dataesr/scientific-paragraphs-categorization huggingface dataset:
B. Stability plots for thorium charge states We scanned the RF voltage amplitude (V RF ) and DC bias voltage applied to the ion trap electrodes (U DC ) while the RGA mass filter was only transmitting to explore the parameter space of our trap. The radial motion of the ions on the quadruple trap is governed by the Mathieu equation  [57]  and we can extract two parameters called a and q that are proportional to U DC and V RF and other constant trap parameters. The expected scaling between charge states of thorium was confirmed. The trap parameters were scanned in 20 V steps for both RF and DC fields, while the detector parameters were fixed. For each data point, we measured the corresponding ion current. The results are presented in figure  6. The amplitude (V RF ) is inferred from the amplitude of the signal generator, accounting for the amplifier and independently measured losses in the helical resonator.
The most precise data on this reaction near 2 GeV were obtained by the BABAR Collaboration  [10]. In this previous work, the e + e -→ K S K L cross section was measured up to 2. 2 GeV. Above 2 GeV, the cross section was found to be consistent with zero within the statistical uncertainties of around 20 pb. In the present work we expand the energy region of the BABAR K S K L measurement up to 2. 5 GeV. The new K S K L measurements, in conjunction with previous BABAR results for other exclusive e + e -processes, are used to investigate the nature of the structure observed by BESIII in e + e -→ K + K -. ¶ Now at: University of South Alabama, Mobile, Alabama 36688, USA * * Also at: Università di Sassari, I-07100 Sassari, Italy † † Also at: Gran Sasso Science Institute, I-67100 LAquila, Italy m(K + K - ) (GeV/c 2 ) σ(e FIG.
Acknowledgments We are grateful for the extraordinary contributions of our PEP-II colleagues in achieving the excellent luminos-ity and machine conditions that have made this work possible. The success of this project also relies critically on the expertise and dedication of the computing organizations that support BABAR. The collaborating institutions wish to thank  SLAC  for its support and the kind hospitality extended to them. This work is supported by the  US Department of Energy and National Science Foundation , the  Natural Sciences and Engineering Research Council (Canada) , the  Commissariat à l'Energie Atomique  and  Institut National de Physique Nucléaire et de Physique des Particules (France) , the  Bundesministerium für Bildung und Forschung and Deutsche Forschungsgemeinschaft (Germany) , the  Istituto Nazionale di Fisica Nucleare (Italy) , the  Foundation for Fundamental Research on Matter  (The Netherlands), the  Research Council of Norway , the  Ministry of Education and Science of the Russian Federation, Ministerio de Economía y Competitividad (Spain) , the  Science and Technology Facilities Council  ( United Kingdom ), and the  Binational Science Foundation (U.
Literature data We have compiled a sample of known CNM absorbers in the literature at z abs > 1. 5 with measurements of both metallicity and N H i. The observable quantities used in this analysis are the column densities of neutral and molecular hydrogen, the gasphase metallicity, and the thermal gas pressure. We furthermore included impact parameters for the seven absorption systems where an emission counterpart has been identified. The collected data are presented in Table  1. Only absorption systems with detections of C i and/or H 2 were included in the compilation. The metallicities were calculated based on the elements Zn and S since these do not suffer from strong dust-depletion effects  (De Cia et al. 2016).
The data presented in Figure  6  are fitted with a linear law: ∆P = a × P0 + b. The propagation rate is estimated by calculating 1 m. d(∆P) dt max. The ignition delay can be defined as the time between the beginning of the laser beam and the beginning of the pressure increase. Figures  7  and 8 , respectively, present ignition delay and propagation rates as functions of initial pressures for argon atmosphere. The propagation rate is estimated by calculating 1 𝑚. 𝑑 ∆𝑃 𝑑𝑡 𝑚𝑎𝑥 The ignition delay can be defined as the time between the beginning of the laser beam and the beginning of the pressure increase. Figures  7  and 8 , respectively, present ignition delay and propagation rates as functions of initial pressures for argon atmosphere. It is clear in Figure  7  that ignition delay decreases when initial pressure increases.
Funding: This research was funded by the  Direction Générale de l'Armement (DGA). The APC was funded by  excellence laboratory CAPRYSSES  ( ANR-11-LABX-0006-01 ). Funding: This research was funded by the  Direction Générale de l'Armement (DGA). The APC was funded by  excellence laboratory CAPRYSSES  ( ANR-11-LABX-0006-01 ).
