We present a two month Suzaku X-ray monitoring of the Seyfert 1 galaxy NGC 5548. The campaign consists of 7 observations (with exposure time ∼ 30 ks each), separated by ∼1 week. This paper focus on the XIS data of NGC 5548. We analyze the response in the opacity of the gas that forms the well known ionized absorber in this source to ionizing flux variations. Despite variations by a factor ∼ 4 in the impinging continuum, the soft X-ray spectra of the source show little spectral variations, suggesting no response from the ionized absorber. A detailed time modeling of the spectra confirms the lack of opacity variations for an absorbing component with high ionization (U X ≈ −0.85), and high outflow velocity (v out ≈ 1040 km s −1 ), as the ionization parameter was found to be consistent with a constant value during the whole campaign. Instead, the models suggest that the ionization parameter of a low ionization (U X ≈ −2.8), low velocity (v out ≈ 590 km s −1 ) absorbing component might be changing linearly with the ionizing flux, as expected for gas in photoionization equilibrium.-2 -However, given the lack of spectral variations among observations, we consider the variations in this component as tentative. Using the lack of variations, we set an upper limit of n e <2.0×10 7 cm −3 for the electron density of the gas forming the high ionization, high velocity component. This implies a large distance from the continuum source (R > 0.033 pc; R > 5000 R S ). If the variations in the low ionization, low velocity component are real, they imply n e >9.8×10 4 cm −3 and R < 3 pc. We discuss our results in terms of two different scenarios: a large scale outflow originating in the inner parts of the accretion disk, or a thermally driven wind originating much farther out. Given the large distance of the wind, the implied mass outflow rate is also large (Ṁ w > 0.08Ṁ accr ) (the mass outflow is dominated by the high ionization component). The associated total kinetic energy deployed by the wind in the host galaxy (> 1.2 × 10 56 erg) can be enough to disrupt the interstellar medium, possibly quenching or regulating large scale star formation. However, the total mass and energy ejected by the wind may still be lower than the one required for cosmic feedback, even when extrapolated to quasar luminosities. Such feedback would require that we are observing the wind before it is fully accelerated.

We present an analysis of a new XMM-Newton observation of the Seyfert 1 Galaxy NGC 985. The EPIC spectra present strong residuals to a single powerlaw model, indicating the presence of ionized absorbing gas and a soft excess. A broad-band fit to the EPIC and RGS spectra shows that the continuum can be well fit with a power-law (Γ ≈ 1.57) and a blackbody component (kT ≈ 0.09 keV). The RGS can be modeled either with two or three absorption components.In the two absorber model the low-ionization one, with logU≈ .05 and logN H ≈ 21.08 accounts for the presence of the Fe M-shell unresolved transition array (Fe VII-XIII), and the high ionization component (logU≈ 1.31 and logN H ≈ 21.99) is required by the presence of several Fe L-shell transitions. The data suggest the presence of a third ionized component with higher ionization, so that the Fe L-shell absorption features are produced by two different components (one producing absorption by Fe XVII-XX, and the other absorption by Fe XX-XXII). However, the presence of the third absorbing component cannot be detected by means of an isolated absorption line in a significant way, so we consider this detection only as tentative. Interestingly, all ionization components have similar kinematics (with outflow velocities ∼ 280 km s −1 ). In addition, whether two or three absorbers are considered, the components appear to be in pressure balance within 1σ. These results give further support to the idea that warm absorbers

We present an analysis of X-ray high quality grating spectra of the Seyfert 1 galaxy NGC 5548 using archival Chandra-HETGS and LETGS observations for a total exposure time of 800 ks. The continuum emission (between 0.2-8 keV) is well represented by a power law (Γ = 1.6) plus a black-body component (kT = 0.1 keV). We find that the well known X-ray warm absorber in this source consists of two different outflow velocity systems. One absorbing system has a velocity of -1110 ± 150 km s −1 and the other of -490 ± 150 km s −1 . Recognizing the presence of these kinematically distinct components allows each system to be fitted independently, each with two absorption components with different ionization levels. The high velocity system consists of a component with temperature of 2.7 ± 0.6 × 10 6 K, log U = 1.23 and another component with temperature of 5.8 ± 1.0 × 10 5 K, log U = 0.67. The high-velocity, high-ionization component produces absorption by charge states Fe xxi-xxiv, while the high-velocity, lowionization component produces absorption by Ne ix-x, Fe xvii-xx, O vii-viii. The low-velocity system required also two absorbing components, one with temperature of 5.8 ± 0.8 × 10 5 K, log U = 0.67, producing absorption by Ne ix-x, Fe xvii-xx, O vii-viii. The other with lower temperature (3.5 ± 0.35 × 10 4 K), and lower ionization (log U = −0.49); producing absorption by O vi-vii and the Fe vii-xii M-shell UTA. Once these components are considered, the data do not require any further absorbers. In particular, a model consisting of a continuous radial range of ionization structures (as suggested by a previous analysis) is not required.

This study analyzed climate change scenarios and their potential impact on water availability for the South-Southeast region (SSR) of Mexico. Precipitation patterns were examined using the Standardized Precipitation Index for three emissions scenarios, Representative Concentration Pathway (RCP) 4.5, RCP 6.0, and RCP 8.5, during the periods of 1960-2016, 2015-2039 (near future), and 2075-2099 (far future). Historical changes in precipitation in the SSR indicated the presence of dry and wet events driven by El Niño-Southern Oscillation, the Pacific Decadal Oscillation, and the Atlantic Multidecadal Oscillation, which are the regional climate modulators. However, the impact of these phases has not been quantified for the future. The results of our climate change projections show that the Grijalva and Usumacinta rivers and surrounding regions (Chiapas and Tabasco) will have an increase in the percentage of dry and wet events in the near future (2015-2039), while there is a medium to low probability of this occurrence in rest of the SSR. By 2075-2099, Grijalva and Usumacinta will continue to have a high probability of dry events due to climate change, and the Yucatan will also exhibit this behavior. RCP 4.5 was projected to be the wettest scenario for the study area, while RCP 8.5 projected an increase in dry events in the area during both periods (2015-2039 and 2075-2099). RCP 6.0 projected a drier 2015-2039 and wetter 2075-2099.

Precipitation patterns in Usumacinta and Grijalva basins (southern Mexico) under a changing climate.