Planet gaps in the dust layer of 3D protoplanetary disks: II. Observability with ALMA
Identifieur interne : 000C97 ( PascalFrancis/Corpus ); précédent : 000C96; suivant : 000C98Planet gaps in the dust layer of 3D protoplanetary disks: II. Observability with ALMA
Auteurs : J.-F. Gonzalez ; C. Pinte ; S. T. Maddison ; F. Menard ; L. FouchetSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
Abstract
Context. The Atacama Large Millimeter/submillimeter Array (ALMA) will have the necessary resolution to observe a planetary gap created by a Jupiter-mass planet in a protoplanetary disk. Because it will observe at submillimeter and millimeter wavelengths, grains in the size range 10 μm to 1 cm are relevant for the thermal emission. For the standard parameters of a T Tauri disk, most grains of this size range are weakly coupled to the gas (leading to vertical settling and radial migration) and the common approximation of well-mixed gas and dust does not hold. Aims. We provide predictions for ALMA observations of planet gaps that account for the specific spatial distribution of dust that results from consistent gas+dust dynamics. Methods. In a previous work, we ran full 3D, two-fluid Smoothed Particle Hydrodynamics (SPH) simulations of a planet embedded in a gas+dust T Tauri disk for different planet masses and grain sizes. In this work, the resulting dust distributions are passed to the Monte Carlo radiative transfer code MCFOST to construct synthetic images in the ALMA wavebands. We then use the ALMA simulator to produce images that include thermal and phase noise for a range of angular resolutions, wavelengths, and integration times, as well as for different inclinations, declinations and distances. We also produce images which assume that gas and dust are well mixed with a gas-to-dust ratio of 100 to compare with previous ALMA predictions, all made under this hypothesis. Results. Our findings clearly demonstrate the importance of correctly incorporating the dust dynamics. We show that the gap carved by a 1 MJ planet orbiting at 40 AU is visible with a much higher contrast than the well-mixed assumption would predict. In the case of a 5 MJ planet, we clearly see a deficit in dust emission in the inner disk, and point out the risk of interpreting the resulting image as that of a transition disk with an inner hole if observed in unfavorable conditions. Planet signatures are fainter in more distant disks but declination or inclination to the line-of-sight have little effect on ALMA's ability to resolve the gaps. Conclusions. ALMA has the potential to see signposts of planets in disks of nearby star-forming regions. We present optimized observing parameters to detect them in the case of 1 and 5 Mj planets on 40 AU orbits.
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NO : | PASCAL 13-0057302 INIST |
---|---|
ET : | Planet gaps in the dust layer of 3D protoplanetary disks: II. Observability with ALMA |
AU : | GONZALEZ (J.-F.); PINTE (C.); MADDISON (S. T.); MENARD (F.); FOUCHET (L.) |
AF : | Université de Lyon, 69003 Lyon, France; Université Lyon 1, Observatoire de Lyon, 9 avenue Charles André, 69230 Saint-Genis Laval, France; CNRS, UMR 5574, Centre de Recherche Astrophysique de Lyon, France; École Normale Supérieure de Lyon/69007 Lyon/France (1 aut.); UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble, UMR 5274/38041 Grenoble/France (2 aut., 4 aut.); Centre for Astrophysics and Supercomputing, Swinburne Institute of Technology, PO Box 218/Hawthorn, VIC 3122/Australie (3 aut.); Physikalisches Institute, Universität Bern/3012 Bern/Suisse (5 aut.) |
DT : | Publication en série; Niveau analytique |
SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 547; No. p. 1; A58.1-A58.12; Bibl. 1/4 p. |
LA : | Anglais |
EA : | Context. The Atacama Large Millimeter/submillimeter Array (ALMA) will have the necessary resolution to observe a planetary gap created by a Jupiter-mass planet in a protoplanetary disk. Because it will observe at submillimeter and millimeter wavelengths, grains in the size range 10 μm to 1 cm are relevant for the thermal emission. For the standard parameters of a T Tauri disk, most grains of this size range are weakly coupled to the gas (leading to vertical settling and radial migration) and the common approximation of well-mixed gas and dust does not hold. Aims. We provide predictions for ALMA observations of planet gaps that account for the specific spatial distribution of dust that results from consistent gas+dust dynamics. Methods. In a previous work, we ran full 3D, two-fluid Smoothed Particle Hydrodynamics (SPH) simulations of a planet embedded in a gas+dust T Tauri disk for different planet masses and grain sizes. In this work, the resulting dust distributions