Research Team Grants in Science and Technology

TEAM RESEARCH PROJECTS (ANILLOS) IN SCIENCE AND TECHNOLOGY AND IN ANTARCTIC SCIENCE 2009

FINAL REPORT

I. PROJECT PRESENTATION

PROJECT TITLE CODE Development of technologies for astronomical observations. Chile: from host to active partner in the construction of the next generation astronomical ACT-86 telescopes PROJECT DIRECTOR SIGNATURE

Leonardo Vanzi

MAIN INSTITUTION Pontificia Universidad Católica de Chile PERIOD INFORMED Jan-2010 – Dec-2013

II. EXECUTIVE SUMMARY

This section should have no more than 3 pages written with any letter style point size 12. Summarize the updated achievements of the project including those related to research objectives, international collaboration, training activities, results dissemination to the scientific community and outreach to non-specialized public. The contents of this section are public and may be published in CONICYT’s website. This summary has to inform the potential reviewers about the progress of the project and the way these advances have come to be. Since this summary has to be available to non-experts in your area we request the use of relatively simple language or explanations when technical term do require.

The objective of the project was to acquire and develop front line technologies in a number of selected areas of science and engineering to be employed in the next generation astronomical telescopes. In particular we aimed to make the participants of the project competitive in the specific fields selected and to convert them in attractive partners for the international observatories present in Chile. With this purpose we defined a number of areas and activities of interests. The participants are Departments and Institutes of the Pontificia Universidad Catolica de Chile joint into the Center of Astro Engineering (AIUC) plus a wide network of international collaborators supporting them. The goal was pursued with the collaboration of international partners leaders in the fields selected. More specifically three main areas of work were defined in the project Anillo:

- Technology. Acquire the necessary know-how and experience in a selected number of technological areas, mainly: (i) technologies for the near-infrared spectral band (NIR), (ii) adaptive optics (AO), (iii) detector read-out systems, (iv) software, data handling, computation and (v) mechanics. - Science. Provide the Chilean scientific community with the tools to carry out front line scientific research. - Outreach. Promote technological and cultural transfer to the Chilean society.

Our efforts started at the AIUC and mostly focused to build experience. The specific activities developed during the project began from the plan set in the original proposal following the main lines defined and developed during the three years of the project. In some cases new work areas were opened. Due to diverse circumstances the initial three years plan of the project extended to almost four.

The activity at the AIUC during this period increased considerably. We started with a small group of researchers pioneering an area that was basically absent at Universidad Católica. After four years we have a robust team, an interesting infrastructure, a solid collaboration network worldwide and we are involved in major projects. All this makes the AIUC an interesting reference for local companies and it is attracting the interest of students and young scientists.

As part of this project we equipped three completely new laboratories at the AIUC: - The Lab of IR technology including equipment for vacuum and cryogenics, IR detectors, read out electronics. - The optical Lab which includes a large optical bench and a variety of opto-mechanical components to arrange optical setups and testing. - The Lab of Adaptive Optics (AO) technology including a full test bench AO system, wavefront (WF) sensor , deformable mirror (DM) and atmospheric turbulence simulator

We installed two fully operational instruments at the UC Observatory Santa Martina, the spectrograph PUCHEROS (Fondecyt n. 1095187) and the fast photometry camera MERLIN. Both instruments are currently in operation and are producing interesting scientific results. The project provided support to the regular operation of the Observatory and supported the development of an entirely new Telescope Control System (TCS).

We developed the study of two AIUC second-generation instruments, the high-resolution spectrograph FIDEOS, an evolution of the first FIESOLE idea and the multi-band imager BOMBOLO. The construction of both instruments was funded by CONICYT through FONDEF and QUIMAL respectively. We started to develop a third idea for a NIR high-resolution spectrograph and tested its technologies in the Lab .

The participation of AIUC in international projects grew from the participation in the phase A study of SIMPLE for the E-ELT to becoming members of the MOONS consortium that is currently starting the construction of the new MOS instrument for the ESO VLT. The AIUC is also part of the European HIRES initiative aimed at providing a high-resolution spectroscopic facility for the E-ELT. The AIUC is an active member of the HAT-South network, is contributing to the ACT project and is member of the G-Clef consortium for the GMT.

Developing software (SW) was a relevant part of our work in the area of technology. We collaborated in this subject with external partners. As results we have the SW of the new TCS for the UC observatory telescopes (including the autoguider) and a new read out system for the IR detectors. SW development is currently our main task within the MOONS consortium. During this Anillo the Geryon clusters experienced an order of magnitude leap. During the first year, the memory of the computer was multiplied by a factor of 2 with the help of this project, and was moved to the new computing room of the AIUC. The disk capacity was also increased by a factor of a few with this project. After the acquisition of Geryon2, the new computing cluster funded primarily by BASAL PFB-06 CATA, the Anillo made an important contribution to the necessary upgrade of the acclimatization of the computing room, which was not initially designed to support the load of two combined clusters. Members of this Anillo carried along these improvements. On the administration side, the Geryon computers were open for use by all astronomers in Chilean institutions, and for this a system of tickets and a good internal organization were set up, and have proven to work reasonably well. In sum this Anillo contributed to turn a single computing cluster in a makeshift room, into a national facility, which has now gained momentum and continues to grow.

In terms of manpower the AIUC grew considerably during the execution of the project. The Anillo supported students working on their undergraduated, master and PhD research thesis in the area of astronomy and engineering. Three post-doc researchers were hired during the course of the project to work in the near IR Lab and on the design of new instruments.

The international collaborations of the AIUC strengthened considerably during the project. In particular with the Observatory of Paris thanks to the program of occultations of minor bodies in the solar system; with the University of Tokyo through the support of the operation of miniTAO; with the University of Durham and Gemini observatory in the field of Adaptive Optics; with INAF in infrared (IR) technologies. Our team members travelled to conferences worldwide, paid visits to institutes abroad and received international guests with the support of this project Anillo.

Considerable efforts have been made in the area of technological transfer. In order to contribute to the productive reality of the country, we have built a two-step process, one from the international observatories in Chile to the academy, and a second one from the academy to local industry,. We participated in a number of initiatives aimed at establishing links with the private sector and helped organize a few other. Although the local reality in this area is poor, we believe we have made our contribution, in particular with some small companies.

In terms of scientific activities, the UC instruments PUCHEROS, MERLIN and the HAT South collaboration reached relevant milestones. All other projects of research met the goals of scientific production, results and publications. The scientific research was particularly active in the fields of variable stars, binary systems, the galactic bulge, clusters, exoplanets and in cosmological numerical simulations. The team maintained a high scientific productivity with 117 refereed papers published in international Journals during the period of the project.

The AIUC supports a lively activity of outreach in astronomy and instrumentation in collaboration with the Institute of Astrophysics and the School of Engineering UC. One of the main outreach activities is related to the UC historic observatory Manuel Foster. During the execution of this project we managed to open the site to the public for the first time in almost two decades and are pushing hard the creation of a Museum of Astronomy at this historic site. Members of the AIUC are actively giving public lectures and are present in the education of schoolteachers and students. During the almost four years of Anillo the AIUC organized several initiatives: international workshops of instrumentation and astronomical technology and workshops for schoolteachers in collaboration with other institutions.

III. RESUMEN EJECUTIVO

Esta sección no deberá extenderse más de 3 páginas escritas en letra tamaño 12 o equivalente. Resuma los logros del proyecto a la fecha, incluyendo aquellos relacionados con los objetivos de investigación, colaboración internacional o nacional, actividades de formación, difusión de resultados a la comunidad científica así como al público no- especializado. Los contenidos de esta sección son públicos y pueden ser colocados en la página WEB de CONICYT. Este resumen debe informar a los potenciales evaluadores sobre los avances del proyecto. Dado que este resumen debe ser asequible a aquellas personas que no son necesariamente expertas en el área, le solicitamos el uso de un lenguaje relativamente simple o de explicaciones cuando los términos técnicos así lo requieran.

El objetivo del proyecto era adquirir y desarrollar las tecnologías de primera línea en una serie de ámbitos seleccionados de la ciencia y la ingeniería para ser empleado en los telescopios astronómicos de próxima generación. En particular, el objetivo fue que los participantes del proyecto competitivo en los ámbitos específicos seleccionados y convertirlos en socios atractivos para los observatorios internacionales presentes en Chile. Con este fin, hemos definido una serie de áreas y actividades de interés. Los participantes son los Departamentos e Institutos de la Universidad Católica de Chile en conjunto con el Centro de Astro Ingeniería ( AIUC ) además de una amplia red de colaboradores internacionales . El objetivo fue perseguido con la colaboración de los socios líderes internacionales en los campos seleccionados. Más específicamente se definieron tres áreas principales de trabajo en el proyecto de Anillo:

- Tecnológicas , : (i) tecnologías para la banda espectral del infrarrojo cercano ( NIR) , ( ii ) la óptica adaptativa (AO) , ( iii ) sistemas de lectura del detector , ( iv ) de software, manejo de datos , computación y ( v ) la mecánica. - Ciencia . Proporcionar a la comunidad científica chilena con las herramientas para llevar a cabo la investigación científica de primera línea . - Extensión . Promover la transferencia tecnológica y cultural de la sociedad chilena.

Nuestros esfuerzos se iniciaron a AIUC y en su mayoría enfocados a adquirir experiencia . Las actividades específicas desarrolladas durante el proyecto comenzó con el plan establecido en la propuesta original siguiendo las grandes líneas definidas y desarrolladas durante los tres años del proyecto . En algunos casos se han abierto nuevas áreas de trabajo. Debido a diversas circunstancias de los tres años del plan inicial del proyecto se extendió a

La actividad en el AIUC durante este período aumentó considerablemente . Empezamos con un pequeño grupo de investigadores pioneros una zona que fue básicamente ausente en la Universidad Católica . Después de cuatro años tenemos un equipo sólido , con una infraestructura interesante , una red de colaboración sólida en todo el mundo y estamos involucrados en proyectos importantes. Todo esto hace que el AIUC una referencia interesante para las empresas locales y que está atrayendo el interés de los estudiantes y

6 jóvenes científicos .

