Suchergebnisse

A few months ago, while I was participating in a conference about open access infrastructures, a delegate from a governmental agency asked, "Why does each library need to maintain a repository for their own scientists?" He was rightfully wondering if a broad collaboration in building a network of archives will provide a durable and extensible technology and service framework for ever-increasing digital scholarly content. The ensuing discussion did not offer a plausible response but accentuated that we do not have in place a plan for building an expandable infrastructure to facilitate communication and exchange of information among rapidly proliferating distinct instances of institutional and subject repositories.

Fecha probable de imp. ; Recoge estructura y funcionamiento de este Tribunal Supremo, así como las cédulas, ordenanzas, decretos, etc., emitidos por dicho órgano desde 1621 hasta 1734 ; Fecha de imp. probable tomada de índice donde se relacionan documentos fechados en 1734 ; Port. con orla tip. ; Enc. Perg. ; Sign.: ¶8, ¶¶4, A-P8, Q4

Obra perteneciente al Fondo Antiguo de la Biblioteca de la USAL

"Los libros de donde he sacado las ordenanzas.son el de la vueva recopilacion de Ordenanzas militares, impresso y publicado en.1728.[e] los.tomos de las Ordananzas militares, impressos en.[1] 720. y reimpressos en.[1] 721.--Prologo. ; Mode of access: Internet.

Aligning National Approaches to Digital Preservation: An Action Assembly Biblioteca de Catalunya (National Library of Catalonia) November 18-20, 2013, Barcelona, Spain ; Auburn University ; Council on Library and Information Resources (CLIR) ; Digital Curation Centre (DCC) ; Digital Preservation Network (DPN) ; Joint Information Systems Committee (JISC) ; University of North Texas ; Virginia Tech ; Interuniversity Consortium for Political and Social Research (ICPSR) ; Innovative Interfaces ; Oracle ; Greendata ; Libnova ; Northeast Document Conservation Center (NEDCC) ; Open Planets Foundation (OPF) ; Springer ; The Aligning National Approaches to Digital Preservation (ANADP) II Action Assembly will align digital preservation efforts internationally between communitiesincluding national libraries, academic libraries, public libraries, research centers, archives, corporations, and funding agencies. ANADP II will be a highly participatory event in which stakeholders will engage in facilitated discussions and action sessions to produce a set of concrete outcomes for the extended digital preservation community in three areas: Community Alignment, Resource Alignment, and Capacity Alignment. These specific action outcomes will include an international tools/services registry, a framework for applying OAIS to Distributed Digital Preservation methodologies, a catalogue of education and training opportunities, and quantitative data gathering around digital preservation costs. History ANADP II will build on a strong foundation. The ANADP community first gathered in Estonia in 2011 with delegates from more than 20 nations to explore a series of targeted opportunities to align efforts in digital preservation. The outcome of that first event, the Aligning National Approaches to Digital Preservation volume, documented some of the most promising areas for future collaborative engagements between national and international digital preservation efforts (the volume is this years winner of the Society of American Archivists Preservation Publication award). Additional work in aligning international digital preservation efforts took place at the ANADP workshops hosted in Singapore (iPRES 2012) and Amsterdam (IDCC 2012). The Action Assembly ANADP II differs in intent and structure from other digital preservation conferences and meetings. Its primary purpose is not to encourage information sharing, but rather to foster and support sustained global networks of influence and action. Alignment in this context is a lightweight mechanism for cooperation. Alignments are formed around small or modular problems that are directly related to the participants own specific needs and interests. ANADP II will be easy to get involved with, participate in, or define new activities within. The ANADP II Action Assembly will consist of four components. Panel Discussions: Attendees will engage actively with panelists in conversations around three broad alignment themes: Community Alignment, Resource Alignment, and Capacity Alignment. Action Sessions: Attendees will participate in action sessions that demonstrate the powerful impact a concentrated alliance can have. There will be two tracks around each alignment theme, and attendees will select the track to/from which they feel they have the most to contribute/learn. Funder Presentations: Attendees will hear from representatives of funding groups that are interested in supporting cross-national digital preservation projects. Patio Perspectives: Attendees will help to identify and develop new alignment projects that those participating in this international event can pursue together. The purpose of ANADP II is to encourage collaboration among existing organizations and demonstrate what can be achieved through these informal alliances. ANADP II will foster a stronger international community of engagement and practice.

