Hasil untuk "History of the arts"

Euclid Collaboration Y. Mellier, Abdurro’uf, J. Barroso et al.

The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. is a medium-class mission in the Cosmic Vision 2015--2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14\,000\,deg$^2$ of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. We also highlight the main science objectives and expected performance.

F. Annibali, A. Ferguson, P. M. Sanchez-Alarcon et al.

We present a detailed analysis of the old, extended stellar component of the Local Group dwarf galaxy IC 10 using deep resolved-star photometry in the VIS and NISP bands of the Euclid Early Release Observations. Leveraging Euclid's unique combination of wide field of view and high spatial resolution, we trace red giant branch (RGB) stars out to $\sim$8 kpc from the galaxy centre, reaching azimuthally-averaged surface brightness levels as faint as $\mu_{HE}\sim$29 mag arcsec$^{-2}$. Our analysis reveals that IC 10's stellar distribution is significantly more extended than previously thought. After correcting for foreground extinction and subtracting contamination from Milky Way stars and background galaxies, we derive a radial stellar density profile from RGB star counts. The profile shows a marked flattening beyond $\sim$5 kpc, and is best fit by a two-component (Sersic + exponential) model, yielding a total stellar mass in old (age $>$1 Gyr) stars of $M_{\star}=(6.7-8.1)\times10^8 M_{\odot}$. The origin of the outer stellar component is unclear. It may be accreted, even possibly associated with the counter-rotating HI gas in the outer regions of IC 10, or it may represent an ancient in-situ stellar halo. We tentatively detect two symmetric stellar overdensities at the edge of our imagery. These roughly align with the direction of IC 10's orbit around M31, suggesting that they may be signatures of tidal stripping. As part of our analysis, we derive a new distance to IC 10 based on the RGB tip, finding $D=762\pm 20$ kpc and the distance modulus is $(m-M)_0=24.41\pm 0.05$.

Euclid Collaboration K. Kraljic, C. Laigle, M. Balogh et al.

The ongoing Euclid mission is aimed at measuring spectroscopic redshifts for approximately two million galaxies using the , ^ line emission detected in near-infrared slitless spectroscopic data from the Euclid Deep Fields, leveraging both the red and blue grisms. These measurements will reach a flux limit of 5 , , ^ 10^ -17 ̊m erg ̊m cm -2 ̊m s -1 in the redshift range 0.4<z<1.8, paving the way to numerous scientific investigations involving galaxy evolution, extending well beyond the mission's core objectives. The achieved luminosity depth will lead to a sufficiently high sampling, enabling the reconstruction of the large-scale galaxy environment. Here, we assess the quality of the reconstruction of the galaxy cosmic web environment with the expected spectroscopic dataset in Euclid Deep Fields. The analysis was carried out on the Flagship and galaxy mock catalogues. The quality of the reconstruction was first evaluated using simple geometrical and topological statistics measured on the cosmic web network; namely, the length of filaments, the area of walls, the volume of voids, and its connectivity and multiplicity. We then quantified how accurately gradients in galaxy properties can be recovered, with respect to the distance from filaments. As expected, the small-scale redshift-space distortions, such as Fingers of God (FoG) effects, have a strong impact on filament lengths and connectivity; however, they can be mitigated by compressing galaxy groups identified with an anisotropic group finder prior to a skeleton extraction. The cosmic web reconstruction is biased when relying solely on emitters. This limitation can be mitigated by applying stellar mass weighting during the cosmic web reconstruction. However, this approach introduces non-trivial biases that need to be accounted for when comparing to theoretical predictions. Redshift uncertainties pose the greatest challenge in recovering the expected dependence of galaxy properties, although the well-established stellar mass transverse gradients towards filaments can still be observed to a lesser extent.

Euclid Collaboration F. Cogato, B. Kubik, R. Barbier et al.