Como parte de este proyecto hemos equipado tres nuevos laboratorios en el AIUC : - El Laboratorio de la tecnología IR incluido equipo de vacío y criogenia , detectores IR , dio lectura a la electrónica. - El laboratorio óptico que incluye un gran banco óptico y una variedad de componentes opto- mecánico para organizar configuraciones y pruebas ópticas . - El Laboratorio de Óptica Adaptativa (AO ) la tecnología que incluye un sistema de banco de pruebas completo AO , de frente de onda (WF ) sensor , espejo deformable ( DM) y el simulador de la turbulencia atmosférica

Instalamos dos instrumentos totalmente operativas en la UC Observatorio de Santa Martina, los pucheros espectrógrafo ( Fondecyt n . 1095187 ) y la cámara de fotometría rápida MERLIN . Ambos instrumentos se encuentran actualmente en operación y están produciendo resultados científicos interesantes . El proyecto brindó apoyo a la operación regular del Observatorio y apoyó el desarrollo de un Sistema de Control de telescopio totalmente nuevo (TCS ) .

Hemos desarrollado el estudio de dos instrumentos de segunda generación AIUC , los FIDEOS espectrógrafo de alta resolución, una evolución de la primera idea de Fiesole y la Bombolo de imágenes multibanda . La construcción de ambos instrumentos fue financiado por CONICYT a través de FONDEF y Quimal respectivamente. Empezamos a desarrollar una tercera idea para un espectrógrafo de alta resolución NIR probó sus tecnologías en el laboratorio .

La participación de AIUC en proyectos internacionales creció de la participación en la fase de un estudio de SIMPLE para el E -ELT para convertirse en miembros del consorcio LUNAS que se está iniciando la construcción del nuevo instrumento MOS para el VLT de ESO . El AIUC también forma parte de la iniciativa HIRES Europea destinado a proporcionar un servicio de espectroscopia de alta resolución para el E -ELT . El AIUC es un miembro activo de la red HAT- Sur, está contribuyendo al proyecto ACT y es miembro del consorcio del G-Clef para el GMT .

El desarrollo de software (SW ) fue una parte importante de nuestro trabajo en el área de la tecnología . Hemos colaborado en este tema con los socios externos. Como resultado tenemos el SO de la nueva TCS para los telescopios del observatorio de la UC (incluyendo la guía automática ) y un nuevo sistema de lectura de los detectores IR . Desarrollo de SW es actualmente nuestra principal tarea dentro del consorcio LUNAS . Durante este Anillo los clusters Geryon experimentaron un orden de magnitud salto . Durante el primer año , la memoria de la computadora se ha multiplicado por un factor de 2 con la ayuda de este proyecto, y se trasladó a la nueva sala de computación del AIUC . La capacidad del disco también se incrementó por un factor de unos pocos con este proyecto . Después de la adquisición de Geryon2 , el nuevo cluster de computación financiado

principalmente por BASAL PFB- 06 CATA , el Anillo hizo una importante contribución a la mejora necesaria de la climatización de la sala de informática , que no fue inicialmente diseñado para soportar la carga de los dos grupos combinados . Los miembros de este Anillo inspirados estas mejoras. Por el lado de la administración , las computadoras Geryon estaban abiertas para su uso por todos los astrónomos de instituciones chilenas , y para ello un sistema de entradas y una buena organización interna se establecieron , y han demostrado que funciona razonablemente bien. En resumen este Anillo contribuyó a convertir un solo cluster de computación en una habitación improvisada , en una instalación nacional , que se ha cobrado impulso y continúa creciendo .

En términos de mano de obra del AIUC creció considerablemente durante la ejecución del proyecto. El Anillo apoya a los estudiantes que trabajan en su undergraduated , master y doctorado tesis de investigación en el área de la astronomía y la ingeniería. Tres investigadores de postdoctorado fueron contratados durante el transcurso del proyecto para trabajar en el IR cercano Lab y en el diseño de nuevos instrumentos.

Las colaboraciones internacionales del AIUC reforzaron considerablemente durante el proyecto. En particular con el Observatorio de París gracias al programa de ocultaciones de los cuerpos menores del sistema solar ; con la Universidad de Tokio a través del apoyo de la operación de miniTAO ; con la Universidad de Durham y el Observatorio Gemini en el campo de la óptica adaptativa ; con INAF en tecnologías de infrarrojos (IR) . Nuestros miembros del equipo viajaron a conferencias en todo el mundo , hicieron visitas a los institutos en el extranjero y se reciben invitados internacionales con el apoyo de este proyecto Anillo.

Considerables esfuerzos se han realizado en el ámbito de la transferencia tecnológica. Con el fin de contribuir a la realidad productiva del país , hemos construido un proceso de dos pasos , uno de los observatorios internacionales en Chile a la academia, y una segunda, de la academia a la industria local . Hemos participado en una serie de iniciativas destinadas a establecer vínculos con el sector privado y a organizar algunos otros . Aunque la realidad local en esta área es pobre, creemos que hemos hecho nuestra contribución , en particular, con algunas pequeñas empresas .

En cuanto a las actividades científicas , los instrumentos de la UC pucheros , Merlín y la colaboración HAT Sur alcanzaron hitos relevantes . Todos los demás proyectos de investigación cumplen los objetivos de la producción científica , los resultados y las publicaciones . La investigación científica se mostró especialmente activa en los campos de estrellas variables , sistemas binarios, el bulbo galáctico , clusters, los exoplanetas y en simulaciones numéricas cosmológicas. El equipo mantiene una alta productividad científica con 117 trabajos publicados en revistas arbitradas internacionales durante el período del proyecto.

El AIUC soporta una intensa actividad de divulgación de la astronomía y la instrumentación en colaboración con el Instituto de Astrofísica y la Escuela de Ingeniería de la Universidad de California . Una de las principales actividades de divulgación se relaciona con el observatorio histórico UC Manuel Foster. Durante la ejecución de este proyecto logramos abrir el sitio al público por primera vez en casi dos décadas y estamos esforzando la creación de un Museo de Astronomía en este sitio histórico. Los miembros de la AIUC están dando activamente conferencias públicas y están presentes en la educación de los maestros y los estudiantes. Durante los casi cuatro años de Anillo del AIUC organizó varias iniciativas: talleres internacionales de la instrumentación y la tecnología astronómica y talleres para maestros de escuela , en colaboración con otras instituciones.

IV. HIGHLIGHTS

In no more than 3 pages indicate the main outcomes during the entire period. This may be in any of the activities or objectives the project has, either originally planned or unexpected. This should be what you consider the most significant results of the period and those that you want to convey to the reviewers and displayed to the community as well. It may well be that in early phases of the project you may have one single important outcome, that is perfectly fine. There will be no particular considerations from the number of highlights you indicate.

Highlight 1 - Human resources The AIUC started as a small pioneering group of few researchers about 5 years ago working in an area virtually absent at the UC and in Chile and it is now an interesting reality at national and international levels. Attracting manpower to our group was one of the most difficult challenges that we faced. We had a difficult time hiring post doc researchers for the project and attracting engineering and astronomy students to the area of astro engineering. This situation was especially complex during the first 2 years of the Anillo, when finding qualified and motivated people for the area was difficult and the competition with more consolidated areas of engineering was extremely hard. However we feel that during the last year the situation improved considerably, critical mass was reached or nearly reached, and, as a result of our efforts we grew considerably in man-power as new students and postdoc joined the AIUC. An interesting indication of our program´s health is that several of these new researchers started to arrive at the AIUC with support form other grants, not from ANILLO. Naturally, ANILLO´s support remains critical in attracting other sources of funding that require complements such as the UC postdoc grant, or the University of Tokyo support or the Gemini Observatory Fellowship.

Highlight 2 – Science Our team obtained relevant results both in the traditional lines of research mainly based on observations obtained at the international observatories and on observations obtained with our own instruments mainly at the UC Observatory Santa Martina, HAT-South telescopes and Geryon cluster. This second line was highlighted by the referees of the project as especially desirable and we invested considerable efforts into it. As a result: - We had the first scientific publication, which include data from PUCHEROS (Chesneau et al. 2014 A&A 563, 71). - Two scientific papers were published based on observations from the camera MERLIN. In particular we contributed to the discovery of a double ring around the centaurus Chariklo. Our observation was among the most conclusive in the discovery, the result was published by Nature in March 2014 (http://www.nature.com/nature/journal/vaop/ncurrent/full/nature13155.html). The

national and international press covered the news broadly, articles appeared worldwide on the major newspapers. - The HATSouth collaboration reached a major milestone in 2013 by publising its first discovery and a paper describing the survey. To date HATSouth has published or submitted papers presenting the discovery of 5 systems (HATS-1b to HATS-5b), and has of order 10 more systems in the last stages of confirmation that are expected to be submitted during this year. - During this Anillo several projects benefitted from using Geryon, including the VVV survey and several statistics and simulations projects, and there are 60 papers which make mention of the Geryon cluster since 2011. Two licenciatura students used this facility for their Práctica de Licenciatura, Sergio Contreras and Salvador Salazar (2012, 2013). Three PhD students benefited from using Geryon, Iván Lacerna (PhD 2012), Felipe Garrido, and Alejandra Muñoz who has recently started her PhD thesis connecting together numerical simulation and observational data. - One undergraduated students (Johanna Coronado) completed her “Memoria” project in Astronomy based on PUCHEROS observations, one Master student in Astronomy (Paz Bluhm) and one undergraduated student in Astronomy (Jorge Anais) started their research projects using data from PUCHEROS.. - HATSouth has served as main topic for one PhD stutdent (Rafael Brahm), and as secondary topic for another PhD student (Nestor Espinoza). It has produced six refereed papers to date, and served as basic topic for three undergraduate thesis..