ACKNOWLEDGMENT T. M. H. , N. S. and S. D. P. would like to acknowledge funding from  ERC-2017-STG "Life-Cycle " (757910), G. J. M. F. received funding from  Ministère de l'Education Nationale de l'Enseignement supérieur et de la Recherche. B. L. received funding by the  French National Research Agency (ANR)  through the  Programme d'Investissement d'Avenir  under contract  17-EURE-0016.
2014; Pereira-Santaella et al. 2018; Fluetsch et al. 2019, and references therein)  (1) Source name (2) Heliocentric radial velocity based on our CO(1-0) data (3), (4) Coordinates of adopted phase center. See Table  2  for the measured position of mm continuum. (5) Observation period (6) Interferometer baselines used (7) RMS sensitivity for a 20 km/s channel width (8) Beam size Notes. Results are from UV fitting a Gaussian model to the NOEMA continuum visibilities, and from fitting a Gaussian model to the ALMA continuum image. IRAS F09111-1007E is not part of our sample but detected along with IRAS F09111-1007W. (1) Source name (2), (3) Continuum position (4), (5) Uncertainties of position. These include only the formal fit errors, to which 2-5% of the beam size should be added to account for phase calibration stability  (Warmels et al.
We adopt an Ω m = 0. 3, Ω Λ = 0. 7 and H 0 = 70 km s -1 Mpc -1 cosmology, redshift-independent distances from the NASA Extragalactic Database (NED), if available, for z<0. 01 galaxies, a  Chabrier (2003)  initial mass function (IMF), a conversion for far-infrared luminosity to star formation rate (SFR) SFR = 1. 9 × 10 -10 L FIR=40-120µm as appropriate for the  Kennicutt (1998)  conversion scaled to Chabrier IMF, and L IR (8-1000 µm)/L FIR (40-120 µm)=1. 9.
ALMA observations The DEC<10 • targets were observed with the Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 4 program 2016. 1. 00177. S in late 2016 to early 2017, using between 38 and 46 antennae. Again, the CO(1-0) line was observed in a relatively compact configuration yielding an ≈2 beam in ALMA Band 3, and observational parameters are listed in Table  1. The pipelinecalibrated data were mapped using standard CASA  (McMullin et al. 2007)  procedures. Three more sources from Table  1  of  Lutz et al. (2016)  were already observed in CO(1-0) in ALMA program 2012. 1. 00306. S (PI E. Sturm) using ∼0. 5 beams. For IRAS 13120-5453, we combined our 2012. 1. 00306. S CO(1-0) data with a similar dataset from 2015. 1. 00287. S (PI K. Sliwa), in order to improve signal-to-noise. Again, we mapped the calibrated data in CASA and include the fourth target of 1 http://www.
Outflow data from the literature We have searched the literature for local galaxies with interferometric low-J CO outflow detections or limits, starting with the Notes. These parameters may differ from those published in the original references. They are reconstructed from the published information in order to be consistent with our adopted separation between line core and line wings, and our definitions for v out and R out. For consistency, they are not corrected for outflow inclination, even if this is constrained in some original references. See also Sect. 3. 2 for details. sources from Table  1  of  Lutz et al. (2016)  that we did not observe, but also including galaxies outside that parameter range. As noted in the introduction, our selection is not complete towards some of the smallest scale and least energetic outflows that were recently reported from very high resolution interferometric studies.
we use published plotted spectra to estimate v out. For 4C 12. 50 we adopt the Dasyra et al. (  2014 ) limit for CO outflow in emission but we add their outflow velocity from CO(3-2) absorption and their size estimate. For the single dish outflow detection of IRAS F17020+4544 and the low resolution interferometry of IRAS 05083+7936 we adopt a fiducial 1 kpc for R out. Our adopted homogenized literature data are summarized in Table  4. From this point on, we treat our observational results and the adopted literature values jointly and consistently, as described in Sect. 4, and call this the 'combined' sample. For literature sources observed in CO transitions other than CO(1-0), we adopt the brightness temperature ratios in Table  4  of  Bothwell et al. (2013)  for conversion to CO(1-0).
Three of the four targets studied here and the vast majority of literature results are consistent with optically thick CO emission in the outflows. But the clear detection of a high ratio (optically thin CO) for IRAS 13120-5453 is a strong warning that this is not true for all outflows, and that associated uncertainties on conversion factor and on outflow masses cannot be fully removed with the present data. Below, we follow much of the local universe molecular outflow literature and adopt α CO(1-0) = 0. 8 M / (K km s -1 pc 2 ) but note that our CO data alone do not determine a preference for this 'ULIRG' value compared to a Galactic one. For a Galactic α CO(1-0) = 4. 36 M / (K km s -1 pc 2 ), recently found to be consistent also with ULIRG gas/dust comparisons (e. g. ,  Tacconi et al. 2018) , derived outflow masses and rates would increase more than five-fold.
