Response of "Bromus diandrus" populations from Castilla-León to sulfosulfuron and glyphosate

Se ha evaluado la respuesta de un total de 87 poblaciones de “Bromus diandrus” (bromo) recogidas en muestreos al azar realizados en campos de cereal de Castilla y León y de una población recogida en el INIA, a los herbicidas glifosato y sulfosulfuron, utilizados durante años para el control de bromo en trigo. Los ensayos se han realizado en invernadero con 3 dosis: control, la dosis de herbicida recomendada en la etiqueta del producto (20 g. m.a. ha-1 para sulfosulfuron y de 800 g. m.a. ha-1 para glifosato) y la mitad de la dosis recomendada, con 5 repeticiones por dosis y 100 semillas por repetición y población. No se encontraron poblaciones resistentes a las dosis recomendadas de ambos herbicidas, pero el 55% de las poblaciones mostraron cierta resistencia a sulfosulfuron y el 14% a glifosato.The response of 87 “B. diandrus” (ripgut brome) populations collected in cereal fields of Castilla-León and of one population collected in INIA (Madrid), to the herbicides glyphosate and sulfosulfuron, used for brome control in wheat during years, has been evaluated. The bioassays were conducted under greenhouse conditions with three doses: control, the recommended label herbicide dose (20 g m.a. ha-1 for sulfosulfuron and 800 g m.a. ha-1 for glyphosate) and half dose, with 5 replications per dose and 100 seeds per replication and population. Resistant populations were not found when the herbicide label dose was applied, but 55% of the populations showed certain resistance to sulfosulfuron and 14% to glyphosate

Response of populations of "Avena sterilis" from Castilla- León to herbicides used for its control

Se ha evaluado la respuesta en invernadero de 25 poblaciones de Avena sterilis L. recogidas en Castilla y León a los herbicidas inhibidores del enzima ACCasa (Acetil Coenzima A carboxilasa) clodinafop- propargil, diclofop-metil y tralkoxidim. Se han utilizado 2 dosis (la dosis recomendada en campo y la dosis doble) además de un control no tratado, con 3 repeticiones por dosis y 25 semillas por repetición. La dosis recomendada fue de 40,8 g. m.a. ha-1 para clodinafop, 900 g. m.a. ha-1 para diclofop y de 400 g. m.a. ha-1 para tralkoxidim. Todas las poblaciones muestreadas fueron susceptibles al herbicida tralkoxidim cuando se empleaba a la dosis recomendada. A pesar de que la mayoría de las poblaciones se clasificaron como sensibles en su respuesta a los herbicidas “fop” utilizados, se detectaron poblaciones que muestran cierto grado de resistencia a ambos herbicidas, en mayor medida al diclofop-metil.The response of 25 populations of Avena sterilis L. collected in Castilla-León to the ACCase (acetyl coenzyme A carboxylase) inhibiting herbicides clodinafop-propargyl, diclofop-methyl and tralkoxydim has been evaluated in the green-house. Two herbicide doses were used(the recommended field rate and the double rate) plus a non-treated control, with 3 replications per dose and 25 seeds per replication. The field rate was 40.8 g a.i. ha-1 for clodinafop, 900 g a.i. ha-1 for diclofop and 400 g a.i. ha-1 for tralkoxydim. All sampled populations were sensitive to tralkoxydim herbicide when used at the recommended field rate. Although most of the populations were classified as sensitive in the response to the used “fop” herbicides, populations showed some degree of resistance to both herbicides but in a greater extent to diclofop-methyl

Consistent accretion-induced heating of the neutron-star crust in MXB 1659-29 during two different outbursts