Highlight 3 – Instruments Building, commissioning and scientific use of our first generation astronomical instrument – PUCHEROS and MERLIN – were achieved during the execution of this project. As foreseen in the initial proposal, the design of two second generation instruments was developed as part of the project Anillo: the high-resolution spectrograph FIDEOS and the multi band imager BOMBOLO. Both are funded by CONICYT and are currently under construction. Our team is member of the MOONS consortium to provide the ESO VLT with a new MOS facility. We are participating in this effort since the initial ESO call for instrumentation. The project has passed phase A, the detailed study and currently it is in the construction phase. Within the consortium we took responsibility for the fibre metrology system and for the entire instrument control SW. The AIUC is member of the G-CLEF consortium through the participation of co investigators. G-CLEF will be one of the first-light instruments on the 24m Giant Magellan Telescope to be installed in the Las Campanas Observatory.

Highlight 4 – National and International Collaborations During the execution of the Anillo project a number of national and international collaborations were consolidated in the AIUC.. We established a new and interesting contact with the Universidad de Valparaiso (UV) for the scientific use of PUCHEROS and for the exploitation of the UC Foster Observatory historic archive. We established collaborations with the Universidad Catolica del Norte (UCN) for the use of the ESO 1 m telescope of La Silla. We are collaborating with UV and UCN on the project FIDEOS. We have an active collaboration with the Gemini observatory in the area of AO. Specifically, we are working in three different subjects: i) Vibration mitigation of AO loops; ii) Development of turbulence profilers for the Multi-Conjugate Adaptive Optics Systems (GeMS); and iii) Adaptive optics for the beam shaping of lasers in the generation of artificial guide-stars. As members of the MOONS and G-Clef consortia we have active exchange with the members of the consortia en in particular with the UK Astronomy Technology Center (ACT) and Harvard Smithsonian Center for Astrophysics (CfA). We strengthened the contact with Ministry of Foreign Affair and Ministry of Economy and we organized in collaboration with them two international workshops in the area of astronomical technologies. The collaboration with the University of Tokyo flourished considerably during the execution of the Anillo project. In November 2013 the University of Tokyo Forum was held at UC with support of AIUC through the Anillo. Other relevant contacts include the Observatory of Paris and the occultation network led by them. The INAF Observatories of Milan and Florence in the area of IR Technology. University of Durham in adaptive optics and the Institutes involved in the broad instrument collaborations MOONS and G-Clef.

Highlight 5 – Service The AIUC established itself as an institution providing service in the area of astro engineering. In turn we highlight a number of relevant positive experiences:  Operation of the Max Planck 2.2 mt telescope at La Silla Observatory. The AIUC, the UC Institute of Astrophysics and UNAB have recently signed a contract with the MPIA to operate the 2.2mt telescope at La Silla.  Operation and maintenance of the U of Tokyo miniTAO telescope. In 2012 a MoU was signed to establish a collaboration between the University of Tokyo (UT) and Pontificia Universidad Católica de Chile, through the AIUC. The initial goal of this agreement is that PUC hires one astronomer for the program, who provides 30 % of his/her time to support miniTAO operation.

 A number of activities were developed within the Atacama Cosmology Telescope project (ACT)  The AIUC manages the Geryon cluster computer to provide supercomputer power to the Chilean astronomical community. Users are established researchers and students at Chilean institutions. Conicyt programs have funded the initial funding and the posterior hardware upgrades.  The AIUC continued its support of the f/5 instrumentation that is periodically installed in the Clay telescope at the Las Campanas observatory. One of the AIUC staff participates of the mounting/dismounting of the f/5 instrumentation, assists in runs and is ready for emergency interventions if needed.

Highilight 6 – Technological Transfer to the national private sector The private initiatives interested in the astro-engineering activities were virtually absent at the beginning of this project. During the execution period of the project we managed to established important contact with local companies and to support spin-off companies. We supported a course of optical fibre handling by Standards (www.standards.cl). We outsourced the instrument control electronics and the MOONS metrology system prototype to HappyVolt (www.happyvolt.com/). We outsource part of the UC Santa Martina TCS SW and above all the MOONS ICS to BlueShadow Astronomy and Engineering.

Highlight 6 - Projects One of the main challenges for the AIUC in its early phase was to provide financial support and continuity to astro-engineering projects. This turned to be an extremely difficult task and we had to face a number of failures mainly because an astro instrumentation culture was not in place in Chile. Anillo at the AIUC helped to build up this culture. After a difficult beginning where a number of proposals failed (FONDAP; FONDEF; Milenio) we have been able to successfully secure funding. Needless to say, this effort was a major investment of time and human resources for the Center. In the process we learnt to better focus our resources and lately the AIUC succeeded in obtaining fresh resources through several Fondecyt projects, 1 FONDEF, 2 QUIMAL, and projects from the international observatories mainly ESO, ALMA and Gemini. We also moved forward in the optimal administration of our economic resources. By hiring an executive secretary and a fund manager (partially funded by Anillo) we currently count on the manpower needed to handle our economic resources and our relations with the funding sources (Conicyt, the University, MinEcon and the International Observatories).

V. ACTIVITIES

This section should have 5 pages as maximum extension. Indicate the activities performed during the entire period. Separate activities by numbered paragraphs. Each activity should have a headline with its name and 2-3 explanatory lines including if they have been performed and if not indicating why.

Project activities were carried out around two main axes: Technology and Science.

1. Technology

1.1 Instrumentation As part of the Anillo project we equipped our IR Lab with two NICMOS based instruments that were decommissioned by the Observatory of Arcetri at the end of the 90’s. We reestablished the operation of both instruments; we modified the dewars, electronics and software. We substituted the old read out electronics with a new SDSU Detector Controler. We rebuilt the instrument control electronics, repair leaks in the dewars, and substituted one of the cryo-motors with a new Pytron device. We tested both instruments in the lab and measured the detectors´ efficiency. It turns out that their performance is consistent with the historic behavior except for the number of bad pixels that was considerably increased. We linked the NICMOS spectrograph to the Santa Martina 50 cm telescope and had first light on the sky in January 2014. This was a milestone that had been required by the referee in the comments of last year report and was also one of the objectives established in the original Anillo proposal. We were able to obtain spectra of a star and estimate the efficiency of the system, which turned to be extremely low. Attempts to observe faint stars failed because of the low efficiency of the system. This terribly low efficiency could be attributed to a poor coupling of the instrument with the telescope via fiber and/or to misalignment of the optics of the spectrograph. We will investigate further the problem. In Fig. 1 we show one of the spectrum acquired at the telescope.

We tested a second IR instrument on sky, a Xeva 640 1.7 camera that was acquired as part of the project Fondecyt n. 1130849 despite this is not a scientific instrument we could observe stars as faint as H=5.5 with S/N=30 in 10 sec.

We developed the design of two-second generation instruments, FIDEOS and BOMBOLO. Developing instruments for medium class telescopes was one of the objectives in the original Anillo proposal. FIDEOS is an improved version of PUCHEROS reaching spectral resolution R=40.000 and employing a science grade e2v 2K CCD, the instrument was thought for a 1 m class telescope. BOMBOLO is an imager observing simultaneously in three bands and it is being developed for the SOAR 4 m telescope.

In the original Anillo program we proposed as a middle term (5-7 yr) objective the participation in the construction of a new instrument for a large telescope. This goal is

14 fulfilled by the AIUC participation in the MOONS project for the ESO VLT. We developed the feasibility study for the MOONS fibre metrology system and we are currently building the prototype system and developing the the Instrument Control Software. MOONS was approved by ESO and it is currently entering into the construction phase. We consider the participation of the AIUC in this large project as a major success of our efforts in the area of instrumentation. SIMPLE for the E-ELT was one of the key projects in the original Anillo proposal as, at that time, we were involved into the phase A study for the instrument. The ideas of SIMPLE and its visible counterpart CODEX however, despite positive evaluation, are being re-considered by ESO and the community. We are currently part of the discussion in the frame of the HIRES initiative for the E-ELT.

The AIUC is member of the G-CLEF consortium through the participation of co- investigators of Profs. Jordán and Guzmán. G-CLEF will be one of the first-light instruments on the 24m Giant Magellan Telescope to be installed in the Las Campanas Observatory. The GMT board approved a preliminary design contract in February 2013, and we are now conducting the review. G-CLEF is the only approved first-light instrument for the next generation giant telescopes with Chilean participation. Our involvement is on the scientific development and quality assurance of the prototype exposure time calculator, and the design and development of the spectrograph CCD focal plane.

Several activities were developed within the Atacama Cosmology Telescope (ACT) project led by Rolando Dünner. A new data processing facility was installed at Católica, storing the RAW data from the telescope and processing it locally to achieve the data selection and calibration that was then provided for map making elsewhere. The data storage also provides extra redundancy to the system. The data reduction of the ACTpol data is a very active area of work today. On the technical side, full electromagnetic simulations of the ACT optics including the polarizing effects of the gaps between panels were developed. The analysis served to quantify possible systematic effects in the data and search for far sidelobes of the telescope. This work will be continued producing a more complete simulation of the optics including ground screens and refractive optics from the camera. Finally, photogrammetry measurements of the ACT optics were carried out to characterize and optimize the surface of the mirrors of the telescope. The new photogrammetry technique improves the previous measurements done with a laser tracker providing day-time and faster measurements.

1.2 AO The main adaptive optics (AO) activity was the development of new methods for wavefront correction of laser beams in amplitude and phase using two deformable mirrors. The effort focused in developing the phase retrieval algorithms to determine the shape of mirrors and the construction of an optical table to implement such methods. We developed and implemented turbulence-profiling methods. We started a collaboration with the Gemini South Observatory to implement these techniques in the new ExAO system being

15 commissioned. PSF reconstruction in AO systems is a new area where we are beginning to work with the Laboratoire d'Astrophysique de Marseille, and we are also finishing a MSc. thesis in the subject for its application to Gemini South’s NICI exoplanet finder.

