dataesr/scientific-paragraphs-categorization huggingface dataset:
5 data sets in all seven AIA EUV channels (94 Å, 131 Å, 171 Å, 193 Å, 211 Å, 304 Å, and 335 Å), focusing on an FOV of 332″ × 282″ (see Figure  1 , right panel)centered at  [-970″, 142″]. For this study, we use a cadence of 5 minutes. The AIA data are read and calibrated to level 1. 5 using the routine aia_prep from the Interactive Data Language SolarSoftware library (IDL SSW). The intensities are first normalized to the exposure times, and a 4 × 4 pixel binning is applied to increase the signal-to-noise ratio. Please see  Froment et al. (2015 Froment et al. ( , 2020) )  for further details. Contrary to previous studies, we also check for the existence of short-term periodicities (<1 hr) in the same region.
Data Preparation For the co-alignment between the AIA and SJI channels, we first resample the AIA data to the SJI plate scale. The coaligning is then achieved by matching the solar limb and ondisk features seen in co-temporal images of AIA 1600 Å and SJI 2832 Å, which form under similar conditions. Once the x and y shifts are obtained at various time instances, an interpolation is performed for any other time sequence and applied to all other channels. As discussed in  Wülser et al. (2018) , IRIS observations are influenced by a modest level of scattered light that is pointing dependent and often difficult to characterize, especially for offlimb observations. Due to this scattered light and imperfect flatfielding, the rastering mode of IRIS results in a background contribution that shows apparent motion relative to the solar image and thereby causes a nontrivial, time-dependent noise in the SJI images that periodically increases the intensity in the image.
Acknowledgments P. A. acknowledges funding from his  STFC Ernest Rutherford Fellowship  (No. ST/R004285/2 ). IRIS is a  NASA  small explorer mission developed and operated by  LMSAL , with mission operations executed at  NASA Ames Research Center  and major contributions to downlink communications funded by  ESA  and the  Norwegian Space Centre. SDO is a mission for  NASAʼs Living With  a Star ( LWS) program. AIA is an instrument on board the  Solar Dynamics Observatory. All SDO data used in this work are available from the  Joint Science Operations Center  (http://jsoc. stanford. edu) without restriction. The  National Solar Observatory (NSO)  is operated by the  Association of Universities for Research in Astronomy, Inc. (AURA) , under cooperative agreement with the  National Science Foundation.
S. S. , P. A, and C. F. were supported by the  Programme National PNST of CNRS/INSU  co-funded by  CNES  and  CEA. This research was supported by the  International Space Science Institute (ISSI) in Bern , through  ISSI International Team  project No. 545  (" Observe Observe Local Think Global: What Solar Observations Can Teach Us about Multiphase Plasmas across Physical Scales " ). We are grateful to an anonymous referee for the careful review and thoughtful comments, which greatly enhanced the clarity and rigor of this work.
2013; Esteban et al. 2022). Atlantic Naisa SFPWs off Madeira have a high survival rate and the population size is stable  (Alves et al. 2015; Verborgh et al. 2022). Although some degree of natal philopatry has been proposed for Atlantic Naisa SFPWs, the analyses of long-term stability of sexed animals within pods were inferred from a limited dataset of whales of known sex  (Alves et al. 2013). We used long-term photographic-identification data of 1275 Atlantic Naisa SFPWs off Madeira, complemented with biopsies of 51 individuals to genetically determine sex following  Alves et al. (2020). Hierarchical cluster analysis was used to classify and illustrate relationships between the genetically sexed and distinctive whales captured on ≥4 encounters with high or full coverage (e. g. , when the proportion of captured individuals per encounter was ≥0.
8;  Alves et al. 2013 ) and where documented pods had >1 animal of known sex. The truncated dataset used in the analysis selected 42 sexed/distinctive whales (24 females, 18 males) and 362 encounters collected year-round between 2003 and 2020. We defined the sampling period (and associations) as all individuals grouped within an encounter. Permutation tests were performed to understand whether preferred associations existed  (Bejder et al. 1998; Whitehead 1999). Associations were calculated using the average-linkage method due to presenting the highest cophenetic correlation coefficient (CCC = 0. 986). The association index corresponding to the maximum modularity was used to define community division by clusters  (Whitehead 2008) , and all analyses were carried out in SOCPROG 2. 9  (Whitehead 2009).
