the scale of a human cell nucleus. Extensions of the DNA models included in DnaFabric software were presented and used to create a fibroblast cell nucleus model filled with the content of the human male genome (diploid cell, ∼. ⋅ 6 4 10 9 pairs of nucleotides). The model was then exported to a file for use in Geant4-DNA simulations. A set of those simulations was created and integrated in the calculation chain, making it possible to simulate the physical, physicochemical and chemical stages that follow the irradiation of a cell nucleus. The simulation of these three stages thus took fully into account the fibroblast cell nucleus model previously generated with its ∼.
A. 5G System, Functional, Logical and Physical Architectures CHARISMA project  [10]  takes into account the fact that at the architectural level, achieving low latency (service level) requires data to be handled (i. e. routed or processed) as close to where it is required (i. e. either at the receiving end or at the source end). Indeed, this implies that a low-latency architecture requires network intelligence to be located as near to the edge as possible, such that traffic which is expected to remain local never needs to travel towards the core of the network; and in this way minimizes transmission latency. Thus CHARISMA's distribution of intelligence closer to the edge provides physical, logical and functional advantages as compared to the more conventional centralised architectural approach.
Intrinsic to such ITS infrastructure is lowlatency as well as application initialization times. At the physical (PHY) layer, a round-trip end-to-end (E2E) latency between user equipment (UE) and central office (CO) of 6. 69 ms has recently been achieved, using ultra-high speed routing at the TrustNode router. Also, the 5G-NORMA project  [12]  instantiates different slices such that each slice may be potentially orchestrated in a different way, and thus be tailored to the requirements of a specific service. This requires the coordination of resources between different slices, which leads to the introduction of a new compound Software-Defined Mobile Network Control (SDMC) architecture. Furthermore, the mm-wave RAN integration for access is the focus of mmMAGIC project, proposing solutions like: tight interworking, multi-connectivity choices and low-band integration  [20].
D. 5G Performance Evaluation Framework The mmMAGIC project has developed a visualization tool to illustrate the potential benefits that mm-wave cell deployment can offer  [19]. The tool is developed on blender which is an open source software. METIS-II developed a holistic 5G RAN performance evaluation framework, which can be used for a fair numerical assessment of 5G KPIs (e. g. user data rates, reliability, control and user plane latencies, mMTC density or energy efficiency) as well as for comparison of technical solutions proposed for 5G. Instructions and corresponding evaluations are provided for each KPI  [35] -  [37].
E. 5G Integrated Transport Networks (FH/BH) The 5G-XHAUL project  [2]  investigates active and passive optical technologies for converged fronthaul/backhaul (FH/BH) services. Specifically, passive WDM-PON technology targets 25 Gbps/wavelength, colorless optical network unit (ONU) deployments and dynamic ONU switch-off for energy saving. Active optical technology is based on Time Shared Optical Networks (TSON)  [29]. Moreover, the goal of the 5G-Crosshaul project  [5]  is to build an adaptive, flexible and software-defined architecture for future 5G transport networks integrating multitechnology fronthaul and backhaul segments. The 5G-Crosshaul architecture thus aims to enable a flexible and software-defined reconfiguration of all networking elements through a unified data plane and control plane interconnecting distributed 5G radio access and core network functions, hosted on in-network cloud infrastructure.
These innovative, customisable and extensible HoN metrics greatly facilitate speedy and more precise identification of common network problems. The COHERENT project aims to develop a unified control and coordination framework for 5G heterogeneous RANs, with the emphasis on SDN for RAN programmability, in particular efficient radio resource modelling and management, and flexible spectrum management. In the first year of the project, COHERENT has made a concrete progress on flexible RAN architecture design, radio resource abstraction, RAN data models and application program interfaces (APIs), virtualization and coordination framework, and flexible spectrum management. The Golden Nugget of the COHERENT project in the first project year is a novel control and coordination architecture, which is presented in  [25].
