X-ray observations of the unique NLS1 galaxy Mrk 1239 spanning 18 yr are presented. Data from XMM-Newton, Suzaku, Swift, and NuSTAR are combined to obtain a broadband, multi-epoch view of the source. There is spectral variability in the 3–10 keV band over the 18 yr. An analysis of the NuSTAR and Suzaku lightcurves also suggests rapid variability in the 3–10  keV band, which is consistent with the NLS1 definition of the source. However, no variability is seen below 3 keV on any timescale. Two distinct physical models are adopted to describe the data above and below . The low energies are dominated by a hot, diffuse gas likely associated with a starburst component at large physical scales. The higher-energy spectrum is dominated by emission from the central region. Ionized partial covering and relativistic blurred reflection are considered for the central region emission. In both cases, the underlying power law has a photon index of Γ ∼ 2.3–2.4. A distant reflector, a neutral partial covering component with a covering fraction near ∼1, and contributions from starburst emission are always required. The blurred reflection model requires a reflection-dominated spectrum, which may be at odds with the low emissivity index and radio properties of the source. By contrast, the two absorption components required in the ionized partial covering model may correspond to the two distinct regions of polarization observed in the optical. Regardless of the physical model, spectral changes between epochs are driven by the absorption components—and on short timescales, by intrinsic active galactic nucleus variability.

Magnesium aluminum-layered double-hydroxide nanoparticles (LDH NPs) are promising drug-delivery vehicles for gene therapy, particularly for siRNA interference; however, the interactions between oligo-DNA and LDH surfaces have not been adequately elucidated. Through a mechanistic study, oligo-DNA initially appears to rapidly bind strongly to the LDH outer surfaces through interactions with their phosphate backbones via ligand exchange with OH on Mg centers and electrostatic forces with Al. These initial interactions might precede diffusion into interlayer spaces, and this knowledge can be used to design better gene therapy delivery systems.

Mrk 1239 is a highly polarized NLS1 in the optical band, whose 0.3 − 3 keV spectrum has remained remarkably consistent over more than two decades of observation. Previous analysis of this object suggested that the soft X-ray band was dominated by emission lines (collisionally and/or photoionized) from the distant host galaxy as the X-ray emission from the central engine was highly obscured. New XMM-Newton data of Mrk 1239 are presented here to investigate the soft X-ray band of this galaxy with high resolution. The first RGS spectra of this source reveal a plethora of ionized emission lines originating from two distinct plasmas, one collisionally ionized and the other photoionized at approximately equal brightness. The best fit model uses apec and xstar grids to account for the collisionally ionized and photoionized components, respectively. The fit improves significantly if the photoionized material is allowed to outflow at ≈500 km s−1, matching the outflow velocity of the forbidden O vii emission line. From constraints on the ionization and density of the photoionized material we can estimate the location of it to be no further than a few pc from the central source, around the outer radius of the torus, which is consistent with the O vii(f) emission line. Properties of the collisionally ionized plasma are consistent with star formation rate (SFR) of $\approx 3 \hbox{$\rm \, M_{\odot }$}\textrm {yr}^{-1}$, which is comparable with several previous measurements of the SFR in this galaxy.

Mrk 1239 is a highly polarized NLS1 in the optical band, whose 0.3 − 3 keV spectrum has remained remarkably consistent over more than two decades of observation. Previous analysis of this object suggested that the soft X-ray band was dominated by emission lines (collisionally and/or photoionized) from the distant host galaxy as the X-ray emission from the central engine was highly obscured. New XMM-Newton data of Mrk 1239 are presented here to investigate the soft X-ray band of this galaxy with high resolution. The first RGS spectra of this source reveal a plethora of ionized emission lines originating from two distinct plasmas, one collisionally ionized and the other photoionized at approximately equal brightness. The best fit model uses and grids to account for the collisionally ionized and photoionized components, respectively. The fit improves significantly if the photoionized material is allowed to outflow at ≈ 500 km s −1 , matching the outflow velocity of the forbidden O emission line. From constraints on the ionization and density of the photoionized material we can estimate the location of it to be no further than a few pc from the central source, around the outer radius of the torus, which is consistent with the O ( 𝑓 ) emission line. Properties of the collisionally ionized plasma are consistent with star formation rate (SFR) of ≈ 3 M yr −1 , which is comparable with several previous measurements of the SFR in this galaxy.

Understanding if and when the accretion disc extends down to the innermost stable circular orbit (ISCO) is important since it is the fundamental assumption behind measuring black hole spin. Here, we examine the 2013 and 2018 NuSTAR and Swift data (0.5 − 50 keV) of the narrow-line Seyfert 1 galaxy, WKK 4438. The X-ray emission can be fitted well with models depicting a corona and blurred reflection originating from a disc around a low spin (a* ≈ 0) black hole. However, such models result in unconventional values for some of the parameters (e.g. inverted emissivity profile and high coronal height). Alternatively, equally good fits can be achieved if the disc is truncated at ∼10 rg and the black hole is spinning at the Thorne limit (a* = 0.998). In these cases, the model parameters are consistent with the interpretation that the corona is centrally located close to the black hole and illuminating the disc at a larger distance.