The National Agricultural Technology Institute (Spanish: Instituto Nacional de Tecnología Agropecuaria), commonly known as INTA, is an Argentine federal extension agency in charge of the generation, adaptation and diffusion of technologies, knowledge and learning procedures for the agriculture, forest and agro-industrial activities within an ecologically clean environment.Even though the institute, created in 1956, depends on the Secretary of Agriculture, Livestock, Fishing and Food of the Ministry of Economy and Production, it has financial and operative autarkic autonomy given by law 25641/02 that provides the Institute with the 0.5% of the importations.
As the James Webb Space Telescope (JWST) pursues its observing journey, several thousands of icy-grain spectra are expected to be measured and analysed. The inventory of ices in particular, via the observations of background sources, is accessible for hundreds of lines of sight (LOSs) per molecular-cloud region, opening the possibility to add strong constraints on the solid phase chemistry in a vast domain of cloud densities. SynthIceSpec is a synthetic infrared (IR) spectrum generator that has been designed as a tool to support observing proposals and to test the outcome of chemical models. It is based on laboratory measurements of pure and mixed ices, where each vibrational component is fitted by a sum of Gaussian profiles. Given an initial ice chemical composition (either set by the user or the outputs of a chemical model), a full JWST spectrum is generated, to which the contribution of silicates; continuum, stellar photospheric absorption bands; and extinction law can be added. For the continuum, stellar photospheric models for a wide range of spectral types can be selected by the program, or, Spectral Energy Distribution (SEDs). We present a few use cases of SynthIceSpec: we probed the impact of dust temperature on CO2 ice formation using IR data and gas-grain modelling. Next, we used SynthIceSpec to explore the detectability of the main feature of CH3CN at 4.45 & micro;m in a cold core environment with the JWST, which was previously tentatively detected in YSOs. The detection thresholds we derive are reasonably low and observable, but identification is directly impacted by the photosphere absorptions that can greatly hinder identification. For some photostellar types, it could remain feasible. Coupled with the Estimated Time Calculator of the Space Telescope Science Institute, SynthIceSpec can be used to find the optimum observational setup for new observations.
The recent discovery of a large number of massive black holes within the first two billion years after the big bang, as well as their peculiar properties, have been largely unexpected based on the extrapolation of the properties of luminous quasars. These findings have prompted the development of several theoretical models for the early formation and growth of black holes, which are, however, difficult to differentiate. We report the metallicity measurement around a gravitationally lensed massive black hole at redshift 7.04 (classified as a Little Red Dot), hosted in a galaxy with very low dynamical mass. The weakness of the [O III]5007 emission line relative to the narrow H beta emission indicates extremely low metallicity, about 4 & times;10(-3) solar, and even more metal poor in the surrounding few 100 pc. We argue that such properties cannot be uncommon among accreting black holes around this early cosmic epoch. Explaining such a low chemical enrichment in a system that has developed a massive black hole is challenging for most theories. Models assuming heavy black hole seeds (such as Direct Collapse Black Holes) or super-Eddington accretion scenarios struggle to explain the observations, although they can potentially reproduce the observed properties in some cases. Models invoking 'primordial black holes' (i.e. putative black holes formed shortly after the big bang) may potentially explain the low chemical enrichment associated with this black hole, although this class of models also requires further developments for proper testing.
James Webb Space Telescope (JWST) has revealed a population of 'Little Red Dots' (LRDs): compact, red objects at redshifts z = 2-9 with 'v'-shaped spectral energy distributions, broad permitted lines, and, often, hydrogen Balmer absorption. We use NIRSpec/IFS data from the BlackTHUNDER survey to study the H alpha line in the LRD Abell2744-QSO1 at z = 7 . 04 , which is a confirmed active galactic nucleus (AGN) due to time-variable equivalent width (EW) in its broad emission lines. The H alpha spectral profile is non-Gaussian, requiring at least two Gaussian components. We also detect a narrow-line Gaussian component, and strong H alpha absorption (EW relative to the continuum similar to 22(+12)(-7) & Aring;), confirming a connection between the strong Balmer break and line absorption. The absorber is at rest with respect to broad H alpha , suggesting that the gas cannot be interpreted as an inflow or outflow, forming instead a long-lived structure. Its velocity dispersion is Q(abs) = 110(-10)(+20) km s(-1), consistent with the value inferred from the analysis of the Balmer break. Based on H alpha , we infer a black hole mass of log(M-center dot/M-circle dot) = 7 . 2 , smaller but close to the previous estimates based on H . The Eddington ratio is 0.09. Combining the high signal-to-noise ratio of the narrow H alpha line with the spectral resolution R = 3 , 700 of the G395H grating, we infer a narrow-line intrinsic dispersion Q(n) = 22(-6)(+5) km s(-1) , which places a stringent constraint on the black hole-to-dynamical mass ratio of this system to be M-center dot/M-dyn= 0 . 15-1 . 2 , confirming the overmassive nature of the black hole and potentially leaving little room for a host galaxy.
