PHR 1315-6555: a bipolar planetary nebula in the compact Hyades-age open cluster ESO 96-SC04
Identifieur interne : 004233 ( PascalFrancis/Curation ); précédent : 004232; suivant : 004234PHR 1315-6555: a bipolar planetary nebula in the compact Hyades-age open cluster ESO 96-SC04
Auteurs : Quentin A. Parker [Australie] ; David J. Frew [Australie] ; Brent Miszalski [Australie, Royaume-Uni, France] ; Anna V. Kovacevic [Australie] ; Peter M. Frinchaboy [États-Unis] ; Paul D. Dobbie [Australie] ; Joachim Köppen [France, Allemagne]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Spectrométrie.
English descriptors
- KwdEn :
Abstract
We present a detailed study of a bipolar, possible Type I planetary nebula (PN), PHR 1315-6555 (PN G305.3-03.1), which was discovered as part of the Macquarie/AAO/Strasbourg Hα planetary nebula project (MASH), and that we considered at the time was an excellent candidate for membership of the distant, compact, intermediate-age open cluster, ESO 96-SC04. The strong evidence for this association is presented here, making this the only known example of a PN physically associated with a Galactic open cluster. Cluster membership is extremely important as it allows for very precise estimates of the fundamental properties of the PN as the cluster is at a known distance. The PN was discovered by one of us (QAP) during systematic MASH searches for new Galactic PNe of the AAO United Kingdom Schmidt Telescope (UKST) Hα survey and had been missed in earlier broad-band surveys, including specific CCD studies of the host cluster. We present original discovery images and Cerro Tololo Inter-American Observatory (CTIO) 4-m MOSAIC-II camera follow-up narrowband images that reveal its bipolar morphology. We also present (i) low-resolution optical spectra that spectroscopically confirm the PN, (ii) accurate radial velocities of PN and cluster stars from high-resolution spectroscopy which show they are consistent and (iii) a reliable, independent distance estimate to the PN using a robust PN distance indicator which agrees with the published cluster distance to within the errors. We also provide preliminary estimates of basic PN properties and abundance estimates from deeper spectra that show it to be of possible Type I chemistry. This is also consistent with its estimated turn-off mass. Taken together, these findings present a powerful case for clear physical association between the PN and host cluster. Results for this association will be of considerable interest to specialists across differing astrophysical disciplines, including PNe, white dwarfs and open clusters.
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Frew</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics & Astronomy, Macquarie University, North Ryde</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Miszalski, Brent" sort="Miszalski, Brent" uniqKey="Miszalski B" first="Brent" last="Miszalski">Brent Miszalski</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics & Astronomy, Macquarie University, North Ryde</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Centre for Astrophysics Research, STRI, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>3 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Observatoire de Strasbourg, 11 Rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Kovacevic, Anna V" sort="Kovacevic, Anna V" uniqKey="Kovacevic A" first="Anna V." last="Kovacevic">Anna V. 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Parker</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics & Astronomy, Macquarie University, North Ryde</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Australian Astronomical Observatory, PO Box 296, Epping</s1><s2>NSW 1710</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Frew, David J" sort="Frew, David J" uniqKey="Frew D" first="David J." last="Frew">David J. Frew</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics & Astronomy, Macquarie University, North Ryde</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Miszalski, Brent" sort="Miszalski, Brent" uniqKey="Miszalski B" first="Brent" last="Miszalski">Brent Miszalski</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics & Astronomy, Macquarie University, North Ryde</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Centre for Astrophysics Research, STRI, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>3 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Observatoire de Strasbourg, 11 Rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Kovacevic, Anna V" sort="Kovacevic, Anna V" uniqKey="Kovacevic A" first="Anna V." last="Kovacevic">Anna V. Kovacevic</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics & Astronomy, Macquarie University, North Ryde</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Frinchaboy, Peter M" sort="Frinchaboy, Peter M" uniqKey="Frinchaboy P" first="Peter M." last="Frinchaboy">Peter M. Frinchaboy</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Department of Physics & Astronomy, Texas Christian University, 2800 South University Dr</s1><s2>Fort Worth, TX 76129</s2><s3>USA</s3><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Dobbie, Paul D" sort="Dobbie, Paul D" uniqKey="Dobbie P" first="Paul D." last="Dobbie">Paul D. Dobbie</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Australian Astronomical Observatory, PO Box 296, Epping</s1><s2>NSW 1710</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>6 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Koppen, Joachim" sort="Koppen, Joachim" uniqKey="Koppen J" first="Joachim" last="Köppen">Joachim Köppen</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Observatoire de Strasbourg, 11 Rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>International Space University, Parc d'Innovation, 1 Rue Jean-Dominique Cassini</s1><s2>67400 Illkirch-Graffenstaden</s2><s3>FRA</s3><sZ>7 aut.