A high energy perspective of the co-evolution of black holes and their host galaxies

Thanks to the Chandra and XMM–Newton surveys, the hard X-ray sky is now probed down to a flux limit where the bulk of the X-ray background is almost completely resolved into discrete sources, at least in the 2–8 keV band. Extensive programs of multiwavelength follow-up observations showed that the large majority of hard X–ray selected sources are identified with Active Galactic Nuclei (AGN) spanning a broad range of redshifts, luminosities and optical properties. A sizable fraction of relatively luminous X-ray sources hosting an active, presumably obscured, nucleus would not have been easily recognized as such on the basis of optical observations because characterized by “peculiar” optical properties. In my PhD thesis, I will focus the attention on the nature of two classes of hard X-ray selected “elusive” sources: those characterized by high X-ray-to-optical flux ratios and red optical-to-near-infrared colors, a fraction of which associated with Type 2 quasars, and the X-ray bright optically normal galaxies, also known as XBONGs. In order to characterize the properties of these classes of elusive AGN, the datasets of several deep and large-area surveys have been fully exploited. The first class of “elusive” sources is characterized by X-ray-to-optical flux ratios (X/O) significantly higher than what is generally observed from unobscured quasars and Seyfert galaxies. The properties of well defined samples of high X/O sources detected at bright X–ray fluxes suggest that X/O selection is highly efficient in sampling high–redshift obscured quasars. At the limits of deep Chandra surveys (∼10−16 erg cm−2 s−1), high X/O sources are generally characterized by extremely faint optical magnitudes, hence their spectroscopic identification is hardly feasible even with the largest telescopes. In this framework, a detailed investigation of their X-ray properties may provide useful information on the nature of this important component of the X-ray source population. The X-ray data of the deepest X-ray observations ever performed, the Chandra deep fields, allows us to characterize the average X-ray properties of the high X/O population. The results of spectral analysis clearly indicate that the high X/O sources represent the most obscured component of the X–ray background. Their spectra are harder (G ∼ 1) than any other class of sources in the deep fields and also of the XRB spectrum (G ≈ 1.4). In order to better understand the AGN physics and evolution, a much better knowledge of the redshift, luminosity and spectral energy distributions (SEDs) of elusive AGN is of paramount importance. The recent COSMOS survey provides the necessary multiwavelength database to characterize the SEDs of a statistically robust sample of obscured sources. The combination of high X/O and red-colors offers a powerful tool to select obscured luminous objects at high redshift. A large sample of X-ray emitting extremely red objects (R−K >5) has been collected and their optical-infrared properties have been studied. In particular, using an appropriate SED fitting procedure, the nuclear and the host galaxy components have been deconvolved over a large range of wavelengths and ptical nuclear extinctions, black hole masses and Eddington ratios have been estimated. It is important to remark that the combination of hard X-ray selection and extreme red colors is highly efficient in picking up highly obscured, luminous sources at high redshift. Although the XBONGs do not present a new source population, the interest on the nature of these sources has gained a renewed attention after the discovery of several examples from recent Chandra and XMM–Newton surveys. Even though several possibilities were proposed in recent literature to explain why a relatively luminous (LX = 1042 − 1043erg s−1) hard X-ray source does not leave any significant signature of its presence in terms of optical emission lines, the very nature of XBONGs is still subject of debate. Good-quality photometric near-infrared data (ISAAC/VLT) of 4 low-redshift XBONGs from the HELLAS2XMMsurvey have been used to search for the presence of the putative nucleus, applying the surface-brightness decomposition technique. In two out of the four sources, the presence of a nuclear weak component hosted by a bright galaxy has been revealed. The results indicate that moderate amounts of gas and dust, covering a large solid angle (possibly 4p) at the nuclear source, may explain the lack of optical emission lines. A weak nucleus not able to produce suffcient UV photons may provide an alternative or additional explanation. On the basis of an admittedly small sample, we conclude that XBONGs constitute a mixed bag rather than a new source population. When the presence of a nucleus is revealed, it turns out to be mildly absorbed and hosted by a bright galaxy.

