Fregenal de la Sierra, Spain
Fregenal de la Sierra, Spain

Time filter

Source Type

Lennon D.J.,STS Inc | Evans C.J.,Royal Observatory Edinburgh | Bastian N.,University of Exeter | Beletsky Y.,ESO | And 27 more authors.
Proceedings of the International Astronomical Union | Year: 2010

The Tarantula Survey is an ESO Large Programme which has obtained multi-epoch spectroscopy of over 1,000 massive stars in the 30 Doradus region of the Large Magellanic Cloud. The assembled consortium will exploit these data to address a range of fundamental questions in both stellar and cluster evolution. © International Astronomical Union 2011.


Moles M.,Institute Astrofsica Of Andaluca
Proceedings of SPIE - The International Society for Optical Engineering | Year: 2014

The Observatorio Astrofísico de Javalambre (OAJ) is designed to carry out large surveys. It consists of two main telescopes: JST/T250,a 2.5m telescope with a FoV of 3 deg diameter,and JAST/T80,a 80cm with a 2 deg FoV. JST/T250 will be devoted during the rst 6 years of operation to complete the Javalambre-PAU Astronomical Survey (J-PAS). It is a photometric survey in a system of 54 filters of 14nm width (from ∼ 350 nm to ∼ 900 nm) plus several broad band filters covering a total area of 8500andsqu;°. The JAST/T80 will start operations during 2014 and will be devoted to perform the J-PLUS survey,covering in 2 years the same area as J-PAS using a system of 12 filters. Both surveys will produce ∼ 1 PB of raw data,a single data release of the final combined mosaics is ∼ 850 TB. The archive and processing will be done in a dedicated data center (UPAD) that will be equipped with > 3 PB to store the data produced by the surveys. This contribution presents the software and hardware architecture designed to store and process the data. The processing pipeline is executed in a computing cluster under a batch queuing system. In a first stage it is devoted to correct instrumental signature on the science images,to perform astrometric and photometric calibration,and the computation of individual image catalogs. In a second stage,the pipeline performs the combination of the mosaics in each sky position and computation of final catalogs. The processing software is connected with a management database to store persistent information about the pipeline operations done on each frame. The information in the final objects' catalogs used by the scientific community will be ingested in a science database. Once the J-PAS survey is finished the information stored in database will be andsim 20 TB. Regarding the storage system it will combine disk and tape technologies. The disk storage system will have capacity to store the data that is accessed by the pipeline providing a high bandwidth to feed several hundreds of concurrent processes. The tape library will store and archive the raw data and earlier data releases with lower access frequency. The storage and processing system for the J-PLUS data is already deployed. It contains the job scheduling nodes,database and service nodes for the whole UPAD. For J-PLUS the disk archive have a capacity of ∼ 100 TB. It contains four processing nodes,and two nodes to manage the science databases using a clustered SQL database engine. © 2014 SPIE.


Lagadec E.,European Southern Observatory | Verhoelst T.,Catholic University of Leuven | Mekarnia D.,Laboratoire Fizeau | Suarez O.,Laboratoire Fizeau | And 11 more authors.
Proceedings of the International Astronomical Union | Year: 2011

Post-AGB stars are key objects for the study of the dramatic morphological changes of low- to intermediate-mass stars on their evolution from the Asymptotic Giant Branch (AGB) towards the planetary nebula stage. There is growing evidences that binary interaction processes may very well have a determining role in the shaping process of many objects, but so far direct evidence is still weak. We aim at a systematic study of the dust distribution around a large sample of post-AGB stars as a probe of the symmetry breaking in the nebulae around these systems. We used imaging in the mid-infrared to study the inner part of these evolved stars to probe direct emission from dusty structures in the core of post-AGB stars in order to better understand their shaping mechanisms. We imaged a sample of 93 evolved stars and nebulae in the mid-infrared using VISIR/VLT, T-Recs/Gemini South and Michelle/Gemini North. We found that all the the proto-planetary nebulae we resolved show a clear departure from spherical symmetry. 59 out of the 93 observed targets appear to be non resolved. The resolved targets can be divided in two categories. The nebulae with a dense central core, that are either bipolar and multipolar. The nebulae with no central core have an elliptical morphology. The dense central torus observed likely host binary systems which triggered fast outflows that shaped the nebulae. © 2012 International Astronomical Union.


Lagadec E.,European Southern Observatory | Verhoelst T.,Catholic University of Leuven | Mekarnia D.,French National Center for Scientific Research | Suarez O.,French National Center for Scientific Research | And 11 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2011

Post-asymptotic giant branch (post-AGB) stars are key objects for the study of the dramatic morphological changes of low- to intermediate-mass stars on their evolution from the AGB towards the planetary nebula stage. There is growing evidence that binary interaction processes may very well have a determining role in the shaping process of many objects, but so far direct evidence is still weak. We aim at a systematic study of the dust distribution around a large sample of post-AGB stars as a probe of the symmetry breaking in the nebulae around these systems. We used imaging in the mid-infrared to study the inner part of these evolved stars to probe direct emission from dusty structures in the core of post-AGB stars in order to better understand their shaping mechanisms. We imaged a sample of 93 evolved stars and nebulae in the mid-infrared using VLT spectrometer and imager for the mid-infrared (VISIR)/VLT, T-Recs/Gemini-South and Michelle/Gemini-North. We found that all the proto-planetary nebulae we resolved show a clear departure from spherical symmetry. 59 out of the 93 observed targets appear to be non-resolved. The resolved targets can be divided into two categories. (i) The nebulae with a dense central core, that are either bipolar and multipolar and (ii) the nebulae with no central core, with an elliptical morphology. The dense central torus observed likely hosts binary systems which triggered fast outflows that shaped the nebulae. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.