</sZ></inist:fA14><country>France</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Institut für Theoretische Physik und Astrophysik, Universität Kiel</s1><s2>24098 Kiel</s2><s3>DEU</s3><sZ>7 aut.</sZ></inist:fA14><country>Allemagne</country></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>Abundance</term><term>Age</term><term>Asymptotic giant branch</term><term>Bipolar nebula</term><term>Galactic cluster</term><term>Morphology</term><term>Open clusters</term><term>Optical spectrum</term><term>Planetary nebulae</term><term>Radial velocity</term><term>Spectroscopy</term><term>Star clusters</term><term>White dwarf stars</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Nébuleuse bipolaire</term><term>Nébuleuse planétaire</term><term>Age</term><term>Amas ouvert</term><term>Amas galactique</term><term>Morphologie</term><term>Spectre optique</term><term>Vitesse radiale</term><term>Amas stellaire</term><term>Spectrométrie</term><term>Abondance</term><term>Naine blanche</term><term>Branche géante asymptotique</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Spectrométrie</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present a detailed study of a bipolar, possible Type I planetary nebula (PN), PHR 1315-6555 (PN G305.3-03.1), which was discovered as part of the Macquarie/AAO/Strasbourg Hα planetary nebula project (MASH), and that we considered at the time was an excellent candidate for membership of the distant, compact, intermediate-age open cluster, ESO 96-SC04. The strong evidence for this association is presented here, making this the only known example of a PN physically associated with a Galactic open cluster. Cluster membership is extremely important as it allows for very precise estimates of the fundamental properties of the PN as the cluster is at a known distance. The PN was discovered by one of us (QAP) during systematic MASH searches for new Galactic PNe of the AAO United Kingdom Schmidt Telescope (UKST) Hα survey and had been missed in earlier broad-band surveys, including specific CCD studies of the host cluster. We present original discovery images and Cerro Tololo Inter-American Observatory (CTIO) 4-m MOSAIC-II camera follow-up narrowband images that reveal its bipolar morphology. We also present (i) low-resolution optical spectra that spectroscopically confirm the PN, (ii) accurate radial velocities of PN and cluster stars from high-resolution spectroscopy which show they are consistent and (iii) a reliable, independent distance estimate to the PN using a robust PN distance indicator which agrees with the published cluster distance to within the errors. We also provide preliminary estimates of basic PN properties and abundance estimates from deeper spectra that show it to be of possible Type I chemistry. This is also consistent with its estimated turn-off mass. Taken together, these findings present a powerful case for clear physical association between the PN and host cluster. Results for this association will be of considerable interest to specialists across differing astrophysical disciplines, including PNe, white dwarfs and open clusters.</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>413</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>PHR 1315-6555: a bipolar planetary nebula in the compact Hyades-age open cluster ESO 96-SC04</s1></fA08><fA11 i1="01" i2="1"><s1>PARKER (Quentin A.)</s1></fA11><fA11 i1="02" i2="1"><s1>FREW (David J.)</s1></fA11><fA11 i1="03" i2="1"><s1>MISZALSKI (Brent)</s1></fA11><fA11 i1="04" i2="1"><s1>KOVACEVIC (Anna V.)</s1></fA11><fA11 i1="05" i2="1"><s1>FRINCHABOY (Peter M.)</s1></fA11><fA11 i1="06" i2="1"><s1>DOBBIE (Paul D.)</s1></fA11><fA11 i1="07" i2="1"><s1>KÖPPEN (Joachim)</s1></fA11><fA14 i1="01"><s1>Department of Physics & Astronomy, Macquarie University, North Ryde</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ></fA14><fA14 i1="02"><s1>Australian Astronomical Observatory, PO Box 296, Epping</s1><s2>NSW 1710</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>6 aut.</sZ></fA14><fA14 i1="03"><s1>Centre for Astrophysics Research, STRI, University of Hertfordshire</s1><s2>Hatfield AL10 9AB</s2><s3>GBR</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Observatoire de Strasbourg, 11 Rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></fA14><fA14 i1="05"><s1>Department of Physics & Astronomy, Texas Christian University, 2800 South University Dr</s1><s2>Fort Worth, TX 76129</s2><s3>USA</s3><sZ>5 aut.