dataesr/scientific-paragraphs-categorization huggingface dataset:
These components accounted for eye artifacts and temporal muscle noise. Experimenter CB used visual inspection of component scalp topographies and power spectrum to reject these artifactual ICA components  [45]. To allow analysis of the ICA components at the group level, we used the EEGLAB Corrmap plugin  [46]  to form clusters of independent components based on the correlations of their scalps topographies. For each subject and each of the 2 conditions meditation practice (MED) and instructed mind wandering (IMW), we applied a spectral decomposition to the continuous data of each channel. We first segmented data into 1-second long epochs with no overlap, and then performed a Fourier transformation on these epochs after tappering the signal with a Hanning window. Finally, spectral power-equal to the square of Fast Fourier Transform (FFT) amplitude-was visualized in log scale (10 times the base-10 logarithm of the spectral power).
Psychometric data collection Subjective psychometric data were collected both prior to the experiment and at the end of each block. During the experiment subjects were allowed to sit at a table at the end of each block and asked to complete a questionnaire regarding their state of mind during the preceding block. We used 10-points scale to assess depth of the meditation (1: not deep at all, 10: deepest) and thought density (1: lot of space between occurrence of thoughts, 10: thoughts were frequent and overlapping). In addition, subjects had to rate on a 1 to 4 scale (1: not all, 4: very much) relaxation and hindrance items extracted from the Meditation Depth Questionnaire (MEDEQ,  [47] ), a validated questionnaire to assess the depth dimension of meditation. The full MEDEQ consists in five categories of questions, however we only used here a subset of two categories.
Robust linear correlations were computed using the skipped Pearson method implemented in the Robust Correlation Matlab toolbox from Pernet et al. [51]. This method protects against any bivariate outliers and uses 95% bootstrapped confidence intervals (CI) to assess significance. The R's ggplot2 package  [52]  was used to plot the distribution of data. Finally, comparisons between groups in the psychometric and demographic sections were performed using Wilcoxon rank-sum test. Comparisons of a given measure within a group were performed using Wilcoxon signed-rank test.
05-see Fig  4B ). When considering the instructed mind-wandering task, we observed a trend for increased gamma over occipital electrodes when comparing each of the three meditators groups to the control group (nonpaired permutation t-tests corrected for multiple comparisons, HYT: p<0. 06, VIP and ISY: p<0. 08). Specific effects of the different meditation practices were investigated by comparing the first 10 minutes of the meditation block in which participants practiced focusing on the breath with the last 10 minutes of the meditation block-corresponding to each group distinct meditation practice-taking only data from the meditator groups. We performed a mixed effects ANOVA taking the median gamma power during the meditation and breath focus conditions for the three meditator groups, leading to significant effect of condition (F(1,45) = 7, p = 0.
At the group level, 53 of these components could be clustered together (14 of the 16 subjects in the control, Vipassana and Himalayan yoga group and 11 of the 16 subjects in the Isha shoonya group) (Fig  5A ). No significant spectral frequency power difference was observed for this ICA cluster between the 4 groups. If eye-movement related artifacts were responsible for the increased gamma power observed between groups in this dataset, we should have observed higher gamma power in the eye movement independent components for meditators compared to the control group. As for the muscle-related artifactual components' activity, eye movement-related artifactual components' activity was removed from the data at the pre-processing stage. The analysis of eye-movement related artifacts activity between the meditation and instructed mind-wandering conditions shows that within the control group only, the spectral frequency power of the related ICA cluster is higher during instructed mind-wandering than during meditation in the range from 25 to 110 Hz (p<0.
001). Within the same eye-movement related ICA cluster, we observed a trend for higher power in the 11-17 Hz frequency range during instructed mind-wandering compared to meditation in the Vipassana group (p<0. 06) but failed to find any significant difference or trend in any frequency range when comparing meditation to instructed mind-wandering in the Himalayan yoga and Isha shoonya groups. We observed a positive correlation between the activity of the cluster of IC corresponding to eye blinks and the activity of the 60-110 Hz frequency range power over parieto-occipital electrodes for datasets of the meditators presents in the IC cluster, in the combined meditation These results show that it is unlikely that the gamma power increase we observe in meditators in comparison to control subjects is due to either temporal muscles or eye artifacts.
