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
ISTEX:5B46009C6CE3C9F24B99D32D464777784EAC6388Le document en format XML
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De Blok</name><affiliations><json:string>Australia Telescope National Facility, PO Box 76, Epping NSW 1710, Australia</json:string><json:string>Department of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB</json:string><json:string>E-mail: Erwin.deBlok@astro.cf.ac.uk</json:string></affiliations></json:item><json:item><name>Albert Bosma</name><affiliations><json:string>Observatoire de Marseille, 2 Place Le Verrier, 13248 Marseille Cedex 4, France</json:string></affiliations></json:item><json:item><name>Stacy McGaugh</name><affiliations><json:string>Department of Astronomy, University of Maryland, College Park, MD 20742‐2421, USA</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>galaxies: fundamental parameters</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: kinematics and dynamics</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>dark matter</value></json:item></subject><articleId><json:string>MNR6330</json:string></articleId><arkIstex>ark:/67375/WNG-Q9DGMZRW-S</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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><qualityIndicators><score>8.98</score><pdfWordCount>12561</pdfWordCount><pdfCharCount>65227</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>22</pdfPageCount><pdfPageSize>595.276 x 782.362 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>165</abstractWordCount><abstractCharCount>1101</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>Simulating observations of dark matter dominated galaxies: towards the optimal halo profile</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>340</volume><issue>2</issue><pages><first>657</first><last>678</last><total>22</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2002</json:string><json:string>2003</json:string></date><geogName></geogName><orgName><json:string>Cardiff University</json:string><json:string>Department Accepted</json:string><json:string>Department of Astronomy, University of Maryland</json:string><json:string>Australia of Physics and Astronomy</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>W. J. G. de Blok</json:string><json:string>Haute Provence</json:string><json:string>Albert Bosma</json:string><json:string>The</json:string><json:string>J. G. de Blok</json:string><json:string>College Park</json:string><json:string>S. McGaugh</json:string><json:string>A. Bosma</json:string><json:string>Stacy McGaugh</json:string></persName><placeName><json:string>Velocity</json:string><json:string>France</json:string><json:string>Marseille</json:string></placeName><ref_url></ref_url><ref_bibl><json:string>Pisano et al. 1998</json:string><json:string>van den Bosch & Swaters 2001</json:string><json:string>Navarro et al. 1996</json:string><json:string>Matthews & Wood 2001</json:string><json:string>de Blok, McGaugh & van der Hulst 1996</json:string><json:string>Weldrake et al. 2003</json:string><json:string>Kravtsov et al. 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(1996, 1997)</json:string><json:string>Athanassoula 2002</json:string><json:string>Burkert (1995)</json:string><json:string>Adler & Westpfahl 1996</json:string><json:string>Firmani et al. 2000</json:string><json:string>Marchesini et al. (2002)</json:string><json:string>de Blok et al. 2001b</json:string><json:string>Dubinksi & Carlberg 1991</json:string><json:string>Zhao 1996</json:string><json:string>Bosma 1978</json:string><json:string>Swaters et al.</json:string><json:string>Weldrake, de Blok, Walter 2003</json:string><json:string>Pisano, Wilcots & Elmegreen 1998</json:string><json:string>Garrido et al. 2002</json:string><json:string>Navarro et al. 1997</json:string><json:string>McGaugh et al. (2001)</json:string><json:string>Puche, Carignan & Bosma 1990</json:string><json:string>Blais-Ouellette et al. 2001</json:string><json:string>de Blok et al. (1996)</json:string><json:string>Wechsler et al. (2002)</json:string><json:string>Moore et al. 1998</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-Q9DGMZRW-S</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences biologiques et medicales</json:string><json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string><json:string>4 - ethologie animale</json:string></inist></categories><publicationDate>2003</publicationDate><copyrightDate>2003</copyrightDate><doi><json:string>10.1046/j.1365-8711.2003.06330.x</json:string></doi><id>5B46009C6CE3C9F24B99D32D464777784EAC6388</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/5B46009C6CE3C9F24B99D32D464777784EAC6388/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/5B46009C6CE3C9F24B99D32D464777784EAC6388/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/5B46009C6CE3C9F24B99D32D464777784EAC6388/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Simulating observations of dark matter dominated galaxies: towards the optimal halo profile</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Science Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2003-04"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">Simulating observations of dark matter dominated galaxies: towards the optimal halo profile</title><title level="a" type="short">LSB halo profiles</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">W. J. G.</forename><surname>De Blok</surname></persName><affiliation>Australia Telescope National Facility, PO Box 76, Epping NSW 1710, Australia<address><country key="AU"></country></address></affiliation><affiliation>Department of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB</affiliation><affiliation>E‐mail: Erwin.deBlok@astro.cf.ac.uk</affiliation></author><author xml:id="author-0001"><persName><forename type="first">Albert</forename><surname>Bosma</surname></persName><affiliation>Observatoire de Marseille, 2 Place Le Verrier, 13248 Marseille Cedex 4, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">Stacy</forename><surname>McGaugh</surname></persName><affiliation>Department of Astronomy, University of Maryland, College Park, MD 20742‐2421, USA<address><country key="US"></country></address></affiliation></author><idno type="istex">5B46009C6CE3C9F24B99D32D464777784EAC6388</idno><idno type="ark">ark:/67375/WNG-Q9DGMZRW-S</idno><idno type="DOI">10.1046/j.1365-8711.2003.06330.x</idno><idno type="unit">MNR6330</idno><idno type="supplier">mnr6330</idno><idno type="toTypesetVersion">file:MNR.MNR6330.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2003.340.issue-2</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">340</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="657">657</biblScope><biblScope unit="page" to="678">678</biblScope><biblScope unit="page-count">22</biblScope><publisher>Blackwell Science Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . 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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 <emph><span>α=−0.2 ± 0.2</span></emph>. 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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 <span type="mathematics">α=−0.2 ± 0.2</span>. 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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. 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