Galactic Scale Feedback Observed in the 3C 298 Quasar Host Galaxy

We present high angular resolution multi-wavelength data of the 3C 298 radio-loud quasar host galaxy (z=1.439) taken using the W.M. Keck Observatory OSIRIS integral field spectrograph with adaptive optics, Atacama Large Millimeter/submillimeter Array (ALMA), Hubble Space Telescope (HST) WFC3, and the Very Large Array (VLA). Extended emission is detected in the rest-frame optical nebular emission lines H$\beta$, [OIII], H$\alpha$, [NII], and [SII], as well as molecular lines CO (J=3-2) and (J=5-4). Along the path of 3C 298's relativistic jets we detect conical outflows of ionized gas with velocities up to 1700 km s$^{-1}$ and outflow rate of 450-1500 M$_\odot$yr$^{-1}$. Near the spatial center of the conical outflow, CO (J=3-2) emission shows a molecular gas disc with a total molecular mass ($\rm M_{H_{2}}$) of 6.6$\pm0.36\times10^{9}$M$_{\odot}$. On the molecular disc's blueshifted side we observe a molecular outflow with a rate of 2300 M$_\odot$yr$^{-1}$ and depletion time scale of 3 Myr. We detect no narrow H$\alpha$ emission in the outflow regions, suggesting a limit on star formation of 0.3 M$_\odot$yr$^{-1}$kpc$^{-2}$. Quasar driven winds are evacuating the molecular gas reservoir thereby directly impacting star formation in the host galaxy. The observed mass of the supermassive black hole is $10^{9.37-9.56}$M$_{\odot}$ and we determine a dynamical bulge mass of 1-1.7$\rm\times10^{10}\frac{R}{1.6 kpc}$ M$_{\odot}$. The bulge mass of 3C 298 resides 2-2.5 orders of magnitude below the expected value from the local M$\rm_{bulge}-M_{BH}$ relationship. A second galactic disc observed in nebular emission is offset from the quasar by 9 kpc suggesting the system is an intermediate stage merger. These results show that galactic scale negative feedback is occurring early in the merger phase of 3C 298, well before the coalescence of the galactic nuclei and assembly on the local relationship.Comment: 23 pages, 11 figures, 4 tables, Accepted for publication in the Astrophysical Journa

Providing stringent star formation rate limits of z∼\sim2 QSO host galaxies at high angular resolution

We present integral field spectrograph (IFS) with laser guide star adaptive optics (LGS-AO) observations of z=2 quasi-stellar objects (QSOs) designed to resolve extended nebular line emission from the host galaxy. Our data was obtained with W. M. Keck and Gemini-North Observatories using OSIRIS and NIFS coupled with the LGS-AO systems. We have conducted a pilot survey of five QSOs, three observed with NIFS+AO and two observed with OSIRIS+AO at an average redshift of z=2.15. We demonstrate that the combination of AO and IFS provides the necessary spatial and spectral resolutions required to separate QSO emission from its host. We present our technique for generating a PSF from the broad-line region of the QSO and performing PSF subtraction of the QSO emission to detect the host galaxy. We detect H$\alpha$ and [NII] for two sources, SDSS J1029+6510 and SDSS J0925+06 that have both star formation and extended narrow-line emission. Assuming that the majority of narrow-line H$\alpha$ is from star formation, we infer a star formation rate for SDSS J1029+6510 of 78.4 M$_\odot$yr$^{-1}$ originating from a compact region that is kinematically offset by 290 - 350 km/s. For SDSS J0925+06 we infer a star formation rate of 29 M$_\odot$yr$^{-1}$ distributed over three clumps that are spatially offset by $\sim$ 7 kpc. The null detections on three of the QSOs are used to infer surface brightness limits and we find that at 1.4 kpc distance from the QSO that the un-reddened star formation limit is $<$ 0.3 M$_\odot$yr$^{-1}$kpc$^{-2}$. If we assume a typical extinction values for z=2 type-1 QSOs, the dereddened star formation rate for our null detections would be $<$ 0.6 M$_\odot$yr$^{-1}$kpc$^{-2}$. These IFS observations indicate that if star formation is present in the host it would have to occur diffusely with significant extinction and not in compact, clumpy regions.Comment: 17 pages, 7 figures, 7 tables, Accepted to Ap

