scholarly journals Neutral Hydrogen Gas in the Taurus?Orion Region Observed with a Multichannel 21 cm Line Receiver

1959 ◽  
Vol 12 (2) ◽  
pp. 127 ◽  
Author(s):  
RX McGee ◽  
JD Murray
Keyword(s):  
Line Profile ◽  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
Hydrogen Line ◽  
Short Time

A multichannel 21 cm hydrogen line receiver has been developed which is capable of producing a complete line profile in the very short time of 2 min.

scholarly journals A Sky Survey of Neutral Hydrogen at l 21 cm. II. The Detailed Distribution of Low Velocity Gas

1963 ◽  
Vol 16 (1) ◽  
pp. 136 ◽  
Author(s):  
RX McGee ◽  
JD Murray ◽  
Janice A Milton
Keyword(s):  
Radial Velocity ◽  
Line Profile ◽  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
Hydrogen Line ◽  
Low Velocity ◽  
Sky Survey

The distributions of intensity and radial velocity of neutral hydrogen gas of low radial velocity are presented in the form of detailed diagrams of T max., the temperature at the peak of a hydrogen line profile, and of the radial velocity value at the Tmax .

scholarly journals Hydrogen Content of Young Stellar Clusters. I. Methods of Observation and Reduction

1973 ◽  
Vol 26 (6) ◽  
pp. 829 ◽  
Author(s):  
HM Tovmassian
Keyword(s):  
Radio Telescope ◽  
Hydrogen Content ◽  
Data Reduction ◽  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
Continuum Emission ◽  
Stellar Clusters ◽  
Hydrogen Line ◽  
Galactic Clusters

Observations of 16 open galactic clusters in their continuum emission and at the neutral hydrogen line have been made with the Parkes 64 m radio telescope in an attempt to determine the total amount of hydrogen gas associated with them. In this, the first of a series of five papers, the observing procedure and the method of data reduction are described.

scholarly journals 21 cm Hydrogen-line Survey of the Large Magellanic Cloud. I. Stellar, Nebular, and Neutral Hydrogen Radial Velocities

1964 ◽  
Vol 17 (4) ◽  
pp. 515 ◽  
Author(s):  
RX McGee
Keyword(s):  
Neutral Hydrogen ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Hydrogen Gas ◽  
Radial Velocities ◽  
Recent Survey ◽  
Hydrogen Line ◽  
Line Survey

A recent survey of the neutral hydrogen in the Large Magellanic Cloud with a 14'�5 beam and the 48�channel H�line receiver has afforded an opportunity to compare the radial velocities of a number of optical objects with the radial velocities of the hydrogen gas in their directions.

Motions of neutral hydrogen at high latitudes

1967 ◽  
Vol 31 ◽  
pp. 265-278 ◽  
Author(s):  
A. Blaauw ◽  
I. Fejes ◽  
C. R. Tolbert ◽  
A. N. M. Hulsbosch ◽  
E. Raimond
Keyword(s):  
Surface Density ◽  
Velocity Dispersion ◽  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
High Latitudes ◽  
Low Velocity

Earlier investigations have shown that there is a preponderance of negative velocities in the hydrogen gas at high latitudes, and that in certain areas very little low-velocity gas occurs. In the region 100° <l< 250°, + 40° <b< + 85°, there appears to be a disturbance, with velocities between - 30 and - 80 km/sec. This ‘streaming’ involves about 3000 (r/100)2solar masses (rin pc). In the same region there is a low surface density at low velocities (|V| < 30 km/sec). About 40% of the gas in the disturbance is in the form of separate concentrations superimposed on a relatively smooth background. The number of these concentrations as a function of velocity remains constant from - 30 to - 60 km/sec but drops rapidly at higher negative velocities. The velocity dispersion in the concentrations varies little about 6·2 km/sec. Concentrations at positive velocities are much less abundant.

scholarly journals Sensitive Search for HI in E and SO galaxies

1983 ◽  
Vol 100 ◽  
pp. 305-306
Author(s):  
Norbert Thonnard
Keyword(s):  
Neutral Hydrogen ◽  
Optical Image ◽  
Type I ◽  
Hydrogen Line ◽  
Upper Limit

Do elliptical and SO galaxies in which type I supernovae (SNI) were detected contain more gas than those without SNI detections? Thirteen E and SO galaxies in the Virgo and Pegasus I clusters, seven with SNI detections and six without, were mapped well beyond the optical image at the 21-cm neutral hydrogen line. No HI was detected. In Virgo, the upper limit to MMI/LB is between 0.0005 and 0.0024.

scholarly journals Warp or lag? The ionized and neutral hydrogen gas in the edge-on dwarf galaxy UGC 1281

2011 ◽  
Vol 414 (4) ◽  
pp. 3444-3457 ◽  
Author(s):  
P. Kamphuis ◽  
R. F. Peletier ◽  
P. C. van der Kruit ◽  
G. H. Heald
Keyword(s):  
Dwarf Galaxy ◽  
Neutral Hydrogen ◽  
Hydrogen Gas

Hydrogen gas re-emission from beam target bombarded by intense neutral hydrogen beam of 75–100 keV, 1.4 MW at the prototype JT-60 injector

1984 ◽  
Vol 128-129 ◽  
pp. 713-716 ◽  
Author(s):  
Takemasa Shibata ◽  
Mamoru Matsuoka ◽  
Yoshihiro Ohara ◽  
Yoshikazu Okumura ◽  
Kiyoshi Shibanuma
Keyword(s):  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
Hydrogen Beam

scholarly journals Line Intensity Mapping during the Epoch of Reionization

2017 ◽  
Vol 12 (S333) ◽  
pp. 250-253
Author(s):  
Marta B. Silva ◽  
Saleem Zaroubi
Keyword(s):  
High Redshift ◽  
Three Dimensional ◽  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
Light Sources ◽  
First Stars ◽  
Galaxy Surveys ◽  
Gas Phases ◽  
Intensity Mapping ◽  
High Redshift Universe

AbstractCharacterizing the properties and the evolution of the first stars and galaxies is a challenging task for traditional galaxy surveys since they are sensitivity limited and can only detect the brightest light sources. Three-dimensional intensity mapping (IM) of transition lines can be a valuable alternative to study the high redshift Universe given that this technique avoids sensitivity limitation problems by measuring the overall emission of a line, with a low resolution, without resolving its sources. While 21cm line IM surveys probe neutral hydrogen gas and can, therefore, be used to probe the state of the IGM and the evolution of the ionization field during the Epoch of Reionization (EoR). IM surveys of other lines, such as CO, CII, Ly-alpha or H-alpha, can be used to probe the galaxies which emitted most of the ionizing radiation responsible for the EoR. These lines will trace the different ISM gas phases, the excitation state of this gas, its metallicity, etc. This study addresses IM of multiple transition lines and how it can be used to probe the EoR and to constrain the redshift evolution of galaxy properties.

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