Molina-Cuberos G.J.,University of the Basque Country | Molina-Cuberos G.J.,Institute Astrofsica Of Andaluca | Godard R.,Royal Military College of Canada | Lopez-Moreno J.J.,Institute Astrofsica Of Andaluca | And 15 more authors.
Planetary and Space Science | Year: 2010

The Huygens Probe measured the electrical conductivity of Titan atmosphere from about 140 km down to the surface, employing relaxation and mutual impedance techniques. Previous analyses have shown some differences on the conductivity measurements obtained with two independent sensorsrelaxation probe (RP) and mutual impedance probe (MIP). A 20-fold maximum discrepancy occurred around the conductivity peak at 6070 km. To understand the nature of such discrepancy, we reassess the RP data by taking into account a geometrical factor related to the electrode finite size and the Debye length of the ionized medium. The present analysis implies replacing the standard Laplace field distribution by a more elaborated model considering the Poisson equation and the resistance between the RP electrodes and the medium. Although a complete understanding of the conductivity profile is still missing, this work brings RP and MIP data to a much better agreement. The conductivity maximum difference derived from the two sensors is now lower a factor of 2. This reassessment is also useful for future instruments and missions. © 2010 Elsevier Ltd. All rights reserved. All rights reserved.


Gonzalez-Galindo F.,Institute Astrofsica Of Andaluca | Gonzalez-Galindo F.,University Paris - Sud | Bougher S.W.,University of Michigan | Lopez-Valverde M.A.,Institute Astrofsica Of Andaluca | And 2 more authors.
Planetary and Space Science | Year: 2010

We have used two different General Circulation Models to study the thermal and wind structure of the Martian upper atmosphere (mesosphere and thermosphere). Both models take into account the effects of waves propagating from the lower atmosphere, although they use different methods for this purpose. We present the results of three simulations that allow us to take into account the seasonal variability of the Martian atmosphere. Simplified dust scenarios and a common set of input parameters are used. The temperatures and winds predicted by both models show an overall good agreement. However, some differences have been identified, generally of a local nature. The magnitude of these differences tends to increase with the amount of dust in the lower atmosphere. The different heating terms of the upper atmosphere predicted by both models are in good agreement, which suggests that the differences between the models have their origin in the propagation of waves from the lower atmosphere. This study has allowed us to confirm the important role of the redistribution of the energy by the winds in producing the longitudelatitude structure of the temperatures. Both models predict also a thermospheric polar warming during the Southern summer solstice, although its intensity seems to be model-dependent and connected to lower atmosphere dust loading. © 2010 Elsevier Ltd. All rights reserved. All rights reserved.


Funke B.,Institute Astrofsica Of Andaluca | Lpez-Puertas M.,Institute Astrofsica Of Andaluca | Bermejo-Pantalen D.,Institute Astrofsica Of Andaluca | Garca-Comas M.,Institute Astrofsica Of Andaluca | And 4 more authors.
Geophysical Research Letters | Year: 2010

We used temperature data from the Michelson Interferometer for Passive Atmospheric Sounding on board ESA's Envisat satellite to analyze the temperature responses in the mesosphere and thermosphere up to 170 km to a major stratospheric sudden warming (SSW) which occurred in January 2009. The temperature observations show clear signatures of a mesospheric cooling and a thermospheric warming, the latter peaking at 120-140 km in agreement with model predictions. From the analysis of the zonal temperature structure during the SSW a pronounced wave 1 pattern was found in the entire middle and upper polar atmosphere with maximum amplitudes around 50 and 140 km. In the mesosphere, the wave amplitude is significantly damped. The wave amplification above is most likely produced by in situ forced planetary waves in the mesosphere and lower thermosphere region. Our observations represent the first experimental evidence of a dynamical coupling of the lower atmosphere and the thermosphere in the 120-150 km range by means of satellite data. © 2010 by the American Geophysical Union.


Mayen-Gijon J.M.,Institute Astrofsica Of Andaluca | Anglada G.,Institute Astrofsica Of Andaluca | Osorio M.,Institute Astrofsica Of Andaluca | Rodrguez L.F.,National Autonomous University of Mexico | And 4 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2014

Although gravitational collapse is supposed to play an essential role in the star formation process, infall motions have been always elusive to detect. So far, only a few observational signatures have been commonly used to claim for the presence of infall. Often these features consist in either 'blue asymmetries' or absorption at redshifted velocities (e.g. inverse P Cygni profiles). Both signatures are based only on the shape of the line profile and they do not guarantee by themselves the presence of dominant infall motions. More robust 'mapping signatures' can be obtained from images that angularly resolve the infalling gas. Here we present Very Large Array observations of the ammonia inversion transitions (2,2), (3,3), (4,4), (5,5) and (6,6) towards the hot molecular core (HMC) near G31.41+0.31 that show the signatures of protostellar infall theoretically predicted by Anglada et al. The intensity of the ammonia emission is compact and sharply increases towards the centre in the blueshifted velocity channel maps, while it shows a more flattened distribution in the redshifted velocity channels. Additionally, the emission becomes more compact with increasing (relative) velocity for both red- and blueshifted channels. We introduce a new infall signature, the 'central blue spot', easily identifiable in the first-order moment maps. We show that rotation produces an additional, independent signature, making the distribution of the emission in the channel maps asymmetric with respect to the central position, but without masking the infall signatures. All these mapping signatures, which are identified here for the first time, are present in the observed ammonia transitions of G31 HMC. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

Loading Institute Astrofsica Of Andaluca collaborators
Loading Institute Astrofsica Of Andaluca collaborators