migración a milab

docs/about/about.md

@@ -2,16 +2,16 @@
 
 The LAGO (Latin American Giant Observatory) project is an extended Astroparticle Observatory at global scale. It is mainly oriented to basic research on three branches of Astroparticle physics: the Extreme Universe, Space Weather phenomena, and Atmospheric Radiation at ground level.
 
-The LAGO detection network consists in single or small arrays of particle detectors at ground level, spanning over different sites located at significantly different latitudes (currently from Mexico up to the Antarctic region) and different altitudes (from sea level up to more than 5000 meters over sea level), covering a huge range of geomagnetic rigidity cut-offs and atmospheric absorption/reaction levels.
+The LAGO detection network consists in single or small arrays of particle [detectors](../activities/detectors.md) at ground level, spanning over different [sites](sites.md) located at significantly different latitudes (currently from Mexico up to the Antarctic region) and different altitudes (from sea level up to more than 5000 meters over sea level), covering a huge range of geomagnetic rigidity cut-offs and atmospheric absorption/reaction levels.
 
-The LAGO Project is operated by the LAGO Collaboration, a non-centralized and distributed collaborative network of more than 80 scientist from more than 25 institutions of 9 latinamerican countries (currently Argentina, Bolivia, Brazil, Colombia, Ecuador, Mexico, Peru and Venezuela. See the complete list of the collaboration members and their institutions).
+The LAGO Project is operated by the LAGO Collaboration, a non-centralized and distributed collaborative network of more than 80 scientist from more than 25 institutions of 9 latinamerican countries (currently Argentina, Bolivia, Brazil, Colombia, Ecuador, Mexico, Peru and Venezuela. [See the complete list of the collaboration members and their institutions](collaboration.md)).
 
-Finally, detectors installed in various universities are used as a tool to teach students about particle and astroparticle physics, in particular by leading them to the measurement of the muon decay.
+Finally, [detectors](../activities/detectors.md) installed in various universities are used as a tool to [teach students](../activities/teaching.md) about particle and astroparticle physics, in particular by leading them to the measurement of the muon decay.
 
 !!! info
 
-    Technical information is available in the Lago wiki, our working tool (not foreseen for General Public, as it is currently under development and for now is very technical).
+    Technical information is available in the [Lago wiki](http://wiki.lagoproject.net), our working tool (not foreseen for General Public, as it is currently under development and for now is very technical).
 
-    A list of publications from the LAGO collaboration and its members is available, as well as some LAGO talks, where a lot of information can be found.
+    A list of [publications](../publications/articles.md) from the LAGO collaboration and its members is available, as well as some [LAGO talks](../publications/talks.md), where a lot of information can be found.
 
-    Finally, an historical news page lists LAGO milestones as they have been reached.
+    Finally, an historical [news page](../news/news.md) lists LAGO milestones as they have been reached.

docs/about/collaboration.md

@@ -6,9 +6,9 @@
 
 ## Organization 
 
-**Principal Investigator: Iván Sidelnik**
+**Principal Investigator: Luis Núñez**
 
-Collaboration Secretary: Diego Cogollo
+Collaboration Secretary: C. Sarmiento-Cano
 
 **Country representatives**
 
@@ -16,7 +16,7 @@ Collaboration Secretary: Diego Cogollo
 - Bolivia: M. Raljevic
 - Brasil: A. Campos-Fauth
 - Chile: A. Vega
-- Colombia: L.A. Núñez
+- Colombia: C. Sarmiento-Cano
 - Ecuador: M. Audelo
 - Guatemala: H.E. Pérez-Figueroa
 - Mexico: H. Salazar
@@ -25,150 +25,148 @@ Collaboration Secretary: Diego Cogollo
 
 **Tasks Coordinators**
 
-- Anderson Campos Fauth: Physics
-- Mauricio Suárez Durán : Simulation and Analyses Task Coordinator
-- Dennis Cazar Ramirez: Detectors
-- Horacio Arnaldi: Electronics
-- R. Mayo-García: Data
+- *Physics*: Anderson Campos Fauth
+- *Simulation and Analyses Task Coordinator*: Mauricio Suárez Durán
+- *Detectors*: Dennis Cazar Ramirez
+- *Electronics*: Horacio Arnaldi 
+- *Data*: R. Mayo-García
 
