dataesr/scientific-paragraphs-categorization huggingface dataset:
Acknowledgements We are grateful to  Sara Ketelsen  from the  American Museum of Natural History ,  Daniel Klingberg  from the  Zoological Museum of the University of Copenhagen (Denmark ),  Cécile Blondel  from the  Muséum National d'Histoire Naturelle of Paris ,  Jorge Vélez-Juarbe  from the  Natural History Museum of Los Angeles County , and  Carlos Rojo  from the  Oceanográfic of Valencia (Spain ) for kindly providing access to the specimens under their care through project number  OCE-06-21. This study has been funded by the  Spanish Ministry of Economy and Competitiveness (MINECO)  (grant numbers  CGL2015-68300P  and  PID2019-111185GB-I00 ) and  Junta de Andalucía  ( P18-FR-3193 ) to B. F.
6 ). As most modern terrestrial inorganic zinc has a relatively narrow range of δ 66 Zn values (Fig. 5 ), the wide range observed in the dataset suggest different Zn sources control the isotopic signatures. These sources provide estimates to contributions which drive the secular change previously reported for Zn isotopes. We will discuss these processes alongside the variations in δ 13 C and δ 66 Zn values and the decoupling of the two isotope systems.
An important focal point of the work has been to address the issue of local versus non local sources of environmental change in this time period. The Zn isotopic variations are measured in several regions of Namibia, suggesting that these signals may record localized events (Site 1, C14, C15), without ruling out global events with impact of local geochemical signatures. These isotopic variations are more likely to be the result of biological fractionation of Zn isotopes  (Isson et al. 2018) , with isotope ratios below the continental average being non-uniquely characteristic of biological processes. These data further support the role of local biological processes, as one would not expect a homogeneous global recovery of the biosphere, and variations in a smaller local reservoir may produce an amplified signal due to mass conservation requirement for a smaller environment.
Acknowledgements We are grateful for support by the  Geological Survey of Namibia  and its then director  Gabi Schneider  with relation to fieldwork organization and sample export management. We would like to thank the handling editors, particularly guest editor  Eugen Libowitzky. We would like to thank the many reviewers of this manuscript, anonymous as well as otherwise. In particular, our thanks to (alphabetically),  Andrey Bekker ,  Philippe Claeys ,  Steven Goderis ,  Julia Parlato , and  Peter Sprung  for their revisions. The scholarly and insightful comments from  Paul F. Hoffman  were of great help in this final iteration. Nasrin Marzban  is gratefully acknowledged for travel expenses.
g. laser ablation inductively coupled plasma mass spectrometry, LA-ICP-MS; Secondary Ion Mass Spectrometry, SIMS). This has the potential to impact on the calculated dates, and result in apparently disturbed isotopic datasets  (Seydoux-Guillaume et al. 2003; Kusiak et al. 2013 Kusiak et al. , 2015;; Peterman et al. 2016). Evidence of mineralogical processes that affect geochronometers and that induce element mobility may be recorded within the crystal. The benefits of examining geochronometers at the nanoscale using transmission electron microscopy (TEM) and atom probe tomography (APT) to address broader issues of element mobility has been demonstrated for zircon  (Utsunomiya et al. 2004; Kusiak et al. 2015 Kusiak et al. , 2019;; Valley et al. 2015; Peterman et al. 2016 Peterman et al. , 2019;; Piazolo et al.
2018). The discordance has been attributed to the presence of nanophases that contain inherited Pb*  (Turuani et al. 2022). The monazite host that lacks Pb*-bearing nanophases has been dated by atom probe at 1. 02 ±0. 26 Ga  (Turuani et al. 2022) , corresponding within error to the lower intercept of the discordia formed by the total monazite dataset, at 1. 09-1. 05 Ga (ID-TIMS and LA-ICP-MS respectively;  Black et al. 1984 , Turuani et al. 2022). This age reflects the amphibolite facies retrogression associated with reworking during the Rayner Structural Episode  (Black et al. , 1983 (Black et al. , , 1987;; Kelly et al. 2000 Kelly et al. , 2002;; Halpin et al. 2005; Horie et al. 2016) , which induced resetting of the U-Th-Pb chronometers at the nanoscale in monazite  (Turuani et al. 2022).
