La Scienza e l'immaginario

L’attività di divulgazione della cultura scientifica ha un ruolo fondamentale sulla società, sia in termini di applicazioni innovative che di pianificazione dell’ambiente. I ricercatori dell’IAS-CNR di Capo Granitola operano da anni nell’ambito della diffusione della cultura scientifica, attraverso processi complessi e percorsi di divulgazione in partnership con istituti scolastici del territorio, realizzando attività seminariali, convegni direttamente nelle scuole, nonché visite didattiche guidate degli alunni nei laboratori dell’Istituto ed esperimenti interdisciplinari sull’ambiente marino. Tali processi divulgativi si sono sviluppati creando numerosi percorsi, in maniera per certi aspetti analoga a quella per cui dalla mescolanza dei tre colori fondamentali si è in grado di ottenere un numero pressoché illimitato di tinte diverse. Lo scopo di questa “mescolanza” è stato quello di ottenere un ventaglio di competenze e strumentazioni che consentissero di indagare i differenti aspetti dell’ecosistema marino da diversi punti di vista ed in maniera sinergica, tale da restituire un quadro il più ricco possibile di “tinte” e particolari. (Scienza e arte di Salvatore Mazzola) La Scienza e l'immaginario di Angela Cuttitta. Il progetto “La Scienza e l’Immaginario” nasce dalla collaborazione tra l’IAS - CNR di Capo Granitola e l’Accademia di Belle Arti di Palermo, che attraverso un approccio multidisciplinare ha voluto sperimentare l’unione tra il mondo scientifico e quello artistico, mettendo i giovani artisti, attraverso proiezioni e seminari scientifici, nelle condizioni di scoprire il mondo dell’ambiente marino e degli ecosistemi in esso presenti. Il progetto è nato dalla consapevolezza di come sia necessario operare sul piano della diffusione e divulgazione della cultura scientifica nei più vasti contesti sociali, a partire dall’ambito scolastico. Le azioni divulgative mirano, infatti, a diffondere la conoscenza dei processi geologici, chimico-fisici, climatici e biologici in modo pervasivo, non limitato a singole categorie/settori. La funzione strategica di tali azioni è quella di stimolare idee ed iniziative nonché di sviluppare una maggiore sensibilità nei confronti dei fenomeni che ci circondano, quale presupposto essenziale per una corretta programmazione politico-gestionale. Lo spirito che ha mosso tutte gli attori del progetto è stato quello di sensibilizzare gli studenti nei confronti della tutela delle risorse marine proprie del loro territorio e di sviluppare e promuovere la cultura come volano dello sviluppo sostenibile, della pace e dell’integrazione sociale, in armonia con quanto indicato dal Consiglio Europeo di Lisbona 2000. Grazie al lavoro di docenti e di ricercatori, l’arte come forma espressiva si è rivelata uno strumento valido e innovativo di divulgazione della cultura scientifica e ha portato alla creazione di suggestioni sui ragazzi che hanno percepito e realizzato forme e armonie espresse in questa mostra. L’impegno per questa manifestazione rappresenta, quindi, un appuntamento importante con le forze vive siciliane nel campo delle scienze del mare segnatamente ad esperti di biologia, chimica, fisica ed al mondo fantastico dell’arte, al fine di esprimere con le varie tecniche pittoriche un momento di riflessione culturale

Impact of straylight on the Science Objectives of SWG3.2

This document provides a preliminary assessment of the impact of stray light on the level-1 science objectives of SWG 3.2 Star formation and Evolution. Stray light is due to X-ray sources located outside the nominal field of view of the Wolter I mirrors and arises from single reflections on the 2nd mirror surface. The stray light hence reaches the focal plane unfocused producing a pattern that reflects the geometry of the mirror modules. Given the limited size of the X-IFU field of view and the fact that the impact of stray light from sources outside the FoV is lowest on-axis, observations with the X-IFU should be less affected than those using the WFI. The majority of the targets related to the science objectives of SWG 3.2 that are either in the mock observing plan or are likely to become targets for Athena are located in star forming regions or open clusters in or near the Galactic plane. Stray X-rays will thus mainly come from bright point-like X-ray sources such as low-mass and high-mass X-ray binaries

Impact of the various mass-saving options identified in the framework of the MCR and delta-MCR on the scientific objectives of SWG3.2

