dataesr/scientific-paragraphs-categorization huggingface dataset:
1 and MAM-850. 2, are located at the peak of the LAE overdensity, possibly pinpointing the core of the protocluster and multiple mergers/interactions (e. g. ,  Miller et al. 2018). The association of the discovered submillimeter sources with BOSS1441 needs however a spectroscopic confirmation. 2. the continuum source at the center of the ELAN MAMMOTH-1, source B  (Cai et al. 2017b) , is associated to a strong detection at 850 µm, MAM-850. 14, with flux density of f 850 = 4. 6 ± 0. 9 mJy ( f Deboosted 850 = 2. 8 ± 1. 0 mJy) and a 3σ upper limit of f 450 < 16. 6 mJy at 450 µm. Together with the data from the literature, the SED of source B agrees with a strongly starbursting galaxy hosting an obscured AGN, and having a FIR luminosity of L SF FIR = 2. 4 +7. 4 -2. 1 × 10 12 L. Source B is thus an ULIRG with a star-formation rate of SFR = 400 +1300 -400 M yr -1 assuming the classical Kennicutt (1998) calibration.
The hot dust contribution allows a better fit to the data. F. Arrigoni Battaia et al. : Overdensity of submillimeter galaxies around the z 2. 3 MAMMOTH-1 nebula c This value is the 95% confidence brightness upper limit from the AllWise Source Catalog. d Detection limit of the FIRST catalog at source position. A. 1) are from AllWISE source catalog  (Wright et al. 2010; orange) , our SCUBA-2 observations (magenta), and the FIRST survey  (Becker et al. 1994; green). We show the SED of M82  (Silva et al. 1998 ; black line), of the average ALESS SMG (dashed brown line), and the average ALESS SMG with A V < 1, and A V ≥ 3  (da Cunha et al. 2015; yellow) , best fitting only our SCUBA-2 data assuming z = 2. 32.
Acknowledgements. We thank the referee  Yuichi Matsuda  for his careful read of the manuscript. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The  National Astronomical Observatory of Japan ;  Academia Sinica Institute of Astronomy and Astrophysics ; the  Korea Astronomy and Space Science Institute ; the  Operation, Maintenance and Upgrading Fund for Astronomical Telescopes and Facility Instruments , budgeted from the  Ministry of Finance (MOF) of China  and administrated by the  Chinese Academy of Sciences (CAS) , as well as the  National Key R&D Program of China  (No. 2017YFA0402700 ). Additional funding support is provided by the  Science and Technology Facilities Council  of the United Kingdom and participating universities in the United Kingdom and  Canada.
Y. Y. 's research was supported by  Basic Science Research Program  through the  National Research Foundation of Korea (NRF)  funded by the  Ministry of Science, ICT & Future Planning  ( NRF-2016R1C1B2007782 ). The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of  Mauna Kea  has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
Hybrid computing to negate embedding costs Although hybrid approaches have also looked at improving the robustness and quality of embeddings  [31] , to the best of our knowledge such approaches have not been used to try and mitigate the cost of performing the embedding itself, which, we recall, is often prohibitive to any speedup. In this paper we propose a general hybrid approach to tackle precisely this problem. In particular we aim to show how a raw speedup that is negated by the embedding time (i. e. , in particular when t proc < T C but T Q > T C ) can nonetheless be exploited to give a practical speedup to certain computational problems. Our approach is motivated by another hybrid quantum-classical algorithmic proposal which predates the rise of quantum annealing and was introduced with the aim of exploiting Grover's algorithm-the wellknown black-box algorithm for quantum unordered database search  [15] -in practical applications  [22].
Procedures All medical and nursing records were reviewed. Demographics data (sex, age, weight, height), race aimed at assessing the influence of the type of metabolism (slow, medium, fast), clinical data (medical and neurological history, allergies, cancer type and site of the primary tumour), and drug exposure (thiotepa and drugs administered concomitantly) from admission to hospital until the day of ASCT were collected for each patient. To assess the impact of potential organic disturbances, biological monitoring of renal and hepatic function from admission to hospital until the day of ASCT was taken into account. Biological monitoring of renal function took into account blood urea and creatinine. The glomerular filtration rate (GFR) was estimated using the Schwartz formula  [23]. Monitoring of liver function took into account transaminases (SGOT, SGPT), gamma-GT, bilirubin, and serum protein.
