dataesr/scientific-paragraphs-categorization huggingface dataset:
Standard errors on V P result from the propagation of uncertainties that are inherent to fitting the ultrasonic data and modeling of the radiographic image data (Section C4 of supporting information). Standard errors on density are estimated from the precision of the high-precision balance that is used for hydrostatic weighing and the propagation of uncertainties that are inherent to modeling the X-ray absorption data (Section A5 of supporting information). Standard errors on pressure of 0. 5 GPa are based on the uncertainties on EOSs of the pressure and temperature calibrants BN and Al 2 O 3  (Dubrovinski et al. , 1998; Wakabayashi & Funamori, 2015)  for the V P measurements and BN and Pt  (Fei et al. , 2007; Wakabayashi & Funamori, 2015)  for the density measurements. BN, boron-nitride; EOS, equation of state.
The FESIC_LP model is identical to the FESIC model in the binary Fe-C domain. We recall that there are no indications in the experimental data analysis that the sample was incompletely molten during the V P measurements that are performed at >3. 5 GPa. Also, the FESIC model is in better agreement with the available measurements in literature of V P  (Terasaki et al. , 2019)  and density  (Morard et al. , 2013)  at high pressures that are relevant for Mercury's core compared to the FESIC_LP model. For these reasons, we consider the FESIC model as the preferred model for characterizing the liquid outer core of Mercury.
Computational details Ab initio calculations were performed to determine the excitation energies of the neutral TCA molecule (see Table  1  ) and the valence and outer valence vertical ionisation energies (see Table  2  ), using the MOLPRO package  [15]. First, the ground state geometry was optimised at the MP2 and CCSD levels using Dunning's cc-pVTZ atomic basis set  [ 16 , 17 ]. It is well known that the calculation of electronic spectra, even for small organic molecules, is a difficult task (for a recent review see ref. [18]  ). While the very fast TD-DFT method is known to have difficulties in describing Rydberg states  [19]  , multi-reference methods such as the CASPT2 or CASSCF/MRCI techniques become prohibitive when a large number of Rydberg orbitals have to be included in the active space.
The vertical ionisation energies were also obtained using Partial Third Order (P3) propagation and Outer Valence Green Function (OVGF) calculations  [24]  , employing the cc-pVTZ basis sets and geometry with the Gaussian16 rev. B. 01 package  [25]. Additional calculations have been performed at the EOMIP-CCSD level  [26] [27] [28]  , using the Q-Chem 4. 3. 0 package  [29].
Absolute photoabsorption cross sections and atmospheric photolysis The present optical measurements were carried out in the pressure range 0. 006-0. 020 mbar, and they revealed no evidence for changes in the absolute cross sections or peak energies as a function of pressure. Thus the present spectra are free of any saturation effects. A literature survey reveals no other previous photoabsorption cross sections of TCA in the 4. 0 -10. 8 eV photon energy range to compare with. However, the agreement of previous cross sections measured at the AU-UV beam line of the ASTRID2 synchrotron facility at Aarhus University, see e. g. [39] [40] [41]  , with the most precise corresponding data available in the literature (see Eden et al. [30]  and references therein), indicates that our adopted procedures do not suffer from systematic errors.
Acknowledgment SK acknowledges the  Portuguese National Funding Agency FCT  through the Grant  PD/BD/142831/2018  and together with PLV the  Research Grants CEFITEC  (  UIDB/0 0 068/2020  ) and  PTDC/FIS-AQM/31281/2017. This work was also supported by the  Radiation Biology and Biophysics Doctoral Training Programme (RaBBiT ; Grant  PD/00193/2012  ) and  UCIBIO  (Grant  UIDB/04378/2020  ). DD acknowledges the support of the OVERSEE and CAPPA grants, managed by the  Agence Nationale de la Recherche  under the frame programs Investissements d'Avenir  ANR-10-LABX-005  and  I-SITE ULNE/ANR-16-IDEX-0 0 04  ULNE , respectively. D. D. also thanks the  Région Hauts de France , the  Ministre de l'Enseignement Suprieur et de la Recherche  ( CPER Climibio ) and the  European Fund for Regional Economic Development  for their support.
This work used HPC resources from  GENCI-TGCC  (Grant No. 2020-A0050801859  ) and the  Centre de Resources Informatiques (CRI)  of the  Université de Lille. This contribution is based upon work from  COST Action CA18212-Molecular Dynamics  in the GAS phase (MD-GAS), supported by  COST (European Cooperation in Science and Technology). Finally, MJB thanks the  Australian Research Council  for partial financial support through grant # DP180101655.
