A new analog trigger system for the Cherenkov Telescope array

La astronomía de rayos γ estudia las partículas más energéticas que llegan a la Tierra desde el espacio. Estos rayos γ no se generan mediante procesos térmicos en simples estrellas, sino mediante mecanismos de aceleración de partículas en objetos celestes como núcleos de galaxias activos, púlsares, supernovas, o posibles procesos de aniquilación de materia oscura. Los rayos γ procedentes de estos objetos y sus características proporcionan una valiosa información con la que los científicos tratan de comprender los procesos físicos que ocurren en ellos y desarrollar modelos teóricos que describan su funcionamiento con fidelidad. El problema de observar rayos γ es que son absorbidos por las capas altas de la atmósfera y no llegan a la superficie (de lo contrario, la Tierra será inhabitable). De este modo, sólo hay dos formas de observar rayos γ embarcar detectores en satélites, u observar los efectos secundarios que los rayos γ producen en la atmósfera. Cuando un rayo γ llega a la atmósfera, interacciona con las partículas del aire y genera un par electrón - positrón, con mucha energía. Estas partículas secundarias generan a su vez más partículas secundarias cada vez menos energéticas. Estas partículas, mientras aún tienen energía suficiente para viajar más rápido que la velocidad de la luz en el aire, producen una radiación luminosa azulada conocida como radiación Cherenkov durante unos pocos nanosegundos. Desde la superficie de la Tierra, algunos telescopios especiales, conocidos como telescopios Cherenkov o IACTs (Imaging Atmospheric Cherenkov Telescopes), son capaces de detectar la radiación Cherenkov e incluso de tomar imágenes de la forma de la cascada Cherenkov. A partir de estas imágenes es posible conocer las principales características del rayo γ original, y con suficientes rayos se pueden deducir características importantes del objeto que los emitió, a cientos de años luz de distancia. Sin embargo, detectar cascadas Cherenkov procedentes de rayos γ no es nada fácil. Las cascadas generadas por fotones γ de bajas energías emiten pocos fotones, y durante pocos nanosegundos, y las correspondientes a rayos γ de alta energía, si bien producen más electrones y duran más, son más improbables conforme mayor es su energía. Esto produce dos líneas de desarrollo de telescopios Cherenkov: Para observar cascadas de bajas energías son necesarios grandes reflectores que recuperen muchos fotones de los pocos que tienen estas cascadas. Por el contrario, las cascadas de altas energías se pueden detectar con telescopios pequeños, pero conviene cubrir con ellos una superficie grande en el suelo para aumentar el número de eventos detectados. Con el objetivo de mejorar la sensibilidad de los telescopios Cherenkov actuales, en el rango de energía alto (> 10 TeV), medio (100 GeV - 10 TeV) y bajo (10 GeV - 100 GeV), nació el proyecto CTA (Cherenkov Telescope Array). Este proyecto en el que participan más de 27 países, pretende construir un observatorio en cada hemisferio, cada uno de los cuales contará con 4 telescopios grandes (LSTs), unos 30 medianos (MSTs) y hasta 70 pequeños (SSTs). Con un array así, se conseguirán dos objetivos. En primer lugar, al aumentar drásticamente el área de colección respecto a los IACTs actuales, se detectarán más rayos γ en todos los rangos de energía. En segundo lugar, cuando una misma cascada Cherenkov es observada por varios telescopios a la vez, es posible analizarla con mucha más precisión gracias a las técnicas estereoscópicas. La presente tesis recoge varios desarrollos técnicos realizados como aportación a los telescopios medianos y grandes de CTA, concretamente al sistema de trigger. Al ser las cascadas Cherenkov tan breves, los sistemas que digitalizan y leen los datos de cada píxel tienen que funcionar a frecuencias muy altas (≈1 GHz), lo que hace inviable que funcionen de forma continua, ya que la cantidad de datos guardada será inmanejable. En su lugar, las señales analógicas se muestrean, guardando las muestras analógicas en un buffer circular de unos pocos µs. Mientras las señales se mantienen en el buffer, el sistema de trigger hace un análisis rápido de las señales recibidas, y decide si la imagen que hay en el buér corresponde a una cascada Cherenkov y merece ser guardada, o por el contrario puede ignorarse permitiendo que el buffer se sobreescriba. La decisión de si la imagen merece ser guardada o no, se basa en que las cascadas Cherenkov producen detecciones de fotones en píxeles cercanos y en tiempos muy próximos, a diferencia de los fotones de