We identified K. pneumoniae strains that exhibited an AmpC phenotype in the absence of PCR-detectable ampC genes. Furthermore, we used genome sequencing and identified other β-lactamase genes that could possibly explain the resistance phenotype of these strains. A total of 257 K. pneumoniae strains were collected from 17 hospitals in Korea. No ethical clearance was required for this study since patient data were not included and the source of the strains was anonymous. The strains were collected in 2014 and were stored at -80°C until use. Before use, the strains were subcultured on MacConkey agar and were deposited in the central laboratory (Seoul St. Mary's Hospital). Of the total isolates, www. annlabmed. org https://doi. org/10. 3343/alm. 2018. 38. 4. 367 39 were intermediately resistant or resistant to cefoxitin, and 31 of these expressed a plasmid-mediated DHA-type AmpC β-lactamase; this enzyme confers resistance to cephamycins and oxyimino-cephalosporins and is most likely characterized by inducible production.
DNA was extracted using the Mo Bio kit (QIAGEN, Hilden, Germany) and sequenced using the Illumina MiSeq system with a 2 × 150 bp approach and a minimum coverage of 100 ×. The reads were assembled using A5-miseq, and the scaffolding was performed using SSPACE. The ResFinder online tool (https:// cge. cbs. dtu. dk/services/ResFinder/) was used to assess the presence of (acquired) antimicrobial resistance genes, while the Bio-Numerics 7 software (Applied Maths, Sint-Martens-Latem, Belgium) was used to define microbial multi locus sequence types (MLST). The same tool was used to assess mutations in the ompK35 and ompK36 genes, which encode porins important for antibiotic uptake; mutation of these genes can lead to impermeability to several types of β-lactam drugs  [5]. The five ampC-PCR-negative K.
Data and methodology The analysis presented builds on a database of references in the oldest journals totally dedicated to the field of OM, which we refer to as our "base" journals: Journal of Operations Management  (JOM, initiated in 1980) , International Journal of Operations and Production Management (IJOPM, also initiated in 1980), and Production and Operations Management (POM, initiated in 1992), extending through the decades of the 1980s, the 1990s, and the 2000s. We assumed that all the articles in these three journals were purely OM articles, thereby avoiding having to decide whether articles from multi-discipline journals like Management Science and Decision Sciences were OM articles or not. We also wanted to be sure to include all forms of OM articles, so we selected JOM for its empirical articles, POM for its more quantitative articles, and IJOPM for its international and practice-oriented articles.
As long as we covered all forms of OM articles, and only OM articles, we felt it was unnecessary to include other journals in the base to reveal the flows of knowledge over the three decades. We primarily relied upon the ISI's Social Science Citation Index (SSCI) for our data but supplemented with other sources when particular issues of our base journals were not listed. Since we were only interested in research journals, we excluded books and any other nonjournal references. We employed MATLAB (MATLAB, 2012), Bibexcel  (Persson et al. , 2009) , UCINET/NetDraw  (Borgatti, 2002; Borgatti et al. , 2012) , and Excel for text manipulation, data preparation/manipulation, and visualization of the networks. As noted earlier, we use citation analysis of the set of journals identified as most important to the field of OM over the three decades 1980-2009 to conduct our study.
Acknowledgments We are grateful to  Celine Degrande  and to  Alexander Savin  for discussions. This work was funded in part by a bilateral agreement, sponsored in Portugal by  FCT -Fundação para a Ciência e a Tecnologia, under program  HIGGS  E SABOR FCT 2015/2016 -PROC 441. 00 FRANCA , and sponsored in France by the  Partenariats Hubert Curien programme PESSOA  under project  33733UH. A. F is partially supported by the  ERC  Advanced Grant Higgs@LHC and by the  European Union 's  Horizon 2020 research and innovation programme  under the  Marie Sklodowska-Curie  grant agreements No  690575  and No  674896. J. C. R. and J. P. S. are supported in part by the  Portuguese FCT  under contract No. UID/FIS/00777/2013.
Our results lend support to higher Φ determinations at z=6 than usually reported. The selection and combined analysis of different galaxy samples at z≥7 will be presented in a forthcoming paper, as well as the evolution of the UV luminosity function between z∼ 4. 5 and 9. WUDS is intended to provide a robust database in the near-IR for the selection of targets for detailed spectroscopic studies, in particular for the EMIR/GTC GOYA Survey.
