X-RAY PROPERTIES OF GROUPS OF GALAXIES. Mulchaey, J., S. Annu. Rev. Astron. Astrophys, 38:289-335, 2000. ![X-RAY PROPERTIES OF GROUPS OF GALAXIES [pdf]](https://bibbase.org/img/filetypes/pdf.svg "pdf")
Paper Website abstract bibtex s Abstract ROSAT observations indicate that approximately half of all nearby groups of galaxies contain spatially extended X-ray emission. The radial extent of the X-ray emission is typically 50–500 h −1 100 kpc or approximately 10–50% of the virial radius of the group. Diffuse X-ray emission is generally restricted to groups that contain at least one early-type galaxy. X-ray spectroscopy suggests the emission mechanism is most likely a combination of thermal bremsstrahlung and line emission. This interpretation requires that the entire volume of groups be filled with a hot, low-density gas known as the intragroup medium. ROSAT and ASCA observations indicate that the temperature of the diffuse gas in groups ranges from approximately 0.3 keV to 2 keV. Higher temperature groups tend to follow the correlations found for rich clusters between X-ray luminosity, temperature, and velocity dispersion. However, groups with temperatures below approximately 1 keV appear to fall off the cluster L X -T relationship (and possibly the L X -σ and σ -T cluster relationships, although evidence for these latter departures is at the present time not very strong). Deviations from the cluster L X -T relationship are consistent with preheating of the intragroup medium by an early generation of stars and supernovae. There is now considerable evidence that most X-ray groups are real, physical sys-tems and not chance superpositions or large-scale filaments viewed edge-on. Assuming the intragroup gas is in hydrostatic equilibrium, X-ray observations can be used to es-timate the masses of individual systems. ROSAT observations indicate that the typical mass of an X-ray group is ∼10 13 h −1 100 M out to the radius to which X-ray emission is currently detected. The observed baryonic masses of groups are a small fraction of the X-ray determined masses, which implies that groups are dominated by dark matter. On scales of the virial radius, the dominant baryonic component in groups is likely the intragroup medium.
@article{
title = {X-RAY PROPERTIES OF GROUPS OF GALAXIES},
type = {article},
year = {2000},
keywords = {dark matter,intragroup medium,masses,metallicity,temperature},
pages = {289-335},
volume = {38},
websites = {https://ned.ipac.caltech.edu/level5/Sept03/Mulchaey/paper.pdf},
id = {55bdb4a7-be19-3469-a1a4-d320cb003da6},
created = {2017-05-09T23:06:39.686Z},
accessed = {2017-05-09},
file_attached = {true},
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group_id = {5a95a0b6-1946-397c-b16a-114c6fdf3127},
last_modified = {2017-07-29T20:18:53.674Z},
tags = {X-ray,beta model},
read = {true},
starred = {false},
authored = {false},
confirmed = {true},
hidden = {false},
citation_key = {Mulchaey2000b},
folder_uuids = {a55b3938-9553-4705-9661-67c5f054d79a},
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abstract = {s Abstract ROSAT observations indicate that approximately half of all nearby groups of galaxies contain spatially extended X-ray emission. The radial extent of the X-ray emission is typically 50–500 h −1 100 kpc or approximately 10–50% of the virial radius of the group. Diffuse X-ray emission is generally restricted to groups that contain at least one early-type galaxy. X-ray spectroscopy suggests the emission mechanism is most likely a combination of thermal bremsstrahlung and line emission. This interpretation requires that the entire volume of groups be filled with a hot, low-density gas known as the intragroup medium. ROSAT and ASCA observations indicate that the temperature of the diffuse gas in groups ranges from approximately 0.3 keV to 2 keV. Higher temperature groups tend to follow the correlations found for rich clusters between X-ray luminosity, temperature, and velocity dispersion. However, groups with temperatures below approximately 1 keV appear to fall off the cluster L X -T relationship (and possibly the L X -σ and σ -T cluster relationships, although evidence for these latter departures is at the present time not very strong). Deviations from the cluster L X -T relationship are consistent with preheating of the intragroup medium by an early generation of stars and supernovae. There is now considerable evidence that most X-ray groups are real, physical sys-tems and not chance superpositions or large-scale filaments viewed edge-on. Assuming the intragroup gas is in hydrostatic equilibrium, X-ray observations can be used to es-timate the masses of individual systems. ROSAT observations indicate that the typical mass of an X-ray group is ∼10 13 h −1 100 M out to the radius to which X-ray emission is currently detected. The observed baryonic masses of groups are a small fraction of the X-ray determined masses, which implies that groups are dominated by dark matter. On scales of the virial radius, the dominant baryonic component in groups is likely the intragroup medium.},
bibtype = {article},
author = {Mulchaey, John S.},
journal = {Annu. Rev. Astron. Astrophys}
}
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The radial extent of the X-ray emission is typically 50–500 h −1 100 kpc or approximately 10–50% of the virial radius of the group. Diffuse X-ray emission is generally restricted to groups that contain at least one early-type galaxy. X-ray spectroscopy suggests the emission mechanism is most likely a combination of thermal bremsstrahlung and line emission. This interpretation requires that the entire volume of groups be filled with a hot, low-density gas known as the intragroup medium. ROSAT and ASCA observations indicate that the temperature of the diffuse gas in groups ranges from approximately 0.3 keV to 2 keV. Higher temperature groups tend to follow the correlations found for rich clusters between X-ray luminosity, temperature, and velocity dispersion. However, groups with temperatures below approximately 1 keV appear to fall off the cluster L X -T relationship (and possibly the L X -σ and σ -T cluster relationships, although evidence for these latter departures is at the present time not very strong). Deviations from the cluster L X -T relationship are consistent with preheating of the intragroup medium by an early generation of stars and supernovae. There is now considerable evidence that most X-ray groups are real, physical sys-tems and not chance superpositions or large-scale filaments viewed edge-on. Assuming the intragroup gas is in hydrostatic equilibrium, X-ray observations can be used to es-timate the masses of individual systems. ROSAT observations indicate that the typical mass of an X-ray group is ∼10 13 h −1 100 M out to the radius to which X-ray emission is currently detected. 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