The MBH - σ⋆ relation is considered a result of co-evolution between the host galaxies and their super-massive black holes. For elliptical-bulge hosting inactive galaxies, this relation is well ...established, but there is still a debate whether active galaxies follow the same relation. In this paper, we estimate black hole masses for a sample of 19 local luminous AGNs (LLAMA) in order to test their location on the MBH - σ⋆ relation. Super-massive black hole masses (MBH) were derived from the broad-line based relations for Hα, Hβ and Paβ emission line profiles for the Type 1 AGNs. We compare the bulge stellar velocity dispersion (σ⋆) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We apply an extinction correction to the observed broad line fluxes and we correct the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. The Hα-based black hole masses of our sample of AGNs were estimated in the range 6.34 ≤ logMBH ≤ 7.75 M⊙ and the σ⋆CaT estimates range between 73 ≤ σ⋆CaT ≤ 227 km s−1. From the so-constructed MBH - σ⋆ relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample. In conclusion, we find that our sample of local luminous AGNs is consistent with the MBH - σ⋆ relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion.
The \(M_{BH}\) - \(\sigma_{\star}\) relation is considered a result of co-evolution between the host galaxies and their super-massive black holes. For elliptical-bulge hosting inactive galaxies, this ...relation is well established, but there is still a debate whether active galaxies follow the same relation. In this paper, we estimate black hole masses for a sample of 19 local luminous AGNs (LLAMA) in order to test their location on the \(M_{BH}\) - \(\sigma_{\star}\) relation. Super-massive black hole masses (\(M_{BH}\)) were derived from the broad-line based relations for H\(\alpha\), H\(\beta\) and Pa\(\beta\) emission line profiles for the Type 1 AGNs. We compare the bulge stellar velocity dispersion (\(\sigma_{\star}\)) as determined from the Ca II triplet (CaT) with the dispersion measured from the near-infrared CO (2-0) absorption features for each AGN and find them to be consistent with each other. We apply an extinction correction to the observed broad line fluxes and we correct the stellar velocity dispersion by an average rotation contribution as determined from spatially resolved stellar kinematic maps. The H\(\alpha\)-based black hole masses of our sample of AGNs were estimated in the range 6.34 \(\leq\) \(\log{M_{BH}}\) \(\leq\) 7.75 M\(_\odot\) and the \(\sigma_{\star CaT}\) estimates range between 73 \(\leq\) \(\sigma_{\star CaT}\) \(\leq\) 227 km s\(^{-1}\). From the so-constructed \(M_{BH}\) - \(\sigma_{\star}\) relation for our Type 1 AGNs, we estimate the black hole masses for the Type 2 AGNs and the inactive galaxies in our sample. In conclusion, we find that our sample of local luminous AGNs is consistent with the \(M_{BH}\) - \(\sigma_{\star}\) relation of lower luminosity AGNs and inactive galaxies, after correcting for dust extinction and the rotational contribution to the stellar velocity dispersion.
We observed the nuclear region of the galaxy NGC 1365 with the integral field unit of the Gemini Multi Object Spectrograph mounted on the GEMINI-South telescope. The field of view covers ...\(13^{\prime\prime} \times 6^{\prime\prime}\) (\(1173 \times 541\) pc\(^{2}\)) centered on the nucleus, at a spatial resolution of \(52\) pc. The spectral coverage extends from \(5600\) \AA\ to \(7000\) \AA, at a spectral resolution \(R=1918\). NGC 1365 hosts a Seyfert 1.8 nucleus, and exhibits a prominent bar extending out to \(100^{\prime\prime}\) (9 kpc) from the nucleus. The field of view lies within the inner Lindblad resonance. Within this region, we found that the kinematics of the ionized gas (as traced by OI, NII, H\(\alpha\), and SII) is consistent with rotation in the large-scale plane of the galaxy. While rotation dominates the kinematics, there is also evidence for a fan-shaped outflow, as found in other studies based on the OIII emission lines. Although evidence for gas inflowing along nuclear spirals has been found in a few barred galaxies, we find no obvious signs of such features in the inner kiloparsec of NGC 1365. However, the emission lines exhibit a puzzling asymmetry that could originate from gas which is slower than the gas responsible for the bulk of the narrow-line emission. We speculate that it could be tracing gas which lost angular momentum, and is slowly migrating from the inner Lindblad resonance towards the nucleus of the galaxy.
We use high spectral resolution (R > 8000) data covering 3800-13000Å to study the physical conditions of the broad line region (BLR) of nine nearby Seyfert 1 galaxies. Up to six broad HI lines are ...present in each spectrum. A comparison - for the first time using simultaneous optical to near-infrared observations - to photoionisation calculations with our devised simple scheme yields the extinction to the BLR at the same time as determining the density and photon flux, and hence distance from the nucleus, of the emitting gas. This points to a typical density for the HI emitting gas of 10\(^{11}\)cm\(^{-3}\) and shows that a significant amount of this gas lies at regions near the dust sublimation radius, consistent with theoretical predictions. We also confirm that in many objects the line ratios are far from case B, the best-fit intrinsic broad-line H\(\alpha\)/H\(\beta\) ratios being in the range 2.5-6.6 as derived with our photoionization modeling scheme. The extinction to the BLR, based on independent estimates from HI and HeII lines, is A\(_V\) \(\le\) 3 for Seyfert 1-1.5s, while Seyfert 1.8-1.9s have A\(_V\) in the range 4-8. A comparison of the extinction towards the BLR and narrow line region (NLR) indicates that the structure obscuring the BLR exists on scales smaller than the NLR. This could be the dusty torus, but dusty nuclear spirals or filaments could also be responsible. The ratios between the X-ray absorbing column N\(_H\) and the extinction to the BLR are consistent with the Galactic gas-to-dust ratio if N\(_H\) variations are considered.