NSB (night sky background), que llegan aleatoriamente. Para detectar cascadas grandes es suficiente con comprobar que más de un cierto número de píxeles en una región hayan detectado más de un cierto número de fotones en una ventana de tiempo de algunos nanosegundos. Sin embargo, para detectar cascadas pequeñas es más conveniente tener en cuenta cuántos fotones han sido detectados en cada píxel (técnica conocida como sumtrigger). El sistema de trigger desarrollado en esta tesis pretende optimizar la sensibilidad a bajas energías, por lo que suma analógicamente las señales recibidas en cada píxel en una región de trigger y compara el resultado con un umbral directamente expresable en fotones detectados (fotoelectrones). El sistema diseñado permite utilizar regiones de trigger de tamaño seleccionable entre 14, 21 o 28 píxeles (2, 3, o 4 clusters de 7 píxeles cada uno), y con un alto grado de solapamiento entre ellas. De este modo, cualquier exceso de luz en una región compacta de 14, 21 o 28 píxeles es detectado y genera un pulso de trigger. En la versión más básica del sistema de trigger, este pulso se distribuye por toda la cámara de forma que todos los clusters sean leídos al mismo tiempo, independientemente de su posición en la cámara, a través de un delicado sistema de distribución. De este modo, el sistema de trigger guarda una imagen completa de la cámara cada vez que se supera el número de fotones establecido como umbral en una región de trigger. Sin embargo, esta forma de operar tiene dos inconvenientes principales. En primer lugar, la cascada casi siempre ocupa sólo una pequeña zona de la cámara, por lo que se guardan muchos píxeles sin información alguna. Cuando se tienen muchos telescopios como será el caso de CTA, la cantidad de información inútil almacenada por este motivo puede ser muy considerable. Por otro lado, cada trigger supone guardar unos pocos nanosegundos alrededor del instante de disparo. Sin embargo, en el caso de cascadas grandes la duración de las mismas puede ser bastante mayor, perdiéndose parte de la información debido al truncamiento temporal. Para resolver ambos problemas se ha propuesto un esquema de trigger y lectura basado en dos umbrales. El umbral alto decide si hay un evento en la cámara y, en caso positivo, sólo las regiones de trigger que superan el nivel bajo son leídas, durante un tiempo más largo. De este modo se evita guardar información de píxeles vacíos y las imágenes fijas de las cascadas se pueden convertir en pequeños \vídeos" que representen el desarrollo temporal de la cascada. Este nuevo esquema recibe el nombre de COLIBRI (Concept for an Optimized Local Image Building and Readout Infrastructure), y se ha descrito detalladamente en el capítulo 5. Un problema importante que afecta a los esquemas de sumtrigger como el que se presenta en esta tesis es que para sumar adecuadamente las señales provenientes de cada píxel, estas deben tardar lo mismo en llegar al sumador. Los fotomultiplicadores utilizados en cada píxel introducen diferentes retardos que deben compensarse para realizar las sumas adecuadamente. El efecto de estos retardos ha sido estudiado, y se ha desarrollado un sistema para compensarlos. Por último, el siguiente nivel de los sistemas de trigger para distinguir efectivamente las cascadas Cherenkov del NSB consiste en buscar triggers simultáneos (o en tiempos muy próximos) en telescopios vecinos. Con esta función, junto con otras de interfaz entre sistemas, se ha desarrollado un sistema denominado Trigger Interface Board (TIB). Este sistema consta de un módulo que irá montado en la cámara de cada LST o MST, y que estará conectado mediante fibras ópticas a los telescopios vecinos. Cuando un telescopio tiene un trigger local, este se envía a todos los vecinos conectados y viceversa, de modo que cada telescopio sabe si sus vecinos han dado trigger. Una vez compensadas las diferencias de retardo debidas a la propagación en las fibras ópticas y de los propios fotones Cherenkov en el aire dependiendo de la dirección de apuntamiento, se buscan coincidencias, y en el caso de que la condición de trigger se cumpla, se lee la cámara en cuestión, de forma sincronizada con el trigger local. Aunque todo el sistema de trigger es fruto de la colaboración entre varios grupos, fundamentalmente IFAE, CIEMAT, ICC-UB y UCM en España, con la ayuda de grupos franceses y japoneses, el núcleo de esta tesis son el Level 1 y la Trigger Interface Board, que son los dos sistemas en los que que el autor ha sido el ingeniero principal. Por este motivo, en la presente tesis se ha incluido abundante información