dataesr/scientific-paragraphs-categorization huggingface dataset:
By heavily relying on visual aids and dynamic layouts, we hope to propose a system that is both simple to learn and to use, even without having read the online manual in detail. Data analysis has been streamlined and made more efficient by automating many of the steps taken during database verification, ultimately providing stronger control over the quality of datasets, and by providing tools for the production of summary tables and statistical analyses. We have routinely used TIPZOO-FMP on a relatively inexpensive second-hand Windows tablet (Lenovo ThinkPad 10) for the analysis of several Middle Palaeolithic sites excavated in southwestern France (n = 6). In our experience, data entry and analysis have been considerably faster with TIPZOO, but no quantitative estimation of the time saved is yet available.
Initial tests with other tablets have proven successful, and several Master's and PhD students from the University of Toulouse -Jean Jaurès are now using TIPZOO for their analyses. TIPZOO is a work in progress, developed over several years, and therefore may have some issues and bugs, but with user and community feedback and subsequent updates, the tool could easily be debugged and improved. New features will also be integrated, such as a better graphical interface for recording use-wear classes, additional reference datasets in TIPZOO-R and TIPZOO-QGIS (currently datasets are focused quite heavily on reindeer), modules that would allow the integration of inter-linked data sets (i. e. other data obtained on faunal remains such as stable isotopes, tooth microwear, cementum analysis, morphometrics, etc.
Conclusion TIPZOO is intended to make data entry, analysis, and visualization in Palaeolithic zooarchaeology easier, faster, and more reliable. It provides tools to effectively implement recently published complex coding systems and better control for undesirable intra-and inter-analyst variability, contributing therefore to greater reproducibility and reliability in data collection, and allows analysts to save time by automating several of the steps involved in data entry and analysis. This should facilitate comparisons of distinct zooarchaeological studies, as well as free up time for zooarchaeologists so that they can concentrate on interpretations rather than data entry and initial analysis. Furthermore, the automatic export of interconnected faunal and spatial data should facilitate three-dimensional spatial analyses, an analytical practice that, despite its fundamental importance, is not sufficiently widespread (see  Discamps et al.
Acknowledgements My deepest thanks go to  E. Bernard ,  E. Capdepon ,  Ch. Dancette  and  M. -C. Soulier , whose critical evaluation of some of TIPZOO-FMP features helped improve it. Part of the images used in TIPZOO-FMP were modified from original diagrams by others (see Pales and Lambert, 1981;Netter, 1989; Castel, 1999, p. 47; Morin, 2004, p. 125;Morin et al. , 2017Morin et al. , , 2019;;Soulier and Costamagno, 2017;Costamagno and Soulier, 2019), and its touch keypad is a modified version of the scripts made available on the web by  Stacy Chamblee  (Chamblee, n. d. ). The reindeer skeleton outline used in TIPZOO-QGIS was drawn by  C. Beauval  and  M. Coutureau , modifying initial drawings by  Cl. Bellier  and  P. Semal. Editing  of the English for this article was conducted by  L. Anderson.
5 mag (at 10σ) in the V IS band, and 24 mag (at 5σ) in each of the Y, J, and H bands  (Laureijs et al. 2011). We associate the Euclid imaging with two possible ground-based visible imaging datasets, which correspond to two limiting cases for photo-z estimation performance. -DES/Euclid. As a demonstration of photo-z performance when combining Euclid with a considerably shallower photometric dataset, we combine our Euclid photometry with that from DES  (Abbott et al. 2018). DES imaging is taken in the g, r, i, and z filters, at 10σ sensitivities of  24. 33, 24. 08, 23. 44, and 22. 69  respectively. -LSST/Euclid. As a demonstration of photo-z performance when combining Euclid with a considerably deeper photometric dataset, we combine our Euclid photometry with that from the Vera C. Rubin Observatory LSST  (LSST Science Collaboration et al.