 ---
 
 ## Collaboration members
 
-- Alberto Morillas, Angelines 3 [A. Alberto]
-- Alvarez Ochoa, Cesar 13 [C. Alvarez-Ochoa]
-- Arceo, R. 13 [R. Arceo]
-- Areso, Omar 10 [O. Areso]
-- Arnaldi, Luis Horacio 2 [L. H. Arnaldi]
-- Asorey, Hernán 2 [H. Asorey]
-- Audelo, M 7 [M. Audelo]
-- Ballina Escobar, Maynor Giovanni 16 [M.G. Ballina-Escobar]
-- Becerra Villamizar, Daniel Camilo 15 [D. C. Becerra-Villamizar]
-- Bertou, Xavier 2 [X. Bertou]
-- Caballero Mora, Karen Salome 13 [K.S. Caballero-Mora]
-- Caiza, R 6 [R. Caiza]
-- Calderón-Ardila, Rolando 11 [R. Calderón-Ardila]
-- Campelo, Josafary 26 [Josafary Campelo]
-- Campos Fauth, Anderson 25 [A. C. Fauth]
-- Carramiñana Alonso, Alberto 12 [A. Carramiñana-Alonso]
-- Carrasco, Esperanza 12 [E. Carrasco]
-- Carrasco, Esperanza 12 [E. Carrasco]
-- Carrera Jarrín, E 24 [E. Carrera-Jarrín]
-- Castillo Delacroix, Lucas Ezequiel 9 [L. E. Castillo Delacroix]
-- Castromonte, César 23 [C. Castromonte]
-- Cazar, D 24 [D. Cazar]
-- Cogollo, Diego 26 [D. Cogollo]
-- Coloma Borja, D.A. 24 [D. Coloma-Borja]
-- Conde Sanchez, Ruben 1 [R. Conde]
-- Cotzomi Paleta, Jorge 1 [J. Cotzomi]
-- Dall'ara, Dario 9 [D. Dallara]
-- Dasso, Sergio 10, 5 [S. Dasso]
-- de Aguiar, Renan 25 [R. Aguiar]
-- de Albuquerque Silva, Alex 26 [A. Albuquerque]
-- de Andrade Pacheco Reis, Jorge Henrique 25 [J.H.A.P.Reis]
-- De León, H. 13 [H. De-León]
-- De León Barrios, Riccardo 20 [R. deLeón-Barrios]
-- Domínguez, D 6 [D. Domínguez]
-- Durán, Jesús Andrés 21 [J.A. Durán]
-- Echiburu, Mauricio 18 [M. Echiburu]
-- Galindo Tellez, Aline 12 [A. Galindo-Tellez]
-- González, Manuel 2 [M. González]
-- Gómez Berisso, Mariano 2 [M. Gómez Berisso]
-- Grisales Casadiegos, Jenniffer 20 [J. Grisales-Casadiegos]
-- Gulisano, Adriana María 10, 29, 30 [A. M. Gulisano]
-- Gutierrez, Christian 5 [C. Gutierrez]
-- Helo, Juan Carlos 14 [J. Helo]
-- Huanca, César 21 [C. Huanca]
-- Ise, Juan Eduardo 9 [J. E. Ise]
-- Kelly Matias do Nascimento, Gyovanna 26 [G. K. M. Nascimento]
-- Leigui de Oliveira, Marcelo Augusto 27 [M. A. Leigui de Oliveira]
-- Lock Miletto, Fernando 25 [F. L. Miletto]
-- Luzio, Vitor Prestes 27 [V. P. Luzio]
-- Machado, Franz 23 [F. Machado]
-- Martinez, Alexander 20 [A. Martínez-Méndez]
-- Martinez Bravo, Oscar Mario 1 [O. Martinez]
-- Mayo-García, Rafael 3 [R. Mayo-García]
-- Mijangos Fuentes, Luis Guillermo 19 [L.G. Mijangos]
-- Miranda, Pedro 21 [P. Miranda]
-- Molina, María Graciela 9 [M. G. Molina]
-- Morales Argueta, Iván René 16 [I.R. Morales]
