Atmospheric turbulence in phase-referenced and wide-field interferometric images: Application to the SKA

Phase referencing is a standard calibration procedure in radio interferometry. It allows to detect weak sources by using quasi-simultaneous observations of closeby sources acting as calibrators. Therefore, it is assumed that, for each antenna, the optical paths of the signals from both sources are similar. However, atmospheric turbulence may introduce strong differences in the optical paths of the signals and affect, or even waste, phase referencing for cases of relatively large calibrator-to-target separations and/or bad weather. The situation is similar in wide-field observations, since the random deformations of the images, mostly caused by atmospheric turbulence, have essentially the same origin as the random astrometric variations of phase-referenced sources with respect to the phase center of their calibrators. In this paper, we present the results of a Monte Carlo study of the astrometric precision and sensitivity of an interferometric array (a realization of the Square Kilometre Array, SKA) in phase-referenced and wide-field observations. These simulations can be extrapolated to other arrays by applying the corresponding corrections. We consider several effects from the turbulent atmosphere (i.e., ionosphere and wet component of the troposphere) and also from the antenna receivers. We study the changes in dynamic range and astrometric precision as a function of observing frequency, source separation, and strength of the turbulence. We find that, for frequencies between 1 and 10 GHz, it is possible to obtain images with high fidelity, although the atmosphere strongly limits the sensitivity of the instrument compared to the case with no atmosphere. Outside this frequency window, the dynamic range of the images and the accuracy of the source positions decrease. [...] (Incomplete abstract. Please read manuscript.)Comment: 9 pages, 11 figures. Accepted for publication in A&A

The resolved structure of the extragalactic supernova remnant SNR 4449-1

We present very long baseline interferometry (VLBI) observations of the milliarcsecond-scale radio structure of the supernova remnant SNR 4449$-$1 in the galaxy NGC 4449. This young and superluminous remnant was observed at 1.6 GHz ($\lambda = 18$\,cm) with the European VLBI Network. The observations confirm earlier identifications of this object with a supernova remnant (SNR) while revealing a somewhat different morphology compared with the structure reported by Bietenholz et al. from VLBI observations at 1.4 GHz. This difference is discussed here in the context of structural sensitivity of both observations. The 1.6 GHz image yields accurate estimates of the size (0.0422 arcsec $\times$ 0.0285 arcsec and 0.8 $\times$ 0.5 pc) and age ($\sim$55 yr) of SNR 4449$-$1. With a total flux of 6.1 $\pm$ 0.6 mJy measured in the VLBI image, the historical lightcurve of the source can be well represented by a power-law decay with a power index of $-$1.19 $\pm$ 0.07. The SNR exhibits a decline rate of the radio emission of 2.2$$ $\pm$ 0.1$$ yr$^{-1}$ and a radio luminosity of 1.74 $\times$ 10$^{35}$ erg s$^{-1}$.Comment: 7 pages, 6 figures, MNRAS preprint, arXiv:1309.401

Optimum estimate of delays and dispersive effects in low-frequency interferometric observations

Modern radio interferometers sensitive to low frequencies will make use of wide-band detectors. For such wide bandwidths, dispersive atmospheric effects introduce variations in the fringe delay which change through the band of the receivers. These undesired dispersive effects must be estimated and calibrated with the highest precision. We studied the achievable precision in the estimate of the ionospheric dispersion and the dynamic range of the correlated fringes for different distributions of sub-bands in low-frequency and wide-band interferometric observations. Our study is focused on the case of sub-bands with a bandwidth much narrower than that of the total covered spectrum (case of LOFAR). We computed the uncertainty of the ionospheric delay, the delay ambiguity, and the dynamic range of the fringes using four different kinds of sub-band distributions: constant spacing between sub-bands, random spacings, spacings based on a power-law distribution, and spacings based on Golomb rulers (sets of integers whose sets of differences have non-repeated elements). For a large number of sub-bands ($> 20$, depending on the delay window) spacings based on Golomb rulers give the most precise estimates of dispersive effects and the highest fringe dynamic ranges. Spacings based on the power-law distribution give similar results, although better than those with the Golomb rulers for smaller number of sub-bands. Random distributions result in large fringe dynamic ranges, but the estimate of dispersive effects is worse. A constant spacing of sub-bands results in very bad fringe dynamic ranges, but good estimates of ionospheric dispersion. Combining all the results, the power-law distribution gives the best compromise between homogeneity in the bandwidth sampling, precision in the estimate of ionospheric effects, dynamic range of the correlated fringes, and group-delay ambiguity.Comment: 8 pages, 7 figures. Accepted for publication in A&

VLBI observations of SN2011dh: imaging of the youngest radio supernova

We report on the VLBI detection of supernova SN2011dh at 22GHz using a subset of the EVN array. The observations took place 14 days after the discovery of the supernova, thus resulting in a VLBI image of the youngest radio-loud supernova ever. We provide revised coordinates for the supernova with milli-arcsecond precision, linked to the ICRF. The recovered flux density is a factor 2 below the EVLA flux density reported by other authors at the same frequency and epoch of our observations. This discrepancy could be due to extended emission detected with the EVLA or to calibration problems in the VLBI and/or EVLA observations.Comment: Letter. Accepted in A&