Several collaborations with international institutions have been started in different areas of adaptive optics mainly, Gemini Observatory (PSF reconstruction, vibration mitigation for GeMS and GPI, turbulence profiling), European Southern Observatory (vibration mitigation for NACO, MACAO, turbulence profiling for AOF), Univ. Santa Cruz, California (complementation of Fourier and spatial techniques for turbulence characterization), Livermore National Laboratory (complementation of Fourier and spatial techniques for turbulence characterization), Univ. of Victoria, Canada (turbulence profiling for RAVEN, an MOAO system for Subaru), LAM, Laboratoire d'Astrophysique de Marseille (PSF reconstruction, turbulence profiling), ALMA Observatory (PSF reconstruction), INAF - Arcetri Astrophysical Observatory (turbulence profiling), University of Durham (MOAO), and Universidad Técnica Federico Santa María, Chile (laser shaping).

1.3 Computing:

During this Anillo at least five milestones of the Computing Laboratory were achieved:

- We doubled the available RAM memory of the original computing cluster Geryon, at the same time as it was moved into the new computing room at the AIUC.

- A safety temperature automatic off-switch was installed with Anillo funds. This switch ensures that the temperature of the computing room never rises above 50 degrees, adding another important safety layer to the room in addition to the temperature sensors of the UPSs.

- A new air conditioning system, with the correct specifications for a computing room with of the order of ~100 servers working at full capacity, was installed. This Anillo project provided funds corresponding to approximately 40% of the total cost, with the rest of the funds coming from Universidad Católica and from the BASAL center, Centro de Astrofísica y Tecnologías Afines. This air conditioning unit makes full use of the false floor of the computing room by pumping cold air below the servers, and extracting the warm air from the ceiling.

- The new generation computing cluster, Geryon2 was installed during this period and, as of 18 December 2013, is open for use by the Chilean astronomical community. The main storage of the new cluster was acquired in part with Anillo funds, and consists of 50Tb of disk space for projects of different kinds, from simulations of the universe to image processing from the ALMA observatory.

2. Science Maitaining an active scientific production within the team was considered of great importance in the project as this allows having the vision to project our technological activity in the future. Scientific research was developed using the international observing facilities accessible to Chilean astronomers, however special efforts were invested in making our own instruments as productive as possible. This latter point was particularly stressed by the referees in their mid term evaluations, we believe we made significant progress in this direction.

2.1 UC Instruments One of the major goals of the Anillo was to make the UC Observatory Santa Martina scientifically productive and to provide the national community with new instruments for astronomical observations. We believe we fully accomplish this with the installation and operation of PUCHEROS and the MERLIN camera. In addition to that we count with the HAT-South station installed and in operation at Las Campanas. All instruments started to produce scientific results within the execution of the project and we count with results published in the major refereed international journals from the three projects, further details are given in the highlights section and publication list. With FIDEOS and BOMBOLO we are moving a step further in this line.

2.2 International Instruments We developed the traditional lines of scientific research, which constitute the bases for our technological activities. In the following we highlight some of the lines of work of the researchers associated with the project.

2.2.1 Origin and evolution of stars and SM BH During this Anillo, the details of the evolution of the stellar content of galaxies were investigated using taking advantage of the Geryon cluster, consisting of a combination of observational data analysis and simulations of galaxy formation, in a wide variety of techniques.

In Amores et al. (2012) we used the cluster to simulate the effect of the Milky Way on the counts of background galaxies, and compared this to those detected in the VVV survey. In Rodríguez & Padilla (2013), we introduced a new model for the intrinsic shape of the stellar distribution in Sloan Digital Sky Survey (SDSS) galaxies. This new model is non-parametric, and for the first time it includes de effect of dust extinction in an independent way. Dust makes a population of galaxies appear rounder since the path length along an edge-on galaxy is longer and more subject to extinction, which results in more edge-on galaxies to fall below the flux detection limit compared to face-on ones. This study is the observational leg of a project where we will study the final configuration of galaxies after their 13.7Gy long evolution to their present-day states using models of galaxy formation. More specifically, on the modeling side in Padilla et al. (2013, submitted), we started improving the details with which the size of galaxy discs are modeled in a semi-analytic model. We introduced for the

17 first time, the effect of misaligned accretion by the galaxy disc, which makes the angular momentum of the galaxy to grow at a slower rate at any point when a galaxy is accreting large quantities of mass (gas and stars, via smooth accretion but also during mergers). This in turn affects the predicted projected density of the disk gas, which in turn affects the star formation rate of the galaxy. In order to reach the point where the model produces reliable three-dimensional shapes of galaxies to compare to the Rodriguez & Padilla results, we still need to model the vertical scale-length of disks, a work we are currently starting to tackle.

Finally, given that there are several semi-analytic models of galaxy formation, we made a study on what predictions are universal among these models, concentrating on the clustering of galaxies (Contreras et al. 2013).

2.2.2 The IMF of SB galaxies In a recent surge of papers, observational evidence has been presented favoring a very bottom heavy Initial Mass Function (IMF) in massive elliptical galaxies. This was based on the strength of the NaI λ~8190Å doublet and the FeH Wing-Ford band at λ~9900 Å which both are strong in dwarfs and weak in giants. These features appear to be stronger in massive elliptical galaxies than in synthetic stellar population models adopting a Milky Way (bottom light) IMF.

Such claims rest entirely on the tacit assumption that existing stellar population models are extremely accurate in reproducing the strength of weak spectral features in the near-IR. We devised a program aimed at submitting these claims to a crucial test. We gathered multiple IFU exposures with FLAMES/GIRAFFE/ARGUS of the Milky Way bulge Window at (l,b)=(-2.65, 1.25) and of a field at the center of the bulge globular cluster NGC6528. The resulting 1D coadded spectra allows us to measure the strength of the NaI feature at λ~8190Å, which has been used to infer a bottom heavy IMF for ellipticals. The observations for this program have been completed at the end of September 2013, and we just completed the extraction, wavelength calibration, sky subtraction and coaddition for all the spectra. For both the bulge and NGC6528, the IMF is known to be bottom light, from star counts of individual stars (Zoccali et al. 2000), hence it will be possible to unambiguously ascertain whether stellar population models actually predict the strength of the feature with sufficient accuracy to set meaningful constraints on the IMF

2.2.3 Multiple Stellar Populations in Globular Clusters In Marino et al. (2013) we performed high-resolution spectroscopy of individual stars in the globular clusters NGC 2808, distributed in different portions of the Horizontal Branch (HB), covering a wide range of temperature. By studying the chemical abundances of this sample, we explored the connection between HB morphology and the chemical enrichment history of multiple stellar populations. Our results showed that: (i) HB stars in NGC 2808 exibit different Na abundance depending on their position in the colour-magnitude diagram, with blue HB stars having higher Na than red HB stars; (ii) the red HB is not consistent with a uniform chemical abundance, with slightly warmer stars exhibiting a statistically significant

18 higher Na content; and (iii) our subsample of blue HB stars with He abundances shows evidence of enhancement with respect to the predicted primordial He content by ΔY=+0.09. Our results strongly support theoretical models that predict He enhancement among second- generation(s) stars in globular clusters and provide observational constraints on the second- parameter governing HB morphology.

2.2.4 The Milky Way bulge The study of the Galactic bulge is an area of research particularly active within the project and generated a significant number of results published in refereed articles, during the whole projects. We summarize here only the highlights: - The Galactic bulge has been discovered to be X-shaped (McWilliam & Zoccali 2010), which clearly indicates that it must be formed by dynamical instability of the disk, though the formation and successive buckling of a bar; - 3D velocities of the stars in different positions within the X-shape have been measured, and they agree with the prediction of bulge formation models including the instability described above (Vasquez et al. 2013); - A map of photometric metallicity was constructed for the whole bulge, from the VVV survey (Gonzalez et al. 2013). The map shows the large scale metallicity gradients of the bulge, that follow the arms of the X-shape; - The RR Lyrae variables in the Galactic bulge, tracing the old and metal poor component, show a spheroidal distribution. They do not follow the bar nor the X-shape. This component must have had a different origin (Dékány et al. 2013); - No evidence for the presence of young/intermediate age stars has been found, even in the outer bulge (Valenti et al. 2013); - The first paper of the Giraffe Inner Bulge Spectroscopic Survey (GIBS) has been published, including target selection and radial velocities for ~6500 bulge K giants. A map of radial velocity and velocity dispersion has been constructed for the inner bulge, allowing comparison with other work in different fields, and the comparison of the kinematic of the Galactic bulge with that of external galaxies observed with Integral Field Units (Zoccali et al. 2014)

2.2.5 MOONS After the participation in the definition of the science case of the E-ELT SIMPLE project a number of researchers associated with the Anillo became team members for the successful VLT-MOONS instrument collaboration. The capacity of MOONS represents a >10-fold increase compared to today's cutting edge NIR multi-object spectrographs. This ~500-fibre "monster" stands to completely revolutionize our understanding of both our own Galaxy and the billions of other galaxies in the Universe by providing statistically meaningful samples of objects even among relatively rare object types. It will be a "game-changer" for rest-frame optical studies of high-z galaxies and AGN, and should be on-sky by 2017. We participated on the science definition team as one of the co-leaders of the multiwavelength follow-up survey group, organizing telecons and helping to craft the 50-page

19 proposal that ultimately helped MOONS because one of ESO's next generation instruments on the VLT. As the instrument starts to take shape and become a reality, the science definition team will hone the proposed science into a number of guaranteed-time programs that will be planned to make the most of the instrument during the first several years of operation. One of the primary goals of MOONS is to observe >100,000 galaxies whose light comes from when the Universe was less than 20% of its current age. The near-infrared spectroscopy from MOONS will provide direct spectral comparisons with previous-studied nearby galaxies and allow us to study how galaxies and supermassive black holes formed and evolved of over much of cosmic time. For a large fraction of distant galaxies, MOONS will offer us the first chance to study them in any detail whatsoever. We are now planning which fields to cover, to which depths, and what further follow-up is needed.

