dataesr/scientific-paragraphs-categorization huggingface dataset:
ACKNOWLEDGMENTS OM thanks  Shunsaku Horiuchi  for helpful discussions. This work made use of computing resources and support provided by the  Physics Institute at the University of Antioquia. OM was partially supported by  COLCIEN-CIAS  through the grant number  111-556-934918. This research has been supported at IAP by the  ERC  Project No. 267117  (DARK) hosted by  Université Pierre et Marie Curie (UPMC)  -Paris 6 and at  JHU  by  NSF  Grant No. OIA-1124403. This work has been also supported by  UPMC  and  STFC. Finally, this project has been carried out in the  ILP LABEX  ( ANR-10-LABX-63 ) and has been supported by  French  state funds managed by the  ANR , within the  Investissements d'Avenir programme  ( ANR-11-IDEX-0004-02 ).
Methods Crystal growth: Single crystals of CuO were grown by the high temperature solution growth method. The starting materials (minimum purity of 99. 999%) were CuO powder and flux of 95% Bi2O3 and 5% B2O3 in ratio of 20:1. The mixture was sealed in a platinum crucible, maintained at 1150 °C for 48 h and then slowly cooled to 920 °C at a rate of 0. 5 degrees per hour. At 920 °C the flux was removed from the crucible by decanting. The crystal quality was checked by neutron back scattering. A sample of size × × Magnetization and torque measurements: Magnetization and magnetic torque in DC fields up to 14 T were measured using commercial SQUID magnetometers from Quantum Design. None of the data have been corrected for ionic diamagnetic core contributions or for demagnetizing-field effect since those corrections are negligibly small.
Acknowledgements The authors are grateful to  Virginie Simonet ,  Michel Viret ,  Michael Kuz 'min,  Josep Fontcuberta  and  Florencio Sanchez  for critical reading of the manuscript. We would like to acknowledge the support from the  Institute Laue-Langevin  ( ILL -Grenoble ) for the neutron diffraction experiments and the support from  HLD at HZDR , a member of the  European Magnetic Field Laboratory (EMFL) , for the high magnetic field experiments. The work was supported by the  Bulgarian Science Fund   FNI-T-02/26  project, by the  French ANR  " Dymage " project  ANR-13-BS04-0013 , by the  Spanish Government  ( MAT2011-29269-C03  and  MAT2014-56063-C2-1-Rprojects ), by the  Generalitat de Catalunya  project  2014 SGR 734 , by the  Brazilian agencies CNPq  (project  407033/2013-0 ) and  CAPES  ( BEX 0298/2015-08 ), and by the  Russian Foundation for Basic Researches  project  13-02-01093.
The automated sequence involved collection of spectra at 30 K intervals during cooling from ∼305 to ∼5 K, with a period of 20 min allowed for thermal equilibration at each temperature. This was followed by heating between ∼5 and ∼300 K, with data collection at 5 K intervals and the same thermal equilibration period at each temperature. Each spectrum contained 65000 data points in the frequency range 100-1200 kHz. Measured temperatures are believed to be accurate to within ±1 K, and temperature stability during data collection is better than ± 0. 1 K. High-temperature spectra were collected with the sample balanced across a pair of corners between the tips of two alumina rods protruding into a horizontal tube furnace. In this system, the transducers are on the ends of the rods, outside the furnace, as described by McKnight et al.
This is a blind search for CO emission using the Atacama Large Millimeter/sub-millimeter Array (ALMA). The goal is to constrain the molecular gas content of an unbiased sample of galaxies. The targeted region is one of the best studied areas of the sky, with exquisitely deep photometry in > 25 X-ray-to-far-infrared (IR) bands, photometric redshifts, and dozens of spectroscopic redshifts. This provides us with an exquisite wealth of ancillary data, which is instrumental to put our CO measurements in the context of galaxy properties. Thanks to the deep field nature of our approach, we avoid potential biases related to the pre-selection of targets, and include both detections and non-detections in our analysis. Our dataset combines 3mm and 1mm observations of the same galaxies, thus providing constraints on the CO excitation.
