dataesr/scientific-paragraphs-categorization huggingface dataset:
These techniques can also be applied to biological materials such as tooth enamel, finger nails and hairs, preferably by mobile systems for application in the field, which need to be developed. Other objects that were exposed at a certain place could also be used. For the computational techniques applied, automatic direct input of dose rate measurement data into databases, interpolation and extrapolation algorithms and tools for prediction of doses are the main routes of further development of efficient techniques. In order to handle a large number of dosimetric samples, strategies and methods to increase measurement capacity must be developed. One solution is automation of sample preparation and measurement, in particular for analysis of dicentric chromosomes and micronuclei where the evaluation of metaphases should be fully automated  (52).
In this context, the availability of databases including autopsy cases should be used to validate any new biokinetic model. The results of these developments should be transferred to operational radiation protection, including guidelines and technical recommendations. In vivo measurements using partial body counters represent a valuable method in internal dosimetry, providing actual information on radionuclide activity within the body of an individual. However, there is no standard calibration procedure, and suitable anthropomorphic phantoms to assess, for example, the skeletal activity of bone-seeking radionuclides are scarce. To reduce the uncertainties in in vivo measurements, the influence of individual body parameters and phantom characteristics on the detection efficiency must be investigated.
Validation of procedures and the traceable calibration of any detector systems used to supply data to monitoring networks will be required, e. g. European Radiological Data Exchange Platform (EURDEP), European Study of Occupational Radiation Exposure (ESOREX), Radioactivity Environmental Monitoring (REM) database. EURADOS intends to support operators of national early warning dosimetry networks and to consult regulatory bodies and the Joint Research Centre (JRC) Ispra concerning legal aspects of environmental radiation monitoring, especially those related to Articles 35 and 36 of the Euratom Treaty. Cooperation between the Institute for Environment and Sustainability (IES) with regard to EURDEP and EURADOS is considered to be a key element in developing further the idea of harmonisation in environmental monitoring.
Any actions required in this context must take into account the stateof-the-art tools currently available and forthcoming publications such as ICRP/OIR Reports  (90)  , revised IDEAS Guidelines for the Estimation of Committed Doses from Incorporation Monitoring Data  (59)  , ISO Standards in internal dosimetry  (91)  and the output of the TechRec project Technical Recommendations for Monitoring Individuals Occupationally Exposed to Internal Radiation currently being prepared for the EC by a consortium of EURADOS voting member institutions. Computational methods form a part of the work programme of all EURADOS WGs. These methods have moved from the domain of experts to become routine tools. Questionnaires performed by EURADOS in the past showed the poor level of QA performed by those using these methods.
In a DSC analysis a temperature gradient is applied to the sample and heat changes due to unfolding events are recorded. The analysis of such data provides a number of parameters of which the most relevant are the Tm value (in cases where unfolding occurs in a two-state process, Tm is the temperature at which half the protein is present in the native state and the half in the unfolded state) and the ΔH value representing the enthalpy change upon unfolding  [8]. Since the Tm value can be determined with high precision, this parameter is thus a very useful marker of protein conformation. Although DSC has been used for many decades in life science, Contents lists available at ScienceDirect journal homepage: www. elsevier. com/locate/bbrep over the last decades it has become increasingly popular in both basic and applied science.
The protein concentration was determined by the Bradford assay. For analysis with DTT, this one was added in the microplate (both in reference cell and sample cell) just before analysis in the calorimeter. There was no alkylation prior to analysis. Due to the irreversibility of the unfolding processes, calorimetric enthalpy values were determined by peak integration using the MicroCal VP capillary automated analysis 2. 0 program. Data were normalized using the concentration of the G-protein that accounts to approximately 25% of the total viral protein. G-protein concentration was thus derived by dividing the total protein concentration by four. We are aware that values reported are therefore approximate, but a similar approach, applied to the haemagglutinin protein based normalization of influenza virus data,  [10, 20]  has permitted to compare experiments from different laboratories.
