The L2 acquisition of Spanish non-nominative subjects by adult L1 English speakers

This study investigates the adult second language (L2) acquisition of non- nominative, non-agentive subjects, a particular feature of the Spanish language also shared by other Indo-European and South Asian languages. The existence of non- nominative elements in Spec, IP with subject-like properties is well-documented in the literature. One of the first attempts to account for this phenomenon in Romance languages is Belletti and Rizzi (1988) on Italian. Masullo (1992, 1993) extends the analysis to Spanish, proposing the Non-Nominative Subject (NNSub) Parameter, whereby a language allows NNSubs as part of its core grammar only if nominative case is assigned in situ. Spanish NNSubs can appear in unaccusative, dethematized, as well as impersonal constructions, and can be dative, accusative, or locative. These constituents are shown in Masullo (1992, 1993) not to occupy an A-bar position above IP, like topics and left-dislocated constituents, but rather Spec, IP, moving from the VP to satisfy the Extended Projection Principle. Languages like English and French, in which nominative case is checked in Spec, BP, disallow NNSubs.The aim of this study is to understand the processes involved in the acquisition language (LI) in the process of acquisition. A study involving three groups of adult English L2 learners of Spanish at a British university and a control group was carried out to determine if L2 learners with a [-NNSub] LÍ setting can reset the parameter to the Spanish [+NNSub] value. The learners belonged to one of three language levels: Intermediate, Advanced and Advanced+ according to the number of years spent at university and their contact with Spanish in a Spanish speaking country. The test battery involved an aural preference task, an elicited imitation task, and a picture description task. Hypothesis A predicted that Intermediate L2 learners would show clear L1 effects on their data and that the NNSub parameter would not show resetting. Hypothesis в predicted that the more advanced L2 learners would be able to reset the NNSub parameter to accommodate NNSubs and dative case in their interlanguage. Results from the aural preference and the elicited imitation tasks show correspondence between the results per category in both tasks. Knowledge of unaccusativity and NNSubs develops steadily up to the Advanced level but it suffers a decline with the Advanced+ learners. Results from the picture description task show that competence increases from the Intermediate to the Advanced level but that the percentage of non-target forms either stays at the same level or goes up with respect to the Advanced+ group. This regression seen in the Advanced^ data might be explained by the recent exposure to naturalistic input that the Advanced learners had just had. The L2 data do not show enough evidence that the NNSub parameter has been reset. Most of the grammatical utterances contain the verbs gustar 'like' and doler 'hurt', verbs which are part of the teaching curriculum. On the other hand, grammatical utterances involving other unaccusative verbs with NNSubs are rare. The fact that teaching of these verbs is insufficient does not help the L2 learners overcome the learnability problem posed by the input. This problem stems from the L2 input not showing clear-cut signals to tell learners which verbs require a NNSub. In addition to this, native speakers' use of optional structures to substitute the constructions with NNSubs makes NNSubs even less salient in the input

First detection of the 448 GHz H2O transition in space

We present the first detection of the ortho-H2O 4_23-3_30 transition at 448 GHz in space. We observed this transition in the local (z = 0.010) luminous infrared (IR) galaxy ESO 320-G030 (IRAS F11506-3851) using the Atacama Large Millimeter/submillimeter Array (ALMA). The water 4_23-3_30 emission, which originates in the highly obscured nucleus of this galaxy, is spatially resolved over a region of ~65 pc in diameter and shows a regular rotation pattern compatible with the global molecular and ionized gas kinematics. The line profile is symmetric and well fitted by a Gaussian with an integrated flux of 37.0 +- 0.7 Jy km s-1 . Models predict this water transition as a potential collisionally excited maser transition. On the contrary, in this galaxy, we find that the 4_23-3_30 emission is primarily excited by the intense far-IR radiation field present in its nucleus. According to our modeling, this transition is a probe of deeply buried galaxy nuclei thanks to the high dust optical depths (tau_100{\mu}m > 1, N_H > 1e24 cm-2) required to efficiently excite it.Comment: Accepted for publication in A&A Letters; 4 pages, 5 figure

Contenido de fosfátidos en el aceite de soja en función del contenido de humedad en la cosecha y el tiempo de almacenamiento del poroto