técnica relativa a estos sistemas. Existen actualmente importantes líneas de desarrollo futuras relativas tanto al trigger de la cámara (implementación en ASICs), como al trigger entre telescopios (trigger topológico), que darán lugar a interesantes mejoras sobre los diseños actuales durante los próximos años, y que con suerte serán de provecho para toda la comunidad científica participante en CTA. ABSTRACT -ray astronomy studies the most energetic particles arriving to the Earth from outer space. This -rays are not generated by thermal processes in mere stars, but by means of particle acceleration mechanisms in astronomical objects such as active galactic nuclei, pulsars, supernovas or as a result of dark matter annihilation processes. The γ rays coming from these objects and their characteristics provide with valuable information to the scientist which try to understand the underlying physical fundamentals of these objects, as well as to develop theoretical models able to describe them accurately. The problem when observing rays is that they are absorbed in the highest layers of the atmosphere, so they don't reach the Earth surface (otherwise the planet would be uninhabitable). Therefore, there are only two possible ways to observe γ rays: by using detectors on-board of satellites, or by observing their secondary effects in the atmosphere. When a γ ray reaches the atmosphere, it interacts with the particles in the air generating a highly energetic electron-positron pair. These secondary particles generate in turn more particles, with less energy each time. While these particles are still energetic enough to travel faster than the speed of light in the air, they produce a bluish radiation known as Cherenkov light during a few nanoseconds. From the Earth surface, some special telescopes known as Cherenkov telescopes or IACTs (Imaging Atmospheric Cherenkov Telescopes), are able to detect the Cherenkov light and even to take images of the Cherenkov showers. From these images it is possible to know the main parameters of the original -ray, and with some -rays it is possible to deduce important characteristics of the emitting object, hundreds of light-years away. However, detecting Cherenkov showers generated by γ rays is not a simple task. The showers generated by low energy -rays contain few photons and last few nanoseconds, while the ones corresponding to high energy -rays, having more photons and lasting more time, are much more unlikely. This results in two clearly differentiated development lines for IACTs: In order to detect low energy showers, big reflectors are required to collect as much photons as possible from the few ones that these showers have. On the contrary, small telescopes are able to detect high energy showers, but a large area in the ground should be covered to increase the number of detected events. With the aim to improve the sensitivity of current Cherenkov showers in the high (> 10 TeV), medium (100 GeV - 10 TeV) and low (10 GeV - 100 GeV) energy ranges, the CTA (Cherenkov Telescope Array) project was created. This project, with more than 27 participating countries, intends to build an observatory in each hemisphere, each one equipped with 4 large size telescopes (LSTs), around 30 middle size telescopes (MSTs) and up to 70 small size telescopes (SSTs). With such an array, two targets would be achieved. First, the drastic increment in the collection area with respect to current IACTs will lead to detect more -rays in all the energy ranges. Secondly, when a Cherenkov shower is observed by several telescopes at the same time, it is possible to analyze it much more accurately thanks to the stereoscopic techniques. The present thesis gathers several technical developments for the trigger system of the medium and large size telescopes of CTA. As the Cherenkov showers are so short, the digitization and readout systems corresponding to each pixel must work at very high frequencies (_ 1 GHz). This makes unfeasible to read data continuously, because the amount of data would be unmanageable. Instead, the analog signals are sampled, storing the analog samples in a temporal ring buffer able to store up to a few _s. While the signals remain in the buffer, the trigger system performs a fast analysis of the signals and decides if the image in the buffer corresponds to a Cherenkov shower and deserves to be stored, or on the contrary it can be ignored allowing the buffer to be overwritten. The decision of saving the image or not, is based on the fact that Cherenkov showers produce photon detections in close pixels during near times, in