Aims. The Seeds Of Life In Space IRAM/NOEMA large program aims at studying a set of crucial complex organic molecules in a sample of sources with a well-known physical structure that covers the various phases of solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the very low luminosity object (VeLLO) L1521F. This type of source is important to study to link prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Methods. Two frequency windows (81.6-82.6 GHz and 96.65-97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. These setups cover transitions of ketene (H2CCO), propyne (CH3CCH), formamide (NH2CHO), methoxy (CH3O), methanol (CH3OH), dimethyl ether (CH3OCH3), and methyl formate (HCOOCH3). Results. Only two transitions of methanol (A+, E2) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E1) in a very compact emission blob (∼7″ corresponding to ∼1000 au) toward the northeast of the L1521F protostar. The CS 2-1 transition is also detected within theWideX bandwidth. Consistently with what has been found in prestellar cores, the methanol emission appears ∼1000 au away from the dust peak. The location of the methanol blob coincides with one of the filaments that have previously been reported in the literature. The excitation temperature of the gas inferred from methanol is (10 ± 2) K, while the H2 gas density (estimated from the detected CS 2-1 emission and previous CS 5-4 ALMA observations) is a factor >25 higher than the density in the surrounding environment (n(H2) ≥ 107 cm-3). Conclusions. Based on its compactness, low excitation temperature, and high gas density, we suggest that the methanol emission detected with NOEMA is (i) either a cold and dense shock-induced blob that formed recently (≤ a few hundred years) by infalling gas or (ii) a cold and dense fragment that may just have been formed as a result of the intense gas dynamics within the L1521F VeLLO system. © 2020 C. Favre et al. ; Russian Science Foundation, RSF: 18–12–00351 ; Australian Education International, Australian Government, AEI: MDM-2017-0737 ; Agence Nationale de la Recherche, ANR: ANR-15-IDEX-02 ; European Research Council, ERC ; Horizon 2020 Framework Programme, H2020: 741002 ; Ministerio de Economía y Competitividad, MINECO: AYA2016-79006-P ; European Regional Development Fund, FEDER: ESP2017-86582-C4-1-R ; Acknowledgements. We thank our referee, Dr. Kazuki Tokuda, (i) for his fruitful comments that have improved the quality of our paper and (ii) for sharing his continuum emission map. This work is supported by the French National Research Agency in the framework of the Investissements d'Avenir program (ANR-15-IDEX-02), through the funding of the "Origin of Life" project of the Univ. Grenoble-Alpes. C.F., C.V. and C.C. acknowledge the funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme, for the Project The Dawn of Organic Chemistry (DOC), grant agreement No 741002. I.J.-S. has received partial support from the Spanish FEDER (project number ESP2017-86582-C4-1-R), and State Research Agency (AEI) through project number MDM-2017-0737 Unidad de Excelencia María de Maeztu–Centro de Astrobiología (INTA-CSIC). A.P. acknowledges the financial support of the Russian Science Foundation project 18–12–00351. A.C.-T acknowledges support from MINECO project AYA2016-79006-P.

Aims. The Seeds Of Life In Space IRAM/NOEMA large program aims at studying a set of crucial complex organic molecules in a sample of sources with a well-known physical structure that covers the various phases of solar-type star formation. One representative object of the transition from the prestellar core to the protostar phases has been observed toward the very low luminosity object (VeLLO) L1521F. This type of source is important to study to link prestellar cores and Class 0 sources and also to constrain the chemical evolution during the process of star formation. Methods. Two frequency windows (81.6-82.6 GHz and 96.65-97.65 GHz) were used to observe the emission from several complex organics toward the L1521F VeLLO. These setups cover transitions of ketene (HCCO), propyne (CHCCH), formamide (NHCHO), methoxy (CHO), methanol (CHOH), dimethyl ether (CHOCH), and methyl formate (HCOOCH). Results. Only two transitions of methanol (A, E) have been detected in the narrow window centered at 96.7 GHz (with an upper limit on E) in a very compact emission blob (∼7″ corresponding to ∼1000 au) toward the northeast of the L1521F protostar. The CS 2-1 transition is also detected within theWideX bandwidth. Consistently with what has been found in prestellar cores, the methanol emission appears ∼1000 au away from the dust peak. The location of the methanol blob coincides with one of the filaments that have previously been reported in the literature. The excitation temperature of the gas inferred from methanol is (10 ± 2) K, while the H gas density (estimated from the detected CS 2-1 emission and previous CS 5-4 ALMA observations) is a factor >25 higher than the density in the surrounding environment (n(H) ≥ 10 cm). Conclusions. Based on its compactness, low excitation temperature, and high gas density, we suggest that the methanol emission detected with NOEMA is (i) either a cold and dense shock-induced blob that formed recently (≤ a few hundred years) by infalling gas or (ii) a cold and dense fragment that may just have been formed as a result of the intense gas dynamics within the L1521F VeLLO system. ; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Context. Low-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows. Aims. The evolution of sulfur chemistry is studied along the outflows driven by the NGC 1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. Methods. We observed various transitions from OCS, CS, SO, and SO2 towards NGC 1333-IRAS4A in the 1.3, 2, and 3 mm bands using the IRAM NOrthern Extended Millimeter Array and we interpreted the observations through the use of the Paris-Durham shock model. Results. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east-south west direction. SO is detected at extremely high radial velocity up to + 25 km s-1 relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 105 cm-3 and relatively warm (T > 100 K) temperatures in most cases. Conclusions. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputtered into the shock gas. In contrast, the longer and likely older outflow triggered by IRAS4A2 is more enriched in species that have a gas phase origin, such as SO2. © ESO 2020. ; V.T. is grateful to Sylvie Cabrit and Guillaume Pineau des Forêts for stimulating discussions on the chemistry in shocks. The authors acknowledge the CALYPSO consortium for the use of the CALYPSO dataset. This work is based on observations carried out with the IRAM PdBI/NOEMA Interferometer under project numbers V05B and V010 (PI: M.V. Persson), U003 (PI: V. Taquet), and L15AA (PI: C. Ceccarelli and P. Caselli). IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). V.T. acknowledges the financial support from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement n. 664931. This work was supported by (i) the PRIN-INAF 2016 "The Cradle of Life – GENESIS-SKA (General Conditions in Early Planetary Systems for the rise of life with SKA)", (ii) the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme, for the Project "The Dawn of Organic Chemistry" (DOC), grant agreement No 741002, and (iii) the European MARIE SKŁODOWSKA-CURIE ACTIONS under the European Union's Horizon 2020 research and innovation programme, for the Project "Astro-Chemistry Origins" (ACO), Grant No 811312. C.F. acknowledges support from the French National Research Agency in the framework of the Investissements d'Avenir program (ANR-15-IDEX-02), through the funding of the "Origin of Life" project of the Université Grenoble-Alpes.