-- Morales Olivares, O.G 13 [O.G Morales-Olivares]
-- Moreno Barbosa, Eduardo 1 [E. Moreno-Barbosa]
-- Muñoz, Pablo 14 [P. Muñoz]
-- Nina, Carlos 21 [C. Nina]
-- Núñez, Luis A. 20 [L.A. Núñez]
-- Otiniano, Luis 4 [L. Otininano]
-- Pagán Muñoz, Raúl 3 [R. Pagán-Muñoz]
-- Parada Jaime, Karoll Michely 15 [K. M. Parada-Jaime]
-- Parada Villamizar, Heidar Marcel 15 [H. M. Parada-Villamizar]
-- Parra, Rodrigo 8 [R. Parra]
-- Peña-Rodríguez, Jesús 20 [J. Peña-Rodríguez]
-- Pereira, Matias 10 [M. Pereira]
-- Perez Cuevas, Yorlan Arneth 15 [Y. A. Perez-Cuevas]
-- Pérez Figueroa, Héctor Eduardo 16 [H. Perez]
-- Pisco-Guabave, Jhonattan 20 [J. Pisco-Guabave]
-- Ponce Lancho, Epifanio 1 [E. Ponce]
-- Quispe, Richard 21 [R. Quispe]
-- Raljevic, Mirko 21 [M. Raljevic]
-- Ramelli, Maximilano 10 [M. Ramelli]
-- Rivera, Hugo 21 [H. Rivera]
-- Rubinstein, Lucas Tomás 10 [L. T. Rubinstein]
-- Rubio-Montero, Antonio Juan 3 [A.J. Rubio-Montero]
-- Sacahuí Reyes, José Rodrigo 16 [J.R. Sacahui]
-- Salazar Ibarguen, Humberto 1 [H. Salazar]
-- Salomón, Nicolás 9 [N. Salomón]
-- Samanés, Jorge 4 [J. Samanes]
-- Santos, Noelia Ayelén 5 [N.A. Santos]
-- Sarmiento-Cano, Christian 11 [C. Sarmiento-Cano]
-- Sidelnik, Iván 2 [I. Sidelnik]
-- Suárez-Durán, Mauricio 15 [M. Suárez-Durán]
-- Subieta, Martín 21 [M. Subieta]
-- Stuani, Luiz Augusto 26 [L. Stuani]
-- Taboada Núñez, Alvaro 11 [A. Taboada-Núñez]
-- Terrazas, Juan Carlos 21 [J. Terrazas]
-- Ticona, Rolando 21 [R. Ticona]
-- Torres Peralta, Ticiano 9 [T. Torres Peralta]
-- Urrutia de Gutierrez, Zaida del Rosario 19 [Z.R. Urrutia]
-- Vásquez, N 6 [N. Vásquez]
-- Vázquez-Ramírez, Adriana 20 [A. Vázquez-Ramírez]
-- Vega, Juan 4 [J. Vega]
-- Vega, Pedro 14 [P. Vega]
-- Vega, Alfredo 17 [A. Vega]
-- Vesga-Ramirez, Alejandra 11 [A. Vesga-Ramirez]
-- Villaseñor Cendejas, Luis 22 [L. Villaseñor-Cendejas]
-- Vitoreti, Douglas 28 [D. Vitoreti]
-- Wiklich Sobrinho, Rafaela 27 [R. Wiklich Sobrinho]
-- Zepeda, Arnulfo 13 [A. Zepeda]
+1. Alberto Morillas, Angelines <sup>3</sup> [A. Alberto]
+1. Alvarez Ochoa, Cesar <sup>15</sup> [C. Alvarez-Ochoa]
+1. Arceo, R. <sup>15</sup> [R. Arceo]
+1. Areso, Omar <sup>12</sup> [O. Areso]
+1. Arnaldi, Luis Horacio <sup>2</sup> [L. H. Arnaldi]
+1. Asorey, Hernán <sup>2</sup> [H. Asorey]
+1. Audelo, M <sup>8</sup> [M. Audelo]
+1. Ballina Escobar, Maynor Giovanni <sup>18</sup> [M.G. Ballina-Escobar]
+1. Becerra Villamizar, Daniel Camilo <sup>17</sup> [D. C. Becerra-Villamizar]
+1. Bertou, Xavier <sup>2</sup> [X. Bertou]