2019; Guglielmo et al. 2020). Such sample results from a combination of spectra coming from numerous instruments installed on 8-meter class telescopes (e. g. VIMOS, FORS2, KMOS, DEIMOS, LRIS, MOSFIRE) including data from previous spectroscopic surveys (e. g. Lilly et al. 2007; Le Fevre et al. 2015; Kashino et al. 2019 ). The most robust spec-z acquired on the Euclid Deep fields with the NISP instrument will be included. Given the diversity of observations, a careful assessment of the sample purity is necessary to limit the fraction of failures below 0. 2%. Encouragingly,  Masters et al. (2019)  do not find any redshift failures within the 72 C3R2 spec-z with duplicated observations. Nonetheless, a larger sample of confirmed spectra is necessary to demonstrate that less than 0. 2% of spectroscopic redshift measurements suffer from catastrophic failure.
This population contaminates preferentially specific tomographic bins. In particular, stars may bias the mean redshift towards higher values, for both direct calibration and debiased zPDF methods. A morphological selection based on VIS highresolution images, combined with a color selection including near-infrared photometry (e. g. Daddi et al. 2004) , is efficient to isolate them  (Fotopoulou & Paltani 2018). A minimal contamination could bias the mean redshift at a level similar to the one discussed in Sect. 5. 1. Nonetheless, future simulations need to include stellar and AGN populations to better assess the level of contamination of the galaxy sample and its impact on the Euclid requirement. Finally,  Laigle et al. (2019)  show that the fraction of outliers in Horizon-AGN remains underestimated in comparison to real dataset.
-Imaging depth is the primary factor in determining the effectiveness of the debiasing technique. We reach the Euclid requirement when combining Euclid and LSST ground-based images. -Insufficient imaging depth can be compensated by selecting well peaked zPDF, but introduces considerable losses to the target sample number density. A balance should therefore be established between the accuracy of z and the statistical signal of the cosmic shear analysis. We test the two approaches on real data sets from COS-MOS and KiDS+VIKING-450, and confirm that a high signalto-noise in the photometry is essential for an accurate estimate of z using the debiased zPDF approach. In the less favourable case (KiDS+VIKING-450), where the photometric sample and a spec-z target sample are approximately of equal depth, we reach an accuracy around 0.
LEGA-C target sample. We select a spectroscopic sample as robust as possible, to ensure that the uncertainty on the mean redshift of the target sample (considered as the truth) is known with an accuracy better than 0. 002. The LEGA-C spectroscopic survey in the COSMOS field provides such a target sample. This spectroscopic sample is built using the high-resolution (R = 3000) mode of VIMOS spectrograph, targeting galaxies at 0. 6 < z < 1 selected in the K s -band to have a stellar mass M > 10 10 M. Given the resolution and the SN reached by the LEGA-C spectra (with 20 h of exposure per spectrum), and the numerous absorption/emission lines detected, we can safely assume that this sample does not include any catastrophic spectroscopic failures. We match the LEGA-C Data Release 2 galaxies  (Straatman et al.
Acknowledgements. We thank the  OU-PHZ of Euclid  for all the useful discussions along these years. OI acknowledges the funding of the  French Agence Nationale de la Recherche  for the project ' SAGACE '. NM acknowledges support from a  CNES  fellowship. H. Hildebrandt is supported by a Heisenberg grant of the  Deutsche Forschungsgemeinschaft  ( Hi 1495/5-1 ) as well as an  ERC Consolidator Grant  (No. 770935 ). A. H. Wright is supported by the  ERC   Consolidator Grant  (No. 770935 ). This work relied on the  HPC resources of CINES (Jade)  under the allocation 2013047012 and c2014047012 made by  GENCI  and on the  Horizon Cluster hosted by Institut d'Astrophysique de Paris. ID acknowledges that he received funding from the  European Union 's  Horizon 2020 research and innovation programme  under the  Marie Skłodowska-Curie  grant agreement No.