The Euclid spacecraft, located at the second Lagrangian point of the Sun-Earth system, hosts the Near-Infrared Spectrometer and Photometer (NISP) instrument. NISP is equipped with a mosaic of 16 HgCdTe-based detectors to acquire near-infrared photometric and spectroscopic data. To meet the spacecraft's constraints on computational resources and telemetry bandwidth, the near-infrared signal is processed onboard via a dedicated hardware-software architecture designed to fulfil the stringent Euclid's data-quality requirements. A custom application software, running on the two NISP data processing units, implements the NISP signal estimator: an ad-hoc algorithm which delivers accurate flux measurements and simultaneously estimates the quality of signal estimation through the quality factor parameter. This paper investigates the properties of the NISP signal estimator by evaluating its performance during the early flight operations of the NISP instrument. First, we revisit the assumptions on which the inference of the near-infrared signal is based and investigate the origin of the main systematics of the signal estimator through Monte Carlo simulations. Then, we test the flight performance of the NISP signal estimator. Results indicate a systematic bias lower than 0.01 e/s for 99% of the NISP pixel array, well within the noise budget of the estimated signal. We also derive an analytical expression for the variance of the NISP signal estimator, demonstrating its validity, particularly when the covariance matrix is not pre-computed. Finally, we provide a robust statistical framework to interpret the QF parameter, analyse its dependence on the signal estimator bias, and show its sensitivity to cosmic ray hits on NISP detectors. Our findings corroborate previous results on the NISP signal estimator and suggest a leading-order correction based on the agreement between flight data and simulations.

Euclid Collaboration Y. Cao, A. Cooray, T. Li et al.

The extragalactic background light (EBL) fluctuations in the optical/near-IR encode the cumulative integrated galaxy light (IGL), diffuse intra-halo light (IHL), and high-$z$ sources from the epoch of reionisation (EoR), but they are difficult to disentangle with auto-spectra alone. We aim to decompose the EBL into its principal constituents using multi-band intensity mapping combined with cosmic shear and galaxy clustering. We develop a joint halo-model framework in which IHL follows a mass- and redshift-dependent luminosity scaling, IGL is set by an evolving Schechter luminosity function, and EoR emission is modelled with Pop II/III stellar emissivities and a binned star-formation efficiency. Using mock surveys in a flat $\Lambda$CDM cosmology with ten spectral bands spanning 0.75-5.0$\rm \mu m$ in the NEP deep fields over about 100$\deg^2$ with source detections down to AB=20.5 for masking, and six redshift bins to $z=2.5$, we fit auto- and cross-power spectra using a MCMC method. The combined SPHEREx$\times$Euclid analysis recovers all fiducial parameters within 1$\sigma$ and reduces 1$\sigma$ uncertainties on IHL parameters by 10-35% relative to SPHEREx EBL-only, while EoR star-formation efficiency parameters improve by 20-35%. Cross-correlations reveal a stronger coupling of IHL than IGL to the shear field, enhancing component separation; conversely, the EoR contribution shows negligible correlation with cosmic shear and galaxy clustering, aiding its isolation in the EBL. Relative to the SPHEREx EBL-only case, the inferred IHL fraction as a function of halo mass is significantly tightened over $10^{11}-10^{14} M_{\odot}$, with uncertainties reduced by 5-30%, and the resulting star-formation rate density constraints extend to $z\sim 11$, with uncertainty reductions of 22-31%.

Euclid Collaboration N. Malavasi, F. Sarron, U. Kuchner et al.

Cosmic filaments are prominent structures of the matter distribution of the Universe. Modern detection algorithms are an efficient way to identify filaments in large-scale observational surveys of galaxies. Many of these methods were originally designed to work with simulations and/or well-sampled spectroscopic surveys. When spectroscopic redshifts are not available, the filaments of the cosmic web can be detected in projection using photometric redshifts in slices along the Line of Sight, which enable the exploration of larger cosmic volumes. However, this comes at the expense of a lower redshift precision. It is therefore crucial to assess the differences between filaments extracted from exact redshifts and from photometric redshifts for a specific survey. We apply this analysis to capture the uncertainties and biases of filament extractions introduced by using the photometric sample of the Euclid Wide Survey. The question that we address in this work is how can we compare two filament samples derived with redshifts of different precisions in the Euclid Wide Survey context. We apply the cosmic web detection algorithm DisPerSE, in the redshift range $0.1 \leq z \leq 0.5$, to the GAlaxy Evolution and Assembly (GAEA) simulated galaxy sample which reproduces several characteristics of the Euclid Wide Survey. We develop a method to compare skeletons derived from photometric redshifts to those derived from true galaxy positions. This method expands the commonly used measure of distance between filaments to include geometrical (angles between filaments) and astrophysical considerations (galaxy mass gradients and connectivity-mass relations). We assess whether this approach strengthens our ability to correctly identify filaments in very large surveys such as the Euclid Wide Survey. [abridged]