3. Outreach

The scientists associated to the Anillo project were active in dissemination of results to the public contributing to the outreach activities of the Institute of Astrophysics UC and organizing independent initiatives. Among the latter we highlight in particular:

- The organization of the First Workshop of Astro Engineering on November 27 -30, 2012 in collaboration with the Chilean Ministery of External Affairs - The organization of the Second Workshop of Astro Engineering on November 4 – 5, 2013 in collaboration with Chilean Ministery of Economy - The organization of the University of Tokyo Forum on November 7 – 8, 2013, in collaboration with the University of Tokyo, the Embassy of Japan in Chile, the Universidad de Chile. The Forum included a important section on Astronomy and Astronomical technology.

The project Anillo supported the re-opening to the public for the first time after almost two decades of the UC historic observatory Manuel Foster, which was visited by hundreds of people during the national “Dia del patrimonio”.

Fig. 1 IR Spectrograph setup for first light at the telescope. In front of the dewar it is visible the fibre link to the telescope, on top of it the Leach read-out electronics, on the monitor the control and acquisition SW.

Fig. 2 First light spectrum of the star Betelgeuse in J band. Positive and negative spectra are shown as product of background subtraction.

VI OUTPUTS

Publications ISI:

1. . lonso-Garc a, M. Mateo, B. Sen, M. Banerjee, M. Catelan, D. Minniti, & K. von Braun (2012), Uncloaking globular clusters in the inner Galaxy, AJ, 143, id. 70 .

2. Amores, E. B.; Sodre, L.; Minniti, D.; Alonso, M. V.; Padilla, N.; Gurovich, S.; Arsenijevic, V.; Tollerud, E. J.; Rodriguez-Ardila, A.; Diaz Tello, J.; Lucas, P. W. AJ, in press (eprint arXiv:1206.4318) “Galaxies behind the Galactic plane: First results and perspectives from the VVV Survey”.

3. Aparicio Villegas, T.; Alfaro, E. J.; Cabrera-Caño, J et al. (including Infante L.) 2011 “Stellar physics with the LH MBR photometric system” .Ph.C.S. 328, 2004.

4. Arrigoni Battaia, F., Gavazzi, G., Fumagalli, M., et al. [including A. Jordan] (2012), "Stripped gas as fuel for newly formed H ii regions in the encounter between VCC 1249 and M 49: a unified picture from NGVS and GUViCS", Astronomy and Astrophysics, 543, A112.

5. Barnes, J. R., Jenkins, J. S., Jones, H. R. A., Rojo, P., Arriagada, P., Jordan, A., Minniti, D., Tuomi, M., Jeffers, S. V., & Pinfield, D. (2012), "Red Optical Planet Survey: a new search for habitable earths in the southern sky", Monthly Notices of the Royal Astronomical Society, 424, 591.

6. Beky, B., Bakos, G.A.., Hartman, J., et al. [including A. Jordan] (2011), "HAT-P-27b: A Hot Jupiter Transiting a G Star on a 3 Day Orbit", The Astrophysical Journal, 734, 109.

7. Bielby, R. M.; Shanks, T.; Weilbacher, P. M.; Infante, L. et al. 2011 “The VLT LBG Redshift Survey - I. Clustering and dynamics of ≈1000 galaxies at z≈ 3” MNR S 414, 2

8. Blakeslee, J. P., Cho, H., Peng, E. W., Ferrarese, L., Jordan, A., & Martel, A. R. (2012), "Optical and Infrared Photometry of Globular Clusters in NGC 1399: Evidence for Color-Metallicity Nonlinearity", The Astrophysical Journal, 746, 88

9. Blakeslee, J. P., Cantiello, M., Mei, S., Cote, P., Barber DeGraaff, R., Ferrarese, L., Jordan, A., Peng, E. W., Tonry, J. L., & Worthey, G. (2010), "Surface Brightness Fluctuations in the Hubble Space Telescope ACS/WFC F814W Bandpass and an Update on Galaxy Distances", The Astrophysical Journal, 724, 657.

10. . Borissova, C. Bonatto, R. urtev, . R. . Clar e, F. Pe aloza, S. . Sale, D. Minniti, . lonso-Garc a, . rtigau, R. Barb , E. Bica, G. L. Baume, M. Catelan, . N. Chen , B. Dias, S. L. Folkes, D. Froebrich, D. Geisler, R. de Grijs, M. M. Hanson, M. Hempel, V. D. Ivanov, M. S. N. Kumar, P. Lucas, F. Mauro, C. Moni Bidin, M. Rejkuba, R. K. Saito, M. Tamura, & I. Toledo (2011), New Galactic star clusters discovered in the VVV survey, A&A, 532, id. A131 .

11. Boselli, A., Boissier, S., Heinis, S., et al. [including A. Jordan] (2011), "The GALEX Ultraviolet Virgo Cluster Survey (GUViCS). I. The UV luminosity function of the central 12 sq. deg", Astronomy and Astrophysics, 528, A107.

12. Burke, M. J., Raychaudhury, S., Kraft, R. P., et al. [including A. Jordan] (2012), "A Transient Sub-Eddington Black Hole X-Ray Binary Candidate in the Dust Lanes of Centaurus A", The Astrophysical Journal, 749, 112.

13. Calamida, A., Bono, G., Corsi, C. E., Iannicola, G., Ripepi, V., Anthony-Twarog, B., Twarog, B., Zoccali, M., Buonanno, R., Cassisi, S., Ferraro, I., Grundahl, F., Pietrinferni, A., & Pulone, L. 2011 - : NGC 6522 As a First Test Case - The Astrophysical Journal, 742, L28.

14. Casassus, S., Perez M., S., Jordan, A., Menard, F., Cuadra, J., Schreiber, M. R., Hales, A. S., & Ercolano, B. (2012), "The Dynamically Disrupted Gap in HD 142527", The Astrophysical Journal, 754, L31.

15. .-N. Chen , J. Borissova, J. R. A. Clarke, C. Bonatto, D. J. Majaess, C. Moni Bidin, S. E. Sale, F. Mauro, R. Kurtev, G. Baume, C. Feinstein, V. D. Ivanov, D. Geisler, M. Catelan, D. Minniti, P. Lucas, R. de Grijs, & M. S. N. Kumar (2012), Massive open star clusters using the VVV survey. I. Presentation of the data and description of the approach, A&A, in press (arXiv:1206.6104).

16. Chilingarian, Igor V.; Mieske, Steffen; Hilker, Michael; Infante, Leopoldo 2011 “Dynamical versus stellar masses of ultracompact dwarf galaxies in the Fornax cluster” MNRAS 412, 1627.

17. Clarkson, W. I., Sahu, K. C., Anderson, J., Rich, R. M., Smith, T. E., Brown, T. M., Bond, H. E., Livio, M., Minniti, D., Renzini, A., & Zoccali, M. 2011 - The First

Detection of Blue Straggler Stars in the Milky Way Bulge - The Astrophysical Journal, 735, 37.

18. M. Correnti, M. Bellazzini, E. Dalessandro, A. Mucciarelli, L. Monaco, & M. Catelan (2011), A low surface brightness halo surrounding the globular cluster NGC 5694, MNRAS, 417, 2411-2416 .

19. Crighton, N. H. M.; Bielby, R.; Shanks, T.; Infante, L. et al. 2011 “The VLT LBG Redshift Survey- II. Interactions between galaxies and the IGM at z˜ 3” MNR S 414, 28.

20. M. Dall’Ora, . inemuchi, V. Ripepi, C. T. Rodgers, G. Clementini, L. Di Fabrizio, H. A. Smith, M. Marconi, I. Musella, C. Greco, C. A. Kuehn, M. Catelan, B. J. Pritzl, & T. C. Beers (2012), Stellar Archaeology in the Galactic Halo with the Ultra-Faint Dwarfs. VI. Ursa Major II, ApJ, 752, id. 42 .

21. Das, Sudeep; Marriage, Tobias A.; Ade, Peter A. R. et al. (including Infante L.) 2011 “The tacama Cosmology Telescope: Measurement of the Cosmic Microwave Background Power Spectrum at 148 and 218 GHz from the 2008 Southern Survey” p 729, 62.

22. A. J. Drake, S. G. Djorgovski, A. Mahabal, et al. (including M. Catelan), (2011), The Discovery and Nature of the Optical Transient CSS100217:102913+404220, ApJ, 735, id. 106 .

23. Dunkley, J.; Hlozek, R.; Sievers, . et al. (including Infante L.) 2011 “The Atacama Cosmology Telescope: Cosmological Parameters from the 2008 Power Spectrum” p 739, 52.

24. Ferrarese, L., Cote, P., Cuillandre, J.-C., et al. [including A. Jordan] (2012), "The Next Generation Virgo Cluster Survey (NGVS). I. Introduction to the Survey", The Astrophysical Journal Supplement Series, 200.

25. M. T. Fitzgerald, J. Criss, T. Lukaszewicz, D. J. Frew, M. Catelan, S. Woodward, L. Danaia, & D. H. McKinnon (2012), RR Lyrae Stars in the Globular Cluster NGC 6101, PASA, 29, 72-77 .

26. Frank, M. J.; Hilker, M.; Mieske, S.; Baumgardt, H.; Grebel, E. K.; Infante, L. 2011 “Spatially resolved inematics of an ultracompact dwarf galaxy” MNR S 414, 70.

27. Glass, L., Ferrarese, L., Cote, P., Jordan, A., Peng, E., Blakeslee, J. P., Chen, C.-W., Infante, L., Mei, S., Tonry, J. L., & West, M. J. (2011), "The ACS Fornax Cluster Survey. IV. Deprojection of the Surface Brightness Profiles of Early-type Galaxies in the Virgo and Fornax Clusters: Investigating the "Core/Power-law Dichotomy"", The Astrophysical Journal, 726, 31.

28. Gonzalez, O. A., Rejkuba, M., Zoccali, M., Hill, V., Battaglia, G., Babusiaux, C., Minniti, D., Barbuy, B., Alves-Brito, A., Renzini, A., Gomez, A., & Ortolani, S. 2011 - Alpha element abundances and gradients in the Milky Way bulge from FLAMES- GIRAFFE spectra of 650 K giants - Astronomy and Astrophysics, 530, A54.