The influence of soybean moisture content-at-harvest and storage time upon total and non-hydratable phosphatides content in oil and bean phospholipase D activity was evaluated. Tests were performed upon soybeans harvested with moisture contents between 14.4 and 33.3% weight wet basis (wb). They were air dried at 25ºC until achieving safe storage moisture contents between 12.8 and 13.5 % wb and were stored at the same temperature for 245 days. Periodically they were analyzed for total and non-hydratable phosphatides content and phospholipase D activity. Total phosphatides initial content was high in soybeans with higher initial moisture levels and decreased slightly with time. Total phosphatides content remained constant at their initial levels in soybeans with lower initial moisture content. Non-hydratable phosphatides content was related to the phospholipase D activity, which decreased 30–35 days after harvest, and then stabilized, with values between 3.0 x 10-4 and 3.8 x 10-4 choline mmol/(min • soybean g).Se evaluó la influencia del contenido de humedad en la cosecha y el tiempo de almacenamiento del poroto de soja sobre el contenido de los fosfátidos totales y no hidratables en el aceite y la actividad de la fosfolipasa D en el poroto. Los porotos fueron cosechados con humedades entre el 14.4 y 33.3 %, secados con aire a 25 ºC hasta 12.8 - 13.5 % y almacenados durante 245 días. Periódicamente se determinó el contenido de fosfátidos y la actividad de la fosfolipasa D. Para los valores más altos de humedad, el contenido inicial de fosfátidos totales fue alto, disminuyendo con el tiempo. En los porotos con humedades más bajas el contenido de fosfátidos totales se mantuvo en sus valores iniciales. El contenido de fosfátidos no hidratables está relacionado con la actividad de la fosfolipasa D, la cual disminuye hasta 30-35 días después de la cosecha y luego se estabiliza en valores entre 3.0 x 10-4 y 3.8 x 10-4 mmol de colina/(min • g de soja)

TIMASSS: The IRAS16293-2422 Millimeter And Submillimeter Spectral Survey. I. Observations, calibration and analysis of the line kinematics

While unbiased surveys observable from ground-based telescopes have previously been obtained towards several high mass protostars, very little exists on low mass protostars. To fill up this gap, we carried out a complete spectral survey of the bands at 3, 2, 1 and 0.8 mm towards the solar type protostar IRAS16293-2422. The observations covered about 200\,GHz and were obtained with the IRAM-30m and JCMT-15m telescopes. Particular attention was devoted to the inter-calibration of the obtained spectra with previous observations. All the lines detected with more than 3 sigma and free from obvious blending effects were fitted with Gaussians to estimate their basic kinematic properties. More than 4000 lines were detected (with sigma \geq 3) and identified, yielding a line density of approximatively 20 lines per GHz, comparable to previous surveys in massive hot cores. The vast majority (~2/3) of the lines are weak and due to complex organic molecules. The analysis of the profiles of more than 1000 lines belonging 70 species firmly establishes the presence of two distinct velocity components, associated with the two objects, A and B, forming the IRAS16293-2422 binary system. In the source A, the line widths of several species increase with the upper level energy of the transition, a behavior compatible with gas infalling towards a ~1 Mo object. The source B, which does not show this effect, might have a much lower central mass of ~0.1 Mo. The difference in the rest velocities of both objects is consistent with the hypothesis that the source B rotates around the source A. This spectral survey, although obtained with single-dish telescope with a low spatial resolution, allows to separate the emission from 2 different components, thanks to the large number of lines detected. The data of the survey are public and can be retrieved on the web site http://www-laog.obs.ujf-grenoble.fr/heberges/timasss.Comment: 41 pages (26 pages of online Tables), 7 Tables and 6 Figure