SDS-PAGE Analyses were carried out on a 4-12% (w/v) SDS gradient PAGE gels (XT Criterion gels from Bio-Rad) using MOPS (Bio-Rad) as running buffer. Prior to analysis, samples were denatured by the addition of 9 ml XT Sample Buffer 4 Â (Bio-Rad) to 25 ml of viral sample. 1. 8 ml of XT 20 Â reducing agent (Bio-Rad) was added prior to an exposure to 100 °C for 5 min. Samples containing 5 mg of viral protein were loaded onto each well. Gels were stained using G250 Coomassie Blue. Densitometry analysis of SDS-PAGE was performed using GS800 densitometer (BioRad). Molecular weight of the major bands and the relative percentage of each band were determined using QuantityOne s software after substraction of the background lane.
Bromelain cleavage of G-protein suppresses first unfolding event To verify this hypothesis we have prepared samples in which the virus was treated with the protease bromelain. It has been reported that such treatment removed the G-protein ectodomain from the viral surface  [28]. To verify the efficiency of this treatment samples were analyzed by SDS-PAGE. Fig. 1B  shows that bromelain treatment quantitatively removes both G protein bands. The unfolding thermogram of bromelain treated samples (Fig. 2E ) is somewhat similar to that of the DTT treated samples and characterized by the absence of the first unfolding event, whereas the second event was very little affected by the protease treatment (Table  1 ). These data provide further support to the notion that the first unfolding event is primarily due to glycoprotein G unfolding.
Therefore, the polarimeter configuration chosen is effective in the 15-to 35-keV energy band. XSPO allows reaching a minimum detectable polarization  80, 81  of 1% for an X5. 1 class flare and 5% for an M5. 2 class flare. (Spectral data are taken from Ref. 82 by summing the flux from two footpoints since the polarimeter configuration used is not able to separate spatially their emission. )  83 During 2 years of mission operation (from 2017 to 2018) about 20 flares are expected to be observed between the X10 and M5 classes, even if the observations will be performed during the decreasing phase of the solar cycle. The main parameters of XSPO are summarized in Table  8.
Mission Profile Trade-off studies performed over Sun-synchronous circular and elliptical orbits and high elliptical orbits, resulted in the selection of a dawn-dusk, Sun-synchronous, circular orbit at an altitude of 800 km. This orbit allows for continuous sunward pointing and limited eclipses, thus allowing long observing campaigns, while still keeping Doppler shift requirements, set by the tunable interferometers, within its limits. As a solar observatory, ADAHELI+ typical observations last 24 h, with continuous data acquisition from ISODY+. Data acquisition is switched to the XSPO instrument only during flare events. The selected orbit 87 allows for 10 months per year of eclipsefree observations. For the remaining 2 months, the duration of the umbra phase has a peak of about 17 min. Doppler shift is always lower than 4 km∕s, and, for over 50% of the time, below 2 km∕s.
Operations Concept ADAHELI+ is a solar observatory for long-duration, high cadence, continuous observations. During data acquisition, the spacecraft operates autonomously without need of intervention from the ground. Several consecutive observation sessions may be stored on the on-board scheduler, allowing a few days of autonomous operations of the space segment. Downloads of payload data are managed through a contact table, containing the ground station visibility periods. These are calculated by the flight dynamic center, based on the satellite attitude defined for the current observation session and are uploaded on board periodically. A similar concept is also applied to the management of the contact with the control station, where the link with the spacecraft is available with any attitude.
Data Downlink The ADAHELI+ ground segment will comprise of 2 main centers located in Italy: satellite monitoring and control will be orchestrated at Fucino Station (S-band), while payload data acquisition will be taken care of at Matera Station (X-band). The geographical proximity of the 2 ground stations provides almost simultaneous visibility. Considering the selected orbit, the daily visibility is about 50 min, divided in 2 groups of 2 or 3 consecutive passages occurring in early morning and late afternoon (local time). However, the attitude constraints during observations, together with the limited coverage of the highperformance X-band antenna, reduce the available contact time to the ground station for data download. The selected orbit, which has been also designed to maximize the visibility, guarantees a visibility time for payload data download of at least 25 min ∕day.
