An expanded Mbh-σ diagram, and a new calibration of active galactic nuclei masses
Identifieur interne : 001D57 ( PascalFrancis/Checkpoint ); précédent : 001D56; suivant : 001D58An expanded Mbh-σ diagram, and a new calibration of active galactic nuclei masses
Auteurs : Alister W. Graham [Australie] ; Christopher A. Onken [Australie] ; E. Athanassoula [France] ; F. Combes [France]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.
Descripteurs français
- Pascal (Inist)
- Noyau galactique actif, Galaxies spirales barrées, Borne supérieure, Trou noir, Analyse régression, Boucle réaction, Trou noir massif, Effondrement, Dispersion vitesse, Déplacement vers le rouge, Quasar, Dynamique, Modèle amas nucléaire, Amas stellaire, Catalogue astronomique, Galaxies actives, Noyau galaxies, Galaxies Seyfert, Cosmologie.
- Wicri :
- topic : Cosmologie.
English descriptors
- KwdEn :
- Active galaxies, Active galaxy nuclei, Astronomical catalogues, Barred spiral galaxies, Black holes, Collapse, Cosmology, Dynamics, Feedback, Galaxy nuclei, Massive black hole, Nuclear cluster model, Quasars, Red shift, Regression analysis, Seyfert galaxies, Star clusters, Upper bound, Velocity dispersion.
Abstract
We present an updated and improved Mbh-σ diagram containing 64 galaxies for which Mbh measurements (not just upper limits) are available. Because of new and increased black hole masses at the high-mass end, and a better representation of barred galaxies at the low-mass end, the 'classical' (all morphological type) Mbh-σ relation for predicting black hole masses is log(Mbh/M◦.) = (8.13 ± 0.05) + (5.13 ± 0.34)log [σ/200 km s-1], with an rms scatter of 0.43 dex. Modifying the regression analysis to correct for a hitherto overlooked sample bias in which black holes with masses <106 M◦. are not (yet) detectable, the relation steepens further to give log (Mbh/M◦.)=(8.15± 0.06) + (5.95±0.44)log[σ/200 km s-1]. We have also updated the 'barless' and 'elliptical-only' Mbh-σ relations introduced by Graham and Hu in 2008 due to the offset nature of barred galaxies. These relations have a total scatter as low as 0.34 dex and currently define the upper envelope of points in the Mbh-σ diagram. They also have a slope consistent with a value 5, in agreement with the prediction by Silk & Rees based on feedback from massive black holes in bulges built by monolithic collapse. Using updated virial products and velocity dispersions from 28 active galactic nuclei, we determine that the optimal scaling factor f - which brings their virial products in line with the 64 directly measured black hole masses - is 2.8+0.7-0.5. This is roughly half the value reported by Onken et al. and Woo et al., and consequently halves the mass estimates of most high-redshift quasars. Given that barred galaxies are, on average, located ˜0.5 dex below the 'barless' and 'elliptical-only' Mbh-σ relations, we have explored the results after separating the samples into barred and non-barred galaxies, and we have also developed a preliminary corrective term to the velocity dispersion based on bar dynamics. In addition, given the recently recognized coexistence of massive black holes and nuclear star clusters, we present the first ever (Mbh + Mnc)-σ diagram and begin to explore how galaxies shift from their former location in the Mbh-σ diagram.
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Graham</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Centre for Astrophysics and Supercomputing, Swinburne University of Technology</s1><s2>Hawthorn, VIC 3122</s2><s3>AUS</s3><sZ>1 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>Hawthorn, VIC 3122</wicri:noRegion></affiliation></author><author><name sortKey="Onken, Christopher A" sort="Onken, Christopher A" uniqKey="Onken C" first="Christopher A." last="Onken">Christopher A. Onken</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Mount Stromlo Observatory, the Australian National University Private Bag, Weston Creek PO</s1><s2>ACT 261</s2><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>ACT 261</wicri:noRegion></affiliation></author><author><name sortKey="Athanassoula, E" sort="Athanassoula, E" uniqKey="Athanassoula E" first="E." last="Athanassoula">E. Athanassoula</name><affiliation wicri:level="4"><inist:fA14 i1="03"><s1>Laboratoire d'Astrophysique de Marseille (LAM), UMR61 10, CNRS/Université de Provence, Technopôle de Marseille Etoile, 38 rue Frédéric Joliot Curie</s1><s2>13388 Marseille</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>13388 Marseille</wicri:noRegion><placeName><settlement type="city">Marseille</settlement><region type="région" nuts="2">Provence-Alpes-Côte d'Azur</region><settlement type="city">Marseille</settlement></placeName><orgName type="university">Université de Provence</orgName></affiliation></author><author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Observatoire de Paris, LERMA, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>75014 Paris</wicri:noRegion><placeName><settlement type="city">Paris</settlement><region type="région" nuts="2">Île-de-France</region></placeName></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Active galaxies</term><term>Active galaxy nuclei</term><term>Astronomical catalogues</term><term>Barred spiral galaxies</term><term>Black holes</term><term>Collapse</term><term>Cosmology</term><term>Dynamics</term><term>Feedback</term><term>Galaxy nuclei</term><term>Massive black hole</term><term>Nuclear cluster