Methods. We analyzed 252 hours of High Energy Stereoscopic System (H. E. S. S. ) observations towardsSNR N132D that were accumulated between December 2004 and March 2016 during a deep survey of the Large Magellanic Cloud, adding 104 hours of observations to the previously published data set to ensure a > 5σ detection. To broaden the gamma-ray spectral coverage required for modeling the spectral energy distribution, an analysis of Fermi-LAT Pass 8 data was also included. Results. We unambiguously detect N132D at VHE with a significance of 5. 7 σ. We report the results of a detailed analysis of its spectrum and localization based on the extended H. E. S. S. data set. The joint analysis of the extended H. E. S. S and Fermi-LAT data results in a spectral energy distribution in the energy range from 1.
1 (68% containment radius). The energy threshold is ∼100 GeV for small zenith angles and below 1 TeV for zenith angles up to 60 • , and the energy resolution is ∼15% (for further details, see  Aharonian et al. 2006). The fifth Cherenkov telescope (CT5) with a diameter of 28 m (mirror area of 614 m 2 ) was added in the center of the CT1-4 array in July 2012, initiating the second phase of the experiment, "H. E. S. S. II". This study mostly uses H. E. S. S. I observations because only about 5% of the data were taken by the full CT1-5 array. H. E. S. S. performance depends on the zenith angle, configuration cuts, and the number of telescopes considered in the reconstruction (for more details, see sections 2. 2 and 2. 3).
Data set: LMC survey Its location in the southern hemisphere makes H. E. S. S. the only currently operating IACT array able to observe the LMC in the VHE band. With its angular size of ∼8 • , the LMC galaxy is compact enough for the H. E. S. S. telescopes to perform a survey. Such a survey was conducted over 13 years, from 2004 to 2017, during which the full LMC galaxy was covered with over 325 hours of observations. The exposure of the LMC is rather inhomogeneous and mostly concentrated on the central region around the Tarantula nebula. H. E. S. S. observations from 2003 to 2012 led to the discovery of three individual VHE gamma-rayemitting sources, including SNR N132D, along with the PWN of N 157B and the superbubble  30 Dor C (Abramowski et al. 2012 , 2015b) , as well as the detection of the gamma-ray binary LMC P3  (Abdalla et al.
2018f). The data set used for our analysis was taken between December 2004 and March 2016. It consists of 252 hours of total exposure time, adding 104 hours to the previously published data set. The zenith angle of these observations spans a range of 45-57 • , with a mean of 46 • , and a mean azimuth angle of 182 •. 5. The data set was selected with a maximum offset of 2 •. 5 around the source to avoid observations with large offset angles with respect to the camera center. For N132D, the observation positions were mostly toward the east side of the SNR. This is due to the nature of the observations, which are part of a survey, instead of being dedicated to N132D: the pointings were mostly directed toward N157B in the Tarantula nebula, which is situated toward the east of N132D. This results in offset angles in the range of 0 •.
H. E. S. S. data analysis Data corresponding to 252 hours were recorded in 28-minute exposures that are called runs. Each calibrated run that passed the quality criteria of a dead time shorter than 30% of the run duration, a low fluctuation in trigger rate, and acceptable weather conditions (see  Aharonian et al. 2006; Hahn et al. 2014 ) was analyzed using the ImPACT framework described by  Parsons & Hinton (2014) , which includes a boosted decision-tree-based event classification algorithm to distinguish gamma rays from the charged particle background  (Ohm et al. 2009 ). This analysis was performed using a special configuration that selected events with a minimum of three shower images in different telescopes. Using this event selection cut allowed us to improve the signal-to-background ratio for this faint gamma-ray source in the presence of a strong diffuse component, or multiple unresolved sources constituting an astrophysical background, which may be present in the vicinity of N132D.
To compute the maps and statistics presented in section 3, ON events were selected from a circle centered on the geometrical center of the X-ray emission (referred to as the "X-ray source position") at RA 5 h 25 m 2. 2 s , Dec -69 • 38 39. OFF events were selected according to a ring-background method  (Berge et al. 2007 ). An additional cut on the energy of reconstructed gammarays was made above 1. 3 TeV in order to improve the signal-tobackground ratio for this hard gamma-ray source and keep only gamma-ray events from a well-determined direction because the angular resolution improves by 10% from 800 GeV to 1. 3 TeV using the ImPACT shower reconstruction software. This resulted Article number, page 3 of 13 in a point spread function (PSF) of 0 •. 06, which corresponds to the 68% containment radius of the fit on the observation position.
