Simulating observations of dark matter dominated galaxies: towards the optimal halo profile
Identifieur interne : 001132 ( Istex/Corpus ); précédent : 001131; suivant : 001133Simulating observations of dark matter dominated galaxies: towards the optimal halo profile
Auteurs : W. J. G. De Blok ; Albert Bosma ; Stacy McgaughSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2003-04.
English descriptors
- KwdEn :
- Arcsec, Asymptotic velocity, Blok, Bosma, Bottom panels, Bottom panels show, Burkert, Burkert halo, Burkert haloes, Central density, Centre, Core radius, Corresponding rotation curve, Dark matter, Data histogram, Data points, Dbmbr, Dispersion, Dynamical, Dynamical centre, Dynamical centres, Error bars, Galaxy, Gaussian, Gaussian scatter, Gure, Halo, Halo model, Halo models, Halo parameters, Halo velocity, Histogram, Independent data points, Inner part, Inner parts, Inner slope, Inner slopes, Kinematical, Kinematical lopsidedness, Kravtsov, Kravtsov curves, Kravtsov halo, Kravtsov haloes, Lopsidedness, Major axis, Mass distribution, Mcgaugh, Mcgaugh figure, Minimum disc, Mnras, Model rotation curves, Models show, Optical centre, Optical centres, Outer parts, Positive slopes, Precise value, Random motions, Random selection, Random value, Real data, Real galaxies, Resolution effects, Right panel, Rotation, Rotation curve, Rotation curves, Scatter, Similar conclusions, Simulation, Slope, Small number, Smbb, Smbb sample, Spiral arms, Star formation, Steeper slopes, Stellar, Swaters, Systematic effects, Systemic velocity, Velocity differences.
- Teeft :
- Arcsec, Asymptotic velocity, Blok, Bosma, Bottom panels, Bottom panels show, Burkert, Burkert halo, Burkert haloes, Central density, Centre, Core radius, Corresponding rotation curve, Dark matter, Data histogram, Data points, Dbmbr, Dispersion, Dynamical, Dynamical centre, Dynamical centres, Error bars, Galaxy, Gaussian, Gaussian scatter, Gure, Halo, Halo model, Halo models, Halo parameters, Halo velocity, Histogram, Independent data points, Inner part, Inner parts, Inner slope, Inner slopes, Kinematical, Kinematical lopsidedness, Kravtsov, Kravtsov curves, Kravtsov halo, Kravtsov haloes, Lopsidedness, Major axis, Mass distribution, Mcgaugh, Mcgaugh figure, Minimum disc, Mnras, Model rotation curves, Models show, Optical centre, Optical centres, Outer parts, Positive slopes, Precise value, Random motions, Random selection, Random value, Real data, Real galaxies, Resolution effects, Right panel, Rotation, Rotation curve, Rotation curves, Scatter, Similar conclusions, Simulation, Slope, Small number, Smbb, Smbb sample, Spiral arms, Star formation, Steeper slopes, Stellar, Swaters, Systematic effects, Systemic velocity, Velocity differences.
Abstract
Low surface brightness galaxies are dominated by dark matter, and their rotation curves thus reflect their dark matter distribution. Recent high‐resolution rotation curves suggest that their dark matter mass‐density distributions are dominated by a constant‐density core. This seems inconsistent with the predictions of cold dark matter (CDM) models which produce haloes with compact density cusps and steep mass‐density profiles. However, the observationally determined mass profiles may be affected by non‐circular motions, asymmetries and offsets between optical and dynamical centres, all of which tend to lower the observed slopes. Here we determine the impact of each of these effects on a variety of halo models, and we compare the results with observed mass‐density profiles. Our simulations suggest that no single systematic effect can reconcile the data with the cuspy CDM haloes. The data are best described by a model with a soft core with an inner power‐law mass‐density slope α=−0.2 ± 0.2. However, no single universal halo profile provides a completely adequate description of the data.
Url:
DOI: 10.1046/j.1365-8711.2003.06330.x
Links to Exploration step
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<front><div type="abstract" xml:lang="en">Low surface brightness galaxies are dominated by dark matter, and their rotation curves thus reflect their dark matter distribution. Recent high‐resolution rotation curves suggest that their dark matter mass‐density distributions are dominated by a constant‐density core. This seems inconsistent with the predictions of cold dark matter (CDM) models which produce haloes with compact density cusps and steep mass‐density profiles. However, the observationally determined mass profiles may be affected by non‐circular motions, asymmetries and offsets between optical and dynamical centres, all of which tend to lower the observed slopes. Here we determine the impact of each of these effects on a variety of halo models, and we compare the results with observed mass‐density profiles. Our simulations suggest that no single systematic effect can reconcile the data with the cuspy CDM haloes. The data are best described by a model with a soft core with an inner power‐law mass‐density slope α=−0.2 ± 0.2. However, no single universal halo profile provides a completely adequate description of the data.</div>
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<abstract>Low surface brightness galaxies are dominated by dark matter, and their rotation curves thus reflect their dark matter distribution. Recent high‐resolution rotation curves suggest that their dark matter mass‐density distributions are dominated by a constant‐density core. This seems inconsistent with the predictions of cold dark matter (CDM) models which produce haloes with compact density cusps and steep mass‐density profiles. However, the observationally determined mass profiles may be affected by non‐circular motions, asymmetries and offsets between optical and dynamical centres, all of which tend to lower the observed slopes. Here we determine the impact of each of these effects on a variety of halo models, and we compare the results with observed mass‐density profiles. Our simulations suggest that no single systematic effect can reconcile the data with the cuspy CDM haloes. The data are best described by a model with a soft core with an inner power‐law mass‐density slope α=−0.2 ± 0.2. However, no single universal halo profile provides a completely adequate description of the data.</abstract>
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