Examination of Reproductive Senescence in Female Southern Hemisphere LFPWs off Aotearoa New Zealand Prolonged post-reproductive lifespans are rare in mammalian species. In contrast with the closely related SFPW, female North Atlantic LFPWs do not appear to have a significant post-reproductive lifespan  (Martin and Rothery 1993; Ellis et al. 2018a). Reproductive senescence has not been previously examined in female Southern Hemisphere LFPWs. However, given that population variability in life history parameters exists for this species (Tables 15. 1 and 15. 2), it is important to investigate the potential existence of a significant post-reproductive lifespan in the Southern Hemisphere LFPW, specifically. Here we present the first investigation of female reproductive senescence for the Southern Hemisphere LFPW, through examination of reproductive data opportunistically collected from stranding events on the Aotearoa New Zealand, coast.
Lack of Evidence for a Post-reproductive Lifespan in LFPWs The observation that pregnancy rates decrease and the duration of the resting periods increases in Southern Hemisphere LFPWs older than 10 years suggests that there is a reduction in fecundity with age, as also reported for the North Atlantic LFPW  (Martin and Rothery 1993). In contrast to the North Atlantic LFPW, reproductive senescence was not evident in Southern Hemisphere LFPWs. However, the maximum female age estimated for Southern Hemisphere LFPWs in this study (33 years) was much lower than that recorded for North Atlantic LFPWs in the Faroe Islands (59 years;  Martin and Rothery 1993) and Newfoundland (56. 5 years; Sergeant 1962; Kasuya et al. 1988) , where longevity exceeded 50 years (Table  15. 1). The smaller sample size in this study, compared with the availability of much larger datasets from North Atlantic drive fisheries (e.
Acknowledgments ELB acknowledges  Ngāti Kuri ,  Ngāi Tokato ,  Te Aupouri ,  Waikato ,  Manawhenua ki Mohua , and  Ngāi Tahu  of the  Department of Conservation Te Papa Atawhai  for providing access to stranded pilot whales on the coast of  Aotearoa New Zealand  for sampling and, in many cases, also providing logistical support in the field. Biological samples from  Aotearoa New Zealand  were collected under marine mammal research permit 39635-MAR issued to ELB by the  Department of Conservation Te Papa Atawhai. ELB also thanks the following people for support with sample collection and/or processing:  Tim Beatson ,  Mat Betty ,  Barbara Bollard ,  Barrack Carle ,  Sarah Dwyer ,  Jeanie Fay ,  Sarah Gardiner ,  Nik Hannam ,  Severine Hannam ,  Bethany Hinton ,  Jessica Hiscox ,  Shabana Honetana ,  Odette Howarth ,  Rebecca Jarvis ,  Emmanuelle Martinez ,  Sinéad Murphy ,  Steve O'Shea ,  Karen Stockin ,  Andrew Wallace ,  Lindsey White , and  Jessie Williams.
Study sites and datasets We characterize the morphologies and morphometries of gullies in 29 craters distributed over the Southern Hemisphere of Mars between 30 • S and 75 • S latitude (Fig. 1 ). These 29 craters are selected based on the availability of publicly released High Resolution Imaging Science Experiment (HiRISE) stereo-pair-based digital terrain models (DTMs) or the presence of suitable HiRISE stereo-pair images to produce a DTM ourselves. The HiRISE stereo-pair images are usually ∼ 0. 25-0. 5 m/pixel  (McEwen et al. , 2007) , so the DTM post spacing is ∼ 1-2 m with vertical precision in the range of tens of centimeters  (Kirk et al. , 2008). Among the 29 gullied craters, publicly released DTMs are available for 25 craters (https://www. uahirise. org/hiwish/maps/dtms. jsp, last access: 18 September 2021) (Table  1 ).
, 2010). 3. Colluvial systems -these are systems dominated by rock-gravity and sediment-gravity flows, with their dominant activity relating to rockfalls, grain flows, and snow avalanches (in periglacial and alpine settings). Debris flows typically constitute only a relatively minor component of geomorphic processes in such systems. The fans of these systems are also commonly known as colluvial cones or talus cones  (Siewert et al. , 2012; De Haas et al. , 2015b). Although these systems may be dominated by one type of geomorphic process, it is important to stress that other processes may also occur. For example, on Earth, water floods are not uncommon on many debris-flow-dominated systems, while debris-flow deposits are commonly recognized on colluvial cones. To compare the morphometric characteristics of the Martian gully systems to terrestrial systems, we have compiled morphometric data of gully alcoves and fans across several continents, mountain ranges, climate zones, and process types on Earth.