contrast to the random arrival of the NSB phtotons. Checking if more than a certain number of pixels in a trigger region have detected more than a certain number of photons during a certain time window is enough to detect large showers. However, taking also into account how many photons have been detected in each pixel (sumtrigger technique) is more convenient to optimize the sensitivity to low energy showers. The developed trigger system presented in this thesis intends to optimize the sensitivity to low energy showers, so it performs the analog addition of the signals received in each pixel in the trigger region and compares the sum with a threshold which can be directly expressed as a number of detected photons (photoelectrons). The trigger system allows to select trigger regions of 14, 21, or 28 pixels (2, 3 or 4 clusters with 7 pixels each), and with extensive overlapping. In this way, every light increment inside a compact region of 14, 21 or 28 pixels is detected, and a trigger pulse is generated. In the most basic version of the trigger system, this pulse is just distributed throughout the camera in such a way that all the clusters are read at the same time, independently from their position in the camera, by means of a complex distribution system. Thus, the readout saves a complete camera image whenever the number of photoelectrons set as threshold is exceeded in a trigger region. However, this way of operating has two important drawbacks. First, the shower usually covers only a little part of the camera, so many pixels without relevant information are stored. When there are many telescopes as will be the case of CTA, the amount of useless stored information can be very high. On the other hand, with every trigger only some nanoseconds of information around the trigger time are stored. In the case of large showers, the duration of the shower can be quite larger, loosing information due to the temporal cut. With the aim to solve both limitations, a trigger and readout scheme based on two thresholds has been proposed. The high threshold decides if there is a relevant event in the camera, and in the positive case, only the trigger regions exceeding the low threshold are read, during a longer time. In this way, the information from empty pixels is not stored and the fixed images of the showers become to little \`videos" containing the temporal development of the shower. This new scheme is named COLIBRI (Concept for an Optimized Local Image Building and Readout Infrastructure), and it has been described in depth in chapter 5. An important problem affecting sumtrigger schemes like the one presented in this thesis is that in order to add the signals from each pixel properly, they must arrive at the same time. The photomultipliers used in each pixel introduce different delays which must be compensated to perform the additions properly. The effect of these delays has been analyzed, and a delay compensation system has been developed. The next trigger level consists of looking for simultaneous (or very near in time) triggers in neighbour telescopes. These function, together with others relating to interfacing different systems, have been developed in a system named Trigger Interface Board (TIB). This system is comprised of one module which will be placed inside the LSTs and MSTs cameras, and which will be connected to the neighbour telescopes through optical fibers. When a telescope receives a local trigger, it is resent to all the connected neighbours and vice-versa, so every telescope knows if its neighbours have been triggered. Once compensated the delay differences due to propagation in the optical fibers and in the air depending on the pointing direction, the TIB looks for coincidences, and in the case that the trigger condition is accomplished, the camera is read a fixed time after the local trigger arrived. Despite all the trigger system is the result of the cooperation of several groups, specially IFAE, Ciemat, ICC-UB and UCM in Spain, with some help from french and japanese groups, the Level 1 and the Trigger Interface Board constitute the core of this thesis, as they have been the two systems designed by the author of the thesis. For this reason, a large amount of technical information about these systems has been included. There are important future development lines regarding both the camera trigger (implementation in ASICS) and the stereo trigger (topological trigger), which will produce interesting improvements for the current designs during the following years, being useful for all the scientific community participating in CTA.

