The Growth of SMBHs in Optically-Thick Starburst Galaxies

2006 ◽  
pp. 466-467
Author(s):  
N. Kawakatu ◽  
M. Umemura ◽  
M. Mori
Keyword(s):  
Starburst Galaxies

The Structure and Morphology of the Ionized Gas in Starburst Galaxies: NGC 5253/5236

1999 ◽  
Vol 118 (2) ◽  
pp. 797-816 ◽  
Author(s):  
Daniela Calzetti ◽  
Christopher J. Conselice ◽  
John S. Gallagher III ◽  
Anne L. Kinney
Keyword(s):  
Starburst Galaxies ◽  
Ionized Gas ◽  
Structure And Morphology

scholarly journals Starburst galaxies strike back: a multi-messenger analysis with Fermi-LAT and IceCube data

2021 ◽  
Vol 503 (3) ◽  
pp. 4032-4049
Author(s):  
Antonio Ambrosone ◽  
Marco Chianese ◽  
Damiano F G Fiorillo ◽  
Antonio Marinelli ◽  
Gennaro Miele ◽  
...  
Keyword(s):  
Cosmic Rays ◽  
Gamma Ray ◽  
Neutrino Flux ◽  
Data Interpretation ◽  
Realistic Model ◽  
High Energy ◽  
Starburst Galaxies ◽  
Neutrino Factory ◽  
High Energy Cosmic Rays ◽  
Astrophysical Objects

ABSTRACT Starburst galaxies, which are known as ‘reservoirs’ of high-energy cosmic-rays, can represent an important high-energy neutrino ‘factory’ contributing to the diffuse neutrino flux observed by IceCube. In this paper, we revisit the constraints affecting the neutrino and gamma-ray hadronuclear emissions from this class of astrophysical objects. In particular, we go beyond the standard prototype-based approach leading to a simple power-law neutrino flux, and investigate a more realistic model based on a data-driven blending of spectral indexes, thereby capturing the observed changes in the properties of individual emitters. We then perform a multi-messenger analysis considering the extragalactic gamma-ray background (EGB) measured by Fermi-LAT and different IceCube data samples: the 7.5-yr high-energy starting events (HESE) and the 6-yr high-energy cascade data. Along with starburst galaxies, we take into account the contributions from blazars and radio galaxies as well as the secondary gamma-rays from electromagnetic cascades. Remarkably, we find that, differently from the highly-constrained prototype scenario, the spectral index blending allows starburst galaxies to account for up to $40{{\ \rm per\ cent}}$ of the HESE events at $95.4{{\ \rm per\ cent}}$ CL, while satisfying the limit on the non-blazar EGB component. Moreover, values of $\mathcal {O}(100\, \mathrm{PeV})$ for the maximal energy of accelerated cosmic-rays by supernovae remnants inside the starburst are disfavoured in our scenario. In broad terms, our analysis points out that a better modelling of astrophysical sources could alleviate the tension between neutrino and gamma-ray data interpretation.

scholarly journals Understanding the origin of radio outflows in Seyfert galaxies using radio polarimetry

2019 ◽  
Vol 15 (S356) ◽  
pp. 247-251
Author(s):  
Biny Sebastian ◽  
Preeti Kharb ◽  
Christopher P. O’ Dea ◽  
Jack F. Gallimore ◽  
Stefi A. Baum ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Radio Emission ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Seyfert Galaxy ◽  
Seyfert Galaxies ◽  
Starburst Galaxies ◽  
Galactic Magnetic Fields ◽  
5 Ghz

AbstractThe role of starburst winds versus active galactic nuclei (AGN) jets/winds in the formation of the kiloparsec scale radio emission seen in Seyferts is not yet well understood. In order to be able to disentangle the role of various components, we have observed a sample of Seyfert galaxies exhibiting kpc-scale radio emission suggesting outflows, along with a comparison sample of starburst galaxies, with the EVLA B-array in polarimetric mode at 1.4 GHz and 5 GHz. The Seyfert galaxy NGC 2639, shows highly polarized secondary radio lobes, not observed before, which are aligned perpendicular to the known pair of radio lobes. The additional pair of lobes represent an older epoch of emission. A multi-epoch multi-frequency study of the starburst-Seyfert composite galaxy NGC 3079, reveals that the jet together with the starburst superwind and the galactic magnetic fields might be responsible for the well-known 8-shaped radio lobes observed in this galaxy. We find that many of the Seyfert galaxies in our sample show bubble-shaped lobes, which are absent in the starburst galaxies that do not host an AGN.