In contrast, the ESTER code deduces the rotation profile in a self-consistent way when constructing stellar models. Hence, it is important to study pulsation modes in such models. One of the first signatures of rotation on stellar pulsations is rotational splittings, the frequency differences between consecutive modes with the same radial order and harmonic degree but different azimuthal orders. At slow rotation rates, rotational splittings can be used to invert 1D or 2D rotation profiles using a first-order perturbative approach (e. g. Deheuvels et al. 2014 , Schou et al. 1998 , Thompson et al. 2003). At high rotation rates, higher-order effects come into play and must be addressed before meaningful information on the rotation profile can be deduced (e. g. Soufi et al. 1998 , Suárez et al.
g. Pápics et al. 2017). A similar study is needed for acoustic modes in rapidly rotating stars. In order to address the above questions, we investigate lowdegree acoustic modes in rapidly rotating stellar models from the ESTER code. One of the advantages of the ESTER code is its multi-domain spectral approach, ideal for introducing discontinuities while retaining a high numerical accuracy. The pulsation modes are calculated using a multi-domain spectral version of the Two-dimensional Oscillation Program (TOP,  Reese et al. 2006 Reese et al. , 2009)). The article is organised as follows: the following section describes stellar models based on the ESTER code. This is then followed by a description of the pulsation calculations as well as the variational principle, with a particular emphasis on the effects of discontinuities.
Stellar models based on the ESTER code The aim of the ESTER project is to produce and evolve selfconsistent stellar models of rapidly rotating stars. Consequently, a fully 2D approach is used in order to solve the relevant fluid equations while taking into account energy conservation when modelling the stationary structure of the star. This leads to centrifugal deformation of the stellar structure, as well as more subtle effects, namely differential rotation and meridional circulation, resulting from baroclinicity. Consequently, the rotation profile depends on both the radial coordinate and colatitude, and the isobars, isochores, and isotherms are distinct. In terms of microphysics, it is possible to apply various equations of state (EOS) in ESTER. These include: the ideal gas law with or without radiation pressure, the OPAL EOS  (Rogers & Nayfonov 2002) , and FreeEOS 1   (Irwin 2012).
In what follows, we applied the ideal gas law (without radiation pressure) in the discontinuous models (see below) and one of the continuous models, in order to avoid introducing numerical errors coming from a tabulated EOS, and the OPAL EOS in the other continuous model for the sake of realism. In terms of opacities, there are two options currently implemented: Kramer's opacities and OPAL opacities  (Iglesias & Rogers 1996). We used Kramer's opacities in conjunction with the ideal gas law to rely entirely on analytical expressions thus reducing numerical errors, and OPAL opacities with the OPAL EOS for the sake of realism and consistency. Models with Kramer's opacity have significantly larger radii and hence lower mean densities. Currently, the ESTER code has some limitations. Firstly, it is unable to simulate convective envelopes.
Indeed, applying a strong entropy diffusion as is done in the convective core is too approximate for the envelope. Various numerical difficulties have so far prevented the code from converging to a convective solution in such regions. Accordingly, ESTER is currently not suitable for stars with masses below ∼ 1. 6 M ⊙. Secondly, the ESTER code is unable to simulate time evolution using a full chain of nuclear reactions. However, it is possible to alter the core composition in order to mimic the effects of stellar evolution or to include a rudimentary implementation of hydrogen combustion. From a numerical point of view, the star is divided into multiple domains in the radial direction. There are two main reasons for doing this. First, this allows us to overcome the limitations inherent to using a spectral approach with its imposed collocation grid.
Pulsation calculations The pulsation modes are calculated using the Two-dimensional Oscillation Program (TOP,  Reese et al. 2006 Reese et al. , 2009)). This program fully takes into account the centrifugal deformation and has been set up to apply a multi-domain spectral approach, in accordance with the models from ESTER. The next subsections describe the set of pulsation equations, the interface conditions that apply between different domains, the boundary conditions, and the numerical approach.
Interface conditions Given that ESTER models are calculated over multiple domains, interface conditions are needed to describe the relation between various quantities on either side of the different boundaries. Furthermore, care is needed when expressing these conditions given that some of the models contain discontinuities. The first condition is simply that the fluid domain is continuous. In other words, the deformation of the boundary must be the same on either side. This yields the following first order expression: ξ -• n = ξ + • n, (7) where n is the normal to the unperturbed surface, and the subscripts '-' and '+' denote quantities below and above the boundary. This condition does allow the fluid to 'slip' along the boundary. A more detailed derivation is given in App. A. 1. A second condition is that the pressure remains continuous across the perturbed boundary.