gov/ssc/data/ for four diffuse sources, LMC-FarWest, LMC-Galaxy, LMC-30DorWest, and LMC-North, provided by the Fermi-LAT collaboration (Ackermann et al. 2016), were used. These sources are outlined with circles in Fig. 2. To model the Galactic and isotropic background diffuse emission, the standard templates gll_iem_v07. fits and iso_P8R3_SOURCE_V2_v1. txt were used. The spectral shapes of the sources were taken from the 4FGL catalog. The normalization and the photon index of N132D were derived from the likelihood analysis along with the normalizations of four strong point sources, including 4FGL J0537. 8-6909 and 4FGL J0540. 3-6920, and all diffuse sources, while the normalizations of fainter point sources were held fixed at the 4FGL catalog values. A binned likelihood analysis was applied to the data using the Fermi Science tool gtlike.
Morphology in the VHE gamma-ray band The position of the VHE gamma-ray source was obtained from a two-dimensional fit of the H. E. S. S. so-called ON map consisting of gamma-ray-like events in the source region and a background map, using the gamma-ray events selected in the OFF region multiplied by a scaling factor map in order to reach the source exposure level. The fit was performed using the Sherpa package  (Freeman et al. 2001) , with a log-likelihood approach (Cash statistic; Cash 1979) and the Levenberg-Marquardt algorithm  (Moré 1978). To obtain the source position, a Gaussian source was convolved with the H. E. S. S. analysis PSF (0 •. 06) multiplied by the exposure map to take any asymmetry in the exposure across the analyzed sky region into account, and with the background amplitude fixed to 1.
In this case, a ratio of n e /n p for CRs is one of the parameters, for which the Article number, page 5 of 13  canonical value is 1/100, based on the ratio of electron-to-proton CRs measured near the Earth (see, e. g. ,  Longair 2011; Katz & Waxman 2008). However, the n e /n p ratio at Earth may not reflect the ratio in SNRs, and there may be variations in SNRs. Here these radiation processes were modeled using theoretical frameworks developed by  Aharonian et al. (2010)  for the synchrotron radiation, by  Khangulyan et al. (2014)  for the inverse Compton mechanism, by  Baring et al. (1999)  for bremsstrahlung emission, and by  Kafexhiu et al. (2014)  for the pion decay. To model the multiwavelength spectrum of N132D for the two scenarios, the Naima package was employed  (Zabalza 2015). We used a single-zone model.
Acknowledgements The support of the  Namibian authorities and of the University of Namibia  in facilitating the construction and operation of H. E. S. S. is gratefully acknowledged, as is the support by the  German Ministry for Education and Research (BMBF) , the  Max Planck Society , the  German Research Foundation (DFG) , the  Helmholtz Association , the  Alexander von Humboldt Foundation , the  French Ministry of Higher Education, Research and Innovation ,  the Centre National de la Recherche Scientifique  ( CNRS/IN2P3  and  CNRS/INSU) , the Commissariat à l'énergie atomique et aux énergies alternatives (CEA), the  U. K. Science and Technology Facilities Council (STFC) , the  Knut and Alice Wallenberg Foundation , the  National Science Centre, Poland  grant no. 2016/22/M/ST9/00382 , the  South African Department of Science and Technology and National Research Foundation , the  University of Namibia , the  National Commission on Research, Science & Technology of Namibia (NCRST) , the  Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF) , the  Australian Research Council (ARC) , the  Japan Society for the Promotion of Science  and by the  University of Amsterdam.
We appreciate the excellent work of the technical support staff in  Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen , and in Namibia in the construction and operation of the equipment. This work benefitted from services provided by the  H. E. S. S. Virtual Organisation , supported by the national resource providers of the  EGI Federation. J. Vink  and  D. Prokhorov  are partially supported by funding from the  European Union 's  Horizon 2020 research and innovation programme  under grant agreement No  101004131  and by the  Netherlands Research School for Astronomy (NOVA).
Conclusions New IRAM 30m HERA CO(2-1) data were combined with VIVA Hi data to investigate the distribution of the total gas within the disk of the Virgo spiral galaxy NGC 4654 and its ability to form stars. NGC 4654 undergoes both, a gravitational interaction with another massive galaxy and nearly edge-on ram pressure stripping. The combined effects of these interactions lead to the formation of an overdense stellar and molecular gas arm toward the northwest, ending with an abnormally high Hi surface density region. Previous studies  (Chung & Kim 2014)  showed that within this region the SFE H 2 is unusually high and the ratio of the molecular fraction to the total mid-plane pressure is significantly lower than that of the rest of the disk. With deeper CO observations of higher spatial resolution (12") and a star-formation map based on GALEX FUV and SPITZER 24 µm data, we pursued this study to understand the physical properties of the ISM in the high Hi surface density region and their impact on the ability of the ISM to form stars.