Introduction It is only recently that cluster samples selected via their Sunyaev-Zeldovich (SZ) signal have reached a significant sizes,   (Piffaretti et al. (2011)  and references therein). Some clusters may appear several times as distinct points due to differences in the mass estimate between surveys. The black dotted lines show the Planck mass limit for the medium-deep survey zone at 20% completeness for a redshift limit of z = 0. 5. The present note describes updates to the construction and properties of the Planck catalogue of SZ sources PSZ1, (hereafter PXXIX2013, Planck Collaboration XXIX 2013), released in March 2013 as part of the first Planck data delivery. The PSZ1 catalogue contains 1227 entries, including 683 so-called previously-known clusters. This category corresponds to the association of Planck SZ source detections with known clusters from the literature.
The association is set to the first identifier as defined in the hierarchy adopted by PXXIX2013, namely: (i) identification with MCXC clusters  (Piffaretti et   (v) searches in the NED and SIMBAD databases. Considerable added value, including consolidated redshift and mass estimates (Fig. 1 ), has been obtained through compilation of this ancillary information. Since its delivery March 2013, we have continued to update the PSZ1 catalogue by focusing on the confirmation of newlydiscovered clusters in PSZ1. This process has first involved updating the redshifts of some previously-known clusters (Sect. 2). We have also made use of recent results from dedicated followup observations conducted by the Planck Collaboration with the RTT150 (Planck Collaboration et al. 2014) and ENO telescopes (Planck Collaboration 2015, in prep.
Redshift updates for previously-known clusters In the external validation process performed in PXXIX2013, a total of 683 PSZ1 sources were associated with clusters published in X-ray, optical, or SZ catalogues, or with clusters found in the NED or SIMBAD databases. We refer to these as previously-known clusters. Their redshifts, when available, were compiled from the literature and a consolidated value was provided with the PSZ1 catalogue. In the present update, we first re-examine the previously-known clusters of the PSZ1 catalogue. The dedicated follow-up of Planck PSZ1 clusters with RTT150 described in Planck Collaboration et al. (2014) provided updates to the redshifts of 19 previously-known clusters. The follow-up of Planck PSZ1 clusters with ENO telescopes further updated the redshifts of five previously-known clusters.
We have updated the redshifts of ten PSZ1 sources associated with SPT clusters provided in  Bleem et al. (2014). Finally, we have queried the NED and SIMBAD databases, and searched in the cluster catalogues constructed from the SDSS data (namely  Wen et al. 2012 and Rozo et al. 2014 ), for additional spectroscopic redshifts. When these were available, we report them in the updated version of the PSZ1 catalogue. The full process led us to change the redshifts of 34 previously-known PSZ1 clusters. We have also changed the published photometric redshift estimate of one ACT cluster (ACT-CL J0559-5249) to a spectroscopic redshift value. In summary, 69 sources from the PSZ1 catalogue associated with previously-known clusters now have updated redshifts. Most of these consist of updates from photometric to spectroscopic values; however, eight redshifts were measured for the first time for previously-known clusters.
3. The origins and types of redshifts are shown in Fig. 3. Association with MCXC clusters  (Piffaretti et al. 2011 ) provides about 49. 8% of the redshifts, all of which are spectroscopic. Follow up observations undertaken by the Planck Collaboration provide 24. 6% of the redshifts, about two thirds of them being spectroscopic. SDSS-based catalogues yield 11. 7% of the redshifts, of which more than half of which are spectroscopic. NED and SIMBAD database searches yield 5. 9% of the redshifts, the vast majority of which are spectroscopic. PanSTARRS data provide 4. 4% of the redshifts, all of which are photometric. Finally, association with the SPT and ACT SZ catalogues represent ∼ 3. 5% of all redshifts, most of which are spectroscopic. For the Planck clusters with measured redshifts, we have provided a homogeneously-defined mass estimated from the Compton Y parameter.
Part of this research has been carried out with telescope time awarded by the CCI International Time Programme. The authors thank the TAC of the MPG/ESO-2. 2m telescope for support of optical follow-up with WFI under Max Planck time. Observations were also conducted with ESO NTT at the La Silla Paranal Observatory. This research has made use of SDSS-III data. Funding for SDSS-III http://www. sdss3. org/ has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and DoE. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration. This research has made use of the following databases: the NED and IRSA databases, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA; SIMBAD, operated at CDS, Strasbourg, France; SZ cluster database http://szcluster-db.