Monitoring the cooling of neutron-star crusts heated during accretion outbursts allows us to infer the physics of the dense matter present in the crust. We examine the crust cooling evolution of the low-mass X-ray binary MXB 1659-29 up to ~505 days after the end of its 2015 outburst (hereafter outburst II) and compare it with what we observed after its previous 1999 outburst (hereafter outburst I) using data obtained from the Swift, XMM-Newton, and Chandra observatories. The observed effective surface temperature of the neutron star in MXB 1659-29 dropped from ~92 eV to ~56 eV from ~12 days to ~505 days after the end of outburst II. The most recently performed observation after outburst II suggests that the crust is close to returning to thermal equilibrium with the core. We model the crust heating and cooling for both its outbursts collectively to understand the effect of parameters that may change for every outburst (e.g., the average accretion rate, the length of outburst, the envelope composition of the neutron star at the end of the outburst) and those which can be assumed to remain the same during these two outbursts (e.g., the neutron star mass, its radius). Our modelling indicates that all parameters were consistent between the two outbursts with no need for any significant changes. In particular, the strength and the depth of the shallow heating mechanism at work (in the crust) were inferred to be the same during both outbursts, contrary to what has been found when modelling the cooling curves after multiple outburst of another source, MAXI J0556-332. This difference in source behaviour is not understood. We discuss our results in the context of our current understanding of cooling of accretion-heated neutron-star crusts, and in particular with respect to the unexplained shallow heating mechanism.Comment: Submitted to A&A. The supplementary video can be found at https://www.youtube.com/watch?v=OpJ053zq9-

Weed control options in conventional and GM maize

En el proyecto AMIGA, que estudia los posibles efectos de los cultivos modificados genéticamente y su manejo sobre el agro-eco-sistema y la biodiversidad, se han evaluado varios tratamientos herbicidas sobre maíz Bt y maíz convencional. Se estableció un ensayo de seis hectáreas durante dos años en el que se han utilizado cinco manejos con herbicida que incluyen tratamiento convencional, reducido, glifosato y dos combinaciones de los anteriores. Se muestreó a lo largo del desarrollo del cultivo para determinar las especies de malas hierbas y artrópodos en el tiempo así como su abundancia y diversidad mediante examen visual y uso de trampas de gravedad y adhesivas amarillas. En este trabajo se presentan datos de abundancia de malas hierbas a madurez fisiológica del cultivo y del total de artrópodos en muestreo visual.Effect on weeds and arthropods In the context of AMIGA project which studies the posible effects of genetically modified crops and their management on the agro-ecosystem and biodiversity, we have studied various herbicide treatments applied on conventional and Bt A field was conducted for two years in a six ha plot. Five herbicide treatments including conventional, reduced, glyphosate and two herbicides combinations were established. We sampled along the cropping period to determine the species of weeds and arthropods over time and their abundance and diversity. The presence of arthropods was determined by visual examination and the use of pitfall and yellow sticky traps. In this work whole abundance of weeds at physiological maturity of the crop and total abundance of arthropod in visual examination are presented

An X-ray Census of Fast Radio Burst Host Galaxies: Constraints on AGN and X-ray Counterparts

We present the first X-ray census of fast radio burst (FRB) host galaxies to conduct the deepest search for AGN and X-ray counterparts to date. Our sample includes seven well-localized FRBs with unambiguous host associations and existing deep Chandra observations, including two events for which we present new observations. We find evidence for AGN in two FRB host galaxies based on the presence of X-ray emission coincident with their centers, including the detection of a luminous ($L_X \approx 5 \times 10^{42} \ \rm erg \ s^{-1}$) X-ray source at the nucleus of FRB20190608B's host, for which we infer an SMBH mass of $\rm M_{\rm BH} \sim 10^{8} \ M_{\odot}$ and an Eddington ratio $L_{\rm bol}/ L_{\rm Edd} \approx 0.02$, characteristic of geometrically thin disks in Seyfert galaxies. We also report nebular emission line fluxes for 24 highly secure FRB hosts (including 10 hosts for the first time), and assess their placement on a BPT diagram, finding that FRB hosts trace the underlying galaxy population. We further find that the hosts of repeating FRBs are not confined to the star-forming locus, contrary to previous findings. Finally, we place constraints on associated X-ray counterparts to FRBs in the context of ultraluminous X-ray sources (ULXs), and find that existing X-ray limits for FRBs rule out ULXs brighter than $L_X \gtrsim 10^{40} \ \rm erg \ s^{-1}$. Leveraging the CHIME/FRB catalog and existing ULX catalogs, we search for spatially coincident ULX-FRB pairs. We identify two ULX in the galaxy NGC 2633 that are spatially coincident with the repeating FRB20180908B and for which the DM-inferred redshift is comparable to the distance of the galaxy, assuming a $\rm DM_{host}$ contribution of $150 \ \rm pc \ cm^{-3}$.Comment: 15 pages, 5 figures; submitted to Ap

The Broad-band Counterpart of the Short GRB 200522A at z=0.5536z=0.5536:A Luminous Kilonova or a Collimated Outflow with a Reverse Shock?