Sect. 3 is devoted to data processing and the construction of the image dataset. Sect. 4 presents the extraction of sources and the construction of photometric catalogs. The characterization of the photometric survey is given in Sect. 5, including the determination of the depth and completeness of the survey, and number counts. Sect. 6 presents the quality achieved in the computation of photometric redshifts up to z∼1. 5, and the global properties of the galaxy population at low-z. Sect. 7 presents the selection of candidates in the redshift interval z∼  [4. 5 -7]. The properties of these samples of galaxies are studied, in particular the luminosity function (LF), and compared to previous findings. Conclusions and perspectives are given in Sect. 8. Throughout this paper, a concordance cosmology is adopted, with Ω Λ = 0.
7, Ω m = 0. 3 and H 0 = 70 km s -1 M pc -1. All magnitudes are given in the AB system  (Oke & Gunn 1983). Table  1  presents the conversion values between Vega and AB systems for our photometric dataset. Data products described in this paper are available through the following website: http: //wuds. irap. omp. eu/.
7. 1). We have also extended the search for high-z candidates in Sect. 7 to an adjacent area of ∼1000 arcmin 2 in the CFHTLS-D3 field, extracted from the WIRDS Survey in this area  (Bielby et al. 2012) , and observed only in J, H and K s bands. This dataset is referenced as "WIRDS" in Table  1 , and corresponds to the area delimited in green in Fig. 2. The seeing in each individual image was determined as the median FWHM of four reference stars. The mean and standard deviation values measured across the sample presented in Table  2  for the different filters are : 0. 66 ± 0. 09 (Y), 0. 58 ± 0. 07 (J), 0. 57 ± 0. 16 (H), and 0. 54 ± 0. 06 (K s ). The seeing distribution in Y and H is a little wider than in the two other filters, leading to a larger rms. In fact, more than ∼90% of the sample has a FWHM better than 0.
75 in these filters, leading to a mean and standard deviation of 0. 65 ± 0. 08 and 0. 53 ± 0. 06 in Y and H respectively when excluding these extreme values. The seeing of individual images was included in the weighting process when building the final stacks, as explained in Sect. 3. Depending on the filter, the averaged seeing values achieved on the stacked images typically range between 0. 55 and 0. 63 , as seen in Table  1. Table  1  summarizes the properties of the photometric dataset used in this paper, when combining the whole WUDS, WIRDS and CFHTLS-D3 observations in this field. The total effective area covered by this survey with >50% and >75% of the total exposure time is also given in Tab. 1 for the different bands. The maximum intersection with all nine filter-bands and >50% of exposure time is limited by the Y-band (i.
The efficiency of this process strongly depends on the dithering strategy, that is using larger offset-paths provides better results. 3. Astrometry and photometric calibration (standard preprocessing; see below). 4. First image stack. Images were sky-subtracted using the previous "local" backgrounds and then registered and combined together into a first stack. 5. Object mask. Sources were detected with SExtractor  (Bertin & Arnouts 1996)  in the first image stacks in order to create an object mask. 6. Second sky-subtraction. The second step was repeated using the object mask to reject pixels located on detected sources when computing the sky value. A second sky-subtraction was applied to the data using these new backgrounds. A&A proofs: manuscript no. WUDS_paper1_accepted_Arxiv Automatic preprocessing at CFHT included steps from 1 to 3 above.
It is worth to note the highly time-consuming process of manual quality-assessment of individual images (using QualityFITS), given the huge number of images in the stacks (∼560 in Y, ∼1420 in J, ∼3670 in H and ∼1920 in K s ), and the fact that the whole process was performed twice. Also weight maps were obtained during this phase, using the WeightWatcher software developed by  Marmo & Bertin (2008). Astrometric calibration was performed with SCAMP 6. The accuracy of internal astrometry ranges between 0. 02 and 0. 035 at 1σ level for all filters. Images were combined using the weighting scheme given in point 7 above, with the SWARP software. The combination was a sigma-clipped mean with a 3σ rejection threshold. The final stacks were matched to the CFHTLS-D3 T0006 images and pixel scale (0.
186 ). The astrometric solution was computed by SCAMP including internal constraints (overlapping frames) and external references (CFHTLS-D3 objects catalog). The accuracy of astrometry in this case is typically σ=0. 05 , with a systematic offset of less than 0. 005. Regarding the accuracy achieved in the determination of ZPs, it ranges from 0. 021 to 0. 023 magnitudes in J, H and K s bands in the WUDS survey alone (it is between 0. 03 and 0. 04 when combining WUDS and WIRDS data on the whole field). It is 0. 067 magnitudes in the Y-band for WUDS (0. 075 for WUDS + WIRDS) due to indirect recalibration. These estimates are based the comparison between individual detections of several 10 4 stars in each band.