Olusola Bamidele Ojo, Huma Pervaiz, Tahir Kamran

From the colonial era, settlers ‘technologies including imperial medicine have shaped the social, cultural and economic landscape of the colonies in diverse dimensions.  In the post-modern world, global medicine still has the trappings of health inequities and imperialism, particularly in lower- and middle-income countries and the Global South. In this regard, this research article examines how Yoruba medicine practitioners deployed their cultural sanctity to withstand the domineering influence of imperial medicine in the early twentieth-century. In the same era, we compare this phenomenon with how Hakims and Vaids in colonial Punjab deployed Urdu literati to reconstruct their social relevance. Thus, we argue that Yoruba medicine was a site of cultural reformation while Punjab medicine was a site of social reconstruction. This historical research engaged archival sources and suitable secondary data, and exposed varied reactions of Indigenous medical practitioners to colonial medical institutions in the early 20th century. A study of this caliber highlights the inextricable interface between culture, medicine, and technology in the context of colonialism. It reinforces the significance of acculturation in cultural encounters to forestall cultural emasculation.

Pablo Esteban Torres

En el siglo XIX, tras las Guerras Napoleónicas, Gibraltar se consolidó como un punto estratégico clave para la política mediterránea del Imperio Británico, y en 1830 fue formalmente declarado Colonia de la Corona. Gobernado por un representante de la monarquía con amplios poderes ejecutivos y legislativos, el Peñón vivió un importante desarrollo social, económico y urbano, impulsado por la prosperidad británica y el debilitamiento de España. Este trabajo se propone reconstruir la biografía del gobernador John Miller Adye (1819-1900) y su gestión entre los años 1883 y 1886, a fin de analizar los cambios ocurridos en la colonia durante un período de la historia de la administración gibraltareña que ha sido escasamente abordado. Estudiar su carrera permite entender mejor el sistema colonial británico en el apogeo del Imperio y cómo este influyó en las relaciones diplomáticas entre ambos países respecto a Gibraltar durante los primeros años de la Restauración Borbónica.

Diana Nechit, Véronique Parisot

Bernard-Marie Koltès occupies a singular place in contemporary theatre: at once poetic and political, his work interrogates the human condition through questions of space, language, and otherness. Every staging of his texts draws the director into a delicate dialogue with the absent author: how to represent without betraying? How to adapt without distorting? This article examines the ethical and legal issues that surround the staging of Koltès, through the analysis of several emblematic cases (Chéreau, Touré, Bident) and by articulating notions of moral rights, artistic fidelity, and poetic responsibility. It aims to explore the fragile balance between memory and invention, between the letter of the text and the living pulse of the stage.

S. Hutschenreuter, J. Alves, L. Posch et al.

We present a non-parametric reconstruction of the three-dimensional velocity field of the Scorpius-Centaurus OB association (Sco- Cen). Using Gaia DR3 astrometry and radial velocities, we infer the velocity field using information field theory on a 70 x 70 x 50 grid at 3 pc resolution. Our model suggests the existence of a primary stellar velocity field with a secondary field that accounts for an additional young kinematic component in Upper Scorpius and Lupus. We find clear tracers of a feedback-driven expansion of the association, while Galactic rotation appears to play a subordinate role. The results confirm the existence of cluster chains and reveal coherent large-scale expansion with characteristic speeds of 1-2 km s$^{-1}$ and local maxima of about 10 km s$^{-1}$. Power spectra indicate an excess of small-scale structure and slopes shallower than Kolmogorov, consistent with energy injection from stellar feedback. Maps of the divergence reveal net positive values, implying an approximate dispersal timescale of 10-15 Myr. A comparison with molecular gas in Lupus and Ophiuchus shows broadly consistent patterns but systematic velocity offsets of several km s$^{-1}$, suggesting partial decoupling for optically visible young stars and gas. The framework presented provides a physically motivated description of the Sco-Cen velocity field and a basis for quantifying the dynamical state and feedback history of OB associations in the local Galaxy.