While the ETSI NFV framework architecture has assumed so far that the NSO and RO functions are played by a single entity (the NFVO), the ETSI NFV has recently approached a similar NSO-RO functional split for single administration. Furthermore, initial design and deployment of a large scale test-bed (the 5GEx sandbox) connecting 13 sites, including 4 operators providing the connectivity backbone, and emulating realistic Internet topologies today. Additionally, SONATA has developed a flexible NFV MANO Service Platform for NFV that is built on a micro-service architecture and released as open-source software under the Apache 2. 0 license. The Service Platform operates and manage the lifecycle of network service on top of a virtual infrastructure manager, like OpenStack. To this end, it deploys the virtual network functions as virtual machines and steers the traffic by implementing service function chains.
This is achieved with the help of an Open Access Manager (OAM) module which is responsible for the lifecycle management of network slices including communications with network, cloud, or device controllers for creation and operation of a slice and exposing it to upper layers for dynamic service provisioning. Also, 5G-NORMA service and domain aware orchestration is responsible, among other functions, for placing virtualized functions in the most appropriate location. Herein, it takes into account the requirements of the corresponding service that needs to be satisfied, the constraints on the placement of functions that interact with each other and the features of the underlying infrastructure. Orchestration takes place end-to-end, spanning the whole mobile network from the user to the packet data network respectively to the service provided for the user.
Finally, the SDK interconnects tightly with the Service Platform and allows monitoring running services in real time. To this end, it enables the developer to collect important data and offers tool to analyze the data in order to debug or improve the service, for example in terms of performance. Moreover, Superfluidity  [14]  develops a framework to automatically map service level Key Performance Indicators (KPIs) to the platform level parameters in the host compute environment. The framework enables the identification of platform features, which most significantly influence the KPIs for a given workload under test. Full stack monitoring is used to capture a telemetry data ranging from low-level hardware metrics to higher-level applications metrics. The data is analysed using an analytics pipeline which identifies the most significantly correlating platforms metrics with service KPI's, based on the use of eight ranking algorithms with a reliability scoring mechanism.
The eight algorithms implemented to date are a mixture of clustering and machine learning classification approaches. In addition, To enforce security in 5G networks Superfluidity takes the following directions; 1) Describe operator policies in a high-level specification language; 2) Describe Reusable Functional Block (RFBs) in a way that is amenable to static analysis through the use of Symbolic Execution Function Language; 3) Perform static analysis of RFB configurations to ensure policy is obbeyed before deployment using SymNet tool (SymNet can run reachability checks over network models by injecting symbolic packets and tracking their path through the network); 4) Ensure that the implementation conforms to the specification at deployment time.
We present VIRAC version 1, a near-infrared proper motion and parallax catalogue of the VISTA VVV survey for 312,587,642 unique sources averaged across all overlapping pawprint and tile images covering 560 deg 2 of the bulge of the Milky Way and southern disk. The catalogue includes 119 million high quality proper motion measurements, of which 47 million have statistical uncertainties below 1 mas yr -1. In the 11 < K s < 14 magnitude range the high quality motions have a median uncertainty of 0. 67 mas yr -1. The catalogue also includes 6,935 sources with quality-controlled 5 σ parallaxes with a median uncertainty of 1. 1 mas. The parallaxes show reasonable agreement with the TYCHO-Gaia Astrometric Solution (TGAS), though caution is advised for data with modest significance. The SQL database housing the data is made available via the web.
2015; Cioni et al. 2016) , or in combination with other datasets  (Cioni et al. 2014 ) such as the Two Micron All Sky Survey (2MASS,  Skrutskie et al. 2006). VVV data comprise typically between 50 and 80 epochs of Ks photometry over five years  (2010 to 2015). In addition, VVV includes two epochs of Z, Y, J and H photometry taken at the beginning and end of the survey. Each epoch is subdivided into independent images that are treated separately in our astrometry. In this paper we present version 1 (V1) of the VVV Infrared Astrometric Catalogue (VIRAC), based on the standard products provided by the v1. 3 pipeline of the Cambridge Astronomical Survey Unit (CASU). This VIRAC V1 catalogue provides relative proper motions and parallaxes for all stars for which they could be measured in the individual pointings (pawprints) of VVV.