Chemical mapping of Mnz13 was carried out using a CAMECA SXFive FE under condition of 7 kV and 100 nA. Additional analytical details are given in Table  S1. Electron backscatter diffraction analyses (EBSD) were undertaken on Mnz13 using a Tescan Lyra3 focused ion beam (FIB) coupled with a SEM, hosted in the John de Laeter Centre at Curtin University in Perth (Australia). The instrument is equipped with an EBSD detector. Data acquisition was conducted under conditions of 20 kV and 149 µA, with a step size of 0. 07 µm, a spot size of 27 nm, a beam intensity of 16 and a working distance of 12. 5 mm.
Atom probe tomography (APT) Eleven atom probe specimens were lifted-out from three monazite crystals (Mnz25, MzA2, Mnz17) and prepared using the Tescan Lyra3 dual Ga + FIB/SEM at Curtin University. More detailed process for the lift-out and targeting methods are described in  Thompson et al. (2007)  and  Rickard et al. (2020). Atom probe analyses were conducted at the Geoscience Atom Probe Facility at Curtin University. The Cameca LEAP 4000X HR instrument was set to a base specimen temperature of 60 K and detection rate of 0. 01 atoms/pulse (1%). In order to optimize acquisition, field evaporation was controlled by a UV laser (λ=355 nm) pulsed at 125 kHz with a pulse energy of 300 pJ for monazite and 30 pJ for galena. Data processing and reconstruction was performed using Cameca's IVAS v3.
8. 4 and AP Suite 6 software. Both atomic and molecular ions, with charge states of 1+ to 3+ were identified in the time-of-flight spectrometry mass/charge spectra. For reconstructing the atom probe data an evaporation field of 27. 02 V/nm and an atomic average for monazite of 0. 01245 nm 3 /atom were used following the recommendations of  Fougerouse et al. (2022). More details are available in Table  S2.
The more Pb* precipitates within monazite crystals as Pb*-bearing nanophases, the less potential there is for Pb* loss from monazite at the grain scale when a second high-grade metamorphic event is superimposed on a much older event in which the monazite initially crystallized. Finally, this study provides new insights for interpretations of dispersed isotopic data. Discordant isotopic datasets may actually provide a record of the effects of several geological events and nanoscale studies are then required to unveil the cryptic signatures of those events. Indeed, in this sample, only nanoscale results have been able to provide evidences to identify the record of the 0. 55 Ga event in the geochronometer  (Turuani et al. 2022 ) and hence to correctly interpret the dispersion in the dataset obtained from several monazite grains.
Coherent observations in GNSS reflectometry are prominent in regions with smooth reflecting surfaces and at grazing elevation angles. However, within these lower elevation ranges, GNSS signals traverse a more extensive atmospheric path, and increased ionospheric effects (e. g. , delay biases) are expected. These biases can be mitigated by employing dual-frequency receivers or models tailored for single-frequency receivers. In preparation for the single-frequency GNSS-R ESA "PRETTY" mission, this study aims to characterize ionospheric effects under variable parameter conditions: elevation angles in the grazing range (5 • to 30 • ), latitude-dependent regions (north, tropic, south) and diurnal changes (day and nighttime). The investigation employs simulations using orbit data from Spire Global Inc.
In the work presented in  [8] , a methodology was introduced for sTEC estimation along the paths of incident and reflected signal rays. This estimation is based on coherent dual-frequency GNSS-R measurements obtained from Spire Global low Earth orbit (LEO) CubeSats. The outcomes have demonstrated a favorable alignment between reflectometry sTEC estimations and the global ionospheric TEC maps (GIM). Furthermore, an algorithm outlined in  [9]  combines sTEC observation from space-borne reflectometry using CubeSats and data collected from ground-based GNSS stations to generate vertical TEC (vTEC) maps in the Arctic region. Simulations conducted within this study under diverse conditions, involving variations in temporal resolution, solar activity levels, and the number of reflection events, have demonstrated enhanced accuracy in vTEC estimations when coherent GNSS-R observations are incorporated.
The outcomes have demonstrated a favorable alignment between reflectometry sTEC estimations and the global ionospheric TEC maps (GIM). Furthermore, an algorithm outlined in  [9]  combines sTEC observation from space-borne reflectometry using CubeSats and data collected from ground-based GNSS stations to generate vertical TEC (vTEC) maps in the Arctic region. Simulations conducted within this study under diverse conditions, involving variations in temporal resolution, solar activity levels, and the number of reflection events, have demonstrated enhanced accuracy in vTEC estimations when coherent GNSS-R observations are incorporated. In the domain of GNSS-R, it has been empirically established that coherent observations are more frequently observed in the presence of smooth reflecting surfaces, such as sea ice, regions with low sea states, or inland waters, and at low grazing angles  [10] [11] [12].