+1. Caballero Mora, Karen Salome <sup>15</sup> [K.S. Caballero-Mora]
+1. Caiza, R <sup>7</sup> [R. Caiza]
+1. Calderón-Ardila, Rolando <sup>13</sup> [R. Calderón-Ardila]
+1. Campelo, Josafary <sup>28</sup> [Josafary Campelo]
+1. Campos Fauth, Anderson <sup>27</sup> [A. C. Fauth]
+1. Carramiñana Alonso, Alberto <sup>14</sup> [A. Carramiñana-Alonso]
+1. Carrasco, Esperanza <sup>14</sup> [E. Carrasco]
+1. Carrera Jarrín, E <sup>26</sup> [E. Carrera-Jarrín]
+1. Castillo Delacroix, Lucas Ezequiel <sup>10</sup> [L. E. Castillo Delacroix]
+1. Castromonte, César <sup>25</sup> [C. Castromonte]
+1. Cazar, D <sup>26</sup> [D. Cazar]
+1. Christian, Gutierrez <sup>5</sup> [C. Gutierrez]
+1. Cogollo, Diego <sup>28</sup> [D. Cogollo]
+1. Coloma Borja, D.A. <sup>26</sup> [D. Coloma-Borja]
+1. Conde Sanchez, Ruben <sup>1</sup> [R. Conde]
+1. Cotzomi Paleta, Jorge <sup>1</sup> [J. Cotzomi]
+1. Dall'ara, Dario <sup>10</sup> [D. Dallara]
+1. Dasso, Sergio <sup>12, 5</sup> [S. Dasso]
+1. de Aguiar, Renan <sup>27</sup> [R. Aguiar]
+1. de Albuquerque Silva, Alex <sup>28</sup> [A. Albuquerque]
+1. de Andrade Pacheco Reis, Jorge Henrique <sup>27</sup> [J.H.A.P.Reis]
+1. De León, H. <sup>15</sup> [H. De-León]
+1. Domínguez, D <sup>7</sup> [D. Domínguez]
+1. Durán, Jesús Andrés <sup>23</sup> [J.A. Durán]
+1. Echiburu, Mauricio <sup>20</sup> [M. Echiburu]
+1. Galindo Tellez, Aline <sup>14</sup> [A. Galindo-Tellez]
+1. González, Manuel <sup>2</sup> [M. González]
+1. Gómez Berisso, Mariano <sup>2</sup> [M. Gómez Berisso]
+1. Grisales Casadiegos, Jenniffer <sup>22</sup> [J. Grisales-Casadiegos]
+1. Gulisano, Adriana María <sup>12, 6, 11</sup> [A. M. Gulisano]
+1. Helo, Juan Carlos <sup>16</sup> [J. Helo]
+1. Huanca, César <sup>23</sup> [C. Huanca]
+1. Ise, Juan Eduardo <sup>10</sup> [J. E. Ise]
+1. Kelly Matias do Nascimento, Gyovanna <sup>28</sup> [G. K. M. Nascimento]
+1. Leigui de Oliveira, Marcelo Augusto <sup>29</sup> [M. A. Leigui de Oliveira]
+1. Lock Miletto, Fernando <sup>27</sup> [F. L. Miletto]
+1. Luzio, Vitor Prestes <sup>29</sup> [V. P. Luzio]
+1. Machado, Franz <sup>25</sup> [F. Machado]
+1. Martinez, Alexander <sup>22</sup> [A. Martínez-Méndez]
+1. Martinez Bravo, Oscar Mario <sup>1</sup> [O. Martinez]
+1. Mayo-García, Rafael <sup>3</sup> [R. Mayo-García]
+1. Mijangos Fuentes, Luis Guillermo <sup>21</sup> [L.G. Mijangos]
+1. Miranda, Pedro <sup>23</sup> [P. Miranda]
+1. Molina, María Graciela <sup>10</sup> [M. G. Molina]
+1. Morales Argueta, Iván René <sup>18</sup> [I.R. Morales]