Limitations of the study Our study involved self-selection of the participants and only collected data at one point in time. Longitudinal studies of meditative practice with random selection of the participants training in meditation would be useful in the delineation of the likely complicated interplay of neurophysiological state and trait effects as they sequentially engage over the course of meditative training. Such studies could also help unravel individual differences in the pre-meditation training baseline that can influence the development of trait and state effects of meditation. One could also argue that our results might have been influenced by the fact that during the meditation condition, the control participants did 2 times 10 minutes of the same breath focus task whereas the meditators did 10 minutes of breath focus and then 10 minutes of a new task in form of their specific meditation practice.
Acknowledgments We are grateful to the  Meditation Research Institute  and the  Swami Rama Sadhaka Grama ashram in Rishikesh (SRSG) ,  India  for the use of their facilities and we wish to thank the late  Swami Veda Bharati  for his continued support and for helping to recruit Himalayan Yoga Tradition meditators. We also would like to acknowledge laboratory assistants  Mina Bhatt ,  Pooja Badoni ,  Vinthia Wirantana , and  Stephanie Pornin  for assisting with the data acquisition. We also thank  Bhavani Balakrishnan  for helping with the recruitment of the Isha practitioners throughout India. We thank  Swami Aman ,  Mr. Ajay Khatri ,  Mr. Sharma , and  Dr. Ravindra Pattanashetty  for their help in recruiting Vipassana practitioners and  Tracy Brandmeyer  for her help in proofreading an earlier version of the manuscript.
Large galaxies with low surface brightness in KiDS Although we work in angular units, we performed an analysis that is as close as possible to the analysis presented in vdB16, where data from the Canada-France-Hawaii Telescope (CFHT) were analysed. As a first step, we used SExtractor  (Bertin & Arnouts 1996)  on the r-band stack to detect sources, using a Gaussian filter with a FWHM of 5 pixels (∼ 1 with our detector) to improve our sensitivity towards faint extended galaxies. The KiDS pixel scale is slightly coarser than CFHT MegaCam (0. 214 /pix versus to 0. 185 /pix), so we require sources to have at least 15 adjacent pixels that are at least 0. 90 sigma above the background. These choices keep the purity of detecting real objects (and not noise fluctuations) high (cf. vdB16). We detected a total of 12 243 224 sources in the KiDS fields.
We measured richnesses down to a fixed magnitude past the characteristic magnitude in the r band, which is M * r = -21. 21 at z = 0. 10  (Blanton et al. 2003). The spectroscopic completeness limit of 19. 8 in the r band allowed us to measure the richness down to M * r + 2. 5 at this redshift. We k-corrected this limit based on a passively evolving stellar population with an age of 10 Gyr, and measured the richness consistently down to the same limit at all redshifts. Fig. 6. Abundance of UDGs as a function of halo mass. Thick black points with errors: same as shown in Fig. 3 , and these include the cluster points from vdB16. Black lines: best-fitting power-law relation including all black data points shown here. Blue squares: richnesses (i. e. the abundance of massive galaxies) in the same GAMA groups, with error bars defined in a similar way.
Acknowledgements. We thank  Annie Robin ,  Emanuele Daddi , and  Ryan Johnson  for insightful discussions, and an anonymous referee for a constructive report with valuable points to improve and clarify this manuscript. The research leading to these results has received funding from the  European Research Council  under the European Union's  Seventh Framework Programme  ( FP7/2007-2013)  /  ERC  grant agreement n • 340519. H. Hoekstra  acknowledges support from the  European Research Council  under  FP7  grant number  279396. C. H. acknowledges support from the  European Research Council  under grant number  647112. H. Hildebrandt is supported by an  Emmy Noether grant  (No. Hi 1495/2-1 ) of the  Deutsche Forschungsgemeinschaft. D. K. is supported by the  Deutsche Forschungsgemeinschaft  in the framework of the TR33 'The Dark Universe'.
Acknowledgements. We thank  Dr Plenchette  for His-ub mutant constructs,  Dr Gotoh ,  Dr Giacca  and  Dr Talianidis  for E2F1 mutant constructs,  Dr LeRomancer  for PRMT antibodies. We thank  Catherine Paul  for enriching discussions and proof reading of the manuscript. This work was supported by grants from the  'Comités de Côte d'Or et de l'Yonne' of the 'Ligue Contre le Cancer' (LD) , the  'Association pour la Recherche sur le Cancer ' (ARC to LD), the  European Union  and the  'Conseil Régional de Bourgogne ', a  French Government grant  managed by the  French National Research Agency  under the  program 'Investissements d'Avenir'  with reference  ANR-11-LABX-0021 , and fellowships from the  'Ministère de l'Enseignement Supérieur et de la Recherche' of France  (to JA, JB and JC), ' Ligue Nationale Contre le Cancer' (VG)  and the  "Fondation pour la Recherche Médicale (FRM)  (to JB).