It analyzes variability in the ionospheric group delay, Doppler shift, and peak electron density height. Additionally, the uncertainty in model-based ionospheric corrections for GNSS-R group delay altimetry is assessed. The analysis is based on utilizing the sTEC obtained from three-dimensional, timedependent models. To assess model uncertainty, the sTEC values computed using the Neustrelitz Electron Density Model (NEDM2020)  [18]  are used as a reference and compared with the sTEC retrievals from NeQuick 2. Simulations are conducted to replicate conditions similar to those of the PRETTY mission, utilizing orbit data from the GNSS-R Spire Global Lemur-2 constellation. To provide a comprehensive analysis, the results are categorized into three elevation angle ranges: very-low (5   The structure of this paper is outlined as follows: Section 2 presents the GNSS-R data descriptions, reflection events, and ray point settings for the simulations.
Hm is obtained for both the incident and reflected rays using the NEDM2020 model. The LEO GNSS-R space-borne configuration, which enables the simultaneous collection of data from multiple reflections, presents several advantages for ionospheric studies. Firstly, thanks to the fast trajectory change of the LEO satellite, the GNSS-R signal rapidly scans along the ionospheric layers, providing a snapshot view of ionospheric structures  [8]. Secondly, the ability to obtain peak electron density points at different locations within a short time interval allows for the mapping of ionospheric structures at varying distances. Assuming the Earth's radius is 6371 km, with a maximum electron density ionospheric shell at a 300 km height, the distance between the incident and reflected Hm points varies depending on the elevation angle as observed in Figure  6.
The LEO GNSS-R space-borne configuration, which enables the simultaneous collection of data from multiple reflections, presents several advantages for ionospheric studies. Firstly, thanks to the fast trajectory change of the LEO satellite, the GNSS-R signal rapidly scans along the ionospheric layers, providing a snapshot view of ionospheric structures  [8]. Secondly, the ability to obtain peak electron density points at different locations within a short time interval allows for the mapping of ionospheric structures at varying distances. Assuming the Earth's radius is 6371 km, with a maximum electron density ionospheric shell at a 300 km height, the distance between the incident and reflected 𝐻𝑚 points varies depending on the elevation angle as observed in Error! Reference source not found.
Discussion The analysis provides valuable insights into how ionospheric parameters such as slant total electron content, relative ionospheric delay, Doppler shift, and peak electron density height vary in response to different conditions. These findings are crucial for optimizing the accuracy of space-borne GNSS-R applications, particularly in altimetry, aiding in the development of robust models, and enhancing the interpretation of data acquired through grazing GNSS-R configurations. Under low-solar-activity conditions (F10. 7 = 75), the resulting sTEC values from NEDM2020 and NeQuick 2 reveal that both models exhibit similar behavior across different scenarios. However, it is important to note that while an extensive evaluation of the models is not carried out in this study, differences in the sTEC computations and the relative total delay are observed.
Extended temporal coverage is essential for deciphering these patterns, especially in dynamic regions allowing analysis of seasonal trends. This study highlights the importance of spatially extended data, particularly in tropical areas with substantial ionospheric variability. Such data is key to comprehending ionospheric parameter evolution across different time scales and regions, influenced by factors like solar activity and geomagnetic storms. GNSS-R (global navigation satellite system reflectometry) stands as a valuable and complementary remote sensing tool in ionospheric studies, effectively addressing areas not covered by alternative methods. This capacity offers significant contributions to the modeling, prediction, and comprehension of ionospheric effects.
Acknowledgements. This study was supported by the  Strategic Priority Research Program of Chinese Academy of Sciences  ( XDA20100300 ) and the  Swiss National Science Foundation  ( 200021E_177652/1 ). 10 https://doi. org/10. 5194/tc-2022-203Preprint. Discussion started: 11 October 2022 c Author(s)  2022. CC BY 4. 0 License.