This dataset includes published data from the Himalayas, Ladakh, India  (Stolle et al. , 2015) , the tropical Andes, Columbia  (Arango et al. , 2021) , Spitsbergen, Svalbard  (Tomczyk, 2021) , British Columbia, Canada  (Kostaschuk et al. , 1986; Jackson et al. , 1987;  and newly presented data), the southern Carpathians, Romania  (Ilinca, 2021) , the Southern Alps, New Zealand (de  Scally and Owens, 2004; de Scally et al. , 2010) , the North Cascade Foothills, USA, the European Alps (including Switzerland, Italy, France, and Austria), and the Pyrenees (from multiple authors compiled by  Bertrand et al. , 2013). The dataset comprises information from colluvial, debris-flow-dominated, and flood-dominated (also including debris flood) systems. In total, it contains 231 colluvial systems, 749 debris-flowdominated systems, and 369 flood-dominated systems.
In total, data were compiled for 1349 systems, although not all information was available for all systems, with data availability ranging from 729 sites for alcove length to all 1349 systems for Melton index and process type. Based on these data, we have made a heatmap of the probability of conditions dominated by flood, debris flow, or colluvial systems for combinations of Melton ratio with alcove length and fan gradient to which we compare the Martian gullies (Fig. 8 ). We have specifically chosen the combinations of Melton ratio with alcove length and fan gradient to infer the Martian gully formative mechanism because they have been widely used in discriminating terrestrial drainage basins and fans prone to flooding from those subject to debris flows, debris floods, and floods (e. g. , de  Scally and Owens, 2004; Wilford et al.
This is consistent with the findings reported in previous studies that showed evidence of formation of deposits morphologically similar to terrestrial debris-flow-like deposits, both in the past and during the present day (e. g. ,  Johnsson et al. , 2014; Dundas et al. , 2019). The present-day sublimation of CO 2 ice on Mars is envisaged to provide the necessary flow fluidization for the emplacement of deposits similar to debris-flow-like deposits on Earth  (De Haas et al. , 2019b). (Sinha et al. , 2022a). The measurement datasets can be downloaded from https://doi. org/10. 6084/m9. figshare. 21717182. v1  (Sinha et al. , 2022b). Author contributions. RKS, TDH, and SJC conceptualized this work. The methodology was developed by RKS, TDH, and SJC. Data curation and formal analyses were performed by RKS.
TDH and AN also contributed to the collection of datasets used in this work. RKS, DR, TDH, and SJC contributed to the interpretation of the data and results. RKS wrote the original draft of this paper, which was reviewed and edited by all authors. Competing interests. At least one of the (co-)authors is a guest member of the editorial board of Earth Surface Dynamics for the special issue "Planetary landscapes, landforms, and their analogues". The peer-review process was guided by an independent editor, and the authors have also no other competing interests to declare. Disclaimer. Publisher's note: Copernicus Publications remains neutral with regard to jurisdictional claims in published maps and institutional affiliations. Special issue statement. This article is part of the special issue "Planetary landscapes, landforms, and their analogues".
and Dwijesh Ray acknowledge the financial support by the Indian Space Research Organisation, Department of Space, Government of India. Susan J. Conway and Axel Noblet are grateful for the financial support from Région Pays de la Loire, project étoiles montantes METAFLOWS (convention no. 2019-14294) as well as the financial support of CNES in support of their HiRISE work. Tjalling De Haas was supported by the Netherlands Organisation for Scientific Research (NWO) (grant 016. Veni. 192. 001). We acknowledge the efforts of team MUTED to develop an online tool (http://muted. wwu. de/, last access: 21 June 2023) for quick identification of the spatial and multi-temporal coverage of planetary image data from Mars. All the planetary datasets used in this work are available for free download at the PDS Geosciences Node Mars Orbital Data Explorer (ODE) (https://ode.
rsl. wustl. edu/mars/, last access: 21 June 2023) and https://www. uahirise. org/ (last access: 21 June 2023). The newly generated DTMs can be downloaded from https://figshare. com/articles/dataset/Self_generated_DEMs/21717164 (last access: 22 July 2023). The measurement datasets can be downloaded from https://figshare. com/articles/dataset/Measurement_data_of_ gully_systems_in_the_southern_mid_latitudes_of_Mars/21717182 (last access: 22 July 2023). This work is a part of the PhD work of Rishitosh K. Sinha. Director PRL, Head of Planetary Science Division, PRL, Head of Planetary Remote Sensing Section, PRL, and Director IIT Gandhinagar are gratefully acknowledged for constant encouragement during the work. Financial support. This research has been supported by the Indian Space Research Organisation, Department of Space, Government of India, Région Pays de la Loire, project étoiles montantes METAFLOWS (convention no.