Conflict of Interest The authors declare no conflict of interest. Author contributions VG and JA a performed most of the experiments. JB first identified the ubiquitination of E2F1 and initiated the work. BD, P-MB, ND, CK and JC performed additional western blot analysis and gene reporter assays. SG performed GST-pull down experiments. GM and DG performed analysis of E2F1 and its mutants, RB brought expertise in ChIP analysis. CG, OM and ES corrected the paper and LD conceived and supervised the project, analyzed the data and wrote the paper with input from all authors. Cell Death and Disease is an open-access journal published by Nature Publishing Group. This work is licensed under a Creative Commons Attribution 4. 0 International License. The images or other third party material in this article are included in the article's Creative Commons license, unless indicated otherwise in the credit line; if the material is not included under the Creative Commons license, users will need to obtain permission from the license holder to reproduce the material.
Demographics: The front page of the survey was shown to 672 persons, 286 gave at least one answer, 162 completed the questionnaire, and 116 persons entered their email addresses. The age of the population (n = 220) has a mean of 32 years (s = 9). The degrees in the population (n = 244) are: master (38%), bachelor (25%), student (18%), no degree (13%), or PhD (6%). As their occupation, 56% of the persons selected software developer, 21% system administrator, and 16% researcher (multiple choice question, n = 287). Participants reported work on up to five different FLOSS projects. For the first project, they estimated their participation with a mean of 5. 3 years (s = 5, n = 180). 60% of them reported a second FLOSS project, 36% a third, 17% a fourth, and 9% a fifth. Raw data and questions are available at https://rawdata.
On GitHub alone, issues mentioning the variable were reported 71 times. The underlying issue usually is that the software package webkitgtk is missing 2. The developers even considered the dependency (installation paths) for RPM-based systems by parsing gre. conf. But for other users on non-RPM-based systems the fallback is to query MOZILLA FIVE HOME which leads to the misleading error. In the workarounds (including parsing gre. conf) needed 213 lines of code. Furthermore, most of the 9006 snippets we found on GitHub referring to the variable are small wrappers trying to set MOZILLA FIVE HOME correctly. Discussion: While the package managers easily answer where the missing files are located, within the application there is no reasonable way to find out. We found similar issues concerning network, firewall, hardware settings, etc.
Related Work Many other configuration libraries have validation capabilities, for example, Apache Commons Configuration. Unlike Elektra they do not have external specifications. Instead they require developers to hardcode them into the applications. Other papers describe the technical details of Elektra  [20, 23, 29]. In particular frontend code generation avoids errors in configuration access  [21, 28]. Other work describes Elektra's specification language  [22, 24]  and how applications participate without code modifications  [25, 26]. Crowston et al. [6]  created a survey of empirical research for FLOSS. Michlmayr et al. [16]  investigated quality issues of FLOSS using interviews. We were able to confirm that documentation often is lacking. Barcomb et al. [2]  used a questionnaire to investigate how developers acquire FLOSS skills.
Understanding the plumbing system structure below volcanoes and the storage conditions (temperature, pressure, volatile content and oxygen fugacity) of erupted magmas is of paramount importance for eruption forecasting and understanding of the factors controlling eruptive dynamics. Phase equilibria experiments have been performed on a Tungurahua andesite (Ecuador) to shed light on the magmatic conditions that lead to the July-August 2006 eruptions and the parameters that controlled the eruptive dynamics. Crystallization experiments were performed on a representative August 2006 mafic andesite product between 950-1025ºC, at 100, 200 and 400 MPa and NNO+1 and +2, and water mole fractions in the fluid (XH 2 O) from 0. 3 to 1 (water-saturation). Comparison of the natural phenocryst assemblage, proportions and phenocryst compositions with our experimental data indicates that the natural andesite experienced two levels of ponding prior to the eruption.
e. , Antisana, Pichincha, Sangay, Cayambe) are known to erupt geochemically distinctive products, characterized by primitive magnesian andesites with Mg#>50  (Kelemen et al. 2014 ) with an adakitic affinity (e. g. ,  Bourdon et al. 2002a,b; Garrison & Davidson 2003; Samaniego et al. 2005; Hidalgo et al. 2012, among others). Intermediate to silicic adakitic magmas have been previously studied (e. g. , Mt. Pinatubo,  Scaillet & Evans, 1999; Prouteau & Scaillet, 2003)  but mafic compositions with an adakitic affinity such as those erupting at Tungurahua have been left virtually uncharacterized experimentally. Although similar rocks such as high-Mg andesites have been investigated by  Blatter & Carmichael (1998) ,  Moore & Carmichael (1998)  and  Wood & Turner (2009) , data on the Tungurahua andesite presented in this study contribute to the experimental database for mafic magmas close to the adakitic series.