In the context of the Athena Mission Consolidation Review, ESA identified a potential non-compliance in mass between the baseline concept and the currently-assumed lift capability of the Ariane 64 launcher to L2. Several mass-saving options have been identified. The ASST and its working groups have been tasked with performing an analysis of the scientific impact of those options that concern the scientific payload. At the stage of this SIMO (Scientific Impact of Mass-saving Options) exercise, rough estimates of the impact on the Level 1 Science Objectives are needed

STRAY19: assessment of the benefits of a stray light baffle on the Science Objectives of SWG3.2

In February 2016, the Athena Working Groups and Topical Panels assessed the impact of X-ray stray light on the Athena science. Since then, the baseline configuration of the Athena mirrors has changed. The cost-constrained reduction of the number of mirror rows from 20 to 15 (current baseline) notably led to an increase of the stray-to-image effective area ratio. The impact of stray light could be reduced via the implementation of a dedicated baffle. ASST thus asked the Working Groups and Topical Panels to assess the scientific benefits of a stray light baffle in the framework of the so-called STRAY19 exercise. The present document provides a preliminary assessment of the quantitative benefits of a stray light baffle on the level-1 science objectives of SWG 3.2 Star formation and Evolution. This document therefore supersedes the previous TN from SWG 3.2 on this subject. Hereafter, we compare a 100% efficient baffle (resulting in no stray light contamination) with the currently estimated level of stray light corresponding to the 15 row mirror as requested by ASST

Assessment of the performance of optical blocking filters for X-IFU observations of massive stars

Massive stars that are bright X-ray sources, and hence constitute the best candidates for in-depth studies of their X-ray emission with the X-IFU, are most of the time also bright in the optical and UV domain. Optical and UV photons that reach the focal plane of the X-IFU can lead to a degradation of the instrument’s energy resolution. Since OB stars have log(LX/Lbol) ~ -7, the number of optical and UV photons that enter the Athena telescope compared to the number of X-ray photons can be huge. Therefore, in order to preserve the full scientific capabilities of the X-IFU, it is important to ensure an efficient attenuation of the flux of non-X-ray photons that reaches the X-IFU detector. Some attenuation is achieved with the set of five thermal filters that will be located inside the X-IFU Aperture Cylinder. Yet, in order to reduce the optical loading to an acceptable level, additional optical blocking filters mounted on a filter wheel are needed. In this technical note, we present simulations of the optical load that will result for observations of OB stars up to an mV magnitude of 2 and considering various combinations of thermal and optical blocking filters

STRAY19: the effects of stray-light on source detection and flux determination in a typical Athena WFI observation relevant to the Science Objectives of SWG3.2

In February 2016, the Athena Working Groups and Topical Panels assessed the impact of X-ray stray light on the Athena science. Since then, the baseline configuration of the Athena mirrors has changed. The cost-constrained reduction of the number of mirror rows from 20 to 15 (current baseline) notably led to an increase of the stray-to-image effective area ratio. The impact of stray light could be reduced via the implementation of a dedicated baffle. ASST thus asked the Working Groups and Topical Panels to assess the scientific benefits of a stray light baffle in the framework of the so-called STRAY19 exercise. The present document provides an assessment of the quantitative benefits of a stray light baffle on the level-1 science objectives of SWG 3.2 Star formation and Evolution, for the case of a typical WFI dithered observation. This document therefore supersedes the previous TN from SWG 3.2 on this subject and it is the companion of the TN “STRAY19: assessment of the benefits of a stray light baffle on the Science Objectives of SWG3.2”. Hereafter, we compare a 100% efficient baffle (resulting in no stray light contamination) with the currently estimated level of stray light corresponding to the 15 row mirror as requested by ASST

Needs for other facilities to achieve the Athena Science Objectives of SWG3.2

This document provides a preliminary inventory of other facilities needed in addition to the Athena observatory to achieve the level-1 science objectives of SWG 3.2 Star formation and Evolution

Assessment of the impact of a 10'' HEW PSF on the possibility to investigate star-forming regions and OB associations in the Milky-Way and the Magellanic Clouds under SWG3.2

This Technical Note investigates the impact of a 10'' HEW PSF on the possibility to study crowded star forming regions in the Milky Way and/or OB associations in the Magellanic Clouds. Various techniques are used to estimate the consequences in terms of source detection efficiency, S/N against a diffuse emission and limiting sensitivity