Discovery of a Double Circumnuclear Ring and Minibar in the Starburst Galaxy M83

1998 ◽  
Vol 116 (6) ◽  
pp. 2834-2840 ◽  
Author(s):  
Debra Meloy Elmegreen ◽  
Frederick R. Chromey ◽  
Aaron R. Warren
Keyword(s):  
Starburst Galaxy

scholarly journals The Discovery of Spiral Arms in the Starburst Galaxy M82

2005 ◽  
Vol 628 (1) ◽  
pp. L33-L36 ◽  
Author(s):  
Y. D. Mayya ◽  
L. Carrasco ◽  
A. Luna
Keyword(s):  
Starburst Galaxy ◽  
Spiral Arms

scholarly journals OH main line masers in the M 82 starburst

2007 ◽  
Vol 3 (S242) ◽  
pp. 427-431
Author(s):  
M. K. Argo ◽  
A. Pedlar ◽  
T. W. B. Muxlow ◽  
R. J. Beswick
Keyword(s):  
Central Region ◽  
Supernova Remnants ◽  
Main Line ◽  
Line Of Sight ◽  
Starburst Galaxy ◽  
Large Array ◽  
Satellite Line ◽  
Very Large Array

AbstractA study of the distribution of OH gas in the central region of the nearby active starburst galaxy M82 has confirmed two previously known bright masers and revealed several new main line masers. Three of these are seen only at 1665 MHz, one is detected only at 1667 MHz, while the rest are detected in both lines. Observations covering both the 1665 and 1667 MHz lines, conducted with both the Very Large Array (VLA) and the Multi-Element Radio Linked Interferometer Network (MERLIN), have been used to accurately measure the positions and velocities of these features. This has allowed a comparison with catalogued continuum features in the starburst such as HII regions and supernova remnants, as well as known water and satellite line OH masers. Most of the main line masers appear to be associated with known HII regions although the two detected only at 1665 MHz are seen along the same line of sight as known supernova remnants.

scholarly journals Neutral versus ionized gas kinematics at z ≃ 2.6: the AGN-host starburst galaxy PKS 0529-549

2018 ◽  
Vol 479 (4) ◽  
pp. 5440-5447 ◽  
Author(s):  
Federico Lelli ◽  
Carlos De Breuck ◽  
Theresa Falkendal ◽  
Filippo Fraternali ◽  
Allison W S Man ◽  
...  
Keyword(s):  
Starburst Galaxy ◽  
Ionized Gas ◽  
Gas Kinematics

scholarly journals Kinematics and Structure of the Starburst Galaxy NGC 7673

1999 ◽  
Vol 522 (1) ◽  
pp. 199-208 ◽  
Author(s):  
N. L. Homeier ◽  
J. S. Gallagher
Keyword(s):  
Starburst Galaxy

scholarly journals First detection of Lyman continuum escape from a local starburst galaxy

2006 ◽  
Vol 448 (2) ◽  
pp. 513-524 ◽  
Author(s):  
N. Bergvall ◽  
E. Zackrisson ◽  
B.-G. Andersson ◽  
D. Arnberg ◽  
J. Masegosa ◽  
...  
Keyword(s):  
Starburst Galaxy ◽  
Lyman Continuum

scholarly journals A Multi-Frequency Study of the Milky Way-Like Spiral Galaxy NGC 6744

2018 ◽  
Vol 35 ◽  
Author(s):  
Miranda Yew ◽  
Miroslav D. Filipović ◽  
Quentin Roper ◽  
Jordan D. Collier ◽  
Evan J. Crawford ◽  
...  
Keyword(s):  
Black Hole ◽  
Milky Way ◽  
Formation Rate ◽  
Radio Continuum ◽  
Starburst Galaxy ◽  
Radio Sources ◽  
Wide Field ◽  
Central Black Hole ◽  
X Ray ◽  
Continuum Data