Restauración del sonido fílmico

La restauración fílmica del audio es un proceso bastante complejo y se ha indagado poco en este campo. Antes de restaurar cualquier archivo, se debe preservar y conservar los archivos de la mejor manera posible. La preservación son las medidas que se deben tomar para garantizar el acceso permanente y la conservación asegura le existencia del archivo en su forma más original. Mientras que la restauración se basa en el estudio de los posibles deterioros que sufren los soportes fílmicos en el tiempo y los procesos que existen para corregirlos. La restauración siempre debe conservar la mayor originalidad posible, es decir debe mantener el audio como originalmente se expuso por primera vez. En la primera etapa, se identifican los posibles deterioros que se producen en los archivos, si conocemos en qué momento fue grabada la películas y cómo fue grabada, es decir con que máquina se realizó la grabación y el soporte fílmico en el que está grabado. Tanto las máquinas como los soportes han ido evolucionando a lo largo de la historia. El estudio de los soportes fílmicos nos permite conocer las degradaciones que sufren a lo largo del tiempo los archivos y por consecuencia, conocer las posibles restauraciones. Para intentar evitar degradaciones mayores, se intenta preservar y conservar en condiciones óptimas para el soporte. Según el soporte del archivo, tendrá unas condiciones típicas de temperatura, humedad, ventilación… en las cuales el material se conserva de la mejor manera. Tras estos pasos, se procede a restaurar. La restauración más típica es con materiales fotoquímicos, pero es bastante compleja y por tanto, en el proyecto se analiza la restauración tras digitalizar los archivos fílmicos. Para poder digitalizar correctamente los archivos, debemos tener presentes las normas y reglas de digitalización que están establecidas. La digitalización permite identificar las alteraciones típicas que aparecen en los materiales fílmicos, gracias a la herramienta del espectrograma podemos conocer las posibles soluciones de restauración para cada alteración. Las alteraciones que podemos encontrar e identificar son: · Zumbidos e Interferencias. · Siseo y Silbido. · Crujidos. · Pops y Clics. · Wow. · Lagunas o Abandonos. · Ruidos intermitentes. · Reverberación. La última parte del proyecto, una vez que se tienen todas las alteraciones típicas de los archivos fílmicos identificadas, se procede al estudio de cada una de ellas con las herramientas del espectrograma y se realiza el estudio de una manera más técnica. Con el espectrograma se determinan las herramientas que solucionan cada alteración como Reverb para la reverberación, Decrackle para los crujidos… y en el marco técnico se determina las características que tiene cada herramienta, es decir el tipo de filtro, ventana… que se puede utilizar para poder restaurar el audio de cada alteración. La restauración digital es un campo aún por investigar, pero se debería de empezar a concienciar que es una solución factible. Que este tipo de restauración puede mantener el sonido original y no va a modificar los archivos, como muchas veces se piensa. Ya que el paso del tiempo, poco a poco, ira degradando y destruyendo los soportes fílmicos en los que se encuentran, y el principal objetivo que se pretende conseguir es que los materiales fílmicos perduren a lo largo de la historia. ABSTRACT. The film audio restoration is a fairly complex process and little research has been done in this field. Before restoring any files, you must preserve and keep the files in the best way possible. The preservation is the measures to be taken to ensure continued access to and preservation ensures existence of the file in its original form. The restoration is based on the study of possible damage suffered by the film media in time and the processes that exist to correct them. The restoration must always retain the most original as possible, i.e. to keep the audio as originally discussed for the first time. In the first stage, potential impairments that occur in the files are identified, if you know what time it was recorded the movies and how it was recorded, i.e. that machine recording and film media on which is recorded took place. Both machines as media have evolved throughout history. The study of film media lets us know the suffering degradations over time and result files, make possible restorations. To try to prevent further degradation, are intended to preserve and keep in good condition for support. Depending on the media file, will have typical conditions of temperature, humidity, ventilation... in which the material is preserved in the best way. After these steps, we proceed to restore. The most typical is with photochemical restoration materials, but is rather complex and therefore the restoration project is analyzed after scanning film archives. To successfully scan the files must be aware of the rules and regulations are established digitization. Digitization allows identifying the typical alterations that appear in the film materials, thanks to the tool spectrogram we know the possible restoration solutions for each alteration. The alterations that can find and identify are: · Buzz and Interference. · Hiss and Hissing. · Crackle. · Pops and Clicks. · Wow and Flutter. · Audio Dropouts. The last part of the project, when we have all the typical alterations identified film archives, proceed to the study of each of them with the tools of spectrogram and the study of a more technical way is done . With the spectrogram tools that solve every alteration as Reverb for reverb, Decrackle for cracks... and the technical framework the features that each tool is determined, i.e. the type of filter, window... that can be used are determined for to restore the audio of each alteration. Digital restoration is an area for future research, but should start aware that it is a feasible solution. This type of restoration can keep the original sound and will not modify files, as is often thought. Since the passage of time, gradually degrading and destroying anger film media in which they are, and the main objective to be achieved is that the film materials endure throughout history.