+1. Morales Olivares, O.G <sup>15</sup> [O.G Morales-Olivares]
+1. Moreno Barbosa, Eduardo <sup>1</sup> [E. Moreno-Barbosa]
+1. Muñoz, Pablo <sup>16</sup> [P. Muñoz]
+1. Nina, Carlos <sup>23</sup> [C. Nina]
+1. Núñez, Luis A. <sup>22</sup> [L.A. Núñez]
+1. Otiniano, Luis <sup>4</sup> [L. Otininano]
+1. Pagán Muñoz, Raúl <sup>3</sup> [R. Pagán-Muñoz]
+1. Parada Jaime, Karoll Michely <sup>17</sup> [K. M. Parada-Jaime]
+1. Parada Villamizar, Heidar Marcel <sup>17</sup> [H. M. Parada-Villamizar]
+1. Parra, Rodrigo <sup>9</sup> [R. Parra]
+1. Peña-Rodríguez, Jesús <sup>22</sup> [J. Peña-Rodríguez]
+1. Pereira, Matias <sup>12</sup> [M. Pereira]
+1. Perez Cuevas, Yorlan Arneth <sup>17</sup> [Y. A. Perez-Cuevas]
+1. Pérez Figueroa, Héctor Eduardo <sup>18</sup> [H. Perez]
+1. Pisco-Guabave, Jhonattan <sup>22</sup> [J. Pisco-Guabave]
+1. Ponce Lancho, Epifanio <sup>1</sup> [E. Ponce]
+1. Quispe, Richard <sup>23</sup> [R. Quispe]
+1. Raljevic, Mirko <sup>23</sup> [M. Raljevic]
+1. Ramelli, Maximilano <sup>12</sup> [M. Ramelli]
+1. Rivera, Hugo <sup>23</sup> [H. Rivera]
+1. Rubinstein, Lucas Tomás <sup>12</sup> [L. T. Rubinstein]
+1. Rubio-Montero, Antonio Juan <sup>3</sup> [A.J. Rubio-Montero]
+1. Sacahuí Reyes, José Rodrigo <sup>18</sup> [J.R. Sacahui]
+1. Salazar Ibarguen, Humberto <sup>1</sup> [H. Salazar]
+1. Salomón, Nicolás <sup>10</sup> [N. Salomón]
+1. Samanés, Jorge <sup>4</sup> [J. Samanes]
+1. Santos, Noelia Ayelén <sup>5</sup> [N.A. Santos]
+1. Sarmiento-Cano, Christian <sup>13</sup> [C. Sarmiento-Cano]
+1. Sidelnik, Iván <sup>2</sup> [I. Sidelnik]
+1. Stuani, Luiz Augusto <sup>28</sup> [L. Stuani]
+1. Suárez-Durán, Mauricio <sup>17</sup> [M. Suárez-Durán]
+1. Subieta, Martín <sup>23</sup> [M. Subieta]
+1. Taboada Núñez, Alvaro <sup>13</sup> [A. Taboada-Núñez]
+1. Terrazas, Juan Carlos <sup>23</sup> [J. Terrazas]
+1. Ticona, Rolando <sup>23</sup> [R. Ticona]
+1. Torres Peralta, Ticiano <sup>10</sup> [T. Torres Peralta]
+1. Urrutia de Gutierrez, Zaida del Rosario <sup>21</sup> [Z.R. Urrutia]
+1. Vásquez, N <sup>7</sup> [N. Vásquez]
+1. Vázquez-Ramírez, Adriana <sup>22</sup> [A. Vázquez-Ramírez]
+1. Vega, Juan <sup>4</sup> [J. Vega]
+1. Vega, Pedro <sup>16</sup> [P. Vega]
+1. Vega, Alfredo <sup>19</sup> [A. Vega]
+1. Vesga-Ramirez, Alejandra <sup>13</sup> [A. Vesga-Ramirez]
+1. Villaseñor Cendejas, Luis <sup>24</sup> [L. Villaseñor-Cendejas]
+1. Vitoreti, Douglas <sup>30</sup> [D. Vitoreti]
+1. Wiklich Sobrinho, Rafaela <sup>29</sup> [R. Wiklich Sobrinho]
+1. Zepeda, Arnulfo <sup>15</sup> [A. Zepeda]
 
