ChemInform Abstract: Synthesis of Asymmetrically Substituted Terpyridines by Palladium‐Catalyzed Direct C—H Arylation of Pyridine N‐Oxides.

Duric, Sasa; Sypaseuth, Fanni D.; Hoof, Santina; Svensson, Emma; Tzschucke, Carl Christoph

doi:10.1002/chin.201423159

Cited by 6 publications

(7 citation statements)

References 1 publication

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“…Therefore, a spectral steepening with height would correspond to the case of large magnetic field (short cooling time scale) and low wind speed. Confirming this, Duric et. al.…”

Section: Introductionsupporting

confidence: 52%

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Radio haloes of star-forming galaxies

Vijayan

Nath

Sharma

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the synchrotron radio emission from extra-planar regions of star forming galaxies. We use ideal magneto-hydrodynamical (MHD) simulations of a rotating Milky Way-type disk galaxy with distributed star formation sites for three star formation rates (SFRs) (0.3, 3, 30 M yr −1 ). From our simulations, we see emergence of galactic-scale magnetised outflows, carrying gas from the disk. We compare the morphology of the outflowing gas with hydrodynamic (HD) simulations. We look at the spatial distribution of magnetic field in the outflows. Assuming that a certain fraction of gas energy density is converted into cosmic ray energy density, and using information about the magnetic field, we obtain synchrotron emissivity throughout the simulation domain. We generate the surface brightness maps at a frequency of 1.4 GHz. The outflows are more extended in the vertical direction than radial and hence have an oblate shape. We further find that the matter right behind the outer shock, shines brighter in these maps than that above or below. To understand whether this feature can be observed, we produce vertical intensity profiles. We convolve the vertical intensity profile with the typical beam sizes of radio telescopes, for a galaxy located at 10 Mpc (similar to NGC 891) in order to estimate the radio scale height to compare with observations. We find that for our SFRs this feature will lie below the RMS noise limit of instruments. The radio scale height is found to be ∼ 300 − 1200 pc , depending on the resolution of the telescope. We relate the advection speed of the outer shock with the surface density of star formation as v adv ∝ Σ 0.3 SFR , which is consistent with earlier observations and analytical estimates.

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“…Therefore, a spectral steepening with height would correspond to the case of large magnetic field (short cooling time scale) and low wind speed. Confirming this, Duric et. al.…”

Section: Introductionsupporting

confidence: 52%

“…In their spectral maps of galaxies, they noticed a steepening of the spectral index (i. e. it becomes more negative) away from the plane of the disk along the minor axis. They explained this by arguing that CRes that populate the halo would have lost energy in the disk before being transported to the halo (Duric et. al.…”

Section: Introductionmentioning

confidence: 99%

Radio haloes of star-forming galaxies

Vijayan

Nath

Sharma

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Radio halos were discovered in several starburst galaxies (Ekers & Sancisi 1977;Allen et al 1978;Carilli et al 1992;Duric et al 1998). These were believed to be composed of the material that was convected up from the central starburst regions, where it was created by super-novae (Lerche & Schlickeiser 1980).…”

Section: Role Of the Jet In Inflating The Radio Bubblementioning

confidence: 99%

The Filamentary Radio Lobes of the Seyfert–Starburst Composite Galaxy NGC 3079

Sebastian

Kharb

O’Dea

et al. 2019

ApJ

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We present results from multi-frequency polarization-sensitive Very Large Array observations of the Seyfert-starburst composite galaxy NGC 3079. Our sensitive radio observations reveal a plethora of radio "filaments" comprising the radio lobes in this galaxy. We analyze the origin of these radio filaments in the context of existing Chandra X-ray and HST emission-line data. We do not find a one-to-one correlation of the radio filaments with the emission line filaments. The north-eastern lobe is highly polarized with polarization fractions ∼ 33% at 5 GHz. The magnetic fields are aligned with the linear extents of the optically-thin filaments, as observed in our, as well as other observations in the literature. Our rotation measure images show evidence for rotation measure inversion in the north-eastern lobe. Our data best fit a model where the cosmic rays follow the magnetic field lines generated as a result of the dynamo mechanism. There could be additional effects like shock acceleration that might also be playing a role. We speculate that the peculiar radio lobe morphology is a result of an interplay between both the superwinds and the AGN jet that are present in the galaxy. The jet, in fact, might be playing a major role in providing the relativistic electron population that is present in the radio lobes.

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“…Consideration of the role of extraplanar magnetic fields and cosmic rays in the dynamics, heating, and/or ionization of the eDIG in NGC 5775 is motivated by the detection of an extensive (z ∼ 12 − 17 kpc, corrected for D) radio continuum halo (Duric et al 1998). More recently, the synchrotron halo of NGC 5775 has been studied by Continuum Halos in Nearby Galaxies -an EVLA Survey (CHANG-ES).…”

Section: Introductionmentioning

confidence: 99%

A Dynamical Study of Extraplanar Diffuse Ionized Gas in NGC 5775*

Boettcher¹,

Gallagher²,

Zweibel³

2019

ApJ

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The structure and kinematics of gaseous, disk-halo interfaces are imprinted with the processes that transfer mass, metals, and energy between galactic disks and their environments. We study the extraplanar diffuse ionized gas (eDIG) layer in the interacting, star-forming galaxy NGC 5775 to better understand the consequences of star-formation feedback on the dynamical state of the thick-disk interstellar medium (ISM). Combining emission-line spectroscopy from the Robert Stobie Spectrograph on the Southern African Large Telescope with radio continuum observations from Continuum Halos in Nearby Galaxies -an EVLA Survey, we ask whether thermal, turbulent, magnetic field, and cosmicray pressure gradients can stably support the eDIG layer in dynamical equilibrium. This model fails to reproduce the observed exponential electron scale heights of the eDIG thick disk and halo on the northeast (h z,e = 0.6, 7.5 kpc) and southwest (h z,e = 0.8, 3.6 kpc) sides of the galaxy at R < 11 kpc. We report the first definitive detection of an increasing eDIG velocity dispersion as a function of height above the disk. Blueshifted gas along the minor axis at large distances from the midplane hints at a disk-halo circulation and/or ram pressure effects caused by the ongoing interaction with NGC 5774. This work motivates further integral field unit and/or Fabry-Perot spectroscopy of galaxies with a range of star-formation rates to develop a spatially-resolved understanding of the role of star-formation feedback in shaping the kinematics of the disk-halo interface.

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ChemInform Abstract: Synthesis of Asymmetrically Substituted Terpyridines by Palladium‐Catalyzed Direct C—H Arylation of Pyridine N‐Oxides.

Abstract: The convenient and scalable synthesis of the title compounds is accomplished in fewer steps compared to known cross‐coupling methods.

Cited by 6 publications

References 1 publication

Radio haloes of star-forming galaxies

Radio haloes of star-forming galaxies

The Filamentary Radio Lobes of the Seyfert–Starburst Composite Galaxy NGC 3079

A Dynamical Study of Extraplanar Diffuse Ionized Gas in NGC 5775*

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