are passed to the Monte Carlo radiative transfer code MCFOST to construct synthetic images in the ALMA wavebands. We then use the ALMA simulator to produce images that include thermal and phase noise for a range of angular resolutions, wavelengths, and integration times, as well as for different inclinations, declinations and distances. We also produce images which assume that gas and dust are well mixed with a gas-to-dust ratio of 100 to compare with previous ALMA predictions, all made under this hypothesis. Results. Our findings clearly demonstrate the importance of correctly incorporating the dust dynamics. We show that the gap carved by a 1 MJ planet orbiting at 40 AU is visible with a much higher contrast than the well-mixed assumption would predict. In the case of a 5 MJ planet, we clearly see a deficit in dust emission in the inner disk, and point out the risk of interpreting the resulting image as that of a transition disk with an inner hole if observed in unfavorable conditions. Planet signatures are fainter in more distant disks but declination or inclination to the line-of-sight have little effect on ALMA's ability to resolve the gaps. Conclusions. ALMA has the potential to see signposts of planets in disks of nearby star-forming regions. We present optimized observing parameters to detect them in the case of 1 and 5 Mj planets on 40 AU orbits. |
CC : | 001E03 |
FD : | Planète Jupiter; Nébuleuse proto planétaire; Grosseur grain; Couplage faible; Répartition spatiale; Dynamique; Méthode SPH; Transfert radiatif; Bruit thermique; Bruit phase; Rapport gaz poussière; Etoile proche; Région formation stellaire; Orbite; Méthode numérique; Système planétaire |
ED : | Jupiter planet; Proto planetary nebula; Grain size; Weak coupling; Spatial distribution; Dynamics; Smoothed particle hydrodynamics method; Radiative transfer; Thermal noise; Phase noise; Gas to dust ratio; Nearby stars; Stellar formation region; Orbits; Numerical method; Planetary system |
SD : | Nebulosa proto planetaria; Acoplamiento débil; Método SPH; Relación gas polvo; Región formación estelar; Método numérico; Sistema planetario |
LO : | INIST-14176.354000506259050570 |
ID : | 13-0057302 |
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Pascal:13-0057302Le document en format XML
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<term>Nearby stars</term>
<term>Numerical method</term>
<term>Orbits</term>
<term>Phase noise</term>
<term>Planetary system</term>
<term>Proto planetary nebula</term>
<term>Radiative transfer</term>
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<term>Spatial distribution</term>
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<term>Nébuleuse proto planétaire</term>
<term>Grosseur grain</term>
<term>Couplage faible</term>
<term>Répartition spatiale</term>
<term>Dynamique</term>
<term>Méthode SPH</term>
<term>Transfert radiatif</term>
<term>Bruit thermique</term>
<term>Bruit phase</term>
<term>Rapport gaz poussière</term>
<term>Etoile proche</term>
<term>Région formation stellaire</term>
<term>Orbite</term>
<term>Méthode numérique</term>
<term>Système planétaire</term>
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<front><div type="abstract" xml:lang="en">Context. The Atacama Large Millimeter/submillimeter Array (ALMA) will have the necessary resolution to observe a planetary gap created by a Jupiter-mass planet in a protoplanetary disk. Because it will observe at submillimeter and millimeter wavelengths, grains in the size range 10 μm to 1 cm are relevant for the thermal emission. For the standard parameters of a T Tauri disk, most grains of this size range are weakly coupled to the gas (leading to vertical settling and radial migration) and the common approximation of well-mixed gas and dust does not hold. Aims. We provide predictions for ALMA observations of planet gaps that account for the specific spatial distribution of dust that results from consistent gas+dust dynamics. Methods. In a previous work, we ran full 3D, two-fluid Smoothed Particle Hydrodynamics (SPH) simulations of a planet embedded in a gas+dust T Tauri disk for different planet masses and grain sizes. In this work, the resulting dust distributions are passed to the Monte Carlo radiative transfer code MCFOST to construct synthetic images in the ALMA wavebands. We then use the ALMA simulator to produce images that include thermal and phase noise for a range of angular resolutions, wavelengths, and integration times, as well as for different inclinations, declinations and distances. We also produce images which assume that gas and dust are well mixed with a gas-to-dust ratio of 100 to compare with previous ALMA predictions, all made under this hypothesis. Results. Our findings clearly demonstrate the importance of correctly incorporating the dust dynamics. We show that the gap carved by a 1 M<sub>J</sub>