75 L kpc -2 , we indeed find the expected very high incidence of molecular outflows that motivated our observations. Of the 18 sources with log(Σ FIR )≥11. 75 L kpc -2 and/or close to optically thick FIR emission that are listed in Table  1  of  Lutz et al. (2016) , all but ESO 173-G015 have deep CO observations probing for outflows, from our own data or from the literature in the combined sample. Of these 17 objects, CO outflows have been detected in 13 sources while upper limits have been derived for IRAS F10173, IC 860, IRAS F14378 and NGC 7479. In several cases, these limits are conservative and a contribution of an outflow to the observed moderate velocity line wings remains a possibility. As expected, high far-infrared surface brightness galaxies are excellent hunting grounds for molecular outflows.
Conclusions We have presented new CO(1-0) interferometry from ALMA and NOEMA, probing molecular outflows in 13 local galaxies with high far-infrared surface brightness, and combined our results with literature data on local universe molecular outflows. Our main findings are: (1) Galaxies with high far-infrared surface brightness log(Σ FIR ) 11. 75 L kpc -2 show the expected high incidence of molecular outflows. 17 of 18 sources in the  Lutz et al. (2016)  sample now have suitable CO data, and 13 of these exhibit molecular outflows. Several of these nearby targets, in particular III Zw 035, are well-suited to spatially resolved studies. (2) Partly constrained by observed line ratios and by spatial structure of the best cases, we adopt in the conversion of CO observables to outflow physical properties α CO(1-0) = 0.
Acknowledgements. We thank the referee for a helpful report. This work is based on observations carried out under project numbers  S16BH ,  S17AR , and  W17CP  with the IRAM NOEMA interferometer. IRAM is supported by  INSU/CNRS (France) ,  MPG (Germany)  and  IGN (Spain). It is also based on ALMA projects ADS/JAO. ALMA# 2016. 1. 00177. S and ADS/JAO. ALMA# 2012. 1. 00306. S. ALMA is a partnership of  ESO  (representing its member states),  NSF (USA)  and  NINS (Japan) , together with  NRC (Canada) ,  MOST  and  ASIAA (Taiwan) , and  KASI (Republic of Korea) , in cooperation with the  Republic of Chile. The Joint ALMA Observatory is operated by  ESO ,  AUI/NRAO  and  NAOJ. We acknowledge reduction support support by IRAM astronomers  Miguel Montarges ,  Michael Bremer , and  Melanie Krips. We thank  Maria Drosdovskaya  and  Stefano Facchini  for help concerning emission of the NS radical.
The fraction of events with multiple candidates is found to be 0. 88% in the entire ∆M range. All candidates are included in the analysis. The resulting ∆M distribution of the signal candidates is shown in Fig. 2 , where a fit to the data is superimposed. Three narrow structures are observed in the Λ + c K - candidate spectrum. These peaking structures are not seen in the wrong-sign (WS) Λ + c K + candidates or Λ + c sideband distributions. The ∆M distribution also shows a broad structure to the left of the three narrow structures consistent with being partially reconstructed Ξ c (3055) → Σ c (2455)(→ Λ + c π)K -and Ξ c (3080) → Σ c (2455)(→ Λ + c π)K -decays , where the pion is not reconstructed. An unbinned maximum-likelihood fit, henceforth denoted the reference fit, is performed to the ∆M distribution to measure the parameters of each peak.
The fit model outlined so far does not accurately describe the data in the mass region close to the kinematic threshold, and thus an additional component is considered. There are no known decays of Σ c (2455)(→ Λ + c π)K -or Σ c (2520)(→ Λ + c π)K -which could enter the sample as partially reconstructed components at ∆M 0. It is observed that the missing component is consistent with being due to the partial reconstruction of the state that peaks around ∆M 140 MeV when it decays directly to the Λ + c K -π + final state without any intermediate resonance. The shape of these partially reconstructed decays is taken from simulated samples generated using the RapidSim package  [39]  and the yield is a free parameter in the fit. The ∆M distribution with the fit to the data superimposed is shown in Fig.
(United Kingdom), RRCKI and Yandex LLC (Russia), CSCS (Switzerland), IFIN-HH (Romania), CBPF (Brazil), PL-GRID (Poland) and OSC (USA). We are indebted to the communities behind the multiple open-source software packages on which we depend. Individual groups or members have received support from AvH Foundation (Germany); EPLANET, Marie Sk lodowska-Curie Actions and ERC (European Union); ANR, Labex P2IO and OCEVU, and Région Auvergne-Rhône-Alpes (France); Key Research Program of Frontier Sciences of CAS, CAS PIFI, and the Thousand Talents Program (China); RFBR, RSF and Yandex LLC (Russia); GVA, XuntaGal and GENCAT (Spain); the Royal Society and the Leverhulme Trust (United Kingdom).