No redshift available 1: MCXC updated compilation 2: Databases NED and SIMBAD-CDS 3: SDSS cluster catalogue from Wen et al. (2012) 4: SDSS cluster catalogue from Szabo et al. (2011) 5: SPT 6: ACT 7: Search in SDSS galaxy catalogue from Planck Collab. from Fromenteau PhD 2010 and Fromenteau et al. (private comm. ) 8: SDSS catalogue from Rozo et al. (2014) 10: Pan-STARRS1 Survey confirmation 20: XMM-Newton confirmation from Planck Collab.
Acknowledgements. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The authors thank N. Schartel, ESA XMM-Newton project scientist, for granting the DDT used for confirmation of SZ Planck candidates. The authors thank TUBITAK, IKI, KFU and AST for support in using RTT150; in particular we thank KFU and IKI for providing significant amount of their observing time at RTT150. We also thank BTA 6-m telescope TAC for support of optical follow-up project. The authors acknowledge the use of the INT and WHT telescopes operated on the island of La Palma by the Isaac Newton Group of Telescopes at the Spanish Observatorio del Roque de los Muchachos of the IAC; the NOT, operated on La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, at the Spanish Observatorio del Roque de los Muchachos; the TNG, operated on La Palma by the Fundacion Galileo Galilei of the INAF at the Spanish Observatorio del Roque de los Muchachos; the GTC telescope, operated on La Palma by the IAC at the Spanish Observatorio del Roque de los Muchachos; and the IAC80 telescope operated on the island of Tenerife by the IAC at the Spanish Observatorio del Teide.
- 1 : 1 No redshift available 1: MCXC updated compilation 2: Databases NED and SIMBAD-CDS 3: SDSS cluster catalogue from Wen et al. (2012) 4: SDSS cluster catalogue from Szabo et al. (2011) 5: SPT 6: ACT 7: Search in SDSS galaxy catalogue from Planck Collab. from Fromenteau PhD 2010 and Fromenteau et al. (private comm. ) 8: SDSS catalogue from Rozo et al. (2014) 10: Pan-STARRS1 Survey confirmation 20: XMM-Newton confirmation from Planck Collab.
To date associations with MCXC clusters provide 49. 8% of the redshifts, all spectroscopic. Follow up observations by the Planck collaboration (FUs) provide 24. 6% of the redshifts, of which 64. 73% are spectroscopic. Associations with clusters from SDSS-based catalogues result in 11. 7% of all redshifts, of which 58. 9% are spectroscopic. Redshifts from the NED and SIMBAD databases represent 5. 9% of all redshifts, with 90. 7% of them spectro- scopic. The confirmation from PanSTARRS data provides 4. 4% of the total number of redshifts, all of them photometric. Finally the associa- tion with SZ catalogues (SPT and ACT) represents 3. 5% of all redshifts, of which 71. 9% are spectroscopic.
Results Wild-type and MCA-deficient mutants have the same growth rate in normal conditions. L. major MCA null mutants have been successfully generated thanks to the use of the Amaxa Nucleofector  40  and the lack of the expression of the Lmjmca gene was confirmed by RT-qPCR (reverse transcription quantitative PCR, data not shown). We then monitored the growth of the promastigote form in vitro. No growth defect phenotype was observed as MCA-deficient cells grew at a rate comparable to the WT strain (Figure  1 ). L. major MCA is implicated in cell death. To induce cell death, we cultivated cells with 40 μM of miltefosine over a 24-h period. Contrary to WT, MCA-deficient cells did not die in these conditions, as shown by significant growth differences between both strains starting 8 h after drug addition (Figure  2a ).
No growth difference could be detected between both strains in normal culture conditions role in the cell survival process autophagy, this process having been related to cell death (reviewed in Mariño et al. 45  ). When WT cells were cultivated in a serum-deprived medium, they entered autophagy as demonstrated by the significant increase in the percentage of cells with puncta of the autophagosome marker ATG8-GFP  46  (Figure  4a ). We could note that autophagy was correlated with a significant decrease in the concentration of cells counted with a Thoma cell counting chamber (Figure  4b ). Yet, no cell death occurred as demonstrated by the absence of TUNEL-positive cells (Supplementary Figure  S2 ). Instead, the concentration decrease was owing to a fast loss of mobility (data not shown), whereas only moving cells were counted with the Thoma chamber.