WUDS Multiband Catalogs This Section presents the extraction of sources and the construction of the photometric catalogs, publicly available at http: //wuds. irap. omp. eu/ To built the final catalogs, WUDS data were combined with public CFHTLS-Deep data on this field, obtained through five bands in the optical domain, namely u * , g, r, i, and z. Therefore, WUDS catalogs include nine filter bands with full wavelength coverage between ∼0. 35 and 2. 3 µm. Hereafter, we refer to this ensemble as WUDS (or WUDS+WIRDS) data. Two near-IR-selected catalogs were built for the needs of this project. The first one (hereafter C1) is based on the Y + J detection image. It was primarily intended to be used for the identification of i and z dropouts in this paper (i. e. , z∼6 and z∼7 candidates respectively).
The second one (C2) is based on the H + K s detection image, as it was intended to be used for the identification of Y and J dropouts (i. e. , z∼7-11 candidates). This later selection will be presented in Paper II. We also computed a catalog based on the i + z detection image to be used for the identification of r-dropouts (i. e. , z∼5 candidates) in addition to the near-IR selected samples. All these catalogs are used in Sect. 7 for the selection of galaxies at z∼  [4. 5 -7]. Sources were detected with the SExtractor package version 2. 8  (Bertin & Arnouts 1996) , using the weight maps mentioned in Sect. 3. Extraction was performed using a very low detection threshold of 0. 8 sigma (SExtractor definition) for a minimum number of four pixels above the threshold, in order to optimize the detection of compact and faint sources.
Completeness and depth The completeness of the WUDS survey has been estimated through simulations of stars and galaxies based on the STUFF and SKYMAKER softwares. Simulated samples of stars/galaxies have been randomly added to real images after masking of objects detected in the stacks, with the appropriate PSF convolution. These sources are then detected with SExtractor, using the same extraction parameters as for science images, therefore the completeness levels are directly obtained as a function of magnitude in the different bands. These values are reported in Tab. 1. The difference between the completeness levels in regions with the highest exposure time (>90% ) and regions with smaller exposure times, for instance regions with >70% and >50% exposure time, is typically 0. 08 and 0. 13 magnitudes worse respectively.
Number counts Galaxy number counts have been obtained in the four bands of WUDS and compared to the literature, as a consistency check for the calibration of the present data set. The separation between stars and galaxies is based on the SExtractor stellarity index  7. Since the reliability of this index for galaxies diminishes toward the faintest magnitudes, we have applied this selection up to a S/N∼10 in the detection images, with galaxies selected by imposing a SExtractor stellarity index <0. 9. These threshold values are based on straightforward simulations, using the same approach as for the determination of the completeness levels in Sect. 5. 1. Figure  5  displays the resulting number counts in the four bands of WUDS, as compared to previous findings from the literature (e. g. ,  Cristóbal-Hornillos et al.
Photometric redshifts Photometric redshifts have been computed with the version v12 of the public code Hyperz (New-Hyperz 8  ), originally developped by  Bolzonella et al. (2000). This method is based on the fitting of the photometric Spectral Energy Distributions (SED) of galaxies. The accuracy of photometric redshifts (z phot ) is used here as a consistency check for the calibration of the whole data set, as well as for the characterization of the different high-z samples in WUDS. The template library used in this paper includes 14 templates: eight evolutionary synthetic SEDs computed with the last version of the Bruzual & Charlot code  (Bruzual & Charlot 2003) , with Chabrier IMF  (Chabrier 2003)  and solar metallicity, matching the observed colors of local galaxies from E to Im types (namely a delta burst -SSP-, a constant star-forming system, and six τ-models with exponentially decaying SFR); a set of four empirical SEDs compiled by  Coleman et al.
9. Results based on H + K detection are the same as for the Y + J-based catalog. We have also considered the 3828 galaxies extracted form the i + z detection image. Figure  6  displays the comparison between photometric and spectroscopic redshifts based on the H + K detection image across the entire field, and the same restricted to the WUDS area, that is with photometry including Y-band data and 1651 spectroscopic sources. Table  4  presents a summary of the z phot quality achieved in this survey based on the usual statistical indicators, namely σ(∆z/(1 + z)), σ(|∆z/(1 + z)|), the median of (∆z/(1 + z)), the normalized median absolute deviation (defined as σ z,MAD = 1. 48 × median (|∆z|/(1 + z)), which is less sensitive to outliers), and the percentage of outliers. These results are based on SExtractor MAG_AUTO magnitudes.