 ## Institutes
 
-- Benemérita Universidad Autónoma de Puebla [BUAP]
-- Centro Atómico Bariloche (CNEA/CONICET/IB) [CAB]
-- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas [CIEMAT]
-- Comisión Nacional de Investigación y Desarrollo Aeroespacial [CONIDA]
-- Departamento de Ciencias de la Atmósfera y los Océanos, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires. [DCAO]
-- Escuela Politécnica Nacional [EPN]
-- Escuela Superior Politécnica de Chimborazo [ESPOCH]
-- European Soutern Observatory (ESO) [ESO]
-- Facultad de Ciencias Exactas y Tecnología (FACET) – Universidad Nacional de Tucumán (UNT) [UNT]
-- Instituto de Astronomía y Física del Espacio, IAFE (UBA-CONICET) [IAFE]
-- Instituto de Tecnologías en Detección y Astropartículas (CNEA, CONICET,UNSAM) [ITeDA]
-- Instituto Nacional de Astrofísica, Óptica y Electrónica [INAOE]
-- Universidad Autónoma de Chiapas [UNACH]
-- Universidad de La Serena [US]
-- Universidad de Pamplona [UP]
-- Universidad de San Carlos [USAC]
-- Universidad de Valparaíso [UV]
-- Universidad de Viña del Mar [UVM]
-- Universidad del Valle de Guatemala [UVG]
-- Universidad Industrial de Santander [UIS]
-- Universidad Mayor de San Andrés [UMSA]
-- Universidad Michoacana de San Nicolás de Hidalgo [UNICH]
-- Universidad Nacional de Ingeniería [UNI]
-- Universidad San Francisco de Quito [USFQ]
-- Universidade Estadual de Campinas [IFGW]
-- Universidade Federal de Campina Grande [UFCG]
-- Universidade Federal do ABC [UFABC]
-- Universidade Federal do Recôncavo da Bahia [UFRB]
-- Instituto Antártico Argentino/DNA
-- Departamento Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina
+1. Benemérita Universidad Autónoma de Puebla [BUAP] 
+1. Centro Atómico Bariloche (CNEA/CONICET/IB) [CAB] 
+1. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas [CIEMAT] 
+1. Comisión Nacional de Investigación y Desarrollo Aeroespacial [CONIDA] 
+1. Departamento de Ciencias de la Atmósfera y los Océanos, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires. [DCAO] 
+1. Departamento Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Argentina [DFUBA] [DFUBA] 
+1. Escuela Politécnica Nacional [EPN] 
+1. Escuela Superior Politécnica de Chimborazo [ESPOCH] 
+1. European Soutern Observatory (ESO) [ESO] 
+1. Facultad de Ciencias Exactas y Tecnología (FACET) – Universidad Nacional de Tucumán (UNT) [UNT] 
+1. Instituto Antártico Argentino [IAA] 
+1. Instituto de Astronomía y Física del Espacio, IAFE (UBA-CONICET) [IAFE] 
+1. Instituto de Tecnologías en Detección y Astropartículas (CNEA, CONICET,UNSAM) [ITeDA] 
+1. Instituto Nacional de Astrofísica, Óptica y Electrónica [INAOE] 
+1. Universidad Autónoma de Chiapas [UNACH] 
+1. Universidad de La Serena [US] 
+1. Universidad de Pamplona [UP] 
+1. Universidad de San Carlos [USAC] 
+1. Universidad de Valparaíso [UV] 
+1. Universidad de Viña del Mar [UVM] 
+1. Universidad del Valle de Guatemala [UVG] 
+1. Universidad Industrial de Santander [UIS] 
+1. Universidad Mayor de San Andrés [UMSA] 
+1. Universidad Michoacana de San Nicolás de Hidalgo [UNICH] 
+1. Universidad Nacional de Ingeniería [UNI] 
+1. Universidad San Francisco de Quito [USFQ] 
+1. Universidade Estadual de Campinas [IFGW] 
+1. Universidade Federal de Campina Grande [UFCG] 
+1. Universidade Federal do ABC [UFABC] 
+1. Universidade Federal do Recôncavo da Bahia [UFRB] 

docs/about/sites.md

@@ -9,3 +9,43 @@ The LAGO projects has detectors in many different sites:
 - And low altitude detectors in Argentina, Colombia, Guatemala and Ecuador
 
 ## Geographical Distribution and Altitudes of LAGO Water Cherenkov Detectors
+
+![LAGO Sites](images/sitios.png "LAGO Sites")
+
+## Chacaltaya
+
+Mount Chacaltaya, close to La Paz, in Bolivia, is the highest altitude cosmic ray laboratory, at 5300 m above sea level.
+
+Being the highest site for LAGO, it is the one with the best signal from GRB. Interestingly enough, being very close to the magnetic equator, it might have a background quite low for such a high altitude.
+
+A prototype detector is currently at the Chacaltaya site, and two large 4 m<sup>2</sup> are being calibrated.
+
+## Sierra Negra
+
+Sierra Negra, close to Puebla, Mexico, is the first high altitude site in operation in LAGO, with its 4600 m above sea level. It has two small 1 m<sup>2</sup> WCD and three bigger 4 m<sup>2</sup> WCD in operation.
+
+The array is taking data since January 2007, providing the first LAGO data.
+
+## Pico Espejo
+
+The Pico Espejo cable car is the world's highest cable car. Its base is located in the Venezuelan city of Mérida at an altitude of 1640 meters, and its terminus is on Pico Espejo, at 4765 meters.
+
+A prototype WCD is taking data at the Universidad de Los Andes. Three 4 m<sup>2</sup> WCD have been deployed at the Pico Espejo station, but they still lack water and instrumentation.
+
+## Peru
+
+Various sites are under investigation in Peru, and the first detector is operating at Marcapomacocha, 4450m asl. The overall high altitude makes many regions possible extra sites for LAGO.
+
+Prototypes are running both in Cusco and Lima.
+
+## Auger Site
+
+The Pierre Auger Observatory is located in Malargüe, in the south of the Mendoza province, in Argentina.
+
+The aim of the observatory is to detect Ultra High Energy Cosmic Rays (UHECR), and more about its science can be found at the main website of the project.
+
+Since Auger is a huge project, with 1600 10 m<sup>2</sup> WCD, it presents an interesting water area to detect GRBs. Its low altitude (1400 m a.s.l.), necesary for the UHECR physics, is however a weakness for GRB detection, reducing its efficiency to one similar to the other sites.
+
+While Auger is not a LAGO site, many scientists from LAGO are also part of Auger (and actually LAGO was born from Auger), so some data analysis is done in common.
+
+Data is being taken since March 2005 and is regularly analyzed.
\ No newline at end of file

docs/activities/detectors.md

@@ -10,16 +10,22 @@ When a particle goes through a medium at such a speed, it produces a cone of lig
 