model</term><term>Quasars</term><term>Red shift</term><term>Regression analysis</term><term>Seyfert galaxies</term><term>Star clusters</term><term>Upper bound</term><term>Velocity dispersion</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Noyau galactique actif</term><term>Galaxies spirales barrées</term><term>Borne supérieure</term><term>Trou noir</term><term>Analyse régression</term><term>Boucle réaction</term><term>Trou noir massif</term><term>Effondrement</term><term>Dispersion vitesse</term><term>Déplacement vers le rouge</term><term>Quasar</term><term>Dynamique</term><term>Modèle amas nucléaire</term><term>Amas stellaire</term><term>Catalogue astronomique</term><term>Galaxies actives</term><term>Noyau galaxies</term><term>Galaxies Seyfert</term><term>Cosmologie</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Cosmologie</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present an updated and improved M<sub>bh</sub>-σ diagram containing 64 galaxies for which M<sub>bh</sub> measurements (not just upper limits) are available. Because of new and increased black hole masses at the high-mass end, and a better representation of barred galaxies at the low-mass end, the 'classical' (all morphological type) M<sub>bh</sub>-σ relation for predicting black hole masses is log(M<sub>bh</sub>/M<sub>◦.</sub>) = (8.13 ± 0.05) + (5.13 ± 0.34)log [σ/200 km s<sup>-1</sup>], with an rms scatter of 0.43 dex. Modifying the regression analysis to correct for a hitherto overlooked sample bias in which black holes with masses <10<sup>6</sup> M<sub>◦.</sub> are not (yet) detectable, the relation steepens further to give log (M<sub>bh</sub>/M<sub>◦.</sub>)=(8.15± 0.06) + (5.95±0.44)log[σ/200 km s<sup>-1</sup>]. We have also updated the 'barless' and 'elliptical-only' M<sub>bh</sub>-σ relations introduced by Graham and Hu in 2008 due to the offset nature of barred galaxies. These relations have a total scatter as low as 0.34 dex and currently define the upper envelope of points in the M<sub>bh</sub>-σ diagram. They also have a slope consistent with a value 5, in agreement with the prediction by Silk & Rees based on feedback from massive black holes in bulges built by monolithic collapse. Using updated virial products and velocity dispersions from 28 active galactic nuclei, we determine that the optimal scaling factor f - which brings their virial products in line with the 64 directly measured black hole masses - is 2.8<sup>+0.7</sup><sub>-0.5</sub>. This is roughly half the value reported by Onken et al. and Woo et al., and consequently halves the mass estimates of most high-redshift quasars. Given that barred galaxies are, on average, located ˜0.5 dex below the 'barless' and 'elliptical-only' M<sub>bh</sub>-σ relations, we have explored the results after separating the samples into barred and non-barred galaxies, and we have also developed a preliminary corrective term to the velocity dispersion based on bar dynamics. In addition, given the recently recognized coexistence of massive black holes and nuclear star clusters, we present the first ever (M<sub>bh</sub> + M<sub>nc</sub>)-σ diagram and begin to explore how galaxies shift from their former location in the M<sub>bh</sub>-σ diagram.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>412</s2></fA05><fA06><s2>4</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>An expanded M<sub>bh</sub>-σ diagram, and a new calibration of active galactic nuclei masses</s1></fA08><fA11 i1="01" i2="1"><s1>GRAHAM (Alister W.)</s1></fA11><fA11 i1="02" i2="1"><s1>ONKEN (Christopher A.)</s1></fA11><fA11 i1="03" i2="1"><s1>ATHANASSOULA (E.)</s1></fA11><fA11 i1="04" i2="1"><s1>COMBES (F.)</s1></fA11><fA14 i1="01"><s1>Centre for Astrophysics and Supercomputing, Swinburne University of Technology</s1><s2>Hawthorn, VIC 3122</s2><s3>AUS</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>Mount Stromlo Observatory, the Australian National University Private Bag, Weston Creek PO</s1><s2>ACT 261</s2><s3>AUS</s3><sZ>2 aut.</sZ></fA14><fA14 i1="03"><s1>Laboratoire d'Astrophysique de Marseille (LAM), UMR61 10, CNRS/Université de Provence, Technopôle de Marseille Etoile, 38 rue Frédéric Joliot Curie</s1><s2>13388 Marseille</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Observatoire de Paris, LERMA, 61 Av. de l'Observatoire</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>4 aut.</sZ></fA14><fA20><s1>2211-2228</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000192921690070</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>2 p.1/4</s0></fA45><fA47 i1="01" i2="1"><s0>11-0199608</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>USA</s0></fA66><fC01 i1="01" l="ENG"><s0>We present an updated and improved M<sub>bh</sub>-σ diagram containing 64 galaxies for which M<sub>bh</sub> measurements (not just upper limits) are available. Because of new and increased black hole masses at the high-mass end, and a better representation of barred galaxies at the low-mass end, the 'classical' (all morphological type) M<sub>bh</sub>-σ relation for predicting black hole masses is log(M<sub>bh</sub>/M<sub>◦.</sub>) = (8.13 ± 0.05) + (5.13 ± 0.34)log [σ/200 km s<sup>-1</sup>], with an rms scatter of 0.43 dex. Modifying the regression analysis to correct for a hitherto overlooked sample bias in which black holes with masses <10<sup>6</sup> M<sub>◦.</sub> are not (yet) detectable, the relation steepens further to give log (M<sub>bh</sub>/M<sub>◦.