Furthermore, the combination of the spectral line survey and the 1mm continuum image allows us to compare CO-and dust-based estimates of the gas mass. In other papers of this series, we present the dataset and the catalog of blindly-selected CO emitters (Paper I,  Walter et al. ) , we study the properties of 1. 2mm-detected sources (Paper II,  Aravena et al. ) , we discuss the inferred constraints on the luminosity functions of CO (Paper III,  Decarli et al. )  and we search for [C ii] emission in z=6-8 galaxies (Paper V,  Aravena et al. ). Paper VI (Bouwens et al. ) places our findings in the context of the dust extinction law for z > 2 galaxies, and Paper VII  (Carilli et al. )  uses ASPECS to put first direct constraints on intensity mapping experiments. Here we put the CO detections in the context of the properties of the associated galaxies.
In sec. 2 we summarize the observational dataset; in sec. 3 we describe our sample; in sec. 4 we present CO-based measurements, which are discussed in the context of galaxy properties in sec. 5. We summarize our findings in sec. 6. Throughout the paper we assume a standard ΛCDM cosmology with H 0 = 70 km s -1 Mpc -1 , Ω m = 0. 3 and Ω Λ = 0. 7 (broadly consistent with the measurements in Planck Collaboration 2015), and a  Chabrier (2003)  stellar initial mass function. Magnitudes are expressed in the AB photometric system  (Oke & Gunn 2003).
The ALMA dataset The details of the ALMA dataset (observations and data reduction) are presented in Paper I of this series. Here we briefly summarize the observational details that are relevant for the present study. The dataset consists of two frequency scans in ALMA band 3 (3 mm, 84-115 GHz) and in band 6 (1 mm, 212-272 GHz). In the case of the 3mm observations, we obtained a single pointing centered at RA = 03:32:37. 900, Dec = -27:46:25. 00 (J2000. 0), close to the Northern corner of the Hubble eXtremely Deep Field (XDF,  Illingworth et al. 2013). The primary beam has a diameter of ≈ 65 at the central frequency of the band (99. 5 GHz). The typical noise rms is ∼ 0. 18 mJy beam -1 per 50 km s -1 channel. The 1 mm observations consist of a 7-pointing mosaic covering approximately the same area as the 3 mm observations.
(2011). X-ray data are taken from the Extended Chandra Deep Field South Survey  (Lehmer et al. 2005 ) and from the Chandra Source Catalogue  (Evans et al. 2010). Photometric redshifts (z photo ) are available for all of the optically-selected sources in the field. At a limiting magnitude i=28 mag, the median uncertainty is δz photo ∼ 0. 5, and it reaches δz photo ∼ 1 at i ≈ 30 mag  (Coe et al. 2006 ). The compilation of  Skelton et al. (2014)  provides even more robust photometric redshifts, thanks to the expanded photometric dataset. The agreement with available spectroscopic redshifts is typically very good in these cases, with a standard deviation on ∆z/(1 + z) of ≈ 0. 01 for  (Skelton et al. 2014 ). In addition, the 3D-HST survey provides HST ACS and WFC3 grism observations of the field, yielding grism redshifts for tens of sources in our pointing  (Momcheva et al.
2016). Slit spectroscopy for 74 (mostly bright) galaxies in the field is also available  (Le Fèvre et al. 2005; Skelton et al. 2014; Morris et al. 2015). Finally, integral field spectroscopy of this field has been secured with ESO VLT/MUSE. These data are part of a Guaranteed Time observing program targeting the UDF. In particular, a single (1 arcmin 2  ) deep (21 hr on source) pointing overlaps with ∼ 70% of the ASPECS coverage. The cubes have been processed and analyzed with the improved MUSE GTO pipeline. These observations will be presented in  Bacon et al. (in prep). Within a radius of 34 from the ALMA 3mm pointing center (approximately the size of the primary beam of our 3mm observations), there are 1302 galaxies from the combination of all the available photometric catalogs. We use the high-z extension of MAGPHYS  (da Cunha et al.