planet orbiting at 40 AU is visible with a much higher contrast than the well-mixed assumption would predict. In the case of a 5 M<sub>J</sub>
planet, we clearly see a deficit in dust emission in the inner disk, and point out the risk of interpreting the resulting image as that of a transition disk with an inner hole if observed in unfavorable conditions. Planet signatures are fainter in more distant disks but declination or inclination to the line-of-sight have little effect on ALMA's ability to resolve the gaps. Conclusions. ALMA has the potential to see signposts of planets in disks of nearby star-forming regions. We present optimized observing parameters to detect them in the case of 1 and 5 M<sub>j</sub>
planets on 40 AU orbits.</div>
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<fC01 i1="01" l="ENG"><s0>Context. The Atacama Large Millimeter/submillimeter Array (ALMA) will have the necessary resolution to observe a planetary gap created by a Jupiter-mass planet in a protoplanetary disk. Because it will observe at submillimeter and millimeter wavelengths, grains in the size range 10 μm to 1 cm are relevant for the thermal emission. For the standard parameters of a T Tauri disk, most grains of this size range are weakly coupled to the gas (leading to vertical settling and radial migration) and the common approximation of well-mixed gas and dust does not hold. Aims. We provide predictions for ALMA observations of planet gaps that account for the specific spatial distribution of dust that results from consistent gas+dust dynamics. Methods. In a previous work, we ran full 3D, two-fluid Smoothed Particle Hydrodynamics (SPH) simulations of a planet embedded in a gas+dust T Tauri disk for different planet masses and grain sizes. In this work, the resulting dust distributions are passed to the Monte Carlo radiative transfer code MCFOST to construct synthetic images in the ALMA wavebands. We then use the ALMA simulator to produce images that include thermal and phase noise for a range of angular resolutions, wavelengths, and integration times, as well as for different inclinations, declinations and distances. We also produce images which assume that gas and dust are well mixed with a gas-to-dust ratio of 100 to compare with previous ALMA predictions, all made under this hypothesis. Results. Our findings clearly demonstrate the importance of correctly incorporating the dust dynamics. We show that the gap carved by a 1 M<sub>J</sub>
planet orbiting at 40 AU is visible with a much higher contrast than the well-mixed assumption would predict. In the case of a 5 M<sub>J</sub>
planet, we clearly see a deficit in dust emission in the inner disk, and point out the risk of interpreting the resulting image as that of a transition disk with an inner hole if observed in unfavorable conditions. Planet signatures are fainter in more distant disks but declination or inclination to the line-of-sight have little effect on ALMA's ability to resolve the gaps. Conclusions. ALMA has the potential to see signposts of planets in disks of nearby star-forming regions. We present optimized observing parameters to detect them in the case of 1 and 5 M<sub>j</sub>
planets on 40 AU orbits.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
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<s5>26</s5>
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<s5>26</s5>
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<s5>27</s5>
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<s5>27</s5>
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<s5>28</s5>
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<s5>28</s5>
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<s5>29</s5>
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<s5>32</s5>
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<s5>32</s5>
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<s5>33</s5>
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<fC03 i1="08" i2="3" l="ENG"><s0>Radiative transfer</s0>
<s5>33</s5>
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<fC03 i1="09" i2="3" l="FRE"><s0>Bruit thermique</s0>
<s5>34</s5>
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<s5>36</s5>
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<s5>38</s5>
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<s5>38</s5>
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<s5>38</s5>
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<s5>39</s5>
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<fC03 i1="14" i2="3" l="ENG"><s0>Orbits</s0>
<s5>39</s5>
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<fC03 i1="15" i2="X" l="FRE"><s0>Méthode numérique</s0>