Acknowledgements. The authors thank  François Lignières ,  Vincent Prat , and  Pierre Houdayer  for useful and interesting discussions. DRR acknowledges the support of the  French Agence Nationale de la Recherche (ANR)  to the  ESRR project  under grant  ANR-16-CE31-0007  as well as financial support from the  Programme National de Physique Stellaire (PNPS)  of the  CNRS/INSU  cofunded by the  CEA  and the  CNES. GMM  acknowledges funding by the  STFC  consolidated grant  ST/R000603/1. DRR, GMM, MR, BP benefited from the hospitality of  ISSI  as part of the SoFAR team early on in 2018 and 2019. This work was granted access to the  HPC resources of IDRIS  under the allocation 2011-99992 made by  GENCI  (" Grand Equipement National de Calcul Intensif ") and to HPC resources of Calmip under project  P0107.
The CORE and CORE-extension projects With the goal to study the fragmentation, disk, outflow, and chemical properties of high-mass star formation, we have embarked on the NOEMA large program CORE, which observes 20 high-mass star-forming regions at a high spatial resolution (0. 3 -0. 4 ) in the 1. 3 mm line and continuum emission. The sample was selected based on being mainly in the evolutionary stage of high-mass protostellar objects (HMPOs), also known as MYSOs (massive young stellar objects). An overview and more details about the program can be found in  Beuther et al. (2018)   1. To broaden the scope of CORE to even younger evolutionary stages, we conducted the CORE-extension part of the project, observing two much younger regions (ISOSS22478 and ISOSS23053) also at high spatial resolution and with a similar 1 See also http://www.
The CORE-extension technical setup While the original CORE program utilized the old receiver and backend system with only a ∼4 GHz wide band in a single sideband between 217. 167 and 220. 834 GHz, the upgraded NOEMA now allows us to use, in dual-polarization, a much broader bandwidth in the double-sideband mode with 7. 8 GHz in each sideband. Specifically, we are covering the frequency ranges from ∼213. 3 to ∼221. 1 GHz as well as from ∼228. 8 to ∼236. 6 GHz. This spectral setup covers a multitude of strong spectral lines from many important molecules, for instance, deuterated species such as DCO + , DNC, or N 2 D + , the temperature tracers H 2 CO or CH 3 CN, CO, and its isotopologues 13 CO and C 18 O, shock tracers like SiO or larger molecules such as CH 3 OH or HCCCH. While the entire bandpass is covered at low spectral resolution (2 MHz corresponding to ∼2.
Calibration and imaging of the data was performed with the clic and mapping software of the gildas package 2. To achieve optimal imaging quality for these mosaics, we applied natural weighting during the imaging process. To create the continuum data, only the line-free parts of the spectrum were used. Since the regions are comparably line-poor, only small parts of the entire bandpass (Sect. 2. 2) had to be excluded. Specifically, we excluded 280 MHz and 1800 MHz of the entire bandpass of ∼15 600 MHz for ISOSS22478 and ISOSS23053, respectively. For the 1. 3 mm continuum data, this resulted in synthesized beams of 0. 92 × 0. 73 (P. A. 51 deg) and 0. 84 × 0. 74 (P. A. 67 deg) for ISOSS22478 and ISOSS23053, respectively. This corresponds to approximate linear resolution elements of ∼2700 and ∼3500 au, respectively.
The last bits of information needed is the temperature of the gas and dust. For both regions several temperature estimates exist. Ragan et al. (2012)  used Herschel far-infrared data and fitted the spectral energy distributions. This resulted in average dust temperatures for ISOSS22478 and ISOSS23053 of ∼21 and ∼22 K, respectively. Both regions were also imaged with the Very Large Array in NH 3 emission, and average temperatures from these data are 13 and 18 K for the two regions, respectively  (Bihr et al. 2015). Within this new NOEMA dataset we also have the H 2 CO lines around 218 GHz that can be used as thermometer as well  (Mangum & Wootten 1993). Details about the temperature derivation and structure are presented in Sect. 4. 2. Relevant for our mass and column density analysis here is that for ISOSS22478 the temperatures range approximately from values around 10 K to roughly 50 K (Table  2 ).