Saline Stress Alters the Temporal Patterns of Xylem Differentiation and Alternative Oxidase Expression in Developing Soybean Roots1

We conducted a coordinated biochemical and morphometric analysis of the effect of saline conditions on the differentiation zone of developing soybean (Glycine max L.) roots. Between d 3 and d 14 for seedlings grown in control or NaCl-supplemented medium, we studied (a) the temporal evolution of the respiratory alternative oxidase (AOX) capacity in correlation with the expression and localization of AOX protein analyzed by tissue-print immunoblotting; (b) the temporal evolution and tissue localization of a peroxidase activity involved in lignification; and (c) the structural changes, visualized by light microscopy and quantified by image digitization. The results revealed that saline stress retards primary xylem differentiation. There is a corresponding delay in the temporal pattern of AOX expression, which is consistent with the xylem-specific localization of AOX protein and the idea that this enzyme is linked to xylem development. An NaCl-induced acceleration of the development of secondary xylem was also observed. However, the temporal pattern of a peroxidase activity localized in the primary and secondary xylem was unaltered by NaCl treatment. Thus, the NaCl-stressed root was specifically affected in the temporal patterns of AOX expression and xylem development.

Digitizing the Historical Periodical Collection at the Al-Aqsa Mosque Library in East Jerusalem

The Arab Press in Palestine developed at the turn of the twentieth century and proliferated for several decades despite restrictions imposed under the Ottoman Empire and during the British Mandate Period (1917-1948). Hardcopies of the early newspapers and periodicals are rare and access to them at a few Palestinian municipal or private libraries is limited. The Al-Aqsa Mosque Library holds one of the largest collections of Palestinian historical newspapers and periodicals. The collection provides a unique and rich source of information about the history of Palestine in the first half of the twentieth century. Access to the collection is limited and brittle paper copies have been rapidly deteriorating. This paper provides an overview of the digitization project aimed at preserving the historical periodical collection located at the AlAqsa Mosque Library

Has the European ICT sector a chance to be competitive? Bruges European Economic Policy (BEEP) Briefing 14/2006