 This light was discovered by a russian physicist named Cherenkov in 1934, and is the responsible for the typical blue glow of water in nuclear reactors. It is used frequently in particle detectors, as a high energy particle going through a water volume will produce this caracteristic light.
 
+![Cherenkov effect](images/cherenkov.jpg "Cherenkov effect")
+
 ### Photomultiplier tubes
 
 Photomultiplier tubes (PMTs) are extremely sensitive light detectors, usually in ultraviolet and blue. A glass vacuum tube houses a photocathode, several dynodes, and an anode. Incident photons strike the photocathode covering the glass and electrons are produced by the photoelectric effect. High voltage between each dynode provoque an avalanche of secondary electrons, literally multiplying the signal. Typical gains of 106 mean a million electrons are detected on the anode for a single photon hitting the glass.
 
+![Photomultiplier tubes](images/phototube.jpg "Photomultiplier tubes")
+
 These detectors can therefore detect single photons, but would be destroyed if turned on in ambient light. They are usually used in light-tight environments, to detect minimum amounts of light.
 
 ### Water Cherenkov tanks
 
 Water Cherenkov tanks are detectors based on the Cherenkov effect. A simple plastic (or metal, fiberglass...) tank is filled with water and closed, in order to be light-tight. Photomultipler tubes are installed inside the detector, looking at the water volume. When a particle crosses the water volume, it will emit light in a Cherenkov cone. The light is then uniformized in the water volume by diffusion on the walls of the tank (usually covered by a highly diffusive material), and finally collected on the photomultiplier tubes.
 
+![Water Cherenkov tanks](images/wcd.jpg "Water Cherenkov tanks")
+
 #### WCD calibration
 
 WCD are easy to calibrate due to their particular signal response to different particles:
@@ -37,3 +43,12 @@ When a GRB occurs, a huge number of high energy photons reach the Earth's atmosp
 Most of the secondary particules of these cascades are photons (about 90%). A good property of WCD is the fact they can detect photons through their conversion in the water volume. This makes WCD good GRB detectors.
 
 What one would expect is that WCD would see an increase in the photon flux when a GRB occurs. It is not easy to detect since there is a continuous high background of particles entering the WCD, but this is the challenge LAGO will try to overcome.
+
+## Gamma Ray Bursts
+
+[GRB](../blog/posts/grb.md) The most violent events in the Universe.
+
+## Solar Physics
+
+[Solar Physics](../blog/posts/solar.md) Understanding the solar activity and its impact on Cosmic Rays.
+

docs/activities/teaching.md

@@ -9,3 +9,4 @@ The analysis of these events allow many different studies. One can observe the d
 Once the detector is calibrated, one of the most interesting studies that can be done with students is the observation of muon decays. By looking at time difference between pulses, one can search pulses happening in a short time window and look for the characteristic 2.2 microsecond life time of the muon. A simple explanation of this decay can be read here.
 
 Many other experiments are possible, and with 2 or 3 detectors one can also reproduce the original measurements of Pierre Auger in the 30's.
+