For instance, hypocenter locations of volcano-tectonic earthquakes are extensively scattered from 6-17 km below the summit, in a large region likely to host a magma body (see Figure  5d  from  Molina et al. , 2005). Recent data have shown that eruption events recorded in 2010 were triggered 6 km below the summit  (Kumagai et al. , 2011) , which is interpreted as the depth at which magma is subjected to pressure disturbances, further resulting in fragmentation of the magma at shallower depths. In addition,  Biggs et al. (2010)  using synthetic aperture radar Downloaded from https://academic. oup. com/petrology/article-abstract/doi/10. 1093/petrology/egx054/4096628/Structure-of-the-plumbing-system-at-Tungurahua by CNRS -ISTO user on 08 September 2017 interferometry (InSAR) images of Tungurahua during the February 2008 eruption, reported a rapid uplift associated with a shallow sill-like magmatic source inside the Tungurahua cone.
Bulk-rock We used as starting material the scoriae lapilli products of the August 2006 episode corresponding to sample TUNG-PS-51B of  Samaniego et al. (2011). Further analytical and petrographic work was performed to complete the available data concerning the petrography and chemistry of the August 2006 products (see below for the analytical conditions). The sample is a Mg-rich mafic andesite (58 wt % SiO 2 ; Table  1 ). It exhibits an adakitic affinity Downloaded from https://academic. oup. com/petrology/article-abstract/doi/10. 1093/petrology/egx054/4096628/Structure-of-the-plumbing-system-at-Tungurahua by CNRS -ISTO user on 08 September 2017  (Defant & Drummond 1990) , marked by elevated MgO (4. 5 wt %) and Na 2 O (3. 9 wt %), high Sr (570 ppm) and La/Yb (12) and a low Y (17 ppm; Table  1 ).
Other mineral phases Dispersed within the vesiculated matrix, we occasionally found (<0. 5 vol. %; Samaniego et al. , 2011)  Ol phenocrysts, normally zoned from Fo 80±2 cores to Fo 75±2 rims  (Samaniego et al. , 2011; Myers et al. , 2014). These crystals show clear evidence of reaction, i. e. they have resorbed rims overgrown by an Opx of composition En 71 Fs 25 Wo 4 and Mg# = 75 Downloaded from https://academic. oup. com/petrology/article-abstract/doi/10. 1093/petrology/egx054/4096628/Structure-of-the-plumbing-system-at-Tungurahua by CNRS -ISTO user on 08 September 2017 (Supplementary Data Appendix natural sample). The origin of such textural relationships and compositional zoning of Ol and related Opx is addressed subsequently. We also found a partially resorbed Ilm crystal (41 wt % TiO 2 , 49 wt % FeO*) surrounded by a Mt crystal with a composition similar to that of the main population (TiO 2 = 13 wt%, Mg# = 5).
Crystal content and phase proportions Liquidus conditions (i. e. , 0 wt. % crystals) have been attained at 1025ºC, 400 MPa, ~9 wt % H 2 O melt and fO 2 ~NNO+1 (Supplementary Data Appendix crystal content, Table  2 ) whereas Downloaded from https://academic. oup. com/petrology/article-abstract/doi/10. 1093/petrology/egx054/4096628/Structure-of-the-plumbing-system-at-Tungurahua by CNRS -ISTO user on 08 September 2017 the maximum amount of crystals (45 wt %) occurs at 1025ºC, 400 MPa, 6. 6 wt % H 2 O melt and fO 2 ~NNO+1. In general, the crystal content of the charges varies with the experimental parameters, mostly T, H 2 O melt and P, whereas a change in fO 2 from NNO+1 to NNO+2 does not have a major influence (see Supplementary Data Appendix crystal content). Lowering H 2 O melt and temperature at a given pressure increases the crystal content (see for instance the 200 and 400 MPa charges; Table  2 ).