We present two-dimensional gaseous kinematics of the inner 1.1 x 1.6kpc^2 of the Seyfert 2 galaxy NGC2110, from optical spectra obtained with the GMOS integral field spectrograph on the Gemini South ...telescope at a spatial resolution of 100pc. Gas emission is observed over the whole field-of-view, with complex - and frequently double - emission-line profiles. We have identified four components in the emitting gas, according to their velocity dispersion (sigma), which we refer to as: (1) warm gas disk (sigma = 100-220km/s); (2) cold gas disk (sigma = 60-90km/s); (3) nuclear component (sigma = 220-600km/s); and (4) northern cloud (sigma = 60-80km/s). Both the cold and warm disk components are dominated by rotation and have similar gas densities, but the cold gas disk has lower velocity dispersions and reaches higher rotation velocities. We attribute the warm gas disk to a thick gas layer which encompasses the cold disk as observed in some edge-on spiral galaxies. After subtraction of a rotation model from the cold disk velocity field, we observe excess blueshifts of 50km/s in the far side of the galaxy as well as similar excess redshifts in the near side. These residuals can be interpreted as due to nuclear inflow in the cold gas, with an estimated ionized gas mass inflow rate of 2.2 x 10^(-2)Msun/yr. We have also subtracted a rotating model from the warm disk velocity field and found excess blueshifts of 100km/s to the SW of the nucleus and excess redshifts of 40km/s to the NE, which we attribute to gas disturbed by an interaction with a nuclear spherical outflow. This nuclear outflow is the origin of the nuclear component observed within the inner 300pc and it has a mass outflow rate of 0.9Msun/yr. In a region between 1" and 4" north of the nucleus we find a new low sigma component of ionized gas which we attribute to a high latitude cloud photoionized by the nuclear source.
Radical nephrectomy (Nx) with vena caval thrombectomy represents the only realistic chance of cure for patients with renal cell carcinoma with extension into the vena cava inferior (VCI). For stage ...III, with tumor extension in the retrohepatic VCI up to the diaphragm, a venous bypass technique is described. From July, 1996 through April, 1998, Nx combined with thrombectomy of the VCI was performed by isolation of the VCI, temporary occlusion of the hepatoduodenal ligament, and temporary extracorporal femoral-axillary veno-venous bypass with the Biomedicus pump. Radical resection of tumor thrombus from the VCI was accomplished under direct vision with minimal blood loss and without cardiopulmonary complications. With a follow-up of 21, 16, 9, 2, and 1 months, respectively, all patients are so far free of complications and without recurrent or metastatic disease.
Die Ursachen der terminalen Niereninsuffizienz im Kindesalter unterscheiden sich deutlich von denen des Erwachsenenalters. Die Therapie der Wahl besteht in der Nierentransplantation. In Deutschland ...wurden im Jahre 2003 117 Kinder und Jugendliche nierentransplantiert. Spezifische Probleme bestehen in der Immunsuppression und den daraus resultierenden Komorbiditäten im Kindesalter. Der vorliegende Beitrag gibt eine Übersicht über die Möglichkeiten und Probleme der Vorbereitung, der Transplantation und des weiteren Verlaufs von Nierentransplantationen im Kindesalter. The reasons for end-stage renal disease in pediatric patients differ from adults. The therapy of choice is renal transplantation. A total of 117 children and adolescents were treated with renal transplantation in 2003 in Germany. Immunosuppressive therapy and related comorbidities are the main problems in pediatric patients. The following article provides a summary of transplantation in children, preparation, and follow-up.PUBLICATION ABSTRACT
We present optical integral field spectroscopy of the circum-nuclear gas of the Seyfert 2 galaxy NGC 1386. The data cover the central 7\(^{\prime\prime} \times 9^{\prime\prime}\) (530 \(\times\) 680 ...pc) at a spatial resolution of 0.9" (68 pc), and the spectral range 5700-7000 \AA\ at a resolution of 66 km s\(^{-1}\). The line emission is dominated by a bright central component, with two lobes extending \(\approx\) 3\(^{\prime\prime}\) north and south of the nucleus. We identify three main kinematic components. The first has low velocity dispersion (\(\bar \sigma \approx \) 90 km s\(^{-1}\)), extends over the whole field-of-view, and has a velocity field consistent with gas rotating in the galaxy disk. We interpret the lobes as resulting from photoionization of disk gas in regions where the AGN radiation cones intercept the disk. The second has higher velocity dispersion (\(\bar \sigma \approx\) 200 km s\(^{-1}\)) and is observed in the inner 150 pc around the continuum peak. This component is double peaked, with redshifted and blueshifted components separated by \(\approx\) 500 km s\(^{-1}\). Together with previous HST imaging, these features suggest the presence of a bipolar outflow for which we estimate a mass outflow rate of \(\mathrm{\dot M} \gtrsim \) 0.1 M\(_{\odot}\) yr\(^{-1}\). The third component is revealed by velocity residuals associated with enhanced velocity dispersion and suggests that outflow and/or rotation is occurring approximately in the equatorial plane of the torus. A second system of velocity residuals may indicate the presence of streaming motions along dusty spirals in the disk.
The reasons for end-stage renal disease in pediatric patients differ from adults. The therapy of choice is renal transplantation. A total of 117 children and adolescents were treated with renal ...transplantation in 2003 in Germany. Immunosuppressive therapy and related comorbidities are the main problems in pediatric patients. The following article provides a summary of transplantation in children, preparation, and follow-up.
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