G. Piccirilli, B. Bahr-Kalus, S. Camera et al.

Synergies between large-scale radio-continuum and optical/near-infrared galaxy surveys are a powerful tool for cosmology. Cross-correlating these surveys can constrain the redshift distribution of radio sources, mitigate systematic effects, and place constraints on cosmological models. We perform the first measurement of the clustering cross-spectrum between radio-continuum sources in the Evolutionary Map of the Universe (EMU) survey and galaxies from the ESA Euclid satellite mission's Q1 release. Our goal is to detect and characterise the cross-correlation signal, test its robustness against systematic effects, and compare our measurements with theoretical predictions. We use data from the Australian SKA Pathfinder's EMU Main Survey, which overlaps with the Euclid Deep Field South. We generate two radio-source catalogues using different source finders to create galaxy maps. We measure the harmonic-space cross-correlation signal using a pseudo-spectrum estimator. The measured signal is compared to theoretical predictions based on a {\Lambda}CDM cosmology, using several models for the EMU source redshift distribution and bias. We report detection above 8{\sigma} of the cross-correlation signal consistent across all tested models and data sets. The measured cross-spectra from the two radio catalogues are in excellent agreement, demonstrating that the cross-correlation is robust against the choice of source-finding algorithm. The measured signal also agrees with theoretical models developed from previous cross-correlation studies and simulations. This pathfinder study establishes a statistically significant cross-correlation between EMU and Euclid. The robustness of the signal is a crucial validation of the methodology, paving the way for future large-scale analyses leveraging the full power of this synergy to constrain cosmological parameters and our understanding of galaxy evolution.

Euclid Collaboration R. Navarro-Carrera, K. Caputi, C. McPartland et al.

Probing the presence and properties of massive galaxies at high redshift is one of the most critical tests for galaxy formation models. In this work, we search for galaxies with stellar masses M*>10^10.25 Msun at z in [5,7], i.e., towards the end of the Epoch of Reionisation, over a total of ~23 deg^2 in two of the Euclid Quick Data Release (Q1) fields: the Euclid Deep Field North and Fornax (EDF-N and EDF-F). In addition to the Euclid photometry, we incorporate Spitzer Infrared Camera (IRAC) and ground-based optical data to perform spectral energy distribution (SED) fitting, obtaining photometric redshifts and derived physical parameters. After applying rigorous selection criteria, we identify a conservative sample of 145 candidate massive galaxies with M*>10^10.25 Msun at z in [5,7], including 5 objects with M*>10^11 Msun. This makes for a surface density of about 6.3 deg^-2 at z in [5,7], which should be considered a lower limit because of the current depth of the Euclid data (H_E<24, 5 sigma in Q1). We find that the inferred stellar masses are consistent with galaxy formation models with standard star-formation efficiencies. These massive galaxies have colour excess E(B-V) values up to 0.75, indicating significant dust attenuation in some of them. In addition, half of the massive galaxies have best-fit ages comparable to the age of the Universe at those redshifts, which suggests that their progenitors were formed very early in cosmic time. About 78% of the massive galaxies lie on the star-forming main sequence (MS) in the SFR-M* plane, ~12% are found in the starburst region, and 10% in the transition zone between the MS and starbursts. We find no significant evidence for outshining or AGN contamination that could account for the elevated specific star-formation rates (sSFR) observed in the ~12% of galaxies classified as starbursts.

Euclid Collaboration C. J. R. McPartland, L. Zalesky, J. Weaver et al.

will provide deep near-infrared (NIR) imaging to ∼26.5 AB magnitude over ∼59 deg^2 in its deep and auxiliary fields. The Cosmic DAWN survey combines dedicated and archival UV--NIR observations to provide matched depth multiwavelength imaging of the deep and auxiliary fields. The DAWN survey will provide consistently measured NIR-selected photometric catalogues, accurate photometric redshifts, and measurements of galaxy properties to a redshift of z∼ 10. The DAWN catalogues include Spitzer IRAC data that are critical for stellar mass measurements at z ≳ 2.5 and high-z science. These catalogues complement the standard catalogues, which will not include Spitzer IRAC data. In this paper, we present an overview of the survey, including the footprints of the survey fields, the existing and planned observations, and the primary science goals for the combined data set.