3 ). The disk of ID. 4 has a scale radius of 5. 8 kpc based on HST imaging (van der Wel et al. 2012); for ID. 3, the estimated radius is 8. 3 kpc (but the overlap with the southern component may partially affect this estimate). ID. 4 appears as an upper limit in the X-ray catalog by  Xue et al. (2011)  (F X < 6. 7 × 10 -17 erg s -1 cm -2 , L X < 4. 3 × 10 41 erg s -1 ). ID. 5 and ID. 8 lie in a crowded region of our field. Skelton et al. (  2014 ) report a spectroscopic redshift z=1. 047 for ID. 5. However, the inspection of the MUSE data reveals two, clearly distinguished line sets of the [O ii] doublet, at z=1. 038 and z=1. 098. The latter matches the redshift of two CO lines which are slightly too faint to be selected in our blind search (S/N≈4. 8, see Paper I). ID. 8 on the other hand is found at another redshift (z=0.
ID. 7 appears as a very compact source (R e = 0. 7 kpc) at z=1. 221. Its Chandra image reveals the presence of a bright AGN (F X = 1. 01 × 10 -14 erg s -1 cm -2 in  Lehmer et al. 2005   Xue et al. 2011) , yielding an X-ray luminosity of L X = 5. 4 × 10 43 erg s -1 ). It is not detected in the 1mm dust continuum. A 3-σ excess is measured at the expected frequency of the CO(2-1) transition. ; 8. 3×10 -15 erg s -1 cm -2 in Evans et al. 2010; 6. 3 × 10 -15 erg s -1 cm -2 in ID. 9 and ID. 10 are both at z ∼ 2. 3. They are among the faintest galaxies in our sample in terms of L IR , just above the 10 11 L cut. ID. 9 appears as a compact bulge. ID. 10 appears as a spiral galaxy with disturbed morphology. ASPECS data cover 3 CO transitions in these galaxies: CO(3-2), CO(7-6), and CO(8-7). None of these Table  1.
CO luminosities and associated H 2 masses We measure the line fluxes (or place limits) for all the CO transitions covered in both the 3mm and 1mm line scans. We extract the CO spectra at the position of the optical coordinates of the sources in our sample. We fit the lowest-J transitions accessible with ASPECS data with a gaussian profile; in the case of a detection, we fit the higher-J lines imposing the same line width. We consider detections cases where the flux obtained in the gaussian fit is >3× its uncertainty. If the line is not detected, we assume a fiducial line width of 300 km s -1 and we use the upper boundary of the 3-σ confidence range on the flux as upper limit. Tab. 2 reports the CO line fluxes, shifts compared with the nominal redshift, and the line width. The detected sources in our sample have a median CO flux of 0.
Since the IR luminosity is proportional to the SFR, and the CO luminosity is used to infer M H2 , the y-axis of this plot conceptually corresponds to a diagonal line (top-left to bottom-right) in Figure  8. The depletion time t depl = MH2/SFR as a function of the specific star formation rate sSFR=SFR/M * for the galaxies in our sample, the secure blind detections in  Decarli et al. (2014) , the PHIBSS sample by  Tacconi et al. (2013) , and the starburst sample in  Silverman et al. (2015). The symbol code is the same as in Fig. 6. Starburst galaxies typically reside in the bottom-right corner of the plot. Our ASPECS sources cover a wide range in parameter space, highlighting the diverse properties of these galaxies. The sources in our sample range over almost 2 dex in sSFR and t depl. Noticeably, ID.