<s5>40</s5>
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<fC03 i1="15" i2="X" l="ENG"><s0>Numerical method</s0>
<s5>40</s5>
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<s5>40</s5>
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<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="ENG"><s0>Planetary system</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="SPA"><s0>Sistema planetario</s0>
<s5>41</s5>
</fC03>
<fN21><s1>035</s1>
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<server><NO>PASCAL 13-0057302 INIST</NO>
<ET>Planet gaps in the dust layer of 3D protoplanetary disks: II. Observability with ALMA</ET>
<AU>GONZALEZ (J.-F.); PINTE (C.); MADDISON (S. T.); MENARD (F.); FOUCHET (L.)</AU>
<AF>Université de Lyon, 69003 Lyon, France; Université Lyon 1, Observatoire de Lyon, 9 avenue Charles André, 69230 Saint-Genis Laval, France; CNRS, UMR 5574, Centre de Recherche Astrophysique de Lyon, France; École Normale Supérieure de Lyon/69007 Lyon/France (1 aut.); UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et d'Astrophysique de Grenoble, UMR 5274/38041 Grenoble/France (2 aut., 4 aut.); Centre for Astrophysics and Supercomputing, Swinburne Institute of Technology, PO Box 218/Hawthorn, VIC 3122/Australie (3 aut.); Physikalisches Institute, Universität Bern/3012 Bern/Suisse (5 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 547; No. p. 1; A58.1-A58.12; Bibl. 1/4 p.</SO>
<LA>Anglais</LA>
<EA>Context. The Atacama Large Millimeter/submillimeter Array (ALMA) will have the necessary resolution to observe a planetary gap created by a Jupiter-mass planet in a protoplanetary disk. Because it will observe at submillimeter and millimeter wavelengths, grains in the size range 10 μm to 1 cm are relevant for the thermal emission. For the standard parameters of a T Tauri disk, most grains of this size range are weakly coupled to the gas (leading to vertical settling and radial migration) and the common approximation of well-mixed gas and dust does not hold. Aims. We provide predictions for ALMA observations of planet gaps that account for the specific spatial distribution of dust that results from consistent gas+dust dynamics. Methods. In a previous work, we ran full 3D, two-fluid Smoothed Particle Hydrodynamics (SPH) simulations of a planet embedded in a gas+dust T Tauri disk for different planet masses and grain sizes. In this work, the resulting dust distributions are passed to the Monte Carlo radiative transfer code MCFOST to construct synthetic images in the ALMA wavebands. We then use the ALMA simulator to produce images that include thermal and phase noise for a range of angular resolutions, wavelengths, and integration times, as well as for different inclinations, declinations and distances. We also produce images which assume that gas and dust are well mixed with a gas-to-dust ratio of 100 to compare with previous ALMA predictions, all made under this hypothesis. Results. Our findings clearly demonstrate the importance of correctly incorporating the dust dynamics. We show that the gap carved by a 1 M<sub>J</sub>
planet orbiting at 40 AU is visible with a much higher contrast than the well-mixed assumption would predict. In the case of a 5 M<sub>J</sub>
planet, we clearly see a deficit in dust emission in the inner disk, and point out the risk of interpreting the resulting image as that of a transition disk with an inner hole if observed in unfavorable conditions. Planet signatures are fainter in more distant disks but declination or inclination to the line-of-sight have little effect on ALMA's ability to resolve the gaps. Conclusions. ALMA has the potential to see signposts of planets in disks of nearby star-forming regions. We present optimized observing parameters to detect them in the case of 1 and 5 M<sub>j</sub>
planets on 40 AU orbits.</EA>
<CC>001E03</CC>
<FD>Planète Jupiter; Nébuleuse proto planétaire; Grosseur grain; Couplage faible; Répartition spatiale; Dynamique; Méthode SPH; Transfert radiatif; Bruit thermique; Bruit phase; Rapport gaz poussière; Etoile proche; Région formation stellaire; Orbite; Méthode numérique; Système planétaire</FD>
<ED>Jupiter planet; Proto planetary nebula; Grain size; Weak coupling; Spatial distribution; Dynamics; Smoothed particle hydrodynamics method; Radiative transfer; Thermal noise; Phase noise; Gas to dust ratio; Nearby stars; Stellar formation region; Orbits; Numerical method; Planetary system</ED>
<SD>Nebulosa proto planetaria; Acoplamiento débil; Método SPH; Relación gas polvo; Región formación estelar; Método numérico; Sistema planetario</SD>
<LO>INIST-14176.354000506259050570</LO>
<ID>13-0057302</ID>
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