Context. Understanding the earliest stages of star formation, and setting it in the context of the general cycle of matter in the interstellar medium, is a central aspect of research with the James Webb Space Telescope (JWST). Aims. The JWST program JOYS (JWST Observations of Young protoStars) aims to characterize the physical and chemical properties of young high-and low-mass star-forming regions, in particular the unique mid-infrared diagnostics of the warmer gas and solid-state components. We present early results from the high-mass star formation region IRAS 23385+6053. Methods. The JOYS program uses the Mid-Infrared Instrument (MIRI) Medium Resolution Spectrometer (MRS) with its integral field unit (IFU) to investigate a sample of high-and low-mass star-forming protostellar systems. Results.
Only a few space-based studies at lower angular resolution with the Infrared Space Observatory (ISO) ⋆ Data (FITS files) are available at the CDS via anonymous ftp to cdsarc. cds. unistra. fr  (130. 79. 128. 5)  or via https:// cdsarc. cds. unistra. fr/viz-bin/cat/J/A+A/673/A121 and Spitzer are reported (e. g. ,  Whittet et al. 1996; van Dishoeck et al. 1998; Gibb et al. 2000; Molinari et al. 2008; An et al. 2011). The most comprehensive ISO legacy study on high-mass protostars is presented in  Gibb et al. (2004). The situation has now changed dramatically with the advent of the James Webb Space Telescope (JWST), launched on December 25, 2021, just a little more than a year ago at the time of writing. Scientific data delivery began only in July 2022, and we present the first results from the European Mid-Infrared Instrument (MIRI) Guaranteed Time Program JWST Observations of Young protoStars (JOYS; PI: E.
For high-mass regions at more typical distances of ∼3 kpc, the linear resolution corresponds roughly to 570, 1740, and 2880 au. We use a set of key diagnostics in the mid-infrared band between 5 and 28 µm, including the continuum spectral energy distribution, a range of atomic and molecular gas lines, and several solid-state bands. More details about the JOYS project will be presented in a forthcoming publication by  van Dishoeck et al. , (in prep. ). Here, we focus on analyzing and interpreting JWST data of the first source fully observed within the JOYS program, the high-mass protostellar object IRAS 23385+6053. This highmass star-forming region was originally identified by IRAS (Infrared Astronomical Satellite) color selection and association with H 2 O maser emission  (Casoli et al. 1986; Cesaroni et al.
The data are not background-subtracted. The error bars at 19 and 21 µm show the approximate 1σ rms below and above 20 µm of ∼0. 5 and ∼2 mJy (note the log-scale), respectively (Sect. 2). Extended Millimeter Array (NOEMA) large program CORE, which studied the physical and chemical properties of 20 highmass star-forming regions  (Beuther et al. 2018; Gieser et al. 2021). A detailed case study of IRAS 23385+6053 from the CORE project is presented in  Cesaroni et al. (2019). Based on the line and continuum emission,  Cesaroni et al. (2019)  identified six cores, a new outflow candidate in the northwest-southeast direction (Fig. 1 , middle panel), and a tentative detection of a disk around a ∼9 M ⊙ protostar within the most massive millimeter core, mmA1 (Fig. 1 , right panel). This first paper in the JOYS series presents an overview of the MIRI spectrum and then focuses on the continuum emission and a few selected molecular and atomic lines (H 2 (0-0)S(  7 ), [FeII]( 4 F 9/2 -6 D 9/2 ), [NeII]( 2 P 1/2 -2 P 3/2 ) and Humphreys α HI(7-6)).
Observations IRAS 23385+6053 was observed within the European MIRI Guaranteed Time Observations (GTO) program JOYS (proposal ID 1290) for 2. 12 h on August 22, 2022. The entire MIRI bandpass from ∼4. 9 to ∼28. 0 µm was covered in a 4-field mosaic (Fig. 1 ) around the central position of right ascension (RA; J2000. 0) 23:40:54. 497 and declination (Dec; J2000. 0) +61:10:27. 83. The total exposure time in each the three MIRI spectral filters was 200 sec, and parallel off-source imaging was conducted in the F1500W filter. A complementary background field was observed for overall background subtraction that is needed, for example an analysis of the broadband ice features. While the full-wavelength spectrum in Fig. 3  shows the nonbackground-subtracted data, all individual narrow gas spectral line data presented in this paper were continuum-subtracted by fitting a polynomial baseline to narrow wavelength ranges around these lines.