We applied two methods to determine the value of the COto-H 2 conversion factor within the disk of NGC 4654. Following  Sandstrom et al. (2013) , the first method consists in the simultaneous determination of the DGR and the conversion factor using Herschel 250µm FIR data as a tracer for total gas surface density. The second method is based on the determination of the DGR from direct metallicity measurements of  Skillman et al. (1996)  corrected according to the calibration of  Curti et al. (2020). Different results were found by the two models: a constant conversion factor and an increased conversion factor by a factor of two in the high Hi surface density region. The comparison of the metallicity and the SFE of the high Hi surface density region in NGC 4654 and NGC 4501, which has similar physical characteristics, supports the assumption of a modified conversion factor for NGC 4654 (see  Sect.
On the neutron-rich side of the nuclear chart, shell closures have been shown to vanish far from stability for the neutron numbers N =20 and N =28  [6, 7] , and new shell closures have been found for N =32 and N =34  [8] [9] [10] [11] [12] [13] [14] [15]. The N =82 shell closure has been studied for neutron-rich nuclei down to Cd  [16] [17] [18]. The data in the neutron-deficient region are incomplete, and the evolution of the N =82 shell towards the proton dripline is not known. In this work, the N =82 shell closure is investigated by mass measurements up to the proton dripline. Series of nuclear isomers are known to occur near shell closures. A unique sequence of isomers exists in the N =81 isotones with even Z, ranging from 131 Sn to 149 Er  [19, 20]. This sequence is remarkable, because the excitation energies of these J π =11/2 -isomers stay approximately constant at 750 keV between 139 Ce and 149 Er  [21] [22] [23] [24] [25] , over a range of eleven isotones.
The mass spectra were analyzed by fitting hyper-EMG functions  [52]  to the unbinned mass data using weighted maximum likelihood estimation  [53]. The isotopes of interest and their respective calibrants are listed in Table  I. The mass values of the calibrants were taken from the Atomic Mass Evaluation AME2020  [54]. The dominating contribution to the systematic uncertainty are shifts in the TOF due to voltage ringing caused by the switching of the reflector voltages  [55, 56]. Its relative value amounts to 3 × 10 -7. The ground state masses of eight Yb isotopes were measured (Table  I ). For 154-157 Yb, the masses were already well known, and the present results are in good agreement with the AME2020  [54]. The masses of 151 Yb and 152 Yb were measured directly for the first time, and their uncertainties could be reduced by a factor of three.
The masses of 150 Yb and 153 Yb were measured for the first time. With these results, the N =82 shell closure can be examined in the extreme proton-rich region. Figure  2  shows the empirical two-neutron-shell gap ∆ 2n (Z, N ) = FIG. 2. Evolution of the two-neutron-shell gap ∆2n at N =82 as a function of the proton number Z and predictions of the theoretical models HFB21  [57] , UNEDF0  [58] , and FRDM2012  [59]. Experimental data are from the AME2020  [54]  and this work. Regions of proton-unbound nuclides are indicated  [54, 60]. Most error bars are hidden in the symbols, lines are drawn to guide the eye. S 2n (Z, N )-S 2n (Z, N +2), where S 2n (Z, N ) = B(Z, N )- B(Z, N -2) is the two-neutron separation energy and B(Z, N ) is the binding energy, for different N =82 isotones. The two-neutron-shell gap shows pronounced maxima when crossing closed shells.
We would like to thank  J. Lassen  and the  TRILIS ion source group  for the excellent beam conditions. This work was supported by the  German Research Foundation (DFG) , grant No. SCHE 1969/2-1 , by the  German Federal Ministry for Education and Research (BMBF) , grant No. 05P16RGFN1  and  05P19RGFN1 , by the  Hessian Ministry for Science and Art  through the  LOEWE Center HICforFAIR , by the  JLU  and  GSI  under the  JLU-GSI strategic Helmholtz partnership agreement , by the  Polish National Science Centre  under Contract No. 2016/21/B/ST2/01227 , by the  Natural Sciences and Engineering Research Council of Canada (NSERC)  under grants  SAPIN-2018-00027  and  RGPAS-2018-522453  and by the  UKRI Science and Technology Facilities Council (STFC)  grant No. ST/P004008/1. Support from the  National Natural Science Foundation of China , grant No.