29. Gonzalez, O. A., Rejkuba, M., Minniti, D., Zoccali, M., Valenti, E., & Saito, R. K. 2011 - The inner Galactic bar traced by the VVV survey - Astronomy and Astrophysics, 534, L14 .

30. Gonzalez, O. A., Rejkuba, M., Zoccali, M., Valenti, E., Minniti, D., Schultheis, M., Tobar, R., & Chen, B. 2012 - Reddening and metallicity maps of the Milky Way bulge from VVV and 2MASS. II. The complete high resolution extinction map and implications for Galactic bulge studies - Astronomy and Astrophysics, 543, A13.

31. Gonzalez, O. A., Rejkuba, M., Zoccali, M., Valenti, E., & Minniti, D. 2011 - Reddening and metallicity maps of the Milky Way bulge from VVV and 2MASS. I. The method and minor axis maps - Astronomy and Astrophysics, 534, A3.

32. Guaita, Lucia; Acquaviva, Viviana; Padilla, Nelson; Gawiser, Eric; Bond, Nicholas A.; Ciardullo, Robin; Treister, Ezequiel; Kurczynski, Peter; Gronwall, Caryl; Lira, Paulina; Schawins i, evin p , 733, 114 (2011) “Ly-alpha-emitting Galaxies at z = 2.1: Stellar Masses, Dust, and Star Formation Histories from Spectral nergy Distribution Fitting”.

33. Guesalaga A., Benoit N., Rigaut F., Osborn J. and Guzmán C. Comparison of vibration mitigation controllers for adaptive optics systems. http://dx.doi.org/10.1364/AO.51.004520. Applied Optics, July 2012, vol.51, 19, pp.4520-4535, 2012.

34. E. Guggenberger, K. Kolenberg, J. M. Nemec, R. Smolec, J. M. Benko, C.-C. Ngeow, J. G. Cohen, B. Sesar, R. Szab , M. Catelan, P. Moskalik, K. Kinemuchi, S. E. Seader, J. C. Smith, P. Tenenbaum, & H. Kjeldsen (2012), The complex case of V445 Lyr observed with Kepler: Two Blazhko modulations, a non-radial mode, possible triple mode RR Lyrae pulsation, and more, MNRAS, 424, 649-665.

35. Hand, Nick; Addison, Graeme E.; Aubourg, Eric et al. (including Infante L.) 2012 “ vidence of Galaxy Cluster Motions with the inematic Sunyaev-Zel'dovich ffect” Ph.Rv.L. 109, 1101.

36. Hajian, Amir; Acquaviva, Viviana; Ade, Peter A. R. et al. (including Infante L.) 2011 “The tacama Cosmology Telescope: Calibration with the Wil inson Microwave Anisotropy Probe Using Cross-correlations” p 740, 86.

37. Hill, V., Lecureur, A., Gómez, A., Zoccali, M., Schultheis, M., Babusiaux, C., Royer, F., Barbuy, B., Arenou, F., Minniti, D., & Ortolani, S. 2011 - The metallicity distribution of bulge clump giants in Baade's window - Astronomy and Astrophysics, 534, A80.

38. Kordopatis, G., Recio-Blanco, A., de Laverny, P., Gilmore, G., Hill, V., Wyse, R. F. G., Helmi, A., Bijaoui, A., Zoccali, M., Bienaym , O. 2011 - A spectroscopic survey of thick disc stars outside the solar neighbourhood - Astronomy and Astrophysics, 535, A107.

39. C. A. Kuehn, H. A. Smith, M. Catelan, B. J. Pritzl, N. De Lee, J. Borissova (2011), Variable Stars in Large Magellanic Cloud Globular Clusters I: NGC 1466, AJ, 142, id. 107 .

40. Lacerna, Ivan; Padilla, Nelson; Stasyszyn, Federico eprint arXiv:1110.6174 (Submitted “The nature of assembly bias - III. Observational properties”

41. Lacerna, Ivan; Padilla, Nelson MNRAS, accepted (eprint arXiv:1207.4476) “The nature of assembly bias - II. Halo spin”

42. Lagos, Claudia Del P.; Padilla, Nelson D.; Strauss, Michael A.; Cora, Sofia A.; Hao, Lei MNR S, 414, 2148 (2011) “Host galaxy-active galactic nucleus alignments in the Sloan Digital S y Survey Data Release”.

43. Lardo, C., Milone, A. P., Marino, A. F., Mucciarelli, A., Pancino, E., Zoccali, M., Rejkuba, M., Carrera, R., & Gonzalez, O. 2012 - C and N abundances of main sequence and subgiant branch stars in NGC 1851 - Astronomy and Astrophysics, 541, A141.

44. Liu, C., Peng, E. W., Jordan, A., Ferrarese, L., Blakeslee, J. P., Cote,P., & Mei, S. (2011), "The ACS Fornax Cluster Survey. X. Color Gradients of Globular Cluster Systems in Early-type Galaxies", The Astrophysical Journal, 728, 116.

45. Marriage, Tobias A.; Acquaviva, Viviana; Ade, Peter A. R. et al. (including Infante L.) 2011 “The tacama Cosmology Telescope: Sunyaev-Zel'dovich-Selected Galaxy Clusters at 148 GHz in the 2008 Survey” p 737, 61.

46. Marino, A. F., Milone, A. P.; Sneden, C. et al. (including Zoccali M.) 2012 - The double sub-giant branch of NGC 6656 (M 22): a chemical characterization - Astronomy and Astrophysics, 541, A15.

47. Marino, A. F., Sneden, C., Kraft, R. P., Wallerstein, G., Norris, J. E., da Costa, G., Milone, A. P., Ivans, I. I., Gonzalez, G., Fulbright, J. P., Hilker, M., Piotto, G., Zoccali, M., & Stetson, P. B. 2011 - The two metallicity groups of the globular cluster M 22: a chemical perspective - Astronomy and Astrophysics, 532, A8

48. Marino, A. F., Milone, A. P., Piotto, G., Villanova, S., Gratton, R., D'Antona, F., Anderson, J., Bedin, L. R., Bellini, A., Cassisi, S., Geisler, D., Renzini, A., & Zoccali, M. 2011 - Sodium-Oxygen Anticorrelation and Neutron-capture Elements in Omega Centauri Stellar Populations - The Astrophysical Journal, 731, 64.

49. Marriage, Tobias A.; Baptiste Juin, Jean; Lin, Yen-Ting et al. (including Infante L.) 2011 “The tacama Cosmology Telescope: xtragalactic Sources at 148 GHz in the 2008 Survey” p 731, 100.

50. Matute, I.; Márquez, I.; Masegosa, J. et al. (including Infante L.) 2012 “Quasi-stellar objects in the ALHAMBRA survey. I. Photometric redshift accuracy based on 23 optical-NIR filter photometry” 542, 20.

51. Menanteau, Felipe; Hughes, John P.; Sifón, Cristóbal et al. (including Infante L.) 2012 “The tacama Cosmology Telescope: CT-CL J0102-4915 "El Gordo," a Massive Merging Cluster at Redshift 0.87” p 748, 7.

52. Meng, Huan Y. A.; Rieke, George H.; Su, Kate Y. L.; Ivanov, Valentin D.; Vanzi, Leonardo; Rujopakarn, Wiphu ApJ 751, 17 “Variability of the Infrared Excess of xtreme Debris Dis s”.

53. Minniti, D., Hempel, M., Toledo, I., et al. [including A. Jordan] (2011), "Discovery of VVV CL001. A low-mass globular cluster next to UKS 1 in the direction of the Galactic bulge", Astronomy and Astrophysics, 527, A81.

54. Monaco, L., Villanova, S., Moni Bidin, C., Carraro, G., Geisler, D., Bonifacio, P., Gonzalez, O. A., Zoccali, M., & Jilkova, L. 2011 - Lithium-rich giants in the Galactic thick disk - Astronomy and Astrophysics, 529, A90.

55. C. Moni Bidin, F. Mauro, D. Geisler, D. Minniti, M. Catelan, M. Hempel, E. Valenti, . . R. Valcarce, . lonso-Garc a, . Borissova, G. Carraro, P. Lucas, .-N. Chen , M. Zoccali, & R. G. Kurtev (2011), Three Galactic globular cluster candidates, A&A, 533, A33 .

56. I. Musella, V. Ripepi, M. Marconi, G. Clementini, M. Dall’Ora, M. I. Moretti, L. Di Fabrizio, C. Greco, G. Coppola, D. Bersier, M. Catelan, A. Grado, L. Limatola, H. A. Smith, & K. Kinemuchi (2012), Stellar Archaeology in the Galactic Halo with the Ultra-Faint Dwarfs: VI. Hercules, ApJ, in press (arXiv:1206.4031).

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58. G. Prieto, M. Catelan, R. Contreras Ramos, B. . Pritzl, H. . Smith, . lonso- Garc a (2012), Variable stars in the globular cluster M28 (NGC 6626), A&A, 543, id. A148 .

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60. M. Rozyzcka, J. Kaluzny, P. Pietrukowicz, W. Pych, M. Catelan, & C. Contreras (2012), VIMOS spectroscopy of photometric variables and straggler candidates in omega Centauri, A&A, 537, id. A89.

61. J. L. Prieto, J. C. Lee, A. J. Drake, R. McNaught, G. Garradd, J. F. Beacom, E. Beshore, M. Catelan, S. G. Djorgovski, G. Pojmanski, K. Z. Stanek, D. M. Szczygiel (2012), SN 2008jb: A "Lost" Core-Collapse Supernova in a Star-Forming Dwarf Galaxy at ~ 10 Mpc, ApJ, 745, id. 70.

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64. Saito, R. K., Zoccali, M., McWilliam, A., Minniti, D., Gonzalez, O. A., & Hill, V. 2011 - Mapping the X-shaped Milky Way Bulge - The Astronomical Journal, 142, 76 .

