Old and New from Multifrequency Astrophysics

In this short review paper we comment on some the most important steps that have been made in the past decades for a better understanding of the physics governing our Universe. The results we discuss come from the many groundand-space-based experiments developed for measuring astrophysical sources in various energy bands. These experimental results are discussed within the framework of current theoretical models. Because of the limited length of this paper, we have selected only a few topics that, in our opinion, have been crucial for the progress of our understanding of the physics of cosmic sources

A Decade of GRB Follow-Up by BOOTES in Spain (2003–2013)

This article covers ten years of GRB follow-ups by the Spanish BOOTES stations: 71 follow-ups providing 23 detections. Follow-ups by BOOTES-1B from 2005 to 2008 were given in a previous article and are here reviewed and updated, and additional detection data points are included as the former articlemerely stated their existence. The all-sky cameras CASSANDRA have not yet detected any GRB optical afterglows, but limits are reported where available.The authors appreciate the auspices of INTA, IHSM-UMA/CSIC, and UMA as well as the financial support by the Junta de Andaluca and the Spanish Ministry of Economy and Competitiveness through the Research Projects P07-TIC-03094, P12-TIC2839, AYA2009-14000-C03-01, AYA 2010-39727-C03-01, and AYA-2015-71718-R. Martin Jelinek was supported by the postdoctoral fellowship of the Czech Academy of Sciences. This study was carried out in the framework of the Unidad Asociada IAA-CSIC at the Group of Planetary Science of ETSI-UPV/EHU. This work was supported by the Ikerbasque Foundation for Science. The Czech CVUT FEL team acknowledges the support by GA CR Grant 13-33324S

Four Years of Realtime GRB Followup by BOOTES-1B (2005-2008)

Four years of BOOTES-1B GRB follow-up history are summarised for the first time in the form of a table. The successfully followed events are described case by case. Further, the data are used to show the GRB trigger rate in Spain on a per-year basis, resulting in an estimate of 18 triggers and about 51 h of telescope time per year for real time triggers. These numbers grow to about 22 triggers and 77 h per year if we include also the GRBs observable within 2 hours after the trigger.Comment: 16 pages, Accepted into Proceedings of AstroRob Malaga 200

Atmosphere-Space Interactions Monitor (ASIM): State of the Art

Atmosphere-Space Interactions Monitor (ASIM) mission is an ESA pay load which will be installed in the Columbus module of the International Space Station (ISS). ASIM is optimized to the observation and monitoring of luminescent phenomena in the upper atmosphere, the so called Transient Luminous Event (TLEs) and Terrestrial Gamma Ray Flashes(TGFs). Both TLEs and TGFs have been discovered recently (past two decades) and opened a new field of research in high energetic phenomena in the atmosphere. We will review the capabilities of ASIM and how it will help researchers to gain deeper knowledge of TGFs, TLEs, their inter-relationship and how they are linked to severe thunderstorms and the phenomena of lightning

A decade of GRB follow-up by BOOTES in Spain (2003-2013)

This article covers ten years of GRB follow-ups by the Spanish BOOTES stations: 71 follow-ups providing 23 detections. Follow-ups by BOOTES-1B from 2005 to 2008 were given in the previous article, and are here reviewed, updated, and include additional detection data points as the former article merely stated their existence. The all-sky cameras CASSANDRA have not yet detected any GRB optical afterglows, but limits are reported where available

OLD AND NEW RESULTS FROM MULTIFREQUENCY ASTROPHYSICS: THE IMPORTANCE OF SMALL TELESCOPES

RESUMEN En este artículo vamos a tratar brevemente algunos ejemplos de los resultados, desde el Big Bang a las fuentes galácticas, obtenidos en diferentes rangos de frecuencia por muchos experimentos espaciales y terrestres. Vamos a señalar los problemas fundamentales que nacen a partir de una comparación de los resultados experimentales multirrango y de las teorías. Vamos a tratar también la importancia de contar con una red de telescopios robóticos que pueden proporcionar monitorizaciónóptica a largo plazo de las diferentes clases de fuentes cósmicas para proporcionar datos fundamentales que permitan el progreso en la comprensión de muchos problemas abiertos. Los resultados seleccionados están limitados por nuestros conocimientos y preferencias y se extienden a lo largo de varias décadas, desde la década de 1970, cuando los experimentos espaciales abrieron prácticamente todas las ventanas para investigar el Universo, hasta nuestros días. Hemos tratado este tema muchas veces: en el artículo de revisión "El impacto de los experimentos espaciales en nuestro conocimiento de la física del Universo" (Giovannelli y Sabau-Graziati, 2004) y en sus revisiones posteriores (e.g. Giovannelli y Sabau-Graziati, 2012a). ABSTRACT In this paper we will briefly discuss several examples of results, from the Big Bang to galactic sources, obtained in different frequency regions by many space-and ground-based experiments. We will remark the fundamental problems born from a comparison of experimental multifrequency results and theories. We will discuss also the importance of having a network of robotic telescopes that can provide long term optical monitoring of different classes of cosmic sources for providing fundamental data for a progress in understanding many problems still open. The results selected are biased by our knowledge and feelings and extend over several decades, starting from the 1970's, when the space experiments opened practically all the windows for investigating the Universe, up to-date. We discussed about this topic many times (e.g. on the review paper "The impact of the space experiments on our knowledge of the physics of the Universe&quot

Observations of Comet 9P/Tempel 1 around the Deep Impact event by the OSIRIS cameras onboard Rosetta

17 pp.-- Final full-text version of the paper available at: http://dx.doi.org/10.1016/j.icarus.2006.09.023.The OSIRIS cameras on the Rosetta spacecraft observed Comet 9P/Tempel 1 from 5 days before to 10 days after it was hit by the Deep Impact projectile. The Narrow Angle Camera (NAC) monitored the cometary dust in 5 different filters. The Wide Angle Camera (WAC) observed through filters sensitive to emissions from OH, CN, Na, and OI together with the associated continuum. Before and after the impact the comet showed regular variations in intensity. The period of the brightness changes is consistent with the rotation period of Tempel 1. The overall brightness of Tempel 1 decreased by about 10% during the OSIRIS observations. The analysis of the impact ejecta shows that no new permanent coma structures were created by the impact. Most of the material moved with ~ 200 m/s. Much of it left the comet in the form of icy grains which sublimated and fragmented within the first hour after the impact. The light curve of the comet after the impact and the amount of material leaving the comet (4.5 - 9 x 10e6 of water ice and a presumably larger amount of dust) suggest that the impact ejecta were quickly accelerated by collisions with gas molecules. Therefore, the motion of the bulk of the ejecta cannot be described by ballistic trajectories, and the validity of determinations of the density and tensile strength of the nucleus of Tempel 1 with models using ballistic ejection of particles is uncertain.The OSIRIS imaging system on board Rosetta is managed by the Max-Planck-Institute for Solar System Research in Katlenburg-Lindau (Germany), thanks to an International collaboration between Germany, France, Italy, Spain, and Sweden. We acknowledge the funding of the national space agencies ASI, CNES, DLR, the Spanish Space Program (Ministerio de Educacion y Ciencia), SNSB and ESA. IRAF is distributed by the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. We acknowledge JPL's Horizons online ephemeris generator for providing the comet's position and rate of motion during the observations. This research has made use of NASA's Astrophysics Data System.Peer reviewe