Variable broad lines and outflow in the weak blazar PBC J2333.9-2343

Indexación: Scopus; Scielo.Funding text #1 1Instituto de Física y Astronomía, Facultad de Ciencias, Universidad de Valparaíso, Gran Bretaña 1111, Playa Ancha, Valparaíso, Chile 2INAF – Istituto di Astrofisica e Planetologia Spaziali di Roma (IAPS-INAF), Via del Fosso del Cavaliere 100, I-00133 Roma, Italy 3INAF – Osservatorio Astronomico di Roma, via Frascati 33, I-00078 Monte Porzio Catone, Italy 4Excellence Cluster Universe, Technische Universität München, Boltzmannstr. 2, D-85748, Garching, Germany 5European Southern Observatory, Karl-Schwarzschild-Str 2, D-85748 Garching b. München, Germany 6Instituto Nacional de Astrofísica, Óptica y Electrónica, Apartado Postal 51-216, 72000 Puebla, México 7Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany 8International Max Planck Research School of Astronomy and Astrophysics at the Universities of Bonn and Cologne, Auf dem Hügel 69, D-53121 Bonn, Germany 9INAF – Osservatorio di Astrofisica e Scienza dello Spazio, via Gobetti 93/3, I-40129 Bo...View all Funding text #2 We acknowledge the referee, M. Villar Martín, for her comments and suggestions that helped to improve the paper. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester, the NASA/IPAC extragalactic database (NED), the STARLIGHT code, and the IRAF software. Based upon observations carried out at the Observatorio Astronómico Nacional on the Sierra San Pedro Mártir (OAN-SPM), Baja California, México. LHG and FP acknowledge the ASI/INAF agreement number 2013-023-R1, LHG partial support from FONDECYT through grant 3170527, MP from ESSTI under the MoST, and from MINECO through research projects AYA2013-42227-P and AYA2016-76682-C3-1-P (AEI/FEDER, UE), LHG and SC from the Spanish grant AYA2013-42227-P, VC by CONACyT research grant 280789, EFJA from the Collaborative Research Center 956, subproject A1, funded by DFG, and GV from the DFG Cluster of Excellence ‘Origin and Structure of the Universe’ (www.universe-cluster.de).PBC J2333.9-2343 is a peculiar active nucleus with two giant radio lobes and a weak blazarlike nucleus at their centre. In this work we show new optical, ultraviolet (UV), and X-ray data taken from the San Pedro Mártir telescope, the New Technology Telescope, NTT/EFOSC2, and the Swift/XRT satellite. The source is highly variable at all frequencies, in particular the strongest variations are found in the broad Hα component with a flux increase of 61±4 per cent between 2009 and 2016, following the X-ray flux increase of 62±6 per cent between 2010 and 2016. We also detected a broad Hβ component in 2016, making the optical classification change from type 1.9 to type 1.8 in 1 yr. We have also detected a broad component of the [OIII]λ5007 line, which is blue-shifted and of high velocity, suggesting an origin from a highly disturbed medium, possibly an outflow. The line flux variability and broad widths are indicative of a jet that is, at least in part, responsible for the ionization of the broad line region (BLR) and narrow line region (NLR). © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.https://academic.oup.com/mnras/article-abstract/478/4/4634/4999938?redirectedFrom=fulltex

Implementation of a multi-zone numerical blow-by model and its integration with cfd simulations for estimating collateral mass and heat fluxes in optical engines

Nowadays reducing green-house gas emissions and pushing the fossil fuel savings in the field of light-duty vehicles is compulsory to slow down climate change. To this aim, the use of new combustion modes and dilution strategies to increase the stability of operations rich in diluent is an effective technique to reduce combustion temperatures and heat losses in throttled operations. Since the combustion behavior in those solutions highly differs from that of typical market systems, fundamental analyses in optical engines are mandatory in order to gain a deep understanding of those and to tune new models for improving the mutual support between experiments and simulations. However, it is known that optical accessible engines suffer from significant blow-by collateral flow due to the installation of the optical measure line. Thus, a reliable custom blow-by model capable of being integrated with both mono-dimensional and three-dimensional simulations was developed and validated against experimental data. The model can work for two different configurations: (a) stand-alone, aiming at providing macroscopic data on the ignitable mixture mass loss/recover through the piston rings; (b) combined, in which it is integrated in CFD engine simulations for the local analysis of likely collateral heat release induced by blow-by. Furthermore, once the model was validated, the effect of the engine speed and charge dilution on the blow-by phenomenon in the optical engine were simulated and discussed in the stand-alone mode. © 2021 by the authors. Licensee MDPI, Basel, Switzerland