The catalogue is available at vvv. herts. ac. uk and it will be made available in the VISTA Science Archive  (VSA, Cross et al. 2012 , see horus. roe. ac. uk/vsa) and the ESO Archive. Following the release of the Gaia 2nd Data Release, the VVV team also plans to provide VIRAC V2, a deeper catalogue based on profile fitting photometry of the VVV dataset that will provide astrometry on the Gaia absolute reference frame. The work of Contreras  Ramos et al. (2017)  is an excellent example of the power of profile fitting for NGC 6544. We will also explore the possibility of further increasing the depth of VIRAC using a shift-and-stack algorithm, as has been done by the ALLWISE project  (Kirkpatrick et al. 2014 ). The VVV project has been extended by a new survey, VVVX, that continues to survey the original VVV area approximately 9 times up to 2020, while extending the area to cover an additional 1100 deg 2 of the Galactic disc and bulge at 25-40 epochs.
We plan to incorporate VVVX data into future astrometric products. Here we describe our proper motion and parallax methodology and present initial results. These include nearby high proper motion stars and brown dwarfs and an illustration of how VIRAC can be used at large distances across the Milky Way. Our results include a complete catalogue of visually confirmed sources with proper motion, µ > 200 mas/yr, complementing the VVV high proper motion catalogue recently published by  Kurtev et al. (2017)  for relatively bright stars with magnitudes Ks < 13. 5. In section 2 we describe the dataset and data selection. Section 3 details the source matching and the proper motion and parallax calculations. In Section 4 we describe our quality checks and quality flags for the proper motion catalogue, using internal self-consistency, visual inspection and comparison to both Tycho-Gaia Astrometric Solution (TGAS,  Michalik, Lindegren & Hobbs 2015)  and the results of  Kurtev et al.
(2017). This section also describes our table of visually confirmed high proper motion stars (the table itself can be found in the appendices) and new proper motion companions to TGAS stars. In Section 5 we describe the parallax catalogue and parallax quality checks using TGAS. In section 6 we describe discoveries of note from the parallax dataset and high proper motion sources. In Section 7 we demonstrate applications at large Galactic distances, in-cluding measurement of the Galactic rotation curve and the motion of the Sagaittarius dwarf galaxy.
(2015). Pipeline data reduction, catalogue generation and calibration of the photometry and astrometry are provided by the Cambridge Astronomical Survey Unit (CASU), see  Lewis, Irwin & Bunclark (2010)  and casu. ast. cam. ac. uk/surveys-projects/vista/technical. The VSA provides further processing (band-merging, production of light curves etc. ) and curation of VVV data and makes it available to the community as an SQL database, providing an alternative to the ESO Archive. The raw VVV FITS file catalogues were processed by a modified version of a fortran routine fitsio cat list (originally provided by CASU) ported to python. This modified version unpacks the binary tables for each extension in the FITS file and calculates calibrated magnitudes from the fluxes. It also flags and computes approximate magnitudes for saturated sources using a ring-shaped aperture, removes columns which are surplus to our requirements and outputs the resultant tables as a single extension FITS file.
This yielded 2100 pawprint sets which corresponds to 6 pawprint sets for each of 346 VVV tiles and 12 pawprint sets for each of 2 VVV tiles (d015 and b390) for which the telescope pointing positions were > 1' from their usual positions at a number of epochs. These two tiles were subject to a change in pointing coordinates due to guiding problems caused by non-stellar profiles of guide stars used by the telescope guiding system. Because of this, observations before and after the change in pointing coordinates are treated separately by our astrometric pipeline, until the final stage of averaging over the independent astrometric solutions. We rejected pawprints based on the following criteria: • Deprecated (i. e. flagged as poor quality) by the quality control procedures used in the public data releases available at the VSA.
1 that the difference in average motion of partially overlapping reference frames is essentially indistinguishable. Care must be taken however, if one wishes to use these data to e. g. investigate Galactic motion across larger scales (see Section 7. 1). For practical purposes, the changes in the astrometric reference frame can typically be neglected on scales of approximately a VVV tile, though there may well be exceptions to this in mid-plane fields with highly structured extinction (which affects the distance and motions of the reference stars).