We present the discovery of the radio afterglow and near-infrared (NIR) counterpart of the Swift short GRB 200522A, located at a small projected offset of $\approx 1$ kpc from the center of a young, star-forming host galaxy at $z=0.5536$. The radio and X-ray luminosities of the afterglow are consistent with those of on-axis cosmological short GRBs. The NIR counterpart, revealed by our HST observations at a rest-frame time of $\approx2.3$ days, has a luminosity of $\approx (1.3-1.7) \times 10^{42}$ erg s$^{-1}$. This is substantially lower than on-axis short GRB afterglow detections, but is a factor of $\approx 8$-$17$ more luminous than the kilonova of GW170817, and significantly more luminous than any kilonova candidate for which comparable observations exist. The combination of the counterpart's color ($i-y = -0.08\pm 0.21$; rest-frame) and luminosity cannot be explained by standard radioactive heating alone. We present two scenarios to interpret the broad-band behavior of GRB 200522A: a synchrotron forward shock with a luminous kilonova (potentially boosted by magnetar energy deposition), or forward and reverse shocks from a $\approx14^{\circ}$, relativistic ($\Gamma_0 \gtrsim 80$) jet. Models which include a combination of enhanced radioactive heating rates, low-lanthanide mass fractions, or additional sources of heating from late-time central engine activity may provide viable alternate explanations. If a stable magnetar was indeed produced in GRB 200522A, we predict that late-time radio emission will be detectable starting $\approx 0.3$-$6$ years after the burst for a deposited energy of $\approx 10^{53}$ erg. Counterparts of similar luminosity to GRB 200522A associated with gravitational wave events will be detectable with current optical searches to $\approx\!250$ Mpc.Comment: 33 pages, 13 figures, 5 tables. Submitted to AAS Journal

Unveiling the origin of the optical and UV emission during the 2017 giant outburst of the Galactic ULX pulsar Swift J0243.6+6124

Context. From late September 2017 to January 2018, the Be X-ray binary (BeXB) Swift J0243.6+6124 underwent a giant outburst that was unprecedently bright. The reported X-ray luminosities were so high that the system was classified as an ultraluminous X-ray source (ULX). It was also the first BeXB pulsar to show radio jet emission. The source was not only bright in X-rays and radio, but also in the optical and ultraviolet (UV) wavelenghts as well. Aims. In this work, we aim to understand the origin of the observed optical/UV fluxes simultaneous to the X-ray emission. Methods. We studied the optical/UV light curves in comparison with the X-ray fluxes along the outburst. We considered the main mechanisms that can explain the optical/UV emission in X-ray binaries. Due to the tight correlation observed between the optical/UV and X-ray light curves, reprocessing of X-rays seems to be the most plausible explanation. We calculated the timescales of the light curve decays and studied the correlation indexes between the optical and X-ray emission. Finally, we built a physical model that considers the X-ray heating of the surface of the donor star, irradiation of the accretion disk, and emission from a viscously heated accretion disk, so that we could reproduce the observed optical/UV spectral energy distributions (SEDs) along the outburst. In our model, we considered the Be circumstellar disk to be co-planar to the orbit and then we neglected its irradiation in the current model. As an input for the model, we used as incident X-ray luminosities those calculated from the bolometric X-ray fluxes obtained from the spectral fit of the Swift/XRT and BAT observations. Results. The timescales of the exponential decay of the outburst are between two and four times longer for the UV and optical light curves than for the X-ray light curve. The correlation index between the optical/UV and X-ray fluxes varies between optical/UV filters and when different X-ray bands are considered and is larger for the rise than for the decay phase of the outburst for the fluxes at redder wavelengths. The modelling of the SED shows that X-ray heating of the companion star surface is the main mechanism contributing to the UV emission and contributes significantly to the optical emission during the whole outburst. The X-ray irradiation of the accretion disk is necessary to reproduce the optical observed fluxes from MJD 58047 to 58120 and contributes significantly to the UV fluxes close to the peak of the outburst. As a first attempt, the fits yield an increasing value of the outer radius of the accretion disk along the outburst. An alternative interpretation points to variations in the geometry of the inner flow and the fraction of reprocessed X-ray emission during the outburst. On the other hand, variations in the geometry of the Be circumstellar disk could also play a role, but they have not been considered in the current model. Conclusions. Reprocessing of X-rays via the X-ray heating of the Be star surface and as irradiation of the accretion disk is the main mechanism that can reproduce the observed optical/UV emission during the 2017−2018 giant outburst of Swift J0243.6+6124