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76. West, M. J., Jordan, A., Blakeslee, J. P., Cote, P., Gregg, M. D., Takamiya, M., & Marzke, R. O. (2011), "The globular cluster systems of Abell 1185", Astronomy and Astrophysics, 528, A115.

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82. Cortés, A., Neichel, B., Guesalaga, A., Osborn, J., Rigaut, F. and Guzman, D. (2012), Atmospheric turbulence profiling using multiple laser star wavefront sensors. Monthly Notices of the Royal Astronomical Society, 427: 2089–2099.

83. Niemack, M.~D., and 41 colleagues 2010.ACTPol: a polarization-sensitive receiver for the Atacama Cosmology Telescope. Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series 7741,

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85. Marino, A. F., et al. 2013 - Helium enhanced stars and multiple populations along the horizontal branch of NGC 2808: direct spectroscopic measurements, MNRAS, in press

86. Amigo, P., Stetson, P. B., Catelan, M., Zoccali, M., & Smith, H. A. 2013 - Time-series BVI Photometry for the Globular Cluster NGC6981, ApJ, 146, 130

87. Valenti, E., Zoccali, M., Renzini, A., Brown, T. M., Gonzalez, O. A., Minniti, D., Debattista, V. P., & Mayer, L. 2013 - Stellar ages through the corners of the boxy bulge, A&A, 559, A98

88. Barbuy, B., Hill, V., Zoccali, M., Minniti, D., Renzini, A., Ortolani, S., Gomez, A., Trevisan, M., & Dutra, N. 2013 - Manganese abundances in Galactic bulge red giants, A Dekany, I., Minniti, D., Catelan, M., Zoccali, M., Saito, R. K., Hempel, M., & Gonzalez, O. A. 2013 - VVV Survey Near-infrared Photometry of Known Bulge RR Lyrae Stars: The Distance to the Galactic Center and Absence of a Barred Distribution of the Metal-poor Population, ApJ, 776, L19

89. Vasquez, S., Zoccali, M., Hill, V., Renzini, A., Gonzalez, O. A., Gardner, E., Debattista, V. P., Robin, A. C., Rejkuba, M., Baffico, M., Monelli, M., Motta, V., & Minniti, D. 2013 - 3D kinematics through the X-shaped Milky Way bulge, A&A, 555, A91

90. Jerjen, H., Da Costa, G. S., Willman, B., Tisserand, P., Arimoto, N., Okamoto, S., Mateo, M., Saviane, I., Walsh, S., Geha, M., Jordán, A., Olszewski, E., Walker, M., Zoccali, M., & Kroupa, P. 2013 - Main-Sequence Star Populations in the Virgo Overdensity Region, ApJ, 769, 14

91. Gonzalez, O. A., Rejkuba, M., Zoccali, M., Valent, E., Minniti, D., & Tobar, R. 2013 - Reddening and metallicity maps of the Milky Way bulge from VVV and 2MASS. III. The first global photometric metallicity map of the Galactic bulge, A&A, 552, A110

92. Padilla, Nelson; Salazar, Salvador; Contreras, Sergio; Cora, Sofia; Ruiz, Andres, 2013, enviado a MNRAS, arXiv1311.3976

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95. Bayliss, D., Zhou, G., Penev, K., Bakos, G.A., Hartman, J.D., Jordan, A., Mancini, L., Mohler-Fischer, M., Suc, V., Rabus, M., Beky, B., Csubry, Z., Buchhave, L., Henning, T., Nikolov, N., Csak, B., Brahm, R., Espinoza, N., Noyes, R.~W., Schmidt, B., Conroy, P., Wright, D.J., Tinney, C.G., Addison, B.C., Sackett, P.D., Sasselov, D.D., Lazar, J., Papp, I., & Sari, P. 2013, "HATS-3b: An Inflated Hot Jupiter

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97. Chen, Y.-T., Kavelaars, J.J., Gwyn, S., Ferrarese, L., Cote, P., Jordan, A., Suc, V., Cuillandre, J.-C., & Ip, W.-H. 2013, "Discovery of a New Member of the Inner Oort Cloud from the Next Generation Virgo Cluster Survey'', The Astrophysical Journal, 775, L8.

98. . Bakos, G.A., Csubry, Z., Penev, K., Bayliss, D., Jordan, A., Afonso, C., Hartman, J.D., Henning, T., Kovacs, G., Noyes, R.W., Beky, B., Suc, V., Csak, B., Rabus, M., Lazar, J., Papp, I., Sari, P., Conroy, P., Zhou, G., Sackett, P.D., Schmidt, B., Mancini, L., Sasselov, D.D., & Ueltzhoeffer, K. 2013, HATSouth: A Global Network of Fully Automated Identical Wide-Field Telescopes'', Publications of the Astronomical Society of the Pacific}, 125, 154.

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101. Povic, M., Huertas-Company, M., Aguerri, J.A.L,.L Infante, et al. 2013, MNRAS, 435, 3444 .

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Publications no ISI:

1. Angeloni, R.; Helminiak, K.; Vanzi, L.; Di Mille, F.; Fugazza, D. 2011 IAUC 9205, 4 2. Braga-Ribas, F.; Sicardy, B.; Ortiz, J. L.; Jehin, E.; Camargo, J. I. B.; Assafin, M.; Behrend, R.; Unda-Sanzana, E.; Colque, J. P.; Morales, N. et al. including L. Vanzi and Leiva R.) 2011 epsc.conf 1060 “Stellar Occultations by TNOs: the anuary 08, 2011 by (208996) 2003 Z84 and the May 04, 2011 by (50000) Quaoar” 2011 Msngr 145, 11 “MOONS: The Multi-Object Optical and Near-infrared Spectrograph” 3. Cirasuolo, M.; Afonso, J.; Bender, R.; Bonifacio, P.; Evans, C.; Kaper, L.; Oliva, E.; Vanzi, L. 4. Ignacio Rodriguez, Benoit Neichel, Markus Hartung, Thomas Haywards, Julian Christou, Francois Rigaut, Dani Guzman, Andres Guesalaga, Vibration characterization and mitigation at the Gemini-South telescope, presented at the AO4ELT2 Conference, Victoria, September 2011. 5. I. Rodriguez, B. Neichel, A. Guesalaga, F. Rigaut, D. Guzman, Kalman and H-infinity controllers for GeMS, Conference of the Optical Society of America on Adaptive Optics, Toronto, Canada, 10-14 July 2011. 6. Minniti, D.; Clariá, J. J.; Saito, R. K.; Hempel, M.; Lucas, P. W.; Rejkuba, M.; Toledo, I.; Gonzalez, O. A.; Alonso-García, J.; Irwin, M. J. et al. (including Vanzi… TC) B 54, 265 “The VVV Survey of the Mil y Way: first year results” 7. Angela Cortes, Benoit Neichel, Francois Rigaut, Dani Guzman, Andres Guesalaga, First results on a Cn2 profiler for GeMS, presented at the AO4ELT2 Conference, Victoria, September 2011. 8. A. Guesalaga, B. Neichel, M. Boccas, C. D'Orgeville, F. Rigaut, D. Guzman, J. Anguita, Improving stability, robustness, and performance of laser systems, Proc. of the SPIE Conference on Astronomical Telescopes and Instruments, Amsterdam, Julio 2012. 9. A. Guesalaga, B. Neichel, F. Rigaut, J. Osborn, D. Guzman, Design of frequency-based controllers for vibration mitigation at the Gemini-South telescope, Proc. of the SPIE Conferrence on Astronomical Telescopes and Instruments, Amsterdam, Julio 2012. 10. E. A. Bendek, M. Hart, A. R. Guesalaga, A. Cortes, B. Neichel, K. B. Powell, K. Newman, GLAO performance characterization, Proc. of the SPIE Conference on Astronomical Telescopes and Instruments, Amsterdam, Julio 2012. 11. C. Kulcsar, G. Sivo, H.-F. G. Raynaud, B. Neichel, F. Rigaut, J. C. Christou, A. R. Guesalaga, C. Correia, J.-P. Véran, E. Gendron, F. Vidal, G. C. Rousset, T. J. Morris, S. Esposito, F. Quiros-Pacheco, G. Agapito, E. Fedrigo, L. Pettazzi, R. M. Clare, R. Muradore, S. C. Meimon, J.-M. Conan, O. Guyon, F. Martinache, Vibrations in AO control: a short analysis of on-sky data around the world, Proc. of the SPIE Conference on Astronomical Telescopes and Instruments, Amsterdam, Julio 2012. 12. Dani Guzman, Alexandre T. Mello, James Osborn, Francisco J. De Cos, Marlon Gómez, Timothy Butterley, Nicole David, Nieves Roqueñi, Richard M. Myers, Andrés R.

Guesalaga, Matias Salas, Tomographic reconstructor for multi-object adaptive optics using artificial neural, Proc. of the SPIE Conference on Astronomical Telescopes and Instruments, Amsterdam, Julio 2012. 13. Gatica, C.; Vanzi, L.; Toledo, I.; Lombardi, G. 2011 Rev. Mx. C 41, 68 “Site Monitoring at the U.C. Observatory of Santa Martina”

Tesis:

1. Angela Cortes, PhD. Programme, Atmospheric characterization from adaptive optics' loop data, Student, final exam expected in July 2014

2. Ivan Lacerna. PhD. Programme,The nature of assembly bias in Lcdm cosmologies,finished January 2012.

3. Ignacio Rodriguez, PhD. Programme, Vibrations characterization and mitigation in adaptive optics loops, , MSc. Student, final exam expected in June 2014

4. Matías Salas, MSc. programme: Construction and programming of an optical bench for multi-object adaptive optics, finished August 2012.

5. Rodrigo Olguín, MSc. programme: Point spread function reconstruction for multi- conjugate adaptive optics, final examan expected im January 2014.

6. Nicole David, MSc. Student: "Design and implementation of a multi-object adaptive optics laboratory bench".

7. Norman Sáez, MSc. Student: "Design and implementation of a real-time software platform of detectors for adaptive optics".