docs/blog/posts/grb.md

+# Gamma Ray Bursts
+
+## Vela 5: discovering GRBs
+
+The Gamma Ray Bursts (GRB) were discovered accidentaly in the 60's by US military satellites in search of non authorized nuclear explosions.
+
+The Vela 5 satellites promptly detected gamma ray bursts similar to what they would expect from such explosions, but coming from space.
+
+![Vela](images/vela.png "Vela")
+
+These bursts where short, from 0.01 to about 100 s, and had most of their energy carried by photons above 100 keV.
+
+They remained mysteries for more than 30 years.
+
+## BATSE: 1991-2000
+
+In 1991, BATSE (Burst And Transient Source Experiment) was sent in space, and started providing very valuable data on GRBs. With its 8 modules, it was able to see the whole sky, and detected about 1 GRB per day.
+
+![batse](images/cgro.jpg "Batse")
+
+BATSE clearly saw 2 distinct populations of bursts, short and long, but except for their duration, no significant diferences were found, due to the lack of additional data.
+
+![Duration](images/batsegrbduration.png "Duration")
+>Time distribution of BATSE GRBs: 2 populations are clearly visible: short (<2 s) and long (>2 s) bursts 
+
+Another important discovery of BATSE is that GRBs are isotropic, as can be seen on the picture above. They is no correlation with our galactic plane, as one would expect if these GRBs are from galactic origin. Furthermore, BATSE saw a deficit on low luminosity (energy) GRBs, indicating that GRBs are either located in galaxy halos, or are from cosmologic origin (in which case the deficit at low energy would be due to the expansion of the universe).
+
+![Map](images/batsegrbmap.png "Map")
+> Map of arrival of BATSE bursts (in galactic coordinates) 
+
+## Beppo-SAX: 1996-2002
+
+Beppo-SAX made some further discoveries possible due to its good angular resolution. While BATSE had about 4 degrees pixels, Beppo-SAX reached about 50" (i.e. 290 times better). It had on board, in addition to a GRB monitor, various X-ray detectors (lower energy than gamma).
+
+![Beppo](images/beppo2.jpg "Beppo")
+
+On February 28th of 1997, Beppo-SAX saw a burst both with its Gamma Ray detector and X-ray. It observed the burst during a few days and saw an afterglow in X: the X-ray image became dimmer on timescales of days.
+
+![GRB](images/grb970228.png "GRB")
+> GRB 970228 in X-ray: Left: on February 28th,Right: 3 days later 
+
+3 months later, GRB 970508 was detected by Beppo-SAX and ground-based spectrometers were able to mesure the optical spectrum of the afterglow. This allowed to measure the redshift of the object: z~0.84. It was the confirmation that GRBs were cosmologicals.
+
+However, this discovery posed a new problem. If GRBs were so distant, then they had to be incredibly powerful: about 1051 to 1054 ergs, the light of a billion galaxies!
+
+## SWIFT: 2004-
+
+SWIFT provided an important discovery: while afterglows had been observed only in long bursts initially, SWIFT allowed a prompt localization of bursts, and optical counterparts of short bursts were observed.
+
+![SWIFT](images/swift.jpg "SWIFT")
+
+This, combined with correlations of long bursts with supernovae, allowed some confidence on the origin of the GRBs, after more than 30 years since their discovery.
+
+## Fermi: 2008-
+
+Fermi has been a game changer in the high energy domain of gamma ray observation. It has observed many GeV photons from GRBs, but even its huge LAT detector has not yet been able to determine the maximum energy of a GRB, due to the low fluences involved. Maybe ground based experiments, such as LAGO or HAWC in Mexico, will be able to contribute in this field. 
+
+![FERMI](images/fermi.jpg "FERMI")
+
+## GRB Theory
+
+![LAGO Sites](images/sitios.png "LAGO Sites")
+
+Long GRBs are usually considered as coming from hypernovae, a kind of supernova originated by super-massive star (>40 solar masses).
+
+Short GRBs are probably produced by the coalescence of compact objects (neutron star or black hole) in a binary system.
+
+A mecanism that could explain the formation in both cases is the fireball model, where a highly relativistic fireball produces the gammas of the burst in internal shocks, while the afterglow is produced when the shock wave reaches the local medium.
\ No newline at end of file

docs/blog/posts/solar.md

+# Solar Physics
+
+In their way to the Earth, the cosmic rays produced in the galaxy by many different sources (called Galactic Cosmic Rays, GCR), find themselves deflected by magnetic fields.
+
+The main effect is produced by the solar magnetic field. When it is intense (ie. when the sun is active), GCR are deflected and the flux at Earth is therefore reduced. When it is lower (ie. when the sun is calm), GCR find their way more easily to the Earth and the flux observed is higher.
+
+By measuring the GCR flux, one can therefore determine indirectly the solar activity. This allows CR experiments to observe the 11 (and 22) years cycles of the sun, as well as violent transients called Forbush decreases.
+
+When a coronal mass ejection (CME) is produced at the sun, a huge mass of magnetised plasma is sent through the interplanetary medium. Upon reaching Earth, this plasma acts as a shield to GCR, and a rapid disminution of GCR flux can be observed (a few percents in a few hours). Then, once the CME goes on his way, the GCR flux slowly comes back to its original value, on a time scale of days. This GCR flux decrease is called Forbush decrease and can be nicely observed by any cosmic ray detector on Earth.
+
+LAGO WCD are being used to study the solar activity. As they can measure different cosmic ray events (electromagnetic part, muons, high energy cosmic ray extended air shower), they can provide a unique information on transient events of solar origin.