Acknowledgements We express our gratitude to our colleagues in the CERN accelerator departments for the excellent performance of the LHC. We thank the technical and administrative staff at the LHCb institutes. We acknowledge support from  CERN  and from the national agencies:  CAPES ,  CNPq ,  FAPERJ  and  FINEP (Brazil) ;  MOST  and  NSFC (China) ;  CNRS/IN2P3  (France);  BMBF ,  DFG  and  MPG (Germany) ;  INFN (Italy) ;  NWO (Netherlands) ;  MNiSW  and  NCN (Poland) ;  MEN/IFA (Romania) ;  MSHE (Russia) ;  MinECo (Spain) ;  SNSF  and  SER (Switzerland) ;  NASU (Ukraine) ;  STFC  ( United Kingdom );  DOE NP  and  NSF (USA). We acknowledge the computing resources that are provided by  CERN ,  IN2P3 (France) ,  KIT  and  DESY (Germany) ,  INFN (Italy) ,  SURF (Netherlands) ,  PIC (Spain) , GridPP.
This data release paper focuses on high-quality spectroscopic redshifts of high-redshift galaxies observed with the KMOS spectrograph in the near-infrared H-and K-bands. A total of 424 highly-reliable redshifts are measured in the 1. 3 ≤ z ≤ 2. 5 range, with total success rates of 60. 7% in the H-band and 32. 8% in the K-band. The newly determined redshifts fill 55% of high (mainly regions with no spectroscopic measurements) and 35% of lower (regions with low-resolution/low-quality spectroscopic measurements) priority empty SOM grid cells. We measured Hα fluxes in a 1. 2 radius aperture from the spectra of the spectroscopically confirmed galaxies and converted them into star formation rates. In addition, we performed an SED fitting analysis on the same sample in order to derive stellar masses, E(B -V), total magnitudes, and SFRs.
C3R2 overview The Complete Calibration of the Color-Redshift Relation (C3R2;  Masters et al. 2017; M17 hereafter)  survey was designed to perform a systematic spectroscopic effort by means of two observing campaigns involving two telescope facilities. Part of the spectroscopic follow-up is conducted with the Keck telescopes using a combination of the DEIMOS, LRIS, and MOSFIRE instruments, with time allocated from all Keck partners (M17). The second part is overseen by the ESO Very Large Telescope (VLT) and its UT1 instruments FORS2 and KMOS. M17 presented the results of the first five nights of observations using the Keck facilities during the 2016A semester, leading to the release of 1283 high-confidence redshifts (Data Release 1). A further 3171 new high-quality spectroscopic redshifts were obtained during 2016B and 2017A semesters and are released in  (Masters et al.
Observation design KMOS is a multiplexed near-infrared integral field system (IFS) with 24 deployable image slicers (commonly referred to as 'arms'), surveying a 7. 2 diameter patrol field area. Each arm has a field of view (FoV) of 2. 8 × 2. 8 (14 × 14 pixel IFS units) and a spatial resolution of 0. 2/spaxel. The IFS units connect to three cryogenic grating spectrometers with 2k×2k Hawaii-2RG HgCdTe detectors. As previously mentioned, among the five available KMOS gratings (IZ, Y J, H, K, HK), our observations make use of the H-and K-bands (plus tentative Y J), characterised by a typical spectral resolution of about 3500. The observations were prepared with the KMOS ARM Allocator (KARMA; Wegner & Muschielok 2008) software, and submitted through the Phase 2 Proposal Preparation (P2PP) tool.
Data reduction The data were reduced with the Software Package for Astronomical Reduction with KMOS (SPARK;  Davies et al. 2013 ) using recipes outlined in the SPARK instructional guide 3. The reduction first applies a correction for detector effects, including  (1)  the correction of the readout channel variations via the reference pixels (pixels without photodiodes but with full electronics readout), and (2) the correction for the picture-frame effects affecting IFUs at the edges of the detector, using median DARK frames. The reduction then proceeds through the standard calibration steps, namely flat fielding, illumination correction, wavelength calibration (the accuracy of the wavelength solution is to the order of 30 km s -1 ), reduction of the spectrophotometric standards, and finally the data cube reconstruction.