PREVENTION OF INTESTINAL ANASTOMOTIC LEAKAGE IN CASE OF PERITONITIS (EXPERIMENTAL RESEARCH)

Background. The problem of development of postoperative complications after operations on the organs of the gastrointestinal tact is extremely important. Failure of intestinal suture, formed in the presence of peritonitis develops from 2.8 to 32 % of patients. Aim. To improve immediate outcomes in the formation of a small intestine anastomosis in conditions of purulent peritonitis. Materials and methods. We conducted immunohistochemical examination of biopsy specimens of the small intestine of 20 patients died of peritonitis and compared the area of the vascular bed in different types of intestinal wall section. The experimental operations were performed in 100 Wistar rats. On the background of established models of peritonitis we performed different variants of small bowel anastomosis, including one with the use of photodynamic therapy. On the 6th day after the surgery, animals were sacrificed, and histological examination of the anastomoses was conducted. Results. Suture strip in the section of the small intestine made at the angle of 60° is supplied substantially better than in the section made at the angle of 90°. The experiment confirmed that the suggested method of anastomosis showed the best results. Conclusion. When one forms the "end-to-end" anastomosis in the small intestine in conditions of purulent peritonitis, it is reasonable to cross the intestinal wall at the angle of 60° and to perform photodynamic therapy on the formed anastomosis

A Comprehensive Study of Dielectric-Conductor Junctions in Low Density Plasmas

In this paper, results are presented of an experimental and theoretical study of snapover, glow discharge, and arc phenomena for different materials immersed in argon or xenon plasmas. The effect of snapover is investigated for several metal-dielectric junctions: copper-teflon, copper-Kapton, copper-glass, aluminum-teflon, aluminum-Kapton, steel-teflon, anodized aluminum with pinholes, and copper-ceramics. I-V curves are measured, and snapover inception voltages, essential parameters (increase in current and collection area due to secondary electrons), and glow discharge inception thresholds are determined. Optical spectra are obtained for glow discharges in both argon and xenon plasmas. These spectra provide information regarding atomic species entrapped in the glow region. A video-camera and linear array were used to confirm that snapover inception is accompanied by very low intensity visible light emission. This result seems to be important for the estimate of the light pollution around spacecraft. Optical spectra (wavelengths 380-650 nm) of arcs are also obtained on a negatively biased chromic acid anodized aluminum plate immersed in low density argon and xenon plasmas. Analysis of these spectra confirms our earlier findings that aluminum atoms are ejected from the arc site. Moreover, it is found that chromium atoms are also quite abundant in the arc plasma. It is believed that the latter results contribute considerably to the understanding of processes of plasma contamination caused by arcin

Characterizing and Improving the Data Reduction Pipeline for the Keck OSIRIS Integral Field Spectrograph

OSIRIS is a near-infrared (1.0--2.4 $\mu$m) integral field spectrograph operating behind the adaptive optics system at Keck Observatory, and is one of the first lenslet-based integral field spectrographs. Since its commissioning in 2005, it has been a productive instrument, producing nearly half the laser guide star adaptive optics (LGS AO) papers on Keck. The complexity of its raw data format necessitated a custom data reduction pipeline (DRP) delivered with the instrument in order to iteratively assign flux in overlapping spectra to the proper spatial and spectral locations in a data cube. Other than bug fixes and updates required for hardware upgrades, the bulk of the DRP has not been updated since initial instrument commissioning. We report on the first major comprehensive characterization of the DRP using on-sky and calibration data. We also detail improvements to the DRP including characterization of the flux assignment algorithm; exploration of spatial rippling in the reduced data cubes; and improvements to several calibration files, including the rectification matrix, the bad pixel mask, and the wavelength solution. We present lessons learned from over a decade of OSIRIS data reduction that are relevant to the next generation of integral field spectrograph hardware and data reduction software design.Comment: 18 pages, 16 figures; accepted for publication in A