1. 2) and ClinVar databases. The Combined 10 Annotation Dependent Depletion (CADD) score of this variant is 41. 11 12 Additional testing in patients following the identification of the TRAPPC2L 13 nonsense variant 14 Serum creatine kinase (CK) are molecules of 360 amino acids, formed by a dimer of 2 15 subunits: M (muscular) and B (brain). There are 3 isoenzymes of CK resulting from the 16 combination of these subunits: CK-BB, CK-MB and CK-MM. Only total CK and CK-MB 17 are routinely measurable. An elevated MB-CK level usually reflects damage to the heart 18 muscle. However, skeletal muscle contains about 7% of MB-CK. Thus, intense 19 muscular exercise or chronic muscular disease can sometimes be the cause of an 20 abnormal CK-MB. Both patients showed elevated levels of total CK over the course of 21 2.
one of the main lines of evidence used to determine the link 15 between a given gene and a phenotype. According to the Clingen clinical validity 16 framework, the level of evidence is limited to support a gene-disease relationship for the 17 TRAPPC2L gene due to the small number of patients reported(12). Thus, the formal 18 variant ACMG/AMP classification is not possible for the identified variant(13,14). Once 19 the gene-disease relationship is established for the TRAPPC2L gene, the following 20 ACMG codes could be attributed: (1) PVS1_strong since nonsense-mediated mRNA 21 decay is not predicted for this nonsense variant as it is located 8bp from the end of the 22 second-to-last-exon. However, there is no loss of function (LoF) variant in the exon 4 in 23 population databases and this specific exon is present in all biologically-relevant 24 transcripts.
9 F. R. has received funding from the Excellence Initiative of Aix-Marseille University -10 A*Midex a French "Investissements d'Avenir programme"-Institute MarMaRa AMX-19-11 IET-007" to carry out research as part of a PhD. 12 CONTRIBUTION 13 14 FR, MA, and CMR drafted and wrote the manuscript in consultation with all authors. 15 FR, SS and BC provided clinical care. CMR, PC and FM performed research WES 16 analyses. MA, FR, SS and BC performed clinical and pathological phenotyping. SG, JM, 17 FM, LV, and BC contributed with interpretation and discussion of results. FR, MA and 18 CMR generated figures and supplementaries. FR coordinated the study. LV provided 19 financial support for the research analysis. 20 ETHICS STATEMENT 21 This study has been approved by the scientific committee of the Assistance Publique 22 Hôpitaux de Marseille (PADS22-337).
Global protected area targets were declared in the 1980s, with the action plan emerging from the third World Parks Congress calling for nations to protect 10% of their area, including hitherto neglected marine and freshwater areas. The CBD, the world's first intergovernmental biodiversity conservation treaty, entered into force in 1993. With overexploitation, and habitat fragmentation and loss being the primary proximate drivers of biodiversity decline, the CBD treaty identified protected areas as a key conservation tool. At the beginning of each decade during a conference of the parties (COP), the 196 parties to the CBD define a new strategic plan to guide national biodiversity strategies. To support global monitoring of progress, parties are encouraged to share information on their area-based conservation estate with the World Conservation Monitoring Center, a joint venture of the UN and the IUCN, for population of the World Database on Protected Areas.
The dashed lines represent the 30x30 target to ensure 30% global coverage for terrestrial (green) and marine (blue) areas by 2030, which is called for by Target 3 of the Convention on Biological Diversity's Kunming-Montreal Global Biodiversity Framework. Source: The World Database on Protected Areas and the World Database on OECMs (UNEP-WCMC and IUCN 2022). areas that allow sustainable use account for the biggest proportion of the protected area estate, while category III protected areas account for least (Figure  2 ). CBD parties are further encouraged to classify their reported protected areas according to the IUCN governance types. Diversity of governing actors is low, with most protected areas governed by government (Figure  2 ).
Effectiveness Effectiveness is generally understood as whether area-based conservation makes a positive difference to biodiversity. However, the agreed-upon approach for measuring this subcomponent is protected area management effectiveness (PAME) evaluations, which examine inputs, processes, outputs, outcomes, etc. Given that evaluations are not applied consistently, effectiveness is tracked globally as the proportion of protected areas with a completed PAME evaluation. According to the global database on PAME, in 2020 only 18. 29% of the area covered by protected areas has been evaluated. This is concerning given that a completed evaluation is a very basic indicator of effective management. Research shows that if protected areas are well resourced and complied with, they are effective in conserving in situ biodiversity.