Context. Massive stars play crucial roles in galactic dynamics and chemical evolution. They are the most significant sources of ionizing UV radiation, their substantial mass-loss rates and explosions inject energy and enrich their surroundings, and their dynamical interactions eject stars and alter the evolution of stellar clusters. Consequently, the study of massive stars is essential for understanding various astrophysical phenomena, including galaxy chemical evolution, interstellar medium dynamics, gamma-ray bursts, and the reionization of the Universe. Key parameters influencing the evolution of massive stars include mass, mass-loss rate, chemical composition, and rotation. The orbits of spectroscopic binaries are particularly valuable because they provide constraints on stellar masses, and when combined with complementary data (e.g., photometry or interferometry), these masses can be fully determined. Aims. The OWN Survey was started two decades ago to study Galactic O- and WN- (hence the name) type southern spectroscopic binaries. In this paper we present the final results for single-lined (SB1) spectroscopic orbits. Methods. The OWN Survey carried out a long-term spectroscopic campaign to search for radial velocity variations indicative of orbital motion in a sample of southern Galactic O- and WN-type stars with high-resolution spectrographs in Argentina and Chile. The OWN spectra were later combined with high-resolution spectra from other sources and, in some cases, photometric time series to derive orbits and disentangled spectra, from which masses were constrained or determined and spectral classifications obtained. High-resolution optical spectra of 212 massive stars were obtained during the similar to 20 years of the OWN project, and each target was observed at least three times. Results. Among the 212 stars, 144 exhibited radial-velocity variations greater than 15 km s(-1). We present a complete and coherent compilation for the 23 systems with single-lined spectroscopic orbits identified in our sample. In Paper II we will perform a similar analysis for the systems with double-lined spectroscopic orbits.
We present a 'Little Red Dot' (LRD) broad-line active galactic nucleus (AGN) at z = 5.077 observed with NIRSpec/MSA (micro-shutter assembly) and NIRSpec/IFU (integral-field unit) by the JADES (JWST Advanced Deep Extragalactic Survey) and BlackTHUNDER (Black holes in THe early Universe aNd their DensE surRoundings) surveys. Combining spatially resolved and high-resolution spectroscopy, we characterize its central engine, host, and environment. Ho has multiple components, including two broad Gaussians, yielding a black-hole mass log(M-center dot/M-circle dot) = 7.65, while [O III]lambda 5007 gives a galaxy dynamical mass log(M-dyn/M-circle dot) 9.1, suggesting an overmassive black hole relative to the host galaxy. The target is immersed in a 7-kpc wide pool of ionized gas and has three neighbours: a satellite galaxy, a possible satellite/gas cloud, and a tentatively detected spatially detached outflow. Hoa shows strong, rest-frame absorption, deeper than the continuum, ruling out a stellar origin. The velocity and velocity dispersion are V-ahs-13 km s(-1) and sigma(abs) = 120 km s(-1). There is tentative evidence (2.6 sigma) of temporal variability in the equivalent width of the Hot absorber over two rest-frame months, suggesting a highly dynamic nucleus. Notably, while the Ha absorber is clearly visible and even dominant in the high-resolution G395H observations, it is not detected in the medium-resolution G395M data of the same epoch. This implies that the current incidence rate of absorbers in LRDs - and especially of rest-frame absorbers - may be severely underestimated, because most LRDs rely on lower resolution spectroscopy. The high incidence rate of rest-frame absorbers in LRDs may indicate a configuration that is either intrinsically stationary, such as a rotating disc, or that exhibits time-averaged stability, such as an oscillatory "breathing mode' accretion with cyclic expansion and contraction of the gas around the supermassive black hole.