Moreover, gamma-ray data are necessary to make correct estimation of neutrino fluxes from point-sources. Several galactic sources, in particular the one detected by the the Milagro Collaboration, have been studied in connection to the possible detection at the IceCube detector with through-going muons  [3] [4] [5] [6] [7]. Recently, the High Altitude Water Cherenkov Observatory (HAWC) has reported new data on galactic sources in recent years, see e. g. [8] [9] [10]. In the 2HWC catalogue  [8] , 39 gamma-ray sources were identified, with an optimal sensitivity at about 7 TeV energies. Subsequently, in the eHWC catalogue of Ref. [10] , nine sources were observed above 56 TeV, all of which are likely Galactic in origin. Among these sources, the eHWC J1825-134 source, located in the southern sky, has been detected with an hard spectrum that extends up to multi-TeV energies, thus it represents a possible PeVatron source.
The compact configuration (TM2, baselines 15 to 704 m) was observed with 42 antennas for an integration time of 11 minutes and a synthesized beam of 0. 31 and the extended (TM1, baselines 21 to 3638m), with 44 antennas for 35 minutes on-source and a synthesized beam of 0. 07. The observations were centred on the nucleus, with a single pointing covering a field of view (FoV) of 18. The galaxy was observed in dual polarization mode with 1. 875 GHz total bandwidth per spectral window, and a channel spacing of 0. 488 MHz corresponding to ∼0. 8 km/s, after Hanning smoothing. The flux calibration was done with radio quasars (J0522-3627, J0519-4546, J0453-3949) close to the position in the sky of the target, which are regularly monitored at ALMA, and resulted in about 10% accuracy. The data from Cycle 3 and 4 were calibrated and concatenated with the CASA software  (version from 4.
5. 3 to 4. 7. 2, (McMullin et al. 2007) , and the imaging and cleaning were performed with the GILDAS software  (Guilloteau & Lucas   The zoom-in of the central 3 ×3 at high resolution (0. 09 ×0. 07 at PA=115 • , contB) is shown in the bottom-right corner. The black cross indicates the adopted phase center, while the white star represents the peak of the continuum emission, assumed to be the AGN position (see Table  1 ). The color scale is in Jy/beam. 2000). The analysis were made in GILDAS together with python packages (radio-astro-tools, APLpy, PySpecKit  Ginsburg et al. 2015; Robitaille & Bressert 2012; Ginsburg & Mirocha 2011). The spectral line maps were obtained after subtraction of the continuum in the uv-plane using the tasks uv_continuum and uv_subtract. Differently than in the paper presenting the data by  Combes et al.
Notes. References: 1: NASA/IPAC Extragalactic Database (NED); 2: (de Vaucouleurs et al. 1991); 3: Veron-Cetty & Veron (1986); 4: Reif et al. (1982); 5: (Dahlem et al. 1990); 6: Combes et al. (2019); 7: (Sanders et al. 2003); 8: this work. ( a ) (α J2000 , δ J2000 ) is the phase tracking center of our interferometric observations. ( b ) Distance is the median values of z-independent distances from NED Steer et al. (2017) ( c ) SFR is derived from infrared luminosity (NED) ( d ) The RA-DEC positions are the new adopted center, derived from the central continuum peak in this work, with an uncertainty of ∼0. 1 (see Sec. 3. 1) ( e ) The RA-DEC positions of the nuclear spiral, used as the kinematical center in Sections 3. 4 and 4. 6.
Acknowledgements. We are very grateful to the referee for very helpful and detailed comments, which improved the presentation of the paper. The  ALMA  staff in Chile and ARC-people at IRAM are gratefully acknowledged for their help in the data reduction. We particularly thank  Philippe Salomé  for useful advice and  Gerold Busch  for the SINFONI data. AA acknowledges financial support by the  Hellenic Foundation for Research and Innovation (HFRI)  and the  General Secretariat for Research and Technology (GSRT) , under the project number  1882  and from the  Spanish MCIU  under grant " Quantifying the impact of quasar feedback on galaxy evolution (QSOFEED) ", with reference  EUR2020-112266 , from the  Consejería de Economía ,  Conocimiento y Empleo del Gobierno de Canarias  and the  European Regional Development Fund (ERDF)  under grant with reference ProID2020010105.
We made use of the  NASA/IPAC Extragalactic Database (NED) , and of the HyperLeda database. This research made use of Astropy, a community developed core Python package for Astronomy. This work was supported by the  Programme National Cosmology and Galaxies(PNCG)  of  CNRS  (INSU with  INP  and  IN2P3 ), co-funded by  CEA , and  CNES.