In this paper we try to present the main trends of evolution of the ICT sector. Its dynamics, supported by a constant technical progress in ICs, compounded with “non convexities” such as network effects and high sunk costs, may either lead to a Schumpeter Mark I or Schumpeter Mark II competition regime. This means that in some segments, the market will be more competitive (Mark I), while in other it will be more monopolistic (Mark II). But a key trend is also the so called “convergence”. But digitization makes it cost effective to integrate different communications, information processing and entertainment systems and devices. Hence, Schumpeter Mark II grows at the core where software production dominates, while Schumpeter Mark I is established at the periphery. In this context, the European ICT industry is potentially smashed between two forces: the cost advantages of Asian countries on one hand, the inventiveness and dynamism of the US industry on the other hand. The way out of this very difficult situation is to create in Europe the conditions of restoring knowledge accumulation in a key sub-sector of ICT, that is software production. To do this, Europe can rely on its tradition of cooperation and knowledge sharing and on a set of institutions that have shown their ability to stimulate inter-regional cooperation. By concentrating on an ambitious project of open source software production in embarked systems and domestic networks, Europe could reach several objectives: to make freely accessible an essential facility, to stimulate competition, to help reaching the Lisbon objectives and to restore the European competitiveness in ICT.

Naẓm al-Jamīʻ al-ṣaghīr, [late 15th century?].

Fine copy of Abū Naṣr al-Farāḥī's (d.1242) versification of al-Jamīʻ al-ṣaghīr fī al-furūʻ, the well-known legal treatise by Muḥammad ibn al-Ḥasan al-Shaybānī (d.804). Excerpts from Kashf al-ẓunūn addressing these two works appear on leaf affixed to 'title page' (p.5).

Relato rio apresentado ao Presidente da Repu blica dos Estados Unidos do Brazil /

Latest issue consulted: 1926.

Qānūnchah fī al-ṭibb, [880, i.e. 1475 or 1476].

Fine copy of al-Jaghmīnī's (d.1344) Qānūnchah, a compendium on medicine and an extract from Ibn Sīnā’s Qānūn. Brockelmann treats this author as distinct from an astronomer of the same name who died in 1221.

al-Asmāʼ al-ḥusná mustakhrajah min al-Qurʼān al-ʻaẓīm wa-Kitāb al-Ṭibb al-nabawī, [15th century?].

A work on prophetic medicine (or the Prophet's medicine) by al-Maqdisī (d.1245) preceded by a short treatise of uncertain authorship on the beautiful names of God.

Hāẕā Kitāb-i Khvājah Ḥāfiẓ-i Shīrāzī, [1280, i.e. 1863 or 1864].

Richly elegant copy of the Dīvān of the masterful poet Ḥāfiẓ (Khvājah Shams al-Dīn Muḥammad Shīrāzī, d.1390?).

Co-registration of magnetoencephalography with magnetic resonance imaging using bite-bar-based fiducials and surface-matching

Objective: To introduce a new technique for co-registration of Magnetoencephalography (MEG) with magnetic resonance imaging (MRI). We compare the accuracy of a new bite-bar with fixed fiducials to a previous technique whereby fiducial coils were attached proximal to landmarks on the skull. Methods: A bite-bar with fixed fiducial coils is used to determine the position of the head in the MEG co-ordinate system. Co-registration is performed by a surface-matching technique. The advantage of fixing the coils is that the co-ordinate system is not based upon arbitrary and operator dependent fiducial points that are attached to landmarks (e.g. nasion and the preauricular points), but rather on those that are permanently fixed in relation to the skull. Results: As a consequence of minimizing coil movement during digitization, errors in localization of the coils are significantly reduced, as shown by a randomization test. Displacement of the bite-bar caused by removal and repositioning between MEG recordings is minimal (∼0.5 mm), and dipole localization accuracy of a somatosensory mapping paradigm shows a repeatability of ∼5 mm. The overall accuracy of the new procedure is greatly improved compared to the previous technique. Conclusions: The test-retest reliability and accuracy of target localization with the new design is superior to techniques that incorporate anatomical-based fiducial points or coils placed on the circumference of the head. © 2003 International Federation of Clinical Neurophysiology. Published by Elsevier Ireland Ltd. All rights reserved.