</sub>)=(8.15± 0.06) + (5.95±0.44)log[σ/200 km s<sup>-1</sup>]. We have also updated the 'barless' and 'elliptical-only' M<sub>bh</sub>-σ relations introduced by Graham and Hu in 2008 due to the offset nature of barred galaxies. These relations have a total scatter as low as 0.34 dex and currently define the upper envelope of points in the M<sub>bh</sub>-σ diagram. They also have a slope consistent with a value 5, in agreement with the prediction by Silk & Rees based on feedback from massive black holes in bulges built by monolithic collapse. Using updated virial products and velocity dispersions from 28 active galactic nuclei, we determine that the optimal scaling factor f - which brings their virial products in line with the 64 directly measured black hole masses - is 2.8<sup>+0.7</sup><sub>-0.5</sub>. This is roughly half the value reported by Onken et al. and Woo et al., and consequently halves the mass estimates of most high-redshift quasars. Given that barred galaxies are, on average, located ˜0.5 dex below the 'barless' and 'elliptical-only' M<sub>bh</sub>-σ relations, we have explored the results after separating the samples into barred and non-barred galaxies, and we have also developed a preliminary corrective term to the velocity dispersion based on bar dynamics. In addition, given the recently recognized coexistence of massive black holes and nuclear star clusters, we present the first ever (M<sub>bh</sub> + M<sub>nc</sub>)-σ diagram and begin to explore how galaxies shift from their former location in the M<sub>bh</sub>-σ diagram.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Noyau galactique actif</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Active galaxy nuclei</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Galaxies spirales barrées</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Barred spiral galaxies</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Borne supérieure</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Upper bound</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Cota superior</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Trou noir</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Black holes</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Analyse régression</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Regression analysis</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Boucle réaction</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Feedback</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Trou noir massif</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Massive black hole</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Agujero negro masivo</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Effondrement</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Collapse</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Desmoronamiento</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Dispersion vitesse</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Velocity dispersion</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Dispersión velocidad</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Déplacement vers le rouge</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Red shift</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Quasar</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Quasars</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Dynamique</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Dynamics</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Modèle amas nucléaire</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Nuclear cluster model</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Amas stellaire</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Star clusters</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Catalogue astronomique</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Astronomical catalogues</s0><s5>40</s5></fC03><fC03 i1="16" i2="3" l="FRE"><s0>Galaxies actives</s0><s5>41</s5></fC03><fC03 i1="16" i2="3" l="ENG"><s0>Active galaxies</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Noyau galaxies</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>Galaxy nuclei</s0><s5>42</s5></fC03><fC03 i1="18" i2="3" l="FRE"><s0>Galaxies Seyfert</s0><s5>43</s5></fC03><fC03 i1="18" i2="3" l="ENG"><s0>Seyfert galaxies</s0><s5>43</s5></fC03><fC03 i1="19" i2="3" l="FRE"><s0>Cosmologie</s0><s5>44</s5></fC03><fC03 i1="19" i2="3" l="ENG"><s0>Cosmology</s0><s5>44</s5></fC03><fN21><s1>129</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist><affiliations><list><country><li>Australie</li><li>France</li></country><region><li>Provence-Alpes-Côte d'Azur</li><li>Île-de-France</li></region><settlement><li>Marseille</li><li>Paris</li></settlement><orgName><li>Université de Provence</li></orgName></list><tree><country name="Australie"><noRegion><name sortKey="Graham, Alister W" sort="Graham, Alister W" uniqKey="Graham A" first="Alister W." last="Graham">Alister W. Graham</name></noRegion><name sortKey="Onken, Christopher A" sort="Onken, Christopher A" uniqKey="Onken C" first="Christopher A." last="Onken">Christopher A. Onken</name></country><country name="France"><region name="Provence-Alpes-Côte d'Azur"><name sortKey="Athanassoula, E" sort="Athanassoula, E" uniqKey="Athanassoula E" first="E." last="Athanassoula">E. Athanassoula</name></region><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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