</sZ></fA14><fA14 i1="06"><s1>International Space University, Parc d'Innovation, 1 Rue Jean-Dominique Cassini</s1><s2>67400 Illkirch-Graffenstaden</s2><s3>FRA</s3><sZ>7 aut.</sZ></fA14><fA14 i1="07"><s1>Institut für Theoretische Physik und Astrophysik, Universität Kiel</s1><s2>24098 Kiel</s2><s3>DEU</s3><sZ>7 aut.</sZ></fA14><fA20><s1>1835-1844</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000192127200310</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0260719</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 a detailed study of a bipolar, possible Type I planetary nebula (PN), PHR 1315-6555 (PN G305.3-03.1), which was discovered as part of the Macquarie/AAO/Strasbourg Hα planetary nebula project (MASH), and that we considered at the time was an excellent candidate for membership of the distant, compact, intermediate-age open cluster, ESO 96-SC04. The strong evidence for this association is presented here, making this the only known example of a PN physically associated with a Galactic open cluster. Cluster membership is extremely important as it allows for very precise estimates of the fundamental properties of the PN as the cluster is at a known distance. The PN was discovered by one of us (QAP) during systematic MASH searches for new Galactic PNe of the AAO United Kingdom Schmidt Telescope (UKST) Hα survey and had been missed in earlier broad-band surveys, including specific CCD studies of the host cluster. We present original discovery images and Cerro Tololo Inter-American Observatory (CTIO) 4-m MOSAIC-II camera follow-up narrowband images that reveal its bipolar morphology. We also present (i) low-resolution optical spectra that spectroscopically confirm the PN, (ii) accurate radial velocities of PN and cluster stars from high-resolution spectroscopy which show they are consistent and (iii) a reliable, independent distance estimate to the PN using a robust PN distance indicator which agrees with the published cluster distance to within the errors. We also provide preliminary estimates of basic PN properties and abundance estimates from deeper spectra that show it to be of possible Type I chemistry. This is also consistent with its estimated turn-off mass. Taken together, these findings present a powerful case for clear physical association between the PN and host cluster. Results for this association will be of considerable interest to specialists across differing astrophysical disciplines, including PNe, white dwarfs and open clusters.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Nébuleuse bipolaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Bipolar nebula</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Nebulosa bipolar</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Nébuleuse planétaire</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Planetary nebulae</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Age</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Age</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Edad</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Amas ouvert</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Open clusters</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Amas galactique</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Galactic cluster</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Conglomerado galáctico</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Morphologie</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Morphology</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Spectre optique</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Optical spectrum</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Espectro óptico</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Vitesse radiale</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Radial velocity</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Amas stellaire</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Star clusters</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Spectrométrie</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Spectroscopy</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Abondance</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Abundance</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Naine blanche</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>White dwarf stars</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Branche géante asymptotique</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Asymptotic giant branch</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Rama gigante asintótica</s0><s5>38</s5></fC03><fN21><s1>178</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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{{Explor lien
|wiki= Wicri/Asie
|area= AustralieFrV1
|flux= PascalFrancis
|étape= Curation
|type= RBID
|clé= Pascal:11-0260719
|texte= PHR 1315-6555: a bipolar planetary nebula in the compact Hyades-age open cluster ESO 96-SC04
}}
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