A panchromatic view of the evolution of supermassive black holes

This PhD Thesis is devoted to the accurate analysis of the physical properties of Active Galactic Nuclei (AGN) and the AGN/host-galaxy interplay. Due to the broad-band AGN emission (from radio to hard X-rays), a multi-wavelength approach is mandatory. Our research is carried out over the COSMOS field, within the context of the XMM-Newton wide-field survey. To date, the COSMOS field is a unique area for comprehensive multi-wavelength studies, allowing us to define a large and homogeneous sample of QSOs with a well-sampled spectral coverage and to keep selection effects under control. Moreover, the broad-band information contained in the COSMOS database is well-suited for a detailed analysis of AGN SEDs, bolometric luminosities and bolometric corrections. In order to investigate the nature of both obscured (Type-2) and unobscured (Type-1) AGN, the observational approach is complemented with a theoretical modelling of the AGN/galaxy co-evolution. The X-ray to optical properties of an X-ray selected Type-1 AGN sample are discussed in the first part. The relationship between X-ray and optical/UV luminosities, parametrized by the spectral index αox, provides a first indication about the nature of the central engine powering the AGN. Since a Type-1 AGN outshines the surrounding environment, it is extremely difficult to constrain the properties of its host-galaxy. Conversely, in Type-2 AGN the host-galaxy light is the dominant component of the optical/near-IR SEDs, severely affecting the recovery of the intrinsic AGN emission. Hence a multi-component SED-fitting code is developed to disentangle the emission of the stellar populationof the galaxy from that associated with mass accretion. Bolometric corrections, luminosities, stellar masses and star-formation rates, correlated with the morphology of Type-2 AGN hosts, are presented in the second part, while the final part concerns a physically-motivated model for the evolution of spheroidal galaxies with a central SMBH. The model is able to reproduce two important stages of galaxy evolution, namely the obscured cold-phase and the subsequent quiescent hot-phase.

Testing future weak lensing surveys through simulations of observations

Weak lensing experiments such as the future ESA-accepted mission Euclid aim to measure cosmological parameters with unprecedented accuracy. It is important to assess the precision that can be obtained in these measurements by applying analysis software on mock images that contain many sources of noise present in the real data. In this Thesis, we show a method to perform simulations of observations, that produce realistic images of the sky according to characteristics of the instrument and of the survey. We then use these images to test the performances of the Euclid mission. In particular, we concentrate on the precision of the photometric redshift measurements, which are key data to perform cosmic shear tomography. We calculate the fraction of the total observed sample that must be discarded to reach the required level of precision, that is equal to 0.05(1+z) for a galaxy with measured redshift z, with different ancillary ground-based observations. The results highlight the importance of u-band observations, especially to discriminate between low (z < 0.5) and high (z ~ 3) redshifts, and the need for good observing sites, with seeing FWHM < 1. arcsec. We then construct an optimal filter to detect galaxy clusters through photometric catalogues of galaxies, and we test it on the COSMOS field, obtaining 27 lensing-confirmed detections. Applying this algorithm on mock Euclid data, we verify the possibility to detect clusters with mass above 10^14.2 solar masses with a low rate of false detections.

Tracing AGN accretion and star formation in Herschel galaxies

In this Thesis, we study the physical properties and the cosmic evolution of AGN and their host galaxies since z∼3. Our analysis exploits samples of star forming galaxies detected with Herschel at far-IR wavelengths (from 70 up to 500 micron) in different extragalactic surveys, such as COSMOS and the deep GOODS (South and North) fields. The broad-band ancillary data available in COSMOS and the GOODS fields, allows us to implement Herschel and Spitzer photometry with multi-wavelength ancillary data. We perform a multicomponent SED-fitting decomposition to decouple the emission due to star formation from that due to AGN accretion, and to estimate both host-galaxy parameters (such as stellar mass, M* and star formation rate, SFR), and nuclear intrinsic bolometric luminosities. We use the individual estimates of AGN bolometric luminosity obtained through SED-fitting decomposition to reconstruct the redshit evolution of the AGN bolometric luminosity function since z∼3. The resulting trends are used to estimate the overall AGN accretion rate density at different cosmic epochs and to trace the first ever estimate of the AGN accretion history from an IR survey. Later on, we focus our study on the connection between AGN accretion and integrated galaxy properties. We analyse the relationships of AGN accretion with galaxy properties in the SFR-M* plane and at different cosmic epochs. Finally, we infer what is the parameter that best correlates with AGN accretion, comparing our results with previous studies and discussing their physical implications in the context of current scenarios of AGN/galaxy evolution.

Alianza perpetua. Bases del manejo ecológico en el noroeste amazónico. En: Avá, nº 19

Este texto explora las relaciones sociales entre humanos y no humanos para los Makuna, un grupo Tukano oriental del noroeste amazónico. A partir del concepto local üsi wasoare (préstamo de vitalidad) se analizan los intercambios chamánicos asociados a las prácticas productivas del grupo y se demuestra como la generación de vida en el cosmos es resultado del trabajo humano orientado por un principio ético que impide la aniquilación de lo no humano.