AbstractWe present a multi-frequency study of the intermediate spiral SAB(r)bc type galaxy NGC 6744, using available data from the Chandra X-Ray telescope, radio continuum data from the Australia Telescope Compact Array and Murchison Widefield Array, and Wide-field Infrared Survey Explorer infrared observations. We identify 117 X-ray sources and 280 radio sources. Of these, we find nine sources in common between the X-ray and radio catalogues, one of which is a faint central black hole with a bolometric radio luminosity similar to the Milky Way’s central black hole. We classify 5 objects as supernova remnant (SNR) candidates, 2 objects as likely SNRs, 17 as H ii regions, 1 source as an AGN; the remaining 255 radio sources are categorised as background objects and one X-ray source is classified as a foreground star. We find the star-formation rate (SFR) of NGC 6744 to be in the range 2.8–4.7 M⊙~yr − 1 signifying the galaxy is still actively forming stars. The specific SFR of NGC 6744 is greater than that of late-type spirals such as the Milky Way, but considerably less that that of a typical starburst galaxy.

FISICA observations of the starburst galaxy, NGC 1569

2006 ◽  
Vol 50 (4-5) ◽  
pp. 433-435
Author(s):  
D.M. Clark ◽  
S.S. Eikenberry ◽  
S.N. Raines ◽  
N. Gruel ◽  
R. Elston ◽  
...  
Keyword(s):  
Starburst Galaxy ◽  
Ngc 1569

scholarly journals The starburst galaxy NGC 253 revisited by H.E.S.S. and Fermi-LAT

2018 ◽  
Vol 617 ◽  
pp. A73 ◽  
Author(s):  
◽  
H. Abdalla ◽  
F. Aharonian ◽  
F. Ait Benkhali ◽  
E. O. Angüner ◽  
...  
Keyword(s):  
Spectral Index ◽  
Power Law ◽  
Cosmic Ray ◽  
High Energy ◽  
Thick Target ◽  
Starburst Galaxy ◽  
Particle Accelerators ◽  
Power Law Distribution ◽  
Particle Population ◽  
Measurement Uncertainties

Context. NGC 253 is one of only two starburst galaxies found to emit γ-rays from hundreds of MeV to multi-TeV energies. Accurate measurements of the very-high-energy (VHE; E > 100 GeV) and high-energy (HE; E > 60 MeV) spectra are crucial to study the underlying particle accelerators, probe the dominant emission mechanism(s) and to study cosmic-ray interaction and transport. Aims. The measurement of the VHE γ-ray emission of NGC 253 published in 2012 by H.E.S.S. was limited by large systematic uncertainties. Here, the most up to date measurement of the γ-ray spectrum of NGC 253 is investigated in both HE and VHE γ-rays. Assuming a hadronic origin of the γ-ray emission, the measurement uncertainties are propagated into the interpretation of the accelerated particle population. Methods. The data of H.E.S.S. observations are reanalysed using an updated calibration and analysis chain. The improved Fermi–LAT analysis employs more than 8 yr of data processed using pass 8. The cosmic-ray particle population is evaluated from the combined HE–VHE γ-ray spectrum using NAIMA in the optically thin case. Results. The VHE γ-ray energy spectrum is best fit by a power-law distribution with a flux normalisation of (1.34 ± 0.14stat ± 0.27sys) × 10−13 cm−2 s−1 TeV1 at 1 TeV – about 40% above, but compatible with the value obtained in Abramowski et al. (2012). The spectral index Γ = 2.39 ± 0.14stat ± 0.25sys is slightly softer than but consistent with the previous measurement within systematic errors. In the Fermi energy range an integral flux of F(E > 60 MeV) = (1.56 ± 0.28stat ± 0.15sys) × 10−8 cm−2 s−1 is obtained. At energies above ∼3 GeV the HE spectrum is consistent with a power-law ranging into the VHE part of the spectrum measured by H.E.S.S. with an overall spectral index Γ = 2.22 ± 0.06stat. Conclusions. Two scenarios for the starburst nucleus are tested, in which the gas in the starburst nucleus acts as either a thin or a thick target for hadronic cosmic rays accelerated by the individual sources in the nucleus. In these two models, the level to which NGC 253 acts as a calorimeter is estimated to a range of fcal = 0.1 to 1 while accounting for the measurement uncertainties. The presented spectrum is likely to remain the most accurate measurements until the Cherenkov Telescope Array (CTA) has collected a substantial set of data towards NGC 253.

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