4. Relations of core parameters. The top panels show the peak column density and mean density plotted against the mass while the bottom panels present the mean density and mass plotted against the equivalent radius. The red and blue colors always show the data for ISOSS22478 and ISOSS23053, respectively. The full pentagons show the results estimated assuming constant temperatures (T 20K ) whereas the crosses present the data assuming the temperatures derived from the H 2 CO line data (T H2CO ). The bottom-left panel presents as green line a fit to the data following the T H2CO approach. The bottom-right panel also presents fits to the data (green continuous lines) and lines of constant mean column density and constant mean density (dashed and dotted lines, respectively) as labeled in the plot.
2019 , 2020). In contrast to this, the mass-size relation in the T 20K approach follows a steeper relation of M ∝ r 3. 0±0. 2 , which is close to the line of constant density at 10 6 cm -3. If the two regions are separated in the T 20K approach, the mass-size relations for ISOSS22478 and ISOSS23053 have power-law dependences of r 2. 4±0. 2 and r 2. 6±0. 2 , respectively. We return to this point in Sect. 5. 1. To investigate the projected separations between cores, we employed a minimum spanning tree analysis using the astroML software package  (VanderPlas et al. 2012 ) that determines the shortest possible distances connecting each of the cores. The derived nearest-neighbor separations are shown in Fig. 5  for both regions combined, and the basic results are listed in Table  3. While projection causes the observed nearest-neighbor separations to be at their lower limits, as compared to their real separation in three dimensions, the sensitivity, and spatial resolution limits that the observation are subject to, implying that the projected nearest-neighbor separations are, rather, likely to be the upper limits.
In reality, having more cores should qualitatively reduce the real projected nearest-neighbor separations. Nevertheless, with a linear spatial resolution of approximately 2700 and 3500 au, it is interesting to note that barely any separations are found at our resolution limit. This is different in comparison to the original CORE sample of more evolved HMPOs where the nearest-neighbor histogram shows a strong peak near the resolution limit. While also for the younger ISOSS sources, we would expect that at higher spatial resolution a few of the cores are likely to split into multiple systems and, hence, some smaller separations would occur, the current data nevertheless show that we are resolving the large-scale fragmentation of the parental gas clumps well. A decrease in spatial separations during the evolution of a star-forming cluster is expected during the collapse of the gas clump.
During the collapse, the densities increase and in the classical Jeans picture, the Jeans length and the corresponding separations decrease. In that scenario, the generally larger separations of the younger ISOSS sources studied here can naturally be explained. It is interesting to note that in a study of the integral shape filament in Orion,  Kainulainen et al. (2017)  found that significant grouping of dense cores is found below scales of 17000 au (see also  Román-Zúñiga et al. 2019) , similar to what we find in Fig. 5. Kainulainen et al. (2017)  infer a second increase in source grouping below separations of 6000 au, which is not visible in our data. However, smaller-scale grouping (below our resolution limit here) was found in the original CORE data at approximately twice the spatial resolution with a peak at roughly 2000 AU  (Beuther et al.
Kinematics and temperatures of the gas We consider what the kinematics of the gas tell us about the formation processes within these two star-forming regions. To look at the dynamics in more detail, in the following we focus on the DCO + (3-2) emission that traces the gas properties at the given early evolutionary stage extremely well (e. g. ,  Gerner et al. 2015). Figures 6 and 10 present an overview of the DCO + data. The left panels show the integrated intensities and the middle and right panels present the 1st and 2nd moment maps (intensity-weighted peak velocities and velocity dispersions), respectively. These are always the merged datasets combining the NOEMA ACD configurations with the IRAM 30 m data (Sect. 3).
We return to this in Sect. 5. 2. Another important parameter is the temperature of the gas in the region. Figure  9  presents the temperature map we derived from the H 2 CO lines around 218 GHz (Table  1 ), which are a well-characterized thermometer of the interstellar gas (e. g. ,  Mangum & Wootten 1993; Rodón et al. 2012; Gieser et al. 2019 ). To derive this temperature map, we used the eXtended CASA Line Analysis Software Suite (xclass, Möller et al. 2017  3  ) tool within the casa software package  (McMullin et al. 2007). In xclass the spectra are fitted pixel by pixel taking also the optical depth into account. The mean uncertainties for the temperatures are on the order of 30%. More details on the xclass fitting are given in Gieser at al. (subm. to A& A). In addition to this, an in-depth analysis of the chemical and temperature structure of cores within the the two regions will be presented in  Gieser et al.