SUMMARY We present a study of the molecular gas properties as derived from CO observations of high-redshift galaxies in ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (UDF). This dataset consists of a blind survey of molecular gas in the ALMA 3mm and 1mm bands targeting a region with the deepest HST imaging available, the so-called XDF. Our observations cover hundreds of high-redshift galaxies with wellcharacterized SEDs, i. e. we can test our expectations in terms of molecular gas content in galaxies without any prior selection through their optical or near-IR properties. This allows us to analyse our CO measurements and limits in the context of the global properties of the associated galaxies, thanks to an exquisite wealth of ancillary multi-wavelength information. We focus on the galaxies for which a secure redshift is available, either via our ASPECS CO observations or from optical/near-IR spectroscopy reported in the literature.
ACKNOWLEDGMENTS We thank the anonymous referee for her/his positive feedback and useful comments. RD thanks  Laura Zschaechner  for insightful discussions. FW, IRS, and RJI acknowledge support through  ERC grants COSMIC-DAWN , DUSTYGAL, and COSMICISM, respectively. M. A. acknowledges partial support from  FONDECYT  through grant  1140099. DR acknowledges support from the  National Science Foundation  under grant number  AST-1614213  to  Cornell University. FEB and LI acknowledge Conicyt grants  Basal-CATA PFB-06/2007  and Anilo  ACT1417. FEB also acknowledge support from  FONDECYT Regular 1141218 (FEB) , and the  Ministry of Economy, Development, and Tourism's Millennium Science Initiative  through grant  IC120009 , awarded to  The Millennium Institute of Astrophysics, MAS. IRS also acknowledges support from  STFC  ( ST/L00075X/1 ) and a  Royal Society / Wolfson Merit  award.
Support for RD and BM was provided by the  DFG priority program 1573  'The physics of the interstellar medium'. AK and FB acknowledge support by the  Collaborative Research Council 956 , sub-project  A1 , funded by the  Deutsche Forschungsgemeinschaft (DFG). PI acknowledges Conict grants  Basal-CATA PFB-06/2007  and Anilo  ACT1417. RJA was supported by  FONDECYT  grant number  1151408. This paper makes use of the following ALMA data: [ADS/JAO. ALMA#  2013. 1. 00146. S and  2013. 1. 00718. 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 cooperation with the  Republic of Chile. The Joint ALMA Observatory is operated by  ESO ,  AUI/NRAO  and  NAOJ.
Introduction The TEXAS facility is part of an ambitious project spread over more than ten years to upgrade the ESRF accelerator, beamlines and infrastructure. The Time-resolved and Extreme-conditions X-ray Absorption Spectroscopy (TEXAS) beamline is based on an upgrade of the former energy-dispersive X-ray absorption spectroscopy (EDXAS) beamline ID24. TEXAS offers the user community new opportunities for investigating rapid processes down to the nanosecond timescale, and matter at extreme conditions of pressure, temperature and magnetic field. The scientific case for TEXAS is schematically illustrated in Fig. 1. The core of the future activities lies at the intersection between 'time resolved' and 'extreme conditions' applications. Whereas XAS at the ESRF and elsewhere addressed applications requiring rapid data acquisition or extreme environments, applications requiring both are still largely unexplored.
The ID24 beamline within the TEXAS facility The TEXAS facility is illustrated in Fig. 2. It is composed of a 70 m-long EDXAS beamline on port ID24, coupled to a 40 m-long general purpose extended X-ray absorption fine structure (EXAFS) beamline on bending-magnet port BM23  (Mathon et al. , 2015a). The concept of combining a general purpose EXAFS beamline and a state-of-the-art high-brilliance EDXAS beamline in a single facility provides the user community with the best possible conditions for the research outlined in Fig. 1. BM23 is the only public ESRF beamline dedicated to 'standard' EXAFS. Its key mission is to provide high-quality EXAFS in a large energy range (5-75 keV), with high signal to noise (S/N) up to large k-range, with a high degree of automation, featuring online EXAFS data reduction and a flexible sample environment.