Self-Consistency The VVV observation method enables a check for selfconsistency between overlapping pawprint sets. Overlaps on the sky between pawprint sets are either between different arrays or different sections of the same array, in different parts of the focal plane. Since the volume of data is so great we select a sample of sources from tiles b216 (outer bulge), b332 (inner bulge, very high source density), d069 (inner disk, containing the Westerlund 1 compact young cluster) and d079 (outer disk) to test self-consistency. On these tiles we perform a 1 ′′ internal match on their 2012. 0 positions to identify coincident detections of sources between multiple pawprint sets. We compare proper motions for sources with solutions in two pawprint sets and no proper motion error flags (see Section 4.
• Parallax measurements from a minimum of two pawprint sets. • The two highest weighted measurements agree within 2σ and 10 mas, are positive, and each measured with at least 2σ significance. • Mean ellipticity (across all epochs) is less than 0. 2. To this selection we apply a similar set of cuts to the epm flag = 0 selection above (see Section 4. 2), albeit applied after the averaging of measurements from separate pawprints (including pawprints in adjacent tiles) and across the entire survey at once. Since the parallax dataset is smaller we reduce the width of the magnitude bins to 50 sources. Sources in a magnitude range where the median parallax uncertainty is greater than 5 mas, and those with parallax uncertainty greater than the median for their magnitude plus three times the spread (defined as the larger of either 0.
Note that we did not attempt a parallax measurement for any source with µ < 20 mas yr -1 , so very distant stars should be removed. Due to the influence of these biases VIRAC parallaxes should be used with caution: their use in combination with colour data is demonstrated below. The most likely distance is often not simply π -1. Bailer-Jones (2015) discuss in detail the problems involved in estimating distances using parallax measurements. The VVVX extension to tfhe VVV survey should allow us to improve the reliability of VIRAC parallaxes over the next few years, even though the formal precision will improve only slightly. Details of 53 pairs of sources from Figure  13  where the VIRAC component is in the 11 < Ks < 14 range and excluding the outlier are given in Table  D2.
7 ′′ due north of the primary. At the TGAS distance of 37. 6 pc, this separation corresponds to 553 au. LTT 7251 B was observed on August 20th, 2016 with the Astronomy Research using the Cornell Infra Red Imaging Spectrograph (ARCoIRIS), a cross-dispersed, single-object, longslit, infrared imaging spectrograph, mounted on Blanco 4 m Telescope, CTIO. The spectra cover a simultaneous wavelength range of 0. 80 to 2. 47 µm, at a spectral resolution of about 3500 λ/∆λ, encompassing the entire zYJHK photometric range. The spectrum was taken with 16 exposures, each 180 sec in ABBA dithering pattern for sky background subtraction. The average airmass was 1. 4 and seeing 1. 2 ′′. We observed the telluric A0 V standard HD163336 immediately after the target. The data were reduced using the Spextool IDL package (version 4.
1,  Cushing, Vacca & Rayner 2004) , a new suite of data reduction algorithms specifically designed for the data format and characteristics of ARCoIRIS by Dr. Katelyn Allers 4. Telluric correction and flux calibration of the post-extraction spectra are achieved through the xtellcorr IDL package  (Vacca, Cushing & Rayner 2003). The reduced spectrum is shown in Figure  16. This source did not fulfil the L dwarf selection criteria described in the previous section because it lacks Z and Y photometry in the standard VVV catalogue products of the CASU pipeline, owing to proximity to a diffraction spike associated with the much brighter primary and the slightly poorer spatial resolution of VISTA in the Z and Y passbands. The colour J -H = 0. 57 also failed our selection criterion, though this may simply be because of the significant uncertainty (0.
VVV J12564163-6202039 VVV J12564163-6202039 (VVV 1256-6202 hereafter) is the only genuine source we identified through visual inspection of sources with µ > 1 ′′ yr -1 , and 10 < σµ (mas yr -1 ) < 30, see section 4. 5. 2. It is listed in the 2MASS Point Source cat-   Cruz et al. (2004). lower : Data in the J, H, and K bands compared with the L5 standard SDSS J083506. 16+195304. 4  (Chiu et al. 2006) , the L9 standard DENIS-P J0255-4700  (Burgasser et al. 2006) , and the L6 standard 2MASSI J1010148-040649  (Reid et al. 2006 ) respectively. All standard spectra were obtained from the SpeX prism library  (Burgasser 2014). alogue as 2MASS J12564352-6202041, detected in J only. VVV 1256-6202 is severely blended with a background source in the 2010 epochs; this is likely the cause of the relatively high uncertainty on the proper motion (hence epm flag=2 for both measurements).
