Institution
Royal Institute and Observatory of the Spanish Navy
Facility•San Fernando, Spain•
About: Royal Institute and Observatory of the Spanish Navy is a facility organization based out in San Fernando, Spain. It is known for research contribution in the topics: Gamma-ray burst & Magnetic anomaly. The organization has 50 authors who have published 106 publications receiving 2565 citations. The organization is also known as: Instituto y Observatorio de Marina de San Fernando.
Topics: Gamma-ray burst, Magnetic anomaly, Afterglow, Geology, Time transfer
Papers published on a yearly basis
Papers
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TL;DR: A new algorithm, developed at the Plataforma Solar de Almeria, which combines these two characteristics of accuracy and simplicity, is presented and allows of the true solar vector to be determined with an accuracy of 0.5 minutes of arc for the period 1999–2015.
367 citations
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TL;DR: In this paper, the deployment and data processing for Spanish stations was funded by Consolider-Ingenio 2010 project TOPO-IBERIA (CSD2006-00041) as well as ALERT-ES (CGL2010-19803-C03-02).
181 citations
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University of Copenhagen1, European Southern Observatory2, Spanish National Research Council3, Space Telescope Science Institute4, Aarhus University5, Kyoto University6, Kyushu University7, Aoyama Gakuin University8, Royal Institute and Observatory of the Spanish Navy9, Marshall Space Flight Center10, INAF11, University of Hertfordshire12
TL;DR: In this paper, optical and near-infrared observations of the dim afterglow of GRB 020124, obtained between 2 and 68 hr after the gamma-ray burst, were presented.
Abstract: We present optical and near-infrared observations of the dim afterglow of GRB 020124, obtained between 2 and 68 hr after the gamma-ray burst. The burst occurred in a very faint (R 29.5) damped Lyα absorber (DLA) at a redshift of z = 3.198 ± 0.004. The derived column density of neutral hydrogen is log(N) = 21.7 ± 0.2, and the rest-frame reddening is constrained to be E(B-V) < 0.065, i.e., AV < 0.20 for standard extinction laws with RV ≈ 3. The resulting dust-to-gas ratio is less than 11% of that found in the Milky Way but consistent with the SMC and high-redshift QSO DLAs, indicating a low metallicity and/or a low dust-to-metal ratio in the burst environment. A gray extinction law (large RV), produced through preferential destruction of small dust grains by the gamma-ray burst, could increase the derived AV and dust-to-gas ratio. The dimness of the afterglow is, however, fully accounted for by the high redshift: if GRB 020124 had been at z = 1, it would have been approximately 1.8 mag brighter—in the range of typical bright afterglows.
116 citations
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INAF1, University of Bologna2, University of Leicester3, University of Amsterdam4, Johns Hopkins University5, Spanish National Research Council6, University of Copenhagen7, Janssen Pharmaceutica8, Max Planck Society9, Space Telescope Science Institute10, Royal Institute and Observatory of the Spanish Navy11, University of Ferrara12, Marshall Space Flight Center13, University of Hertfordshire14, European Southern Observatory15
TL;DR: It is suggested that the bump can be modeled with a SN having the same temporal profile as the other proposed hypernova SN2002ap, but 1.3 mag brighter at peak, and located at the GRB redshift.