Amphiboles Experimental Amph is a Ti-or Fe-tschermakitic hornblende according to the classification of  Leake et al. (1997). The limited amount of data available on Amph prevents us from discussing in detail the compositional dependence of amphibole with intensive parameters. Nevertheless, for a given experimental series at constant T and P, a decrease in H 2 O melt Downloaded from https://academic. oup. com/petrology/article-abstract/doi/10. 1093/petrology/egx054/4096628/Structure-of-the-plumbing-system-at-Tungurahua by CNRS -ISTO user on 08 September 2017 produces amphiboles with lower Mg# and slightly higher Ti (Table  8 ). Traditionally, changes in Al IV and Al VI in Amph have been related to changes in pressure and temperature, respectively, and used as thermobarometers (i. e. ,  Ridolfi & Renzulli, 2012).
Pre-eruptive conditions of the 2006 andesitic products at Tungurahua To understand the storage conditions of the 2006 andesite and the magmatic processes occurring prior to the eruption, we compare our experimental data with information previously gained from the natural rock. The comparison of experimental and natural mineral assemblages, compositions, and modal proportions provides tight constraints on the preeruptive conditions (T, P, H 2 O melt , fO 2 ) of the Tungurahua magma prior to the 2006 eruption. We first use the information gained from the main unzoned population of phenocrysts (Cpx+Opx+Mt+Pl) and the core composition of the zoned crystals (Cpx, Pl, Opx) to infer the crystallization conditions of these minerals. Second, we constrain the origin of the Mg-rich (Cpx, Opx) and Ca-rich (Pl) phenocryst rims.
Therefore, the data consistently point to a shallow origin for crystallizing the mafic rim compositions. However, it is worth noting that under the conditions of charge T24, a small proportion (<0. 2 wt %) of Ol (Fo 77 ) is present together with the Mg-and Ca-rich mineral assemblage (Table  2 ; Fig. 3b ). It is emphasized that Fo 77 is in the range of compositions of Downloaded from https://academic. oup. com/petrology/article-abstract/doi/10. 1093/petrology/egx054/4096628/Structure-of-the-plumbing-system-at-Tungurahua by CNRS -ISTO user on 08 September 2017 olivine rims (Fo 75±2 ; Fig. 4 ) which are commonly resorbed. Thus, there is a need to clarify the origin of olivine and the mechanism of olivine resorption in the plumbing system (see below).
To do so, the distribution of Fe* content in Pl, as proposed by  Ruprecht & Wörner (2007)  has been used: a rimward increase of both Ca and Fe* in Pl crystals would suggest a mixing process involving a mafic magma. In our case, the An 65-70 rims have FeO* contents (~0. 5-0. 6 wt %) similar to the An 50±5 cores (Table  1 , Supplementary Data Appendix natural;  Samaniego et al. , 2011)  which rules out the foreign basaltic magma hypothesis to explain the Ca and Mg-rich rim compositions. This conclusion is consistent with the lack of basaltic magmas at Tungurahua. Magmas with the highest Ca/Na (able to crystallize An-rich plagioclase) are represented by basaltic andesitic whole-rocks and melt inclusions whose SiO 2 contents are 54 wt % minimum (Fig. 1c ;  Hall et al. 1999; Samaniego et al. 2011; Myers et al.
3a ), shifting the system outside the olivine stability field (Fig. 3a ). In the 200 MPa phase diagram, the field for shallow pre-eruptive conditions straddles the Ol stability curve so that a temperature drop < 975°C or an fO 2 increase above NNO+2 would also lead to Ol resorption Downloaded from https://academic. oup. com/petrology/article-abstract/doi/10. 1093/petrology/egx054/4096628/Structure-of-the-plumbing-system-at-Tungurahua by CNRS -ISTO user on 08 September 2017 (Fig. 3a ). The transition from an Ol-bearing to an Ol-free phase assemblage has been experimentally simulated at 975°C, 200 MPa between charges T24 and T25 (Table  2 ). Opx in the Ol-free charge T25 is En 75 , close to Opx compositions in Ol reaction rims (En 71-72 ; Supplementary Data Appendix natural;  Samaniego et al.
CONCLUSIONS The combination of new petrological and phase equilibrium data obtained on the 2006 eruptive products of Tungurahua allow us to determine the storage conditions of the andesitic magmas emitted during this eruption, as well as to infer the structure of the plumbing system below the volcano. Our results suggest that the Tungurahua andesitic magmas are hot (1000-975ºC) and water-rich (5-6 wt%). These characteristics seem to be a constant feature at this volcano since, historically, Tungurahua has emitted rather homogeneous andesitic magmas. The July-August 2006 plumbing system was characterised by two magma reservoirs located at 15-16 km (400 MPa) and 8-10 km (200 MPa), both simultaneously active during this time period. Magmas stored at 400 MPa interacted with those residing at 200 MPa, resulting in a complex inverse zonation of the phenocrysts.