Acknowledgements. We thank  Jeremy Mottram  for providing us with the LmjMCA-deficient strain, the LmjMCA antibody and for the construction of the pGL1078 GFP-ATG8 vector. We thank  Ger van Zandbergen  for providing the pGL1078 GFP-ATG8 vector. This work was supported by the grants  FNRS N. 3100A0-116665/1  and N. 310030-135616  (NF). GFS was supported by  Agence Nationale de Recherche  through the  French Government's Investissements d'Avenir programme: Laboratoire d'Excellence 'Integrative Biology of Emerging Infectious Diseases'  (Grant No. ANR-10-LABX-62-IBEID ). MD was the recipient of a Bourse de stage from the  International Division of the Pasteur Institut and of a Bourse Fin de these scientifique  from the  Fondation de Recherche Médicale Equipe FRM  programme (FDT20110922563).
Several observations and techniques can be used to retrieve the densities of N 2 and CH 4 in the upper atmosphere. One technique uses UV airglow measurements from the Cassini Ultraviolet Imaging Spectrograph (UVIS)  (Stevens et al. 2011 (Stevens et al. , 2015)). However, these results have a vertical resolution of about 100 km and are dependent on the accurate knowledge of the instrument function and radiometric calibration of UVIS, which has an uncertainty of ∼15%  (Stevens et al. 2011). The analysis of airglow data also depends on a complex model of the emission processes of N 2. Another technique uses atmospheric emissions in the infrared. García-Comas et al. (2011)  modeled CH 4 emissions and, comparing their model to limb observations performed by the Cassini/Visual-Infrared Mapping Spectrometer (VIMS), derived methane abundances in the range 500 -1100 km.
Moreover, the low stellar flux (compared with the solar flux) leads to relatively low signal-to-noise ratio (S/N). Solar occultations are a valuable method to retrieve the composition of the upper atmosphere. The first solar occultation by Titan was measured by the UVS instrument  (Broadfoot et al. 1977)  onboard the Voyager 1 spacecraft. This instrument covers the wavelength range 500 -1700 Å and has a resolution of 10 Å. Although UVS measured an ingress and an egress occultations, the analysis of  Smith et al. (1982)  concentrated on the ingress leg because it had better geometrical characteristics. They used the data to confirm that the atmosphere is composed mainly of N 2 , with a small abundance of CH 4. Their results were used to constrain several subsequent models of the upper atmosphere (e.
Data corresponding to these absorption regions are therefore relatively straightforward to analyze (after the instrument corrections detailed in Section 2) and should provide reliable results. The higher spectral resolution of UVIS compared to UVS allows to better identify and use solar features for the retrieval. A closer observation and better spacecraft stability (except for observations with pointing instabilities) provide better altitude resolution and reduce the corrections needed when processing the data with respect to Voyager 1/UVS. The small spread in latitude/longitude of the observations allows to associate the derived vertical profiles with precise geographical coordinates. Thus, based on a simple technique (when compared with those used to the analysis of Titan's airglow), using well known absorption features, and being independent of calibration, UVIS solar occultations in the continuum region of the absorption cross sections are among the most reliable methods to retrieve local density profiles of N 2 , CH 4 , and temperatures in the upper atmosphere of Titan.
In this work we present number density profiles of N 2 , CH 4 , and temperatures in the thermosphere of Titan, retrieved from 8 solar occultations observed by Cassini/UVIS during the flybys T10, T26, T53, T58, T62 (ingress and egress), and T78 (ingress and egress). These observations cover the period from January 2006 to September 2011. The solar occultation from T53 was analyzed by  Capalbo et al. (2013) , the first published results from UVIS solar occultations. In Section 2 of the present work we detail instrument corrections and data analysis, including a correction of effects of unstable pointing that, if not corrected, would render some of the observations unusable. Section 3 presents the occultations analyzed, including their temporal and spatial coverage. The results are presented in Section 4, followed by a summary and conclusions in Section 5.