We reduced the data using a development version of the JWST calibration pipeline  (Bushouse et al. 2022) with v. 11. 16. 16  and Calibration Reference Data System (CRDS) context "jwst_1017. pmap", respectively. We used this development version as it includes cosmic ray shower flagging in the jump step of the Detector1Pipeline. The pipeline includes fringe correction via Spec2Pipeline using a fringe flat field derived from spatially extended sources  (Mueller et al. , in prep. ). We further reduced the fringing by applying the residual_fringe step  (Kavanagh et al. , in prep. ) , which is included in the JWST calibration pipeline package but not switched on by default. As discussed in  Pontoppidan et al. (2022) , the accuracy of spacecraft pointing information for MRS exposures can be affected by guide star catalog errors and roll uncertainty.
H 2 , [FeII], and [NeII] line emission The MIRI spectral line data now allow us to get a better understanding of the underlying outflow structures in IRAS 23385+6053. While  Molinari et al. (1998)  reported one outflow roughly in the north-south direction,  Cesaroni et al. (2019)  recently suggested that a second outflow in the northwestsoutheast direction should also exist (Fig. 1 , right panel). The shocked H 2 emission as well as CH 3 OH maser emission at 44 and 95 GHz additionally confirm the existence of shocked gas  (Kurtz et al. 2004; Wolf-Chase et al. 2012). Here, we focus on the high-spatial-resolution H 2 (0-0) S(7) line at 5. 511 µm and the [FeII]( 4 F 9/2 -6 D 9/2 ) line at 5. 34 µm. Furthermore, we compare the results with SiO(2-1) data at 3. 6 mm wavelengths obtained with NOEMA as part of the CORE+ project  (Gieser et al.
37 µm. Rigliaco et al. (2015)  explored this HI(7-6) line at 12. 37 µm in Spitzer data of classical T Tauri stars, and they found a tentative correlation between the integrated HI(7-6) luminosity and the accretion luminosity. We now explore this relation also for IRAS 23385+6053. Figure  9  presents the spectrum of the HI(7-6) line extracted from the position in between mid-infrared sources A and B, and averaged over an aperture with radius Fig. 9. HI(7-6) spectrum at 12. 37 µm centered right in the middle between sources A and B (Fig. 4 ) and averaged over an aperture with radius 2 ′′. The red line presents a single Gaussian fit to the spectrum, whereas the blue line shows a two-component Gaussian fit to the spectrum. of 2 ′′. While the red line shows a single Gaussian fit, the blue line presents a two-component Gaussian fit.
Other HI emission lines (e. g. , HI(6-5) or HI(8-7)) are also in the observed bandpass but remain undetected in IRAS23395+6053. Therefore, more observations of other high-mass star-forming regions are required to explore the capability of tracing accretion with the HI(7-6) and other recombination lines in more depth. This will become possible, given the fact that most JOYS targets are still pending in the JWST queue. With a sample of approximately two dozen regions, sufficient data will become available to derive statistically unambiguous values. The present work is a first step toward realizing this.
Our investigation of a potential accretion rate tracer, the Humphreys α HI(7-6) line, revealed a 3-4σ detection. Using the relation between integrated HI(7-6) line luminosity and accretion luminosity, and depending on extinction correction, we can estimate accretion luminosities to be between 142 and 5070 L ⊙. Assuming furthermore a reasonable protostellar mass and radius, these luminosities convert to accretion rate estimates of between ∼2. 6 × 10 -6 and ∼0. 9 × 10 -4 M ⊙ yr -1. Putting this in context with an accretion rate estimate based on outflow observations, IRAS 23385+6053 may already be close to the end of the main accretion phase. However, with data for one region so far, and with only a 3-4σ detection, these results have to be taken with a bit of caution. Observations of more high-mass star-forming regions are needed to further evaluate the possibility of estimating accretion rates with the HI(7-6) line.
Nevertheless, the present work shows that the Humphreys α line has the potential to become an important accretion rate tracer with JWST. Future MIRI observations, also within the JOYS program, will set much tighter constraints on that. In summary, these first JWST MIRI MRS observations of a high-mass star-forming region reveal important new results of the protostellar distribution, the outflow properties, and the accretion rates in IRAS 23385+6053. The complementary atomic and molecular gas lines as well as the ice features are discussed in companion papers. While interesting in themselves, these data notably show the enormous potential for JWST to boost star formation research.