Els conflictes de la conca del riu Tordera

Acompanyat del vídeo "La conca de la Tordera", disponible a: http://upcommons.upc.edu/video/handle/2099.2/936La conca de la Tordera des de fa temps ha patit tots els impactes: sobreexplotació dels aqüífers, contaminació, salinització des pous, regressió dels deltes, ocupació de la llera per indústries, habitatges i infrastructures, etc.. Per tot això és interessant estudiar la conca de la Tordera, una conca molt degradada per la pressió antròpica, i que actualment està fent grans esforços per tal d’intentar recuperar-la

Radio emission of SN1993J. The complete picture: II. Simultaneous fit of expansion and radio light curves

We report on a simultaneous modelling of the expansion and radio light curves of SN1993J. We have developed a simulation code capable of generating synthetic expansion and radio light curves of supernovae by taking into consideration the evolution of the expanding shock, magnetic fields, and relativistic electrons, as well as the finite sensitivity of the interferometric arrays used in the observations. Our software successfully fits all the available radio data of SN 1993J with an standard emission model for supernovae extended with some physical considerations, as an evolution in the opacity of the ejecta material, a radial drop of the magnetic fields inside the radiating region, and a changing radial density profile of the circumstellar medium beyond day 3100 after explosion.Comment: 12 pages, 12 figures, accepted for publication in A&

rPICARD: A CASA-based Calibration Pipeline for VLBI Data

Currently, HOPS and AIPS are the primary choices for the time-consuming process of (millimeter) Very Long Baseline Interferometry (VLBI) data calibration. However, for a full end-to-end pipeline, they either lack the ability to perform easily scriptable incremental calibration or do not provide full control over the workflow with the ability to manipulate and edit calibration solutions directly. The Common Astronomy Software Application (CASA) offers all these abilities, together with a secure development future and an intuitive Python interface, which is very attractive for young radio astronomers. Inspired by the recent addition of a global fringe-fitter, the capability to convert FITS-IDI files to measurement sets, and amplitude calibration routines based on ANTAB metadata, we have developed the the CASA-based Radboud PIpeline for the Calibration of high Angular Resolution Data (rPICARD). The pipeline will be able to handle data from multiple arrays: EHT, GMVA, VLBA and the EVN in the first release. Polarization and phase-referencing calibration are supported and a spectral line mode will be added in the future. The large bandwidths of future radio observatories ask for a scalable reduction software. Within CASA, a message passing interface (MPI) implementation is used for parallelization, reducing the total time needed for processing. The most significant gain is obtained for the time-consuming fringe-fitting task where each scan be processed in parallel.Comment: 6 pages, 1 figure, EVN 2018 symposium proceeding

Spurious source generation in mapping from noisy phase-self-calibrated data

Phase self-calibration (or selfcal) is an algorithm often used in the calibration of interferometric observations in astronomy. Although a powerful tool, this algorithm presents strong limitations when applied to data with a low signal-to-noise ratio. We analyze the artifacts that the phase selfcal algorithm produces when applied to extremely noisy data. We show how the phase selfcal may generate a spurious source in the sky from a distribution of completely random visibilities. This spurious source is indistinguishable from a real one. We numerically and analytically compute the relationship between the maximum spurious flux density generated by selfcal from noise and the particulars of the interferometric observations. Finally, we present two simple tests that can be applied to interferometric data for checking whether a source detection is real or whether the source is an artifact of the phase self-calibration algorithm.Comment: 7 pages, 2 figures. Accepted in A&A on 12 December 200

Aportació a la flora micològica del Parc Nacional d'Ordesa i Monte Perdido (Pirineus Centrals)

Presentem un catàleg florístic de les espècies recol·lectades en el curs d'una exploració de l Parc Nacional d'Ordesa i Monte Perdido (Pirineus centrals) a la tardor de 1989, en el qual comentem i Il·lust rem les que considerem més interessants, com són Lentinus adhaerens (A. et S. : Fr.) Fr., Naucoria permixta P. D. Orton, Tephrocybe baeosperma (Romagn.) Moser i Xeromphalina cornui (Quél.) Favre.Contribution to the fungus flora or the National Park or Ordesa and Monte Perdido (Central Pyrenean range, NE Spain). This work is a florístic catalogue of the fungi collected during an exploration of rhe National Park of Ordesa and Monte Perdido, in the fall of 1989. Commentaries and iconography are provided in the case or int eresting species, such as Lentinus adhaerens (A. et S. : Fr.) Fr., Naucoria permixta P. D. Orton, Tephrocybe baeosperma (Romagn.) Moser and Xeromphalina cornui (Quél.) Favre

Aportació a la flora micològica del Parc Nacional d'Ordesa i Monte Perdido (Pirineus Centrals)

Presentem un catàleg florístic de les espècies recol·lectades en el curs d'una exploració de l Parc Nacional d'Ordesa i Monte Perdido (Pirineus centrals) a la tardor de 1989, en el qual comentem i Il·lust rem les que considerem més interessants, com són Lentinus adhaerens (A. et S. : Fr.) Fr., Naucoria permixta P. D. Orton, Tephrocybe baeosperma (Romagn.) Moser i Xeromphalina cornui (Quél.) Favre.Contribution to the fungus flora or the National Park or Ordesa and Monte Perdido (Central Pyrenean range, NE Spain). This work is a florístic catalogue of the fungi collected during an exploration of rhe National Park of Ordesa and Monte Perdido, in the fall of 1989. Commentaries and iconography are provided in the case or int eresting species, such as Lentinus adhaerens (A. et S. : Fr.) Fr., Naucoria permixta P. D. Orton, Tephrocybe baeosperma (Romagn.) Moser and Xeromphalina cornui (Quél.) Favre