The pipeline proper motions for the source are -1112±12 and -13±16 mas yr -1 in α cos δ and δ respectively. The pipeline median Ks magnitude is 15. 77 ± 0. 04. Note that while we use robust methods where possible, pipeline outputs for this source are swayed to some extent by the blended early epochs. This source does not have a parallax in VIRAC; measurements were attempted in the two overlapping pawprint sets separately but they did not agree. To try to improve on the pipeline values with a more bespoke solution, we use VVV Ks band observations of the source from all pawprint sets for a single fit, omitting data from the 2010 observing season. The median Ks band magnitude for these 82 epochs is 15. 737 ± 0. 056. Using astrometric reference sources this time drawn from within 1 ′ radially about the target but an otherwise similar fitting procedure we measure proper motions of -1116.
3 ± 4. 1 and 3. 9±4. 0 mas yr -1 in α cos δ and δ respectively and a parallax of 5. 3 ± 7. 1 mas. The ZY JH photometry that we have included in VIRAC taken from VVV DR4 at the VSA, mostly corresponding to the first set of multi-filter data taken at the beginning of the survey. This source is blended with the background source in the early observations and hence shows null (99. 999) ZY JH detections in VIRAC. We therefore obtained the ZY JHKs tile catalogue photometry produced from the second set of multi-filter observations made at the end of the survey. These magnitudes are given in Table  3. This field was also observed as part of the VPHAS+ survey  (Drew et al. 2014) , giving us a i bandpass psf fit magnitude from DR2 5 (also given in Table  3 ,  Drew et al. 2016 ) but non-detections in the r and Hα observations.
8-2. 5 µm spectrum (see Figure  17 ) with the Folded-port InfraRed Echellette (FIRE) spectrograph  (Simcoe et al. 2008 ) mounted on the Magellan Baade Telescope at Las Campanas Observatory, Chile. The spectrum was taken in the low resolution prism mode with a 1 ′′ slit width, yielding spectral resolution R≈250, in conditions of mediocre seeing (1. 2 to 1. 5 ′′ at full-width-halfmaximum) so the data are not of the best quality. The total exposure time was 20 min, nodding along the slit with individual exposures of 60 s duration. The star HIP 58411 was used for telluric correction and the data were reduced with the FIREHOSE software package using standard methods. Wavelength calibration was done with a NeAr lamp shining 5 cdsarc. u-strasbg. fr/viz-bin/Cat?II/341  on a screen in the telescope dome, external to the instrument.
The parallax catalogue includes ten sources with d < 25 pc, nine of which are new discoveries. We have demonstrated that VIRAC astrometry is useful for objects at a large Galactic distance through: a measurement of the Galactic rotation curve at l = 300 • out to d ≈ 12 kpc; a measurement of the absolute proper motion of the Sagittarius dwarf spheroidal galaxy in VVV tile b211; a measurement of the absolute proper motion of the Galactic bulge in VVV tile b201; and kinematic distance measurements of two young stellar objects. Due to some doubt over the accuracy of the relative to absolute proper motion correction in these fields these results at large Galactic distances are very much preliminary. A precise relative to absolute correction based on the forthcoming Gaia 2nd data release and VIRAC V2 will enable more serious work on these topics.
ACKNOWLEDGMENTS We are grateful to  Dr Floor van Leeuwen  for a very helpful referee report, and to  Dr Katelyn Allers  and  Sean Points  ( ARCoIRIS instrument scientist ) for assistance during spectroscopic observation of LTT 7251 B. LCS acknowledges a studentship funded by the  Science & Technology Facilities Research Council (STFC)  of the UK; LCS, PWL, HRAJ, FM, JED and DJP acknowledge the support of a consolidated grant ( ST/J001333/1  and  ST/M001008/1 ) also funded by  STFC. We acknowledge use of data from the  ESO Public Survey programme ID 179. B-2002 taken with the VISTA telescope, data products from CASU, and funding from the  FONDAP Center for Astrophysics 15010003 , the  BASAL CATA Center for Astrophysics and Associated Technologies   PFB-06 , the  FONDECYT  from  CONICYT.