F. Lepori, S. Schulz, I. Tutusaus et al.

Gravitational redshift and Doppler effects give rise to an antisymmetric component of the galaxy correlation function when cross-correlating two galaxy populations or two different tracers. In this paper, we assess the detectability of these effects in the spectroscopic galaxy survey. We model the impact of gravitational redshift on the observed redshift of galaxies in the Flagship mock catalogue using a Navarro--Frenk--White profile for the host haloes. We isolate these relativistic effects, largely subdominant in the standard analysis, by splitting the galaxy catalogue into two populations of faint and bright objects and estimating the dipole of their cross-correlation in four redshift bins. In the simulated catalogue, we detect the dipole signal on scales below $ Mpc $, with detection significances of $4,σ$ and $3,σ$ in the two lowest redshift bins, respectively. At higher redshifts, the detection significance drops below $2,σ$. Overall, we estimate the total detection significance in the spectroscopic sample to be approximately $6,σ$. We find that on small scales, the major contribution to the signal comes from the nonlinear gravitational potential. Our study on the Flagship mock catalogue shows that this observable can be detected in Euclid Data Release 2 and beyond.

J. Cuillandre, M. Bolzonella, A. Boselli et al.

The Euclid ERO programme targeted the Perseus cluster of galaxies, gathering deep data in the central region of the cluster over $0.7 deg^2 $, including the cluster core up to 0.25,r_200. The dataset reaches a point-source depth of IE = 28.0 (YE, = 25.3), AB magnitudes at $5,σ$ with a FWHM mag arcsec for radially integrated galaxy profiles. The exceptional depth and spatial resolution of this wide-field multi-band data enable simultaneous detection and characterisation of both bright galaxies and low surface brightness ones, along with their globular cluster systems, from the optical to the NIR . Cluster membership was determined using several methods in order to maximise the completeness and minimise the contamination of foreground and background sources. We adopted a catalogue of 1100 dwarf galaxies, detailed in the corresponding ERO paper, that includes their photometric and structural properties. We identified all other sources in the Euclid images and obtained accurate photometric measurements using AutoProf or AstroPhot for 137 bright cluster galaxies and SourceExtractor for half a million compact sources. This study advances beyond previous analyses of the cluster and enables a range of scientific investigations, which are summarised here. We derived the luminosity and stellar mass functions (LF and SMF) of the Perseus cluster in the Euclid band thanks to supplementary u, g, r, i, z, and Hα data from the CFHT . Our LF and SMF are the deepest recorded for the Perseus cluster, highlighting the groundbreaking capabilities of the Euclid telescope. We fit the LF and SMF with a Schechter plus Gaussian model. The LF features a dip at M( ≃ -19 and a faint-end slope of S ≃ -1.2 to -1.3. The SMF displays a low-mass-end slope of α_ S ≃ -1.2 to -1.35. These observed slopes are flatter than those predicted for dark matter halos in cosmological simulations, offering significant insights for models of galaxy formation and evolution.

H. Atek, R. Gavazzi, J. Weaver et al.

We present the first analysis of the Early Release Observations (ERO) program that targets fields around two lensing clusters, Abell 2390 and Abell 2764. We use imaging data from the Visible instrument (VIS) and the Near-Infrared Spectrometer and Photometer (NISP) to produce photometric catalogs for a total of $ 500\,000$ objects. The imaging data reach a typical depth of $5\ in the range 25.1--25.4 AB in the NISP bands and 27.1--27.3 AB in the VIS band. Using the Lyman-break method in combination with photometric redshifts, we searched for high-redshift galaxies. We identified $30$ Lyman-break galaxy (LBG) candidates at $z>6$ and 139 extremely red sources (ERSs), most of which likely lie at lower redshift. The VIS imaging is deeper than the NISP imaging, which means that we can routinely identify high-redshift Lyman-break galaxies at about a magnitude of 3, which reduces contamination by brown dwarf stars and low-redshift galaxies. The difficulty of spatially resolving most of these sources in 0 $ imaging means that it is difficult to distinguish between galaxies and quasars. Spectroscopic follow-up campaigns of these bright sources will help us to constrain the bright end of the ultraviolet galaxy luminosity function and the quasar luminosity function at $z>6$, and it will constrain the physical nature of these objects. Additionally, we performed a combined strong- and weak-lensing analysis of A2390, and we show that will contribute to constraining the virial mass of galaxy clusters better. We also identify optical and near-infrared counterparts of known $z>0.6$ clusters in these data. These counterparts exhibit strong-lensing features. This establishes that can characterize high-redshift clusters. Finally, we provide a glimpse of the ability of to map the intracluster light out to larger radii than current facilities, which enables us to understand the cluster assembly history better and to map the dark matter distribution. This initial dataset illustrates the diverse spectrum of legacy science that is possible with the survey.