Creation of a Digital Corpus of Bulgarian Dialects

The paper presents our considerations related to the creation of a digital corpus of Bulgarian dialects. The dialectological archive of Bulgarian language consists of more than 250 audio tapes. All tapes were recorded between 1955 and 1965 in the course of regular dialectological expeditions throughout the country. The records typically contain interviews with inhabitants of small villages in Bulgaria. The topics covered are usually related to such issues as birth, everyday life, marriage, family relationship, death, etc. Only a few tapes contain folk songs from different regions of the country. Taking into account the progressive deterioration of the magnetic media and the realistic prospects of data loss, the Institute for Bulgarian Language at the Academy of Sciences launched in 1997 a project aiming at restoration and digital preservation of the dialectological archive. Within the framework of this project more than the half of the records was digitized, de-noised and stored on digital recording media. Since then restoration and digitization activities are done in the Institute on a regular basis. As a result a large collection of sound files has been gathered. Our further efforts are aimed at the creation of a digital corpus of Bulgarian dialects, which will be made available for phonological and linguistic research. Such corpora typically include besides the sound files two basic elements: a transcription, aligned with the sound file, and a set of standardized metadata that defines the corpus. In our work we will present considerations on how these tasks could be realized in the case of the corpus of Bulgarian dialects. Our suggestions will be based on a comparative analysis of existing methods and techniques to build such corpora, and by selecting the ones that fit closer to the particular needs. Our experience can be used in similar institutions storing folklore archives, history related spoken records etc.

Electronic Presentation of Bulgarian Educational Archives: an Ontology-Based Approach

The paper presents an ongoing effort aimed at building an electronic archive of documents issued by the Bulgarian Ministry of Education in the 40ies and 50ies of the 20th century. These funds are stored in the Archive of the Ministry of the People’s Education within the State Archival Fund of the General Department of Archives at the Council of Ministers of Bulgaria. Our basic concern is not the digitization process per se, but the subsequent organization of the archive in a clear and easily-searchable way which would allow various types of users to get access to the documents of interest to them. Here we present the variety of the documents which are stored in the archival collection, and suggestions on their electronic organization. We suggest using ontologies- based presentation of the archive. The basic benefit of this approach is the possibility to search the collection according to the stored content categories.

Digitisation Processing and Recognition of Old Greek Manuscipts (the D-SCRIBE Project)

After many years of scholar study, manuscript collections continue to be an important source of novel information for scholars, concerning both the history of earlier times as well as the development of cultural documentation over the centuries. D-SCRIBE project aims to support and facilitate current and future efforts in manuscript digitization and processing. It strives toward the creation of a comprehensive software product, which can assist the content holders in turning an archive of manuscripts into a digital collection using automated methods. In this paper, we focus on the problem of recognizing early Christian Greek manuscripts. We propose a novel digital image binarization scheme for low quality historical documents allowing further content exploitation in an efficient way. Based on the existence of closed cavity regions in the majority of characters and character ligatures in these scripts, we propose a novel, segmentation-free, fast and efficient technique that assists the recognition procedure by tracing and recognizing the most frequently appearing characters or character ligatures.

Maltese Experience with Digitizing Cultural Heritage

The article gives an account of the various microfilming initiatives taken in Malta during the last thirty years. Various archives have managed to microfilm their holdings under co-operation agreements with international societies, or manuscript libraries. The advent of digital technology is now posing new challenges and opportunities for the archives sector. The idea of a National Memory Project that will try to bridge the different approaches in the preservation of records in the various public, private, and ecclesiastical archives in Malta is discussed. Technical challenges are highlighted, as are the opportunities that arise from collaboration and active participation in international projects such as the European Visual Archives (EVA), and the SEEDI initiative.