Selection Criteria We have used two different methods to select high-z galaxies. The first one is the usual three-band dropout technique applied to a combination of WUDS data and deep optical data from the CFHTLS-D3, that is a photometric catalog including the nine filter-bands (ugrizY JHK s ). Different redshift intervals have been defined using an appropriate combination of filters. The second method is based on pure photometric redshifts and probability distributions, taking full advantage from the wide wavelength coverage. In all cases, a S/N higher than 5σ was requested in the filters encompassing the rest-frame UV, irrespective of the detection image, together with a non-detection (<2σ level) in all filters bluewards from the Lyman limit. In this respect, CFHTLS-D3 data are particularly useful to provide robust non-detection constraints for candidates at z∼  [4.
Conclusions and Perspectives In this paper we have introduced and characterized the WIRCam Ultra Deep Survey (WUDS), a 4-band near-IR photometric sur- Notes. ∆Φ includes the 68% (1σ) confidence level intervals from the bootstrap procedure, Poisson uncertainties and field-to-field variance. Notes. ∆Φ includes the 68% (1σ) confidence level intervals from the bootstrap procedure, Poisson uncertainties and field-to-field variance. vey covering ∼400 arcmin 2 on the CFHTLS-D3 field (Groth Strip). This public survey was specifically tailored to set strong constraints on the cosmic SFR and the UV luminosity function brighter or around L in the z∼6-10 domain. Regarding the properties of the data at low-z, and according to the estimates presented in this article, WUDS should allow the users to detect early-type galaxies with stellar masses down to log(M /M )>10.
5±1. 0, and late-type galaxies down to log(M /M )>9. 9±0. 60 up to z∼3. 5. The quality of the photometric redshifts achieved for the WUDS survey is comparable to the one obtained by other large surveys when using a similar number of filters and a similar depth. As part of this effort, we have focused in this article on the selection of galaxy samples at z∼ [4. 5 -7] and the determination of the UV LF at z=5 and z=6, taking advantage from the deep optical data available from the CFHTLS-Deep Survey. We have also extended the research to an adjacent shallower area of ∼1000 arcmin 2 extracted from the WIRDS Survey, and observed in three near-IR bands. Using two different approaches, the classical LBG color-selection technique and photometric redshifts blindly applied to dropout samples, we have selected high-z galaxies and computed the UV LF.
At z=5, the combined determination of M and Φ is more accurate then previous results due to a better statistics in the intermediate-luminosity regime. The evolution in the UV LF between z=5 and z=6 is consistent with a small dimming in both Φ and L. These results are consistent with previous findings in terms of the M and Φ values, knowing that WUDS covers a particularly interesting interval at intermediate luminosities. The selection and combined analysis of different galaxy samples at z≥7 will be presented in a forthcoming paper, as well as the evolution of the UV luminosity function between z∼ 4. 5 and 9 (Laporte et al. , submitted to A & A, Paper II). Photo-metric data and catalogs will be set publicly available at the http://wuds. irap. omp. eu/ web site. WUDS is intended to provide a robust database in the near-IR for the selection of targets for the Galaxy Origins and Young Assembly (GOYA) Survey.
Acknowledgements. Part of this work was supported by the  French CNRS , the  French Programme National de Cosmologie et Galaxies (PNCG)  of  CNRS/INSU  with  INP  and  IN2P3 , co-funded by  CEA  and  CNES. We acknowledge support from the  Spanish Programa Nacional de Astronomía y Astrofísica  under grant  AYA 2006-02358  and the  Swiss National Science Foundation. Partially funded by the  Spanish MEC  under the  Consolider-Ingenio 2010 Program  grant  CSD2006-00070 : First Science with the GTC (http://www. iac. es/consolider-ingenio-gtc/). This work recieved support from  Agence Nationale de  la recherche bearing the reference  ANR-09-BLAN-0234 , and from the  ECOS SUD Program   C16U02. This work has been carried out thanks to the support of the  OCEVU Labex  ( ANR-11-LABX-0060 ) and the A* MIDEX  project ( ANR-11-IDEX-0001-02 ) funded by the " Investissements d'Avenir" French government program  managed by the  ANR.