Euclid Collaboration T. Castro, A. Fumagalli, R. E. Angulo et al.

The mission, designed to map the geometry of the dark Universe, presents an unprecedented opportunity for advancing our understanding of the cosmos through its photometric galaxy cluster survey. Central to this endeavor is the accurate calibration of the mass- and redshift-dependent halo bias (HB), which is the focus of this paper. Our aim is to enhance the precision of HB predictions, which is crucial for deriving cosmological constraints from the clustering of galaxy clusters. Our study is based on the peak-background split (PBS) model linked to the halo mass function (HMF), and it extends it with a parametric correction to precisely align with results from an extended set of $N$-body simulations carried out with the code. Employing simulations with fixed and paired initial conditions, we meticulously analyzed the matter-halo cross-spectrum and modeled its covariance using a large number of mock catalogs generated with Lagrangian perturbation theory simulations with the code. This ensures a comprehensive understanding of the uncertainties in our HB calibration. Our findings indicate that the calibrated HB model is remarkably resilient against changes in cosmological parameters, including those involving massive neutrinos. The robustness and adaptability of our calibrated HB model provide an important contribution to the cosmological exploitation of the cluster surveys to be provided by the mission. This study highlights the necessity of continuously refining the calibration of cosmological tools such as the HB to match the advancing quality of observational data. As we project the impact of our calibrated model on cosmological constraints, we find that given the sensitivity of the survey, a miscalibration of the HB could introduce biases in cluster cosmology analysis. Our work fills this critical gap, ensuring the HB calibration matches the expected precision of the survey.

Alicia Sempere Marin

La vida y figura de San Francisco de Asís despertaron un gran interés durante la segunda mitad del pasado siglo. En ese contexto se encargó al artista José María Párraga (1937-1997) la realización de todo un ciclo decorativo para la recientemente establecida Parroquia de San Francisco de Asís en la ciudad de Murcia. Párraga, cuya vasta producción incluye un amplio espectro de manifestaciones artísticas enmarcadas en un estilo personal e inclasificable, diseñó una serie de pirograbados, relieves y murales para la iglesia y su entorno, proyecto del que se conservan asimismo dibujos preparatorios.

Indrė Užuotaitė

Pratarmė

Haleem Kadhim

يدور هذا البحث حول نظرية من نظريات المعنى، هي نظرية المعنى في السياق التي استطاعت أن تُخرج البحث اللغوي من عباءة مفهوم الأنظمة الثابتة والنسق المغلق إلى عالم الكلام والاستعمال اللغوي وانفتاح النسق، فصار للمعنى منهج عملي استطاع أن يكسر الحاجز الذي وضعته النظريات الصدقية في بحثها عن المعنى المنطقي الذي تبناه في ما بعد علم الدلالة ردحا من الزمن.     لقد دخل المعنى، مع نظرية السياق، إلى عالم أوسع بعد أن اجتاز حدود اللغة بوصفها ظاهرة اجتماعية، ومن ثمّ صار النسق الاجتماعي الثقافي مصدرا رئيسا من مصادر المعنى، وصار هتاف (فتخنشتاين): (لا تسل عن المعنى، وإنّما اسأل عن الاستعمال) شعاراً لنظرية السياقً، وأبحاث (مالينوفسكي) في تراث المجتمعات البدائية وتأريخها طريقاً لـــ(فيرث) لأن يؤسس لنظرية السياق ويضع أسسها، فأصبح المعنى عنده في السياق، أو هو وظيفة في سياق.     لكنّ مفهوم السيّاق قد توسع مع الدراسات التداولية والوظيفية، حتى كادت أن تسمى التداولية بالسياقية، بناء على تأثير السياق في هذه الدراسات التي أعطت دورا واسعا للمتكلّم لصياغة المعنى إنتاجا، وللمخاطَب تلقياً وتأويلا، فهما معا قادران على الإنتاج والتأويل؛ قادران على وضع المعنى في سياقه، ومنغمسان معا في الخلفية المعرفية التي تجمعهما في مجتمع لغوي معيّن.