ACKNOWLEDGMENTS We thank  Emily Darling  and the editor for their helpful comments. G. G. G. and V. M. A. gratefully acknowledge support from the  Australian Research Council , including a  Discovery Early Career Research Award  ( DE210101918 ) to G. G. G. and a  Future Fellowship  to V. M. A. (FT220100210). J. C. thanks  BiodivERsA (METRODIVER)  and  Fondation de France (MultiNet)  for financial support.
Millimeter-wave absorption The new absorption data discussed here are spectra of HCO + in 33 directions along Galactic anticenter sightlines toward ALMA phase calibrators as given in the Tables here and projected on sky maps in Figure  1. As before, the HCO + spectra were acquired with a spectral resolution of 0. 205 km s -1 sampled at 0. 102 km s -1 intervals without the so-called spectral averaging that bins data. We also acquired spectra of HCN, C 2 H, HCO, and several isotopologs. Counts of detections are shown in Figure  2 , but results for species other than HCO + will be discussed in detail in later work. Statistics of the HCO + detections are shown in.
IRAM 30m CO emission We took frequency-switched CO emission profiles at the IRAM 30m telescope in August 2019 toward the 28 anticenter sightlines with detected HCO + absorption. The CO spectra are shown in Figure  B. 1. These CO data were taken as five-point maps toward the target and displaced by 2 HPBW (2x22 ′′ ) in the four cardinal directions, using a pointing pattern that was designed to detect HCO + and HCN emission in the presence of spectral line absorption in the target direction. For the HCO + emission that will be discussed in subsequent work, the HCO + emission profile is formed by averaging spectra along the four outlying directions. For CO the present results use the average of all five pointings because contamination by absorption is not measurable given the strength of the emission and/or the continuum.
Acknowledgements. The  National Radio Astronomy Observatory (NRAO)  is a facility of the  National Science Foundation , operated by  Associated Universities, Inc. This work was supported by the  French program "Physique et Chimie du Milieu Interstellaire" (PCMI)  funded by the  Conseil National de la Recherche Scientifique (CNRS)  and  Centre National d'Etudes Spatiales (CNES). This work is based in part on observations carried out under project number  003-19  with the IRAM 30m telescope]. IRAM is supported by  INSU/CNRS (France) ,  MPG (Germany)  and  IGN (Spain). This paper makes use of the following ALMA data -ADS/JAO. ALMA#2016. 1. 00714. S  -ADS/JAO. ALMA# 2018. 1. 00115. S ALMA is a partnership of  ESO  (representing its member states),  NSF (USA)  and  NINS (Japan) , together with  NRC (Canada) ,  NSC  and  ASIAA (Taiwan) , and  KASI ( Republic of Korea) , in coop-eration with the  Republic of Chile.
Assessment and data collection Data was collected every 3 months during the first two years, then every 6 months thereafter until study end, as per standard practice. An investigator assessed the therapeutic response including the refractory status to lenalidomide (Twenty-six (6. 9%) patients were reported to be lenalidomide-refractory, although this was a non-inclusion criterion) and disease progression according to International Myeloma Working Group (IMWG) criteria  [16]  as in usual practice at each site (no central review). Safety data were collected for up to 30 days after the last treatment dose administration. Treatment discontinuation was based on the investigator judgment. Post-IXA-Rd data were collected for subsequent therapies description and survival status. Patient cytogenetic abnormalities, Eastern Cooperative Oncology Group performance status (ECOG-PS) and International Staging System (ISS) were not routinely conducted in all sites but were collected at IXA-Rd initiation when available.
Comorbidities were estimated with the Charlson's Comorbidity Index and frailty was evaluated using the simplified frailty score based on age, Charlson's Comorbidity Index and ECOG-PS  [17]. All patients provided their consent to participate to the study as per local regulations. Data were remotely monitored regularly during the study and each site was visited at least once by a monitoring Clinical Research Assistant. Monthly safety reconciliation with the sponsor safety database were performed and annual data reviews were organized. This study was conducted in accordance with the ethical principles of the Declaration of Helsinki  [18] , the principles of the International Society for Pharmacoepidemiology guidelines for Good Pharmacoepidemiology Practice  [19] , and in compliance with the General Data Protection Regulation (GDPR)  [20].