Ultracold collisions of oxygen molecules

Collision cross sections and rate constants between two ground- state oxygen molecules are investigated theoretically at translational energies below $\sim 1$K and in zero magnetic field. We present calculations for elastic and spin- changing inelastic collision rates for different isotopic combinations of oxygen atoms as a prelude to understanding their collisional stability in ultracold magnetic traps. A numerical analysis has been made in the framework of a rigid- rotor model that accounts fully for the singlet, triplet, and quintet potential energy surfaces in this system. The results offer insights into the effectiveness of evaporative cooling and the properties of molecular Bose- Einstein condensates, as well as estimates of collisional lifetimes in magnetic traps. Specifically, $^{17}O_{2}$ looks like a good candidate for ultracold studies, while $^{16}O_{2}$ is unlikely to survive evaporative cooling. Since $^{17}O_{2}$ is representative of a wide class of molecules that are paramagnetic in their ground state we conclude that many molecules can be successfully magnetically trapped at ultralow temperatures.Comment: 15 pages, 9 figure

Optical Spectroscopy of nearby type1-LINERs

We present the highlights from our recent study of 22 local (z$<$0.025) type-1 LINERs from the Palomar Survey, on the basis of optical long-slit spectroscopic observations taken with TWIN/CAHA, ALFOSC/NOT and HST/STIS (Cazzoli et al. 2018). Our goals were threefold: (a) explore the AGN- nature of these LINERs by studying the broad (BLR-originated) H$\alpha$ component; (b) derive a reliable interpretation for the multiple narrow components of emission lines by studying their kinematics and ionisation mechanism (via standard BPTs); (c) probe the neutral gas in the nuclei of these LINERs for the first time. Hence, kinematics and fluxes of a set of emission lines, from H$\beta$ to [SII], and the NaD doublet in absorption have been modelled and measured, after the subtraction of the underlying light from the stellar component.Comment: Proceedings of the IAU Symposium 356, 'Nuclear activity in galaxies across cosmic time'. Based on Cazzoli et al. 2018, MNRAS, 480, 1106 available at https://academic.oup.com/mnras/article/480/1/1106/505038

Molecular vibration in cold collision theory

Cold collisions of ground state oxygen molecules with Helium have been investigated in a wide range of cold collision energies (from 1 $\mu$K up to 10 K) treating the oxygen molecule first as a rigid rotor and then introducing the vibrational degree of freedom. The comparison between the two models shows that at low energies the rigid rotor approximation is very accurate and able to describe all the dynamical features of the system. The comparison between the two models has also been extended to cases where the interaction potential He - O$_2$ is made artificially stronger. In this case vibration can perturb rate constants, but fine-tuning the rigid rotor potential can alleviate the discrepancies between the two models.Comment: 11 pages, 3 figure

Unexplored outflows in nearby low luminosity AGNs: the case of NGC 1052

Outflows play a central role in galaxy evolution shaping the properties of galaxies. Understanding outflows and their effects in low luminosity AGNs, such as LINERs, is essential (e.g. they are a numerous AGN population in the local Universe). We obtained VLT/MUSE and GTC/MEGARA optical IFS-data for NGC1052, the prototypical LINER. The stars are distributed in a dynamically hot disc, with a centrally peaked velocity dispersion map and large observed velocity amplitudes. The ionised gas, probed by the primary component is detected up to $\sim$30arcsec ($\sim$3.3 kpc) mostly in the polar direction with blue and red velocities ($\mid$V$\mid$$<$250 km/s). The velocity dispersion map shows a notable enhancement ($\sigma$$>$90 km/s) crossing the galaxy along the major axis of rotation in the central 10arcsec. The secondary component has a bipolar morphology, velocity dispersion larger than 150 km/s and velocities up to 660 km/s. A third component is detected but not spatially resolved. The maps of the NaD absorption indicate optically thick neutral gas with a velocity field consistent with a slow rotating disc ($\Delta$V = 77$\pm$12 km/s) but the velocity dispersion map is off-centred without any counterpart in the flux map. We found evidence of an ionised gas outflow with mass of 1.6$\pm$0.6 $\times$ 10$^{5}$ Msun, and mass rate of 0.4$\pm$0.2 Msun/yr. The outflow is propagating in a cocoon of gas with enhanced turbulence and might be triggering the onset of kpc-scale buoyant bubbles (polar emission). Taking into account the energy and kinetic power of the outflow (1.3$\pm$0.9 $\times$ 10$^{53}$ erg and 8.8$\pm$3.5 $\times$ 10$^{40}$ erg/s, respectively) as well as its alignment with both the jet and the cocoon, and that the gas is collisionally ionised, we consider that the outflow is jet-powered, although some contribution from the AGN is possible.Comment: A&A accepted 04/04/2022, 31 pages, 12 figures and 3 appendixe