Un nuevo viaje de Teseo : De la Antigüedad a la Edad Media y al Renacimiento inglés

El presente trabajo propone explorar el modo cómo la literatura inglesa se apropia de la figura del héroe ático por antonomasia, Teseo, prefiriendo a las historias relacionadas con la aventura aquellas que lo muestran como figura garante del orden y de la sabiduría. Proponemos rastrear el modo cómo el héroe es presentado en el "Cuento del caballero" de los Canterbury Tales, representando no sólo el discurso patriarcal sino y, al mismo tiempo, quien desata las contiendas y quien las re-ordena. En este sentido, la figura del cuento- épico en el sentido bajtiniano del término- testimonia el discurso del orden, donde el varón es el eje vertebrador de la sociedad civil y familiar. Shakespeare, que había tomado contacto con las fuentes clásicas y medievales-tanto italianas como inglesas- incorpora en su Sueño de una noche de verano a un nuevo Teseo, que no sólo discurre acerca de la imaginación sino que también retoma la idea de orden a partir de la proclama de que es necesario someter las trampas de la imaginación a la prueba de la "fría razón". A partir de estos dos ejemplos, trataremos de reflexionar el modo cómo la literatura inglesa se apropió de estos mitos clásicos

Clinamen : Entre libertad y determinismo en De Rerum Natura de Lucrecio

En el presente trabajo se trabaja principalmente en la noción de clinamen, el cual debe entenderse como una desviación azarosa que ocurre en el átomo. Lucrecio argumenta, siguiendo la tradición atomista que lo precede, que el fundamento ontológico de la realidad, es que toda la naturaleza está compuesta de átomos y vacío. El filósofo adhiere a una concepción esencialmente mecanicista del cosmos: el hecho de que el mundo no es una creación de los dioses, hace que la naturaleza sea una constante repetición de los hechos. El concepto de clinamen lleva a Lucrecio plantear, además, el problema del determinismo y la libertad: si todo movimiento es siempre una relación causal con un antes, ¿de dónde viene este poder independiente del destino, a través del cual nos movemos hacia donde la voluntad de cada uno conduce? En segundo lugar, si todos los movimientos de los átomos son inflexiblemente determinados, la capacidad humana para decidir y asumir la responsabilidad de su accionar no podrían explicarse

El concepto de espíritu en el 'formalismus' de Max Scheler

Tabla de contenidos: Scheler en el pensamiento filosófico contemporáneo. El 'formalismus' y el concepto scheleriano de espíritu. El espíritu y la actitud fenomenológica. La esencia del espíritu. El ámbito del espíritu. La naturaleza del espíritu y la teoría de los estratos emocionales. El espíritu y los valores. Espíritu y persona. Espíritu, yo y cuerpo-propio. Espíritu personal finito y espíritu personal infinito. Origen, porvenir temporal y destino final del espíritu humano. El espíritu según 'El puesto del hombre en el cosmos'. Conclusiones.

Dioses, Dios

"We are not jealous of gods, we do not serve them, we do not fear them, but at the risk of our lives, we attest for their multiple existence, and are stirred to be of their chancy keeping when they are no more remembered of". What could mean such a sentence written by René Char? Is it still possible to think and to experiment, here and now, after centuries of monotheism, something like a plurality of gods? What is it to be a pagan? Rereading Homer, and then Plato, Nietzsche and Lyotard, we could risk the following de´Çü nition: pagan is someone able to suppose, between performance and cosmos, that the one coming up to him is, may be, some god.

La polémica acerca de la generación del mundo en el tiempo : Plotino frente a sus predecesores

En este trabajo analizaremos algunos de los argumentos que Plotino ofrece en su tratado II, 1 (Sobre el Cielo, el 40 en el orden cronológico) para sostener la eternidad del mundo sin que esto signifique, a sus ojos, un distanciamiento de las enseñanzas del Timeo platónico. Nos concentraremos en las objeciones que Plotino formula en el primer capítulo del tratado a dos argumentos que defienden la eternidad del cosmos e intentaremos mostrar que, aunque es posible hallar estos dos argumentos en el Timeo, no es hacia este diálogo a donde Plotino dirige sus críticas. En efecto, sostenemos que es importante tener en cuenta las perspectivas divergentes a este respecto de Atico y de Aristóteles puesto que podrían contribuir, por una parte, a iluminar el modo según el cual Plotino reelabora la filosofía platónica y, por otra, a poner de manifiesto los supuestos metafísicos que subyacen a su postulación de la eternidad del mundo