Mapping Obscured Star Formation in the Host Galaxy of FRB 20201124A

We present high-resolution 1.5--6 GHz Karl G. Jansky Very Large Array (VLA) and $\textit{Hubble Space Telescope}$ ($\textit{HST}$) optical and infrared observations of the extremely active repeating fast radio burst (FRB) FRB$\,$20201124A and its barred spiral host galaxy. We constrain the location and morphology of star formation in the host and search for a persistent radio source (PRS) coincident with FRB$\,$20201124A. We resolve the morphology of the radio emission across all frequency bands and measure a star formation rate SFR $\approx 8.9\,M_{\odot}$ yr$^{-1}$, a factor of $\approx 4-6$ larger than optically-inferred SFRs, demonstrating dust-obscured star formation throughout the host. Compared to a sample of all known FRB hosts with radio emission, the host of FRB$\,$20201124A has the most significant obscured star formation. While ${\it HST}$ observations show the FRB to be offset from the bar or spiral arms, the radio emission extends to the FRB location. We propose that the FRB progenitor could have formed $\textit{in situ}$ (e.g., a magnetar central engine born from the explosion of a massive star). It is still plausible, although less likely, that the progenitor of FRB$\,$20201124A migrated from the central bar of the host, e.g., via a runaway massive star. We further place a limit on the luminosity of a putative PRS at the FRB position of $L_{\rm 6.0 \ GHz}$$\lesssim$2.6$\times$$10^{27}$erg s$^{-1}$Hz$^{-1}$, two orders of magnitude below any PRS known to date. However, this limit is still broadly consistent with both magnetar nebulae and hypernebulae models assuming a constant energy injection rate of the magnetar and an age of$\gtrsim 10^{5}$ yr in each model, respectively.Comment: 21 pages, 6 figures, 3 tables, Submitte

A Radio Flare in the Long-Lived Afterglow of the Distant Short GRB 210726A: Energy Injection or a Reverse Shock from Shell Collisions?

We present the discovery of the radio afterglow of the short $\gamma$-ray burst (GRB) 210726A, localized to a galaxy at a photometric redshift of $z\sim 2.4$. While radio observations commenced $\lesssim 1~$day after the burst, no radio emission was detected until $\sim11$~days. The radio afterglow subsequently brightened by a factor of $\sim 3$ in the span of a week, followed by a rapid decay (a ``radio flare''). We find that a forward shock afterglow model cannot self-consistently describe the multi-wavelength X-ray and radio data, and underpredicts the flux of the radio flare by a factor of $\approx 5$. We find that the addition of substantial energy injection, which increases the isotropic kinetic energy of the burst by a factor of $\approx 4$, or a reverse shock from a shell collision are viable solutions to match the broad-band behavior. At $z\sim 2.4$, GRB\,210726A is among the highest redshift short GRBs discovered to date as well as the most luminous in radio and X-rays. Combining and comparing all previous radio afterglow observations of short GRBs, we find that the majority of published radio searches conclude by $\lesssim 10~$days after the burst, potentially missing these late rising, luminous radio afterglows.Comment: 28 pages, 10 figures, submitted to Ap