scholarly journals Why Post-starburst Galaxies Are Now Quiescent

2018 ◽  
Vol 861 (2) ◽  
pp. 123 ◽  
Author(s):  
K. Decker French ◽  
Ann I. Zabludoff ◽  
Ilsang Yoon ◽  
Yancy Shirley ◽  
Yujin Yang ◽  
...  
Keyword(s):  
Starburst Galaxies

Excitation Mechanism of Near‐Infrared [Feii] Emission in Seyfert and Starburst Galaxies

2000 ◽  
Vol 528 (1) ◽  
pp. 186-200 ◽  
Author(s):  
Hideaki Mouri ◽  
Kimiaki Kawara ◽  
Yoshiaki Taniguchi
Keyword(s):  
Near Infrared ◽  
Starburst Galaxies ◽  
Excitation Mechanism

scholarly journals 3.29. Radio recombination lines from starburst galaxies

1998 ◽  
Vol 184 ◽  
pp. 147-148
Author(s):  
K.R. Anantharamaiah
Keyword(s):  
Millimeter Wave ◽  
Dynamic Range ◽  
Starburst Galaxies ◽  
Aperture Synthesis ◽  
Emission Region ◽  
Full Extent ◽  
Radio Recombination Lines

Starburst activity is often heavily obscured by dust. To see through the dust and measure the full extent, power and dynamics of the starburst, we are surveying hydrogen radio recombination lines (RRLs) from famous nearby starburst galaxies. Exploiting the improved sensitivity and dynamic range of aperture synthesis arrays such as the VLA and the AT and millimeter-wave telescopes such as SEST and the IRAM-30m telescope, we have searched for RRLs in about 25 starburst galaxies. RRLs have been detected in 14 galaxies. The observations were made variously at 1.4, 4.9, 8.4, 86, 135 and 232 GHz (Anantharamaiah et al 1993, Zhao et al 1996, 1997, Phookun et al 1997). Table 1 summarizes the observations. In all the cases the detected line originates in the nuclear starburst region and the emission region is resolved with a beam of 1–3″.

scholarly journals Wide Area X-ray Surveys for AGN and Starburst Galaxies

2008 ◽  
Author(s):  
Andrew Ptak ◽  
Coryn A.L. Bailer-Jones
Keyword(s):  
Starburst Galaxies ◽  
Wide Area ◽  
X Ray ◽  
Area X

scholarly journals Spatially Resolved Spectroscopy of Starburst and Post-Starburst Galaxies in the Rich z ∼0.55 Cluster CL 0016+16

2010 ◽  
Vol 27 (3) ◽  
pp. 360-373 ◽  
Author(s):  
Michael B. Pracy ◽  
Warrick J. Couch ◽  
Harald Kuntschner
Keyword(s):  
Age Distribution ◽  
Starburst Galaxies ◽  
Small Sample ◽  
Spectral Signature ◽  
Rich Cluster ◽  
Spatially Resolved ◽  
Radial Profiles ◽  
Field Samples ◽  
The Rich ◽  
Spatially Resolved Spectroscopy

AbstractWe have used the Low Resolution Imaging Spectrograph on the W. M. Keck I telescope to obtain spatially resolved spectroscopy of a small sample of six ‘post-starburst’ and three ‘dusty-starburst’ galaxies in the rich cluster CL 0016+16 at z=0.55. We use this to measure radial profiles of the Hδ and [OII]λ3727 lines which are diagnostic probes of the mechanisms that give rise to the abrupt changes in star formation rates in these galaxies. In the post-starburst sample we are unable to detect any radial gradients in the Hδ line equivalent width — although one galaxy exhibits a gradient from one side of the galaxy to the other. The absence of Hδ gradients in these galaxies is consistent with their production via interaction with the intracluster medium; however, our limited spatial sampling prevents us from drawing robust conclusions. All members of the sample have early-type morphologies, typical of post-starburst galaxies in general, but lack the high incidence of tidal tails and disturbances seen in local field samples. This argues against a merger origin and adds weight to a scenario where truncation by the intra-cluster medium is at work. The post-starburst spectral signature is consistent over the radial extent probed with no evidence of [OII]λ3727 emission and strong Hδ absorption at all radii, i.e. the post-starburst classification is not an aperture effect. In contrast the ‘dusty-starburst’ sample shows a tendency for a central concentration of [OII]λ3727 emission. This is most straightforwardly interpreted as the consequence of a central starburst. However, other possibilities exist such as a non-uniform dust distribution (which is expected in such galaxies) and/or a non-uniform starburst age distribution. The members of the sample exhibit late-type and irregular morphologies.

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