[en] Texaphyrins are expanded porphyrin macrocycles that selectively localize and are retained in cancerous lesions. The function of the texaphyrin can be manipulated by the incorporation of different metal ions into the macrocycle's central cavity. Gadolinium texaphyrin (Gd-Tex) and lutetium texaphyrin (Lu-Tex) were evaluated as radiation sensitizers. Radiation sensitization studies were performed using SMT-F and EMT6 mammary tumor-bearing mice. Single and multifraction dose regimens were performed. SMT-F bearing DBA/2N mice and EMT6 bearing Balb/c mice were intravenously administered with Gd-Tex of Lu-Tex (5-40 μmol/kg) 30 minutes to 5 hours prior to radiation (10-50 Gray) for the single fraction studies. The more radioresistant EMT-6 sarcoma model was used for the multifraction studies. The tumor bearing animals were injected with Gd-Tex (5, 20, or 40 μmol/kg) to 2 hours prior radiation (1, 2, or 4 Gray), this regimen was performed for five consecutive days. Gd-Tex is paramagnetic and has a strong fluorescence signal. Tumor selectivity was determined by MRI and fluorescence spectral imaging before and up to 24 hours following the administration of Gd-Tex. Gd-Tex but not Lu-Tex, proved to be an effective radiation sensitizer. Administration of Gd-Tex (40 μmol/kg) prior to a single dose of 30 Gray radiation provided a significant improvement in survival in SMT-F-bearing DBA/2N mice as compared to animals receiving radiation alone (p = 0.0034). A significant radiation sensitization effect was also found in multiple fraction studies (five consecutive days) with Balb/C mice bearing EMT-6 neoplasma-- following 1 Gray of radiation for 5 days there was a significant difference between the 20 and 40 μmol/kg group and controls (p = 0.003, p = 0.005 respectively). MRI and fluorescence spectral imaging studies of tumor bearing animals revealed excellent contrast enhancement of the tumor which persisted up to 24 hours. Texaphyrins localize in neoplasms as visualized using MRI or fluorescence imaging. The paramagnetic Gd-Tex is an effective radiosensitizer that is detectable by both MRI and fluorescence imaging. Lu-Tex did not appear to be a radiation sensitizer in these studies. Gd-Tex is presently being evaluated in clinical trials as a radiation sensitizer

[en] We report spectropolarimetric observations of the quasar E1821+643 (z = 0.297), which suggest that it may be an example of gravitational recoil due to anisotropic emission of gravitational waves following the merger of a supermassive black hole (SMBH) binary. In total flux, the broad Balmer lines are redshifted by ∼1000 km s^-1 relative to the narrow lines and have highly red asymmetric profiles, whereas in polarized flux the broad Hα line exhibits a blueshift of similar magnitude and a strong blue asymmetry. We show that these observations are consistent with a scattering model in which the broad-line region has two components, moving with different bulk velocities away from the observer and toward a scattering region at rest in the host galaxy. If the high-velocity system is identified as gas bound to the SMBH, this implies that the SMBH is itself moving with a velocity ∼2100 km s^-1 relative to the host galaxy. We discuss some implications of the recoil hypothesis and also briefly consider whether our observations can be explained in terms of scattering of broad-line emission originating from the active component of an SMBH binary, or from an outflowing wind.

[en] We used the CLUMPY torus models and a Bayesian approach to fit the infrared spectral energy distributions and ground-based high angular resolution mid-infrared spectroscopy of 13 nearby Seyfert galaxies. This allowed us to put tight constraints on torus model parameters such as the viewing angle i, the radial thickness of the torus Y, the angular size of the cloud distribution σ_torus, and the average number of clouds along radial equatorial rays N₀. We found that the viewing angle i is not the only parameter controlling the classification of a galaxy into type 1 or type 2. In principle, type 2s could be viewed at any viewing angle i as long as there is one cloud along the line of sight. A more relevant quantity for clumpy media is the probability for an active galactic nucleus (AGN) photon to escape unabsorbed. In our sample, type 1s have relatively high escape probabilities, P_esc ∼ 12%-44%, while type 2s, as expected, tend to have very low escape probabilities. Our fits also confirmed that the tori of Seyfert galaxies are compact with torus model radii in the range 1-6 pc. The scaling of the models to the data also provided the AGN bolometric luminosities L_bol(AGN), which were found to be in good agreement with estimates from the literature. When we combined our sample of Seyfert galaxies with a sample of PG quasars from the literature to span a range of L_bol(AGN) ∼ 10⁴³-10⁴⁷ erg s^-1, we found plausible evidence of the receding torus. That is, there is a tendency for the torus geometrical covering factor to be lower (f₂ ∼ 0.1-0.3) at high AGN luminosities than at low AGN luminosities (f₂ ∼ 0.9-1 at ∼10⁴³-10⁴⁴ erg s^-1). This is because at low AGN luminosities the tori appear to have wider angular sizes (larger σ_torus) and more clouds along radial equatorial rays. We cannot, however, rule out the possibility that this is due to contamination by extended dust structures not associated with the dusty torus at low AGN luminosities, since most of these in our sample are hosted in highly inclined galaxies.