NDLI: Nuclear star formation on 100 parsec scales: 10" resolution radio continuum, hi and co observations

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Nuclear star formation on 100 parsec scales: 10" resolution radio continuum, hi and co observations

Content Provider	NASA Technical Reports Server (NTRS)
Author	Martin, Robert N. Ho, Paul T. P. Turner, Jean L.
Copyright Year	1987
Description	A program of radio line and continuum studies of star formation in nearby spiral galaxies is reported. The objective is a search for hot gas and peculiar dynamics in spiral nuclei with 10" to 30" angular resolution. Vigorous star formation is found to be a common phenomenon in the inner kpc of spirals. Arcsecond resolution observations of radio continuum emission at 6 and 2 cm were used to separate the thermal and nonthermal radio components. It was found that thermal and nonthermal emission are well mixed even on sizescales of 10 pc. To understand the reason for the increased level of star formation activity in spiral nuclei, HI and CO emission in these galaxies is studied. The CO transition was detected in M51, M82, NGC 253, NGC 6946 and IC 342 with T sub a approx. 0.5 to 2.0 K, at 20" angular resolution. The dynamics and spatial distribution of nuclear gas are being studied using VLA HI maps with 30" synthesized beams. Evidence for noncircular motions in HI was found in the nucleus of IC 342.
File Size	287570
Page Count	4
File Format	PDF
Alternate Webpage(s)	http://archive.org/details/NASA_NTRS_Archive_19870014889
Archival Resource Key	ark:/13960/t5w71bz4n
Language	English
Publisher Date	1987-05-01
Access Restriction	Open
Subject Keyword	Astrophysics Stellar Spectra Ionized Gases Neutral Gases Angular Resolution Radio Bursts Star Distribution High Temperature Gases Nonthermal Radiation Galactic Nuclei Radio Emission Thermal Emission Star Formation Spiral Galaxies Carbon Monoxide Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science
Content Type	Text
Resource Type	Article

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