Abstract: We report on photometric, spectroscopic and polarimetric monitoring of the optical and near-infrared (NIR) afterglow of GRB020405. Ground-based optical observations, performed with 8 different telescopes, started about 1 day after the high-energy prompt event and spanned a period of ∼10 days; the addition of archival HST data extended the coverage up to ∼150 days after the GRB. We report the first detection of the afterglow in NIR bands. The detection of Balmer and oxygen emission lines in the optical spectrum of the host galaxy indicates that the GRB is located at redshift z = 0.691. Fe II and Mg II absorption systems are detected at z = 0.691 and at z = 0.472 in the afterglow optical spectrum. The latter system is likely caused by absorbing clouds in the galaxy complex located ∼2" southwest of the GRB020405 host. Hence, for the first time, the galaxy responsible for an intervening absorption line system in the spectrum of a GRB afterglow is spectroscopically identified. Optical and NIR photometry of the afterglow indicates that, between 1 and 10 days after the GRB, the decay in all bands is consistent with a single power law of index a = 1.54 ′0.06. The late-epoch VLT J-band and HST optical points lie above the extrapolation of this power law, so that a plateau (or "bump") is apparent in the VRIJ light curves at 10-20 days after the GRB. The light curves at epochs later than day ∼20 after the GRB are consistent with a power-law decay with index α' = 1.85 ′ 0.15. While other authors have proposed to reproduce the bump with the template of the supernova (SN) 1998bw, considered the prototypical "hypernova", we suggest that it can also be modeled with a SN having the same temporal profile as the other proposed hypernova SN2002ap, but 1.3 mag brighter at peak, and located at the GRB redshift. Alternatively, a shock re-energization may be responsible for the rebrightening. A single polarimetric R-band measurement shows that the afterglow is polarized, with P = 1.5 ′ 0.4% and polarization angle 0 = 172° ′8°. Broad-band optical-NIR spectral flux distributions show, in the first days after the GRB, a change of slope across the J band which we interpret as due to the presence of the electron cooling frequency v c . The analysis of the multiwavelength spectrum within the standard fireball model suggests that a population of relativistic electrons with index p ∼ 2.7 produces the optical-NIR emission via synchrotron radiation in an adiabatically expanding blastwave, with negligible host galaxy extinction, and the X-rays via Inverse Compton scattering off lower-frequency afterglow photons.
98 citations
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TL;DR: In this paper, the authors present UBVRCIC photometry of the optical afterglow of the gamma-ray burst GRB 021004 taken at the Nordic Optical Telescope between approximately 8 hours and 30 days after the burst.
Abstract: We present UBVRCIC photometry of the optical afterglow of the gamma-ray burst GRB 021004 taken at the Nordic Optical Telescope between approximately 8 hours and 30 days after the burst. These data are combined with an analysis of the 87 ks Chandra X-ray observations of GRB 021004 taken at a mean epoch of 33 hr after the burst to investigate the nature of this GRB. We find an intrinsic spectral slope at optical wavelengths of ?UH = 0.39 ? 0.12 and an X-ray slope of ?X = 0.94 ? 0.03. There is no evidence for color evolution between 8.5 hr and 5.5 days after the burst. The optical decay becomes steeper approximately 5 days after the burst. This appears to be a gradual break due to the onset of sideways expansion in a collimated outflow. Our data suggest that the extragalactic extinction along the line of sight to the burst is between AV ? 0.3 and 0.5 and has an extinction law similar to that of the Small Magellanic Cloud. The optical and X-ray data are consistent with a relativistic fireball with the shocked electrons being in the slow cooling regime and having an electron index of p = 1.9 ? 0.1. The burst occurred in an ambient medium that is homogeneous on scales larger than approximately 1018 cm but inhomogeneous on smaller scales. The mean particle density is similar to what is seen for other bursts (0.1 cm-3 n 100 cm-3). Our results support the idea that the brightening seen at approximately 0.1 days was due to interaction with a clumpy ambient medium within 1017?1018 cm of the progenitor. The agreement between the predicted optical decay and that observed approximately 10 minutes after the burst suggests that the physical mechanism controlling the observed flux at t ? 10 minutes is the same as the one operating at t > 0.5 days.
97 citations
Authors
Showing all 53 results
Name | H-index | Papers | Citations |
---|---|---|---|
J. Martin Davila | 4 | 10 | 84 |
T. López Moratalla | 3 | 5 | 20 |
F. J. Galindo | 3 | 6 | 56 |
J. Galindo | 2 | 2 | 14 |
Manuel Catalán-Morollón | 2 | 3 | 19 |
Francisco José González González | 2 | 2 | 12 |
Cristina García Silva | 2 | 2 | 19 |
F. J. González-González | 2 | 2 | 19 |
J.M. Dávila | 2 | 2 | 200 |
J. Galindo | 2 | 2 | 5 |
Maria del Carmen Velez Lopez | 2 | 2 | 6 |
J. L. Muiños | 2 | 4 | 6 |
T. López-Moratalla | 2 | 2 | 19 |
J. Garate Pasquin | 2 | 4 | 47 |
MartÍn Lara-Coira | 1 | 1 | 337 |