Refine the redshift assignment with KUBEVIZ Maps of the emission-line fluxes were obtained from the reduced data cube using the IDL routine KUBEVIZ  (Fossati et al. 2016 ). The code simultaneously fits groups of lines (defined as 'line sets', e. g. Hα and the Nii λ6548. 05, λ6583. 45 doublet, or the Oiii λ 4958. 91, λ 5006. 84 doublet) using a combination of 1D Gaussian functions with fixed relative velocities. The continuum level is evaluated as the median value of the flux with an intensity from 40% to 60% within the total range of values inside two symmetric wavelength windows around each line set, and then subtracted. During the fit, KUBEVIZ takes into account the noise from the 'stat' data cube, thus optimally suppressing sky-line residuals. Furthermore, we reject the spaxels with SNR < 4.
SED fitting analysis The physical properties of galaxies were derived again for the spectroscopically confirmed targets, by taking advantage of the use of z spec as a constraint to the fit. We applied the SED fitting code LePhare to the spectrophometric catalogues obtained from merging the spectroscopic redshift measurement with the multi-band photometry collected from the parent surveys. A detailed list of the filters used in the three fields is reported in Table  4 , and the appropriate reference to the parent photometric catalogues is given in the table caption. The code is provided with spectroscopic redshifts and total magnitudes as input, and we set the priors on fitting parameters and galaxy libraries (based on a collection of different star formation histories, SFHs) taking advantage of the knowledge of the average properties of our target galaxies: these are high-redshift, star-forming galaxies, with consistent Hα emission.
5 dex). The distribution of the derived SFR and stellar masses in the SFR mass plane is shown in Fig. 12. The star-forming main sequence (MS, black dashed line) parametrisation adopted is a broken power law defined in the stellar mass range 9. 2 ≤ log 10 (M /M ) ≤ 11. 2 using UV and infrared SFRs from 3D-HST data at 0. 5 ≤ z ≤ 2. 5 in all CANDELS fields  (Whitaker et al. 2014 ). In the H-band, the SFRmass relation is lower than that at higher redshift (K-band). In particular, the distribution of both the KMOS H-and K-band sources is systematically higher than the star-forming main sequence. As already discussed in the SR analysis (Fig. 5 , bottom-right panel), this trend indicates that due to the low stellar mass of the galaxies observed, the SR is biased towards highly star-forming galaxies above the MS.
two multi-object spectrographs LUCI1 and LUCI2. Our observing strategy is to simultaneously observe the same pointing using H-and K-band masks with LUCI1 and LUCI2, maintaining the same integration time of KMOS observations (1 h). This allows us to observe many galaxies simultaneously in both filters, and helps us understand how much of the non-detection can be assessed with a broader wavelength range in the spectrum (e. g. in case of the more insecure photo-z estimates in K band targets). The physical properties of the released galaxies We measured the physical properties of the spectroscopically confirmed galaxies using their KMOS resolved spectra and their optical and near-infrared photometry from public data release catalogues in the three fields. We measured total Hα fluxes in 1. 2 radius apertures from the total 1D spectrum obtained after correcting each spaxel for its peculiar velocity, and we computed other physical parameters such as stellar masses, absolute magnitudes, and extinction from SED fitting with fixed spectroscopic redshift.
The stellar mass distribution of our sample peaks at log 10 (M /M ) = 9. 69 and is similar within the error bars across the three fields. We finally derived SFRs from the aperture Hα flux following the  Kennicutt (1998)  prescription, taking into account enhanced extinction towards nebular lines in the star-forming regions according to  Kashino et al. 2019. We studied the distribution of our galaxies in the SFR mass plane and compared our data points with the best fit high-redshift main sequence from  Whitaker et al. (2014). Galaxies observed during our KMOS programme are located, on average, at higher SFRs with respect to the average population of similar stellar masses. This result is due, especially at low stellar masses, to the limitations imposed by our observing strategy, of which the primary goal was to maximise the number of spectroscopic redshifts measured.
Acknowledgements. The Euclid Consortium acknowledges the  European Space Agency  and the support of a number of agencies and institutes that have supported the development of Euclid. A detailed complete list is available on the Euclid web site (http://www. euclid-ec. org). In particular the  Academy of Finland , the  Agenzia Spaziale Italiana , the  Belgian Science Policy , the  Canadian Euclid Consortium , the  Centre National d'Etudes Spatiales , the  Deutsches Zentrum für Luft-und Raumfahrt , the  Danish Space Research Institute , the Fundação para a Ciênca e a Tecnologia, the  Ministerio de Economia y Competitividad , the  National Aeronautics and Space Administration , the  Netherlandse Onderzoekschool Voor Astronomie , the  Norvegian Space Center , the  Romanian Space Agency , the  State Secretariat for Education, Research and Innovation (SERI)  at.