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The H II regions of Holmberg II
Publications of the Astronomical Society of the Pacific, 1994Calibrated H-alpha and continuum CCD frames are used to measure the emission-line luminosities and mophological characteristics of 82 H II regions in the dwarf irregular galaxy, Ho II, in the M81 group. The assemblage of H II regions is statistically normal: the luminosity function fits a power law with -1.70 and the size distribution is roughly ...
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Annual Review of Astronomy and Astrophysics, 1990
Article de synthese sur les regions H II extragalactiques traitant des morphologies, de la cinematique, des etoiles ionisantes et des abondances ...
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Article de synthese sur les regions H II extragalactiques traitant des morphologies, de la cinematique, des etoiles ionisantes et des abondances ...
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The H II regions of NGC 6822. I - an atlas of 157 H II regions
Publications of the Astronomical Society of the Pacific, 1988A CCD survey at Hα results in a catalog of 157 H II regions in the Local Group irregular galaxy NGC 6822. Most of them are newly detected, faint surface-brightness objects. Positions and maps are given, and identifications are correlated with those of previous studies.
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Publications of the Astronomical Society of the Pacific, 1994
Calibrated H-alpha and continuum CCD frames are used to measure the emission-line luminosities, sizes and morphological characteristics of 25 H II regions in the dwarf irregular galaxy Sextans A, a probable member of the Local Group. The luminosity function fits a power law with slope--1.70 and the size distribution is roughly exponential with a scale ...
Paul Hodge +2 more
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Calibrated H-alpha and continuum CCD frames are used to measure the emission-line luminosities, sizes and morphological characteristics of 25 H II regions in the dwarf irregular galaxy Sextans A, a probable member of the Local Group. The luminosity function fits a power law with slope--1.70 and the size distribution is roughly exponential with a scale ...
Paul Hodge +2 more
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1974
The luminosity of the brightest H ii regions of M31 was determined with the NRAO 3-element interferometer at 3.7 cm and 11 cm wavelength. It is unlikely that M31 has any superbright Hn regions such as W51 or W49; our Galaxy has between 10 and 20 H ii regions that are more luminous than any in M31.
J. H. Spencer, B. F. Burke
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The luminosity of the brightest H ii regions of M31 was determined with the NRAO 3-element interferometer at 3.7 cm and 11 cm wavelength. It is unlikely that M31 has any superbright Hn regions such as W51 or W49; our Galaxy has between 10 and 20 H ii regions that are more luminous than any in M31.
J. H. Spencer, B. F. Burke
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1987
By virtue of its spectrometers having simultaneous multichannel integration capability and relatively large input apertures, the International Ultraviolet Explorer satellite has been the first instrument capable of effective study of the ultraviolet spectra of the gas from extended H ii regions. This review will concentrate on discussing the results of
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By virtue of its spectrometers having simultaneous multichannel integration capability and relatively large input apertures, the International Ultraviolet Explorer satellite has been the first instrument capable of effective study of the ultraviolet spectra of the gas from extended H ii regions. This review will concentrate on discussing the results of
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Publications of the Astronomical Society of the Pacific, 1974
This is a review of the current status of the study of H II regions in other galaxies, especially their spatial distribution and relation to galactic structure. An extensive table compiles all available data on the H-alpha surveys of galaxies.
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This is a review of the current status of the study of H II regions in other galaxies, especially their spatial distribution and relation to galactic structure. An extensive table compiles all available data on the H-alpha surveys of galaxies.
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1974
The study of HII regions is very old. In the 17th century Christiaan Huygens had already observed and described the Orion nebula. Our understanding of this and similar objects increased dramatically between 1925 and 1940 when quantum theory made it possible to interprete the emission line spectra quantitatively.
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The study of HII regions is very old. In the 17th century Christiaan Huygens had already observed and described the Orion nebula. Our understanding of this and similar objects increased dramatically between 1925 and 1940 when quantum theory made it possible to interprete the emission line spectra quantitatively.
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