Variability of near-infrared emission lines in NGC 4151 - Implications for nuclear star formation

1992 ◽  
Vol 80 ◽  
pp. 205 ◽  
Author(s):  
Andrea H. Prestwich ◽  
Gillian S. Wright ◽  
Robert D. Joseph
Keyword(s):  
Star Formation ◽  
Near Infrared ◽  
Infrared Emission ◽  
Emission Lines ◽  
Ngc 4151 ◽  
Near Infrared Emission

Near-infrared emission-line spectra of the Orion Nebula, NGC 4151, and other Seyfert galaxies

1990 ◽  
Vol 352 ◽  
pp. 561 ◽  
Author(s):  
Donald E. Osterbrock ◽  
Richard A. Shaw ◽  
Sylvain Veilleux
Keyword(s):  
Emission Line ◽  
Near Infrared ◽  
Seyfert Galaxies ◽  
Infrared Emission ◽  
Orion Nebula ◽  
Ngc 4151 ◽  
Near Infrared Emission

scholarly journals Infrared Emission-Lines and the Stellar Temperature

1993 ◽  
Vol 155 ◽  
pp. 89-89 ◽  
Author(s):  
Sueli M. Viegas ◽  
Ruth Gruenwald
Keyword(s):  
Near Infrared ◽  
Planetary Nebulae ◽  
Infrared Emission ◽  
Emission Lines ◽  
Heavy Elements ◽  
Atomic Transitions ◽  
Stellar Temperature ◽  
Near Infrared Emission

Observations of near infrared emission-lines are becoming available and can be a powerful tool to improve our knowledge on planetary nebulae properties. For wavelengths in the range 1 to 5 μm, the emission-lines correspond to atomic transitions of high ionized species of heavy elements. In particular, the [Si VI] 1.96μm and [Si VII] 2.48μm lines have already been detected (Ashley and Hyland, 1988).

scholarly journals Near-Infrared Spectroscopy of NGC 253: Starburst and Surroundings

1996 ◽  
Vol 171 ◽  
pp. 407-407 ◽  
Author(s):  
D. Lutz ◽  
F. Prada
Keyword(s):  
Stellar Population ◽  
Near Infrared ◽  
Velocity Dispersion ◽  
Mass Function ◽  
Infrared Emission ◽  
Initial Mass Function ◽  
Emission Lines ◽  
Lower Mass ◽  
Dynamical Mass ◽  
Near Infrared Emission

Near-infrared longslit spectra of NGC 253 obtained with IRSPEC at the ESO NTT are presented. By analysis of the 12CO 2.29μm bandhead we find that the stellar population in the central starburst region (r ∼ 150 pc) rotates more slowly than the gas, but has a velocity dispersion of 128 km/s, about twice the value found for emission lines from the gas in this region. This implies an about five times higher dynamical mass than previously derived (Rieke et al. 1980), removing the need to invoke a lower mass cutoff in the starburst initial mass function. The peak of near-infrared emission is displaced from the dynamical center.

scholarly journals Near-Infrared Emission-Line Spectra of the Orion Nebula, NGC 4151, and Other Seyfert Galaxies

1989 ◽  
Vol 134 ◽  
pp. 298-300
Author(s):  
D. E. Osterbrock ◽  
R. A. Shaw ◽  
S. Veilleux
Keyword(s):  
Near Infrared ◽  
Good Deal ◽  
Seyfert Galaxies ◽  
Infrared Emission ◽  
Orion Nebula ◽  
Ngc 4151 ◽  
Relative Line ◽  
Infrared Spectral ◽  
Moderate Resolution ◽  
Near Infrared Emission

CCDs make the near-infrared spectral region out to about 1.1 μ observable. A good deal of information on the spectra of AGNs in this range has been published, which we are trying to systematize and extend at Lick. Our original lens-grism spectrograph camera is opaque over the region λ8600-λ10250, no doubt as a result of a coating on one of the elements of the Nikon lens, making this program impossible with it. However our newer “UV-Schmidt” camera is quite effective in this region. With it we have obtained well exposed spectra at moderate resolution (FWHM ≈ 7 Å) of NGC 4151 in three overlapping segments covering the region 7000–11000 Å. Also, for comparison we obtained similar spectra of NGC 1976, the Orion Nebula. The wavelengths and relative line fluxes were measured, and most of the lines were identified. The strongest three lines in both objects are, in order, [S III] λ9532, He I λ10830, and [S III] λ9069. The Orion Nebula spectrum is very helpful for identifying lines in NGC 4151, and for comparison with it. Among the lines identified in NGC 1976, many of them previously known, are [O II], [S II], [Ar III], [Fe II], [Ni II], [Ni III], [Cl II], [C I], in addition to O I λ8446, many H I Paschen lines and He I.

scholarly journals Near Infrared Emission of Neutral Carbon from Photon-Dominated Regions

1992 ◽  
Vol 150 ◽  
pp. 333-334
Author(s):  
V. Escalante ◽  
A. Sternberg ◽  
A. Dalgarno
Keyword(s):  
Field Intensity ◽  
Radiative Recombination ◽  
Near Infrared ◽  
Planetary Nebulae ◽  
Infrared Emission ◽  
Emission Lines ◽  
Radiation Fields ◽  
Ngc 7027 ◽  
Near Infrared Emission ◽  
Intense Radiation

Detailed calculations are reported of the intensities of the near infrared forbidden lines of neutral carbon atoms at λ 985.0 nm, 982.3 nm and 872.7 nm emitted from dense clouds subjected to intense radiation fields. The metastable levels that produce the lines are excited by radiative recombination of the C+ ions produced by photoionization. Impacts of electrons with C atoms in the heated edge zones of the clouds contribute an insignificant part to the excitation. The lines observed in M42 and NGC 2024 can be interpreted as arising in gas with densities in excess of 105 cm−3 and radiation fields with intensities between 103 and 106 times the average interstellar field intensity. Radiative recombination of C+ ions may also be an important source of the emission lines detected in the planetary nebulae NGC 6270 and NGC 7027.

Near‐Infrared Emission Lines of V723 Cassiopeiae (Nova Cassiopeiae 1995)

2002 ◽  
Vol 573 (2) ◽  
pp. 794-802 ◽  
Author(s):  
Richard J. Rudy ◽  
Catherine C. Venturini ◽  
David K. Lynch ◽  
S. Mazuk ◽  
R. C. Puetter
Keyword(s):  
Near Infrared ◽  
Infrared Emission ◽  
Emission Lines ◽  
Near Infrared Emission

scholarly journals Near-infrared Emission Lines in Starburst Galaxies at 0.5 < z < 0.9: Discovery of a Merger Sequence of Extreme Obscurations

2018 ◽  
Vol 862 (2) ◽  
pp. L22 ◽  
Author(s):  
A. Calabrò ◽  
E. Daddi ◽  
P. Cassata ◽  
M. Onodera ◽  
R. Gobat ◽  
...  
Keyword(s):  
Near Infrared ◽  
Infrared Emission ◽  
Starburst Galaxies ◽  
Emission Lines ◽  
Near Infrared Emission
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