8. Johanna Coronado undergraduated: “Modelling detached eclipsing binaries using radial velocities from the PUCH ROS”.

9. - avier Valenzuela, Comparison of two turbulence profilers for the SO’s daptive Optics Facility, PhD. Student, first semester in PhD. Program.

10. -Sebastián Zúñiga, MSc. Student, final exam expected in December 2014

11. Clementine Bechet, April 2013 – May 2014; grant from the school of engineering; project: control algorithms for the correction of wavefront phase and amplitude using multiple deformable mirrors,Postdocs,

12. Silvio Rodríguez: research assistant, Geryon web-page developer,students.

13. Ignacio Gargiulo: postgraduate student from U. de La Plata, Argentina, in an interchange program,students.

14. Marcelo Tala: undergraduated student starting his thesis on optical echelle spectrographs,students

15. Rafael Brahm, doctorado, trabajando en la tesis (sin titulo aun).

16. Nestor Espinoza, doctorado, trabajando en la tesis (sin titulo aun).

17. Paula Aguirre, doctorado.

18. Joaquín Prieto, doctorado.

19. Jorge Gonzalez, doctorado.

20. Alvaro Rojas Arriagada defended his MSc thesis under the supervision of MZ. Thesis title: “Metallicity Distribution across the Galactic bulge semi-major axis”

21. Alejandra Muñoz, tesista de doctorado.

22. Sergio Contreras, estudiante de doctorado.

23. Felipe Garrido, estudiante de doctorado.

24. -Geryon postdocs Álvaro Orsi (Fondecyt Postdoctoral) and Tomás Tecce (Gemini funds postdoc).

25. Paz Bluhm Ceballos, Magister , defensa Julio 2014,” Follow-up of giant starts binary systems with PUCHEROS”

Visits:

1. N. Padilla visited Durham University in July 2011 and July 2012, Rutgers U. in October 2011, MPE in Garching, Germany in February 2012, U. La Plata in May 2012.

2. T. Tecce visited Durham University in November-February 2012, and IAFE, Argentina, in April 2012, and July 2012.

3. T. Tecce: New Frontiers in Relativistic and Numerical Astrophysics Workshop 4. IAFE, Buenos Aires, Argentina, June 15, 2012.

5. N. Padilla, T. Tecce, A. Orsi: Second Workshop on Numerical and Observational Astrophysics: From the First Structures to the Universe Today IAFE, Buenos Aires, Argentina, November 14-18, 2011.

6. N. Padilla, T. Tecce, A. Orsi: Galaxy Formation in a Hierarchical Universe Workshop DAA - PUC, Santiago, Chile, March 3-4, 2011.

A. Guesalaga visited Durham in June 2012.

7. D. Guzman visited Durham in July 2012.

8. Jordan visited Observatoire de Geneve, Suiza, (Sept 2011 y Julio 2012); Carnegie Observatories, Pasadena, CA (Oct-Nov 2012); UCLA, Los Angeles, CA (Oct-Nov 2012); HATS meeting, Australian National University, Canberra (junio 2012

9. L. Vanzi visited the Observatory of Edimburgh in October 2011; the Observatory of Geneva in July 2011.

Charlas:

1. Jordan A. coloquio departamento de Fisica de la Facultad de Ciencias Fisica y Matematicas de la Universidad de Chile (Junio 2011);

2. Jordan A. coloquio departamento de Astronomia de la Universidad de Concepcion (Mayo 2012);

3. Jordan A. Keynote speaker en conferencia "Dynamics of Hot Stellar Systems", ESO, Santiago, Abril 2011

4. Zoccali M., May 2012 - “The Galactic Bulge” Informal Discussion at the European Southern Observatory in Garching, Germany

5. Zoccali, M. Mar 2012 – “The Complex Structure and Stellar Population of the Galactic Bulge”

6. Zoccali M., Colloquium at INAF – Osservatorio Astronomico di Collurania Teramo, Italy

7. Zocali M., Feb 2012 – “The Complex Structure and Stellar Population of the Galactic Bulge” Colloquium at the stronomy Department, University of Trieste, Italy

8. Zoccali M, Jan 2012 – “The Complex Structure and Stellar Population of the Galactic Bulge” International Conference on “Chemical voIution of the Mil y Way”, Sesto Pusteria, Italy

9. Zoccali M., Dec 2011 – “The Complex Structure and Stellar Population of the Galactic Bulge” Colloquium at IN F – Osservatorio Astronomico di Padova, Italy

10. Zoccali M. Dec 2011 – “The Complex Structure and Stellar Population of the Galactic Bulge” Colloquium at IN F – Osservatorio Astronomico di Bologna, Italy

11. Zoccali M., Sep 2011 – “The Stellar Population of the Galactic Bulge” Lectures at the PhD School about “Galaxy Bulges” and “From Stars to Planets” in rice, Italy

12. Zoccali M., Aug 2011 – “Mapping the Galactic Bulge” invited review tal at the International Conference “The LTs in the ra of Surveys” in Ischia, Italy

13. Zoccali, Nov 2013 – The VVV Survey talk at the Latin American Regional IAU Meeting (LARIM) in Florianópolis, Brasil

14. Zoccali, Aug 2013 – Exploring the Core of our Galaxy Colloquium at the Institute of Astrophysics PUC, Santiago, Chile

15. Zoccali , Aug 2013 – Explorando el corazón de nuestra Galaxia , Public Conference at the UC, within the programme “F sica para las tardes de invierno”, Santiago, Chile

16. Zoccali, Aug 2013 –Abundandes and Kinematics of the Galactic Bulge , talk at the Workshop of the International Network of Catholic Astronomical Institutions, Santiago, Chile

17. Zoccali, May 2013 – Abundances, Kinematics and the 3D structure of the Galactic Bulge Tal at the Conference about “The role of bars in galaxy evolution”, Granada, Spain

18. Zoccali,May 2013 – Chemical Abundances in the Galactic bulge invited review talk – Conference for the 50yr of the Cerro Tololo Observatory, La Serena, Chile

19. Zoccali,Mar 2013 – The Structure and Stellar Population of the Galactic Bulge Physics Department, Universidad de Chile, Santiago, Chile

20. Padilla,MORPH2013 Workshop, ESO, Santiago, Chile, November 2013, contributed talk.

21. Padilla,Workshop on Galaxy Bias, ICTP Trieste, Italy, October 2013, invited speaker.

22. Padilla,Lyman alpha as an astrophysical tool, Stockholm, Sweeden, September 2013, contributed talk.

23. Padilla,Ripples in the Cosmos”, Durham, ngland, uly 2013, contributed

24. Jordan,IAU symposium 299: EXPLORING THE FORMATION AND EVOLUTION OF PLANETARY SYSTEMS, Victoria, Canada, Jun 2-7 2013.

VI. LESSONS LEARNED

The following section can be used in case of available information related to the possible difficulties, inconveniences or similar issues in the management of the project within the host institution, between CONICYT and the host institution, institution and researchers or any other combination of participants and activities involved. The idea is to resolve these issues on behalf of better practices in the current and future handling of these initiatives.

Information provided in this section must be concise, stating all variables involved and outcomes. Do not extend further than 2 pages.

A number of aspects had certainly been underestimated in our initial assessment and planning of the Anillo project. Among them we highlight the following:

- The lack of national background, culture, and industry in the area of astro engineering affected our ability to recruit qualified manpower at all levels from students to qualified researchers, as well as our ability to find local solutions to our technological challenges. - The time schedule for the procurement and shipment to Chile of the equipment exceeded our most pessimistic estimates and generated considerable delays in the execution of the project. - The complexity of the administration of the resources of the project was significantly greater than expected. This was particularly evident during the first year of the project. The AIUC did not count initially with the professionals needed to handle this aspect of the project. The problem was solved starting from the second year thanks to the experience acquired and by hiring highly professional administrative personnel.

VII. INDICATORS

The following section is has no further purpose but to organize some of the previous information. Indicators have only statistical reasons to be asked for. If you require or would like to define indicators particular to your activities, results or impact please let us know including them at the end of this table. This program is aware that quantitative indicators do not cover most of the actual impact of your activities and thus they are not evaluated

ASTRO Discipline INGENIERIA Total project budget MM$450 Percentage of the project costs contributed by non-governmental 38% General sources N° of main researchers 5 N° of associated researchers 6 Gender (%) of the previous categories 9% F Y 91 M Nº of ISI publications 117 Nº of non- ISI publications 13 Percentage of co-authored publications with researchers not 100% participating in the project Percentage of co-authored publications between Researchers of 75% Scientific production this project Average impact index of journals with ISI 2 Publications resulting from this project 44 Average number of citations per article 5 N° of presentations in international congresses 24 N° of presentations in national congresses 10 N° of patents applied 0 N° of patents registered 0

N° of licenses and/or material transfer agreements 0

Commercial results or N° of Spin-offs 0 others Percentage of the annual funding of the project received from 0 private companies N° of spin-offs N° of applications from results directed to other sectors Than 0 academic (private, public, schools) Nº of undergraduate students 5 Nº of Master’s students 7 Training of young Nº of Ph.D. students 12 researchers and students Nº of postdocs participating in the project 6 N° of undergraduate theses finished 5 N° of graduated theses finished (Master) 1

N° of graduated theses finished (Ph.D.) 4 Percentage of theses co-tutored by researchers participant in 100% this project. Percentage of theses co-tutored with researchers external to this

project N° of stays/visits to other centers/institutions by students or 9 researchers of this project N° of stays/visits from students or researchers of other centers 2 or institutions N° of other projects related or within this/activities with national

collaboration N° of other projects related or within this/activities with 3 international collaboration N° of public or private entities (not enterprises) 9 Involved in this project 0 Nº of dissemination/extramural events 5 Dissemination and Nº of times the project appears in mass media 0 extramural activities Total Nº of attendants to extramural events 582 Nº of national academics attending 537 Nº of international academics attending 45 Nº of attending representatives from other sectors than 0 academic N° of documents, reports, proceedings resulting from 0 dissemination/extramural events or activities