The recent implementation of continuous scanning (quick-EXAFS) and of a micro-XAS station on BM23 provides a link between the time-resolved and extremeconditions activities on BM23 and ID24. The possibility to achieve a focal spot of 4 mm Â 4 mm on BM23, coupled to the recent availability of nano-polycrystalline diamond (NPD) anvils  (Irifune et al. , 2003)  is a real breakthrough for highpressure XAS investigations. High-quality large k-range EXAFS can be recorded on BM23 in static mode or with mild time-resolution, be it at ambient conditions, at high pressure in a diamond anvil cell or in situ and in operando in a chemical reactor. These data are often of paramount importance to complement lower quality data (lower S/N, smaller k-range, etc. ) recorded under more challenging conditions on ID24.
, 2012; Marini et al. , 2013)  has therefore been specifically designed and is illustrated in Fig. 24. The doublesided laser-heating system is designed in such a way that the optical components do not interfere with the direct X-ray beam, allowing true simultaneous measurements of temperature from both sides of the sample as well as the X-ray absorption spectra. The DAC is mounted into a water-cooled copper holder and is supported by a mini-hexapod stage. The sample within the DAC is heated by means of two 1070 nm 120 W IR fiber lasers, focused on both sides of the sample. The lasers operate either in pulsed (pulse width ' 0. 1-100 ms) or in continuous mode. Fast data acquisition is required because laser-heated samples are unstable and can react with their environment. The sample temperature is measured by collecting and analyzing the emitted radiation from both sides of the sample using a Princeton Instruments SP300i spectrometer, and fitting it to Planck's law within a grey body approximation.
Acknowledgements We would like to acknowledge the  ESRF  support groups and other divisions for their assistance during the beamline design, construction and commissioning phases, and in particular:  R. Baker ,  R. Barrett ,  P. Berkvens ,  L. Besset ,  J. -C. Biasci ,  T. Boisserenq ,  J. Borrel ,  D. Bugnazet ,  O. Chamond ,  J. Chavanne ,  J. -M. Clement ,  C. Cohen ,  Y. Dabin ,, L. Ducotte,  P. Duru ,  P. Fajardo ,  C. Ferrero ,  P. Guerin ,  J. -P. Guigay ,  R. Hino ,  R. Huber ,  J. -C. Labiche ,  C. Lefevre ,  N. Levet ,  P. Mackrill ,  G. Malandrino ,  T. Manning ,  P. Marion ,  T. Martin ,  F. Monnier ,  J. Morse ,  F. Pegot ,  C. Ponchut ,  C. Rolland ,  M. Sanchez Del Rio ,  D. Schirr-Bonnans ,  R. Steinmann ,  C. Richard ,  T. Rouveyrol ,  F. Torrecillas ,  P. van der Linden ,  A.
Context. Cyanopolyynes are chains of carbon atoms with an atom of hydrogen and a CN group on either side. They are detected almost everywhere in the interstellar medium (ISM), as well as in comets. Aims. We present an extensive study of the cyanopolyynes distribution in the solar-type protostar IRAS16293-2422. The goals are (i) to obtain a census of the cyanopolyynes in this source and of their isotopologues; (ii) to derive how their abundance varies across the protostar envelope; and (iii) to obtain constraints on the history of IRAS16293-2422 by comparing the observations with the predictions of a chemical model. Methods. We analysed the data from the IRAM-30m spectral survey towards IRAS16293-2422. The derived (SLED) of each detected cyanopolyyne was compared with the predictions from the radiative transfer code (GRAPES) to derive the cyanopolyyne abundances across the envelope of IRAS16293-2422.
Species identification We searched for the lines of cyanopolyynes and their isotopologues using the spectroscopic databases Jet Propulsion Laboratory (JPL;  Pickett et al. 1998)  and the Cologne Database for Molecular Spectroscopy (CDMS;  Müller et al. 2005). We then used the package CASSIS (Centre d'Analyse Scientifique de Spectres Instrumentaux et Synthtiques) (http://cassis. irap. omp. eu) to fit a Gaussian to the lines. For the line identification we adopted the following criteria: 1. The line is detected with more than 3σ in the integrated line intensity. 2. The line is not blended with other molecular lines. 3. The line intensity is compatible with the spectral line energy distribution (SLED): since cyanopolyyynes are linear molecules, their SLED is a smooth curve, so that lines are discarded when their intensities are out of the SLED defined by the majority of the lines, as shown in Fig.
Model description As in our previous work  (Jaber et al. 2014) , we used the package GRAPES (GRenoble Analysis of Protostellar Envelope Spectra), which is based on the code described in  Ceccarelli et al. (1996 Ceccarelli et al. ( , 2003)) , to interpret the SLED of the detected cyanopolyynes. Briefly, GRAPES computes the SLED from a spherical infalling envelope for a given density and temperature structure. The code uses the beta escape probability formalism to locally solve the level population statistical equilibrium equations and consistently computes each line optical depth by integrating it over the solid angle at each point of the envelope. The predicted line flux is then integrated over the whole envelope after convolution with the telescope beam. The abundance X (with respect to H 2 ) of the considered species is assumed to vary as a function of the radius with a power law α in the cold part of the envelope, and as a jump to a new abundance in the warm part, corresponding to the sublimation of ices (e.
). The last column reports the telescope beam at the frequency of the line. a : Discarded line because it is probably contaminated by the molecular cloud (see text, Sect. 4. 2). b : Discarded line because it does not satisfy criteria 3 to 5 of Sect. 3. 2. c The HC3N and DC3N line frequencies are the same in the CDMS and JPL database. In contrast, the JPL HC5N line frequencies are systematically overestimated with respect to those of CDMS, giving VLSR shifted by ∼ 1 km/s with respect to the VLSR derived for the HC3N and DC3N lines. We therefore used the HC5N line frequencies from the CDMS database. d We consider the detection of this line to be tentative.
The gas-phase chemical network is based on the UMIST database  (McElroy et al. 2013 ) augmented with updates from the KIDA database as well as new rate coefficients for the HC 3 N and HC 5 N network as estimated by  Loison et al. (2014). The chemical evolution was followed until chemical equilibrium was reached. To understand the chemical origin of the HC 3 N abundance that we measured in the cold envelope of IRAS16293 (∼ 10 -11 ), we modelled a gas density of 2 × 10 6 cm -3 and a gas temperature of 20 K, which are the values inferred by  Crimier et al. (2010)  at a radius equivalent to the observations telescope beam (see Sect. 4. 2. 1). We ran a small grid of models where we varied the carbon and oxygen elemental abundances in the range of 0. 3-1 and 1-3 ×10 -4 , respectively; -the nitrogen elemental abundance: 6 (solar) and 2 ×10 -5 ; -the cosmic-ray ionisation rate: 5×10 -17 s -1 (assumed as our standard value) and 10 times higher.
Two different amplitudes of noise were used, σ = 153 pA or σ = 235 pA, and the mean was adapted according to the injected holding current. Individual protocols were composed of 500 ms without noise followed by 20 s of the noise waveform. The membrane potential V was recorded in response to the noisy current injection, and the ionic transmembrane current I m was calculated by subtracting the capacitive current I C from the injected current I in (Eq 5). The after-hyperpolarization and the initial repolarization phase of each action potential (10 ms after the peak) were excluded from the analysis. As the distribution of the data points is approximately Gaussian for a given voltage, the dynamic IV curve can be defined as the average of I m versus V (Fig 3C ): I dyn ðVÞ ¼ mean½I m ðV; tÞ ð6Þ The capacitance (used to evaluate the capacitive current) was estimated by minimizing the variance of I m within individual voltage bins.