PHR 1315−6555: a bipolar planetary nebula in the compact Hyades‐age open cluster ESO 96‐SC04
Identifieur interne : 006359 ( Main/Exploration ); précédent : 006358; suivant : 006360PHR 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, 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 ] ; 2011-05-21.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Spectrométrie.
English descriptors
- KwdEn :
- 2mass, 2mass data, Abundance, Abundance estimates, Acker, Age, Angular proximity, Arcsec, Astron, Asymptotic giant branch, Asymptotic reddening, Balmer decrements, Band image, Bipolar, Bipolar morphology, Bipolar nebula, Carraro, Carraro munari, Central star, Central stars, Chemical abundances, Cluster, Cluster distance, Cluster mass, Cluster member, Cluster membership, Cluster stars, Cspn, Cspn magnitude, Ctio, Discovery images, Distance estimates, Emission lines, Excellent agreement, Excitation class, Frew, Frew parker, Frinchaboy, Galactic, Galactic cluster, Galactic disc, Galactic longitude, Galactic scaleheight arguments, Globular cluster, Good agreement, Host cluster, Ifmr, Independent distance estimate, Initial discovery, Janes, Janes phelps, Kingsburgh barlow, Large distances, Luminosity, Macquarie university, Mash, Metallicity, Middle panel, Miszalski, Mnras, Monoceros stream, Monthly notices, Morphology, Nebula, Open cluster, Open cluster velocity dispersions, Open clusters, Optical spectra, Optical spectrum, Phelps, Photometry, Physical association, Physics astronomy, Planetary nebula, Planetary nebula project, Planetary nebulae, Possible type, Preliminary estimates, Progenitor, Progenitor mass, Progenitor star, Quotient image, Radial velocities, Radial velocity, Reddening, Reddening estimates, Reid parker, Saao, Saao spectrum, Same area, Schmidt plates, Sight line, Spatial coincidences, Spectral observations, Spectroscopy, Star clusters, Symbiotic stars, Total dirbe reddening estimate, Uxes, Velocity agreement, White dwarf stars, Zanstra temperature, Zanstra temperatures, Zijlstra.
- Teeft :
- 2mass, 2mass data, Abundance estimates, Acker, Angular proximity, Arcsec, Astron, Asymptotic reddening, Balmer decrements, Band image, Bipolar, Bipolar morphology, Carraro, Carraro munari, Central star, Central stars, Chemical abundances, Cluster, Cluster distance, Cluster mass, Cluster member, Cluster membership, Cluster stars, Cspn, Cspn magnitude, Ctio, Discovery images, Distance estimates, Emission lines, Excellent agreement, Excitation class, Frew, Frew parker, Frinchaboy, Galactic, Galactic disc, Galactic longitude, Galactic scaleheight arguments, Globular cluster, Good agreement, Host cluster, Ifmr, Independent distance estimate, Initial discovery, Janes, Janes phelps, Kingsburgh barlow, Large distances, Luminosity, Macquarie university, Mash, Metallicity, Middle panel, Miszalski, Mnras, Monoceros stream, Monthly notices, Morphology, Nebula, Open cluster, Open cluster velocity dispersions, Open clusters, Optical spectra, Phelps, Photometry, Physical association, Physics astronomy, Planetary nebula, Planetary nebula project, Planetary nebulae, Possible type, Preliminary estimates, Progenitor, Progenitor mass, Progenitor star, Quotient image, Radial velocities, Radial velocity, Reddening, Reddening estimates, Reid parker, Saao, Saao spectrum, Same area, Schmidt plates, Sight line, Spatial coincidences, Spectral observations, Symbiotic stars, Total dirbe reddening estimate, Uxes, Velocity agreement, Zanstra temperature, Zanstra temperatures, Zijlstra.
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 narrow‐band 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.
Url:
DOI: 10.1111/j.1365-2966.2011.18259.x
Affiliations:
- Allemagne, Australie, France, États-Unis
- Alsace (région administrative), Grand Est, Texas
- Illkirch–Graffenstaden
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type="published" when="2011-05-21">2011-05-21</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>2mass</term><term>2mass data</term><term>Abundance</term><term>Abundance estimates</term><term>Acker</term><term>Age</term><term>Angular proximity</term><term>Arcsec</term><term>Astron</term><term>Asymptotic giant branch</term><term>Asymptotic reddening</term><term>Balmer decrements</term><term>Band image</term><term>Bipolar</term><term>Bipolar morphology</term><term>Bipolar nebula</term><term>Carraro</term><term>Carraro munari</term><term>Central star</term><term>Central stars</term><term>Chemical abundances</term><term>Cluster</term><term>Cluster distance</term><term>Cluster mass</term><term>Cluster member</term><term>Cluster membership</term><term>Cluster stars</term><term>Cspn</term><term>Cspn magnitude</term><term>Ctio</term><term>Discovery images</term><term>Distance estimates</term><term>Emission lines</term><term>Excellent agreement</term><term>Excitation class</term><term>Frew</term><term>Frew parker</term><term>Frinchaboy</term><term>Galactic</term><term>Galactic cluster</term><term>Galactic disc</term><term>Galactic longitude</term><term>Galactic scaleheight arguments</term><term>Globular cluster</term><term>Good agreement</term><term>Host cluster</term><term>Ifmr</term><term>Independent distance estimate</term><term>Initial discovery</term><term>Janes</term><term>Janes phelps</term><term>Kingsburgh barlow</term><term>Large distances</term><term>Luminosity</term><term>Macquarie university</term><term>Mash</term><term>Metallicity</term><term>Middle panel</term><term>Miszalski</term><term>Mnras</term><term>Monoceros stream</term><term>Monthly notices</term><term>Morphology</term><term>Nebula</term><term>Open cluster</term><term>Open cluster velocity dispersions</term><term>Open clusters</term><term>Optical spectra</term><term>Optical spectrum</term><term>Phelps</term><term>Photometry</term><term>Physical association</term><term>Physics astronomy</term><term>Planetary nebula</term><term>Planetary nebula project</term><term>Planetary nebulae</term><term>Possible type</term><term>Preliminary estimates</term><term>Progenitor</term><term>Progenitor mass</term><term>Progenitor star</term><term>Quotient image</term><term>Radial velocities</term><term>Radial velocity</term><term>Reddening</term><term>Reddening estimates</term><term>Reid parker</term><term>Saao</term><term>Saao spectrum</term><term>Same area</term><term>Schmidt plates</term><term>Sight line</term><term>Spatial coincidences</term><term>Spectral observations</term><term>Spectroscopy</term><term>Star clusters</term><term>Symbiotic stars</term><term>Total dirbe reddening estimate</term><term>Uxes</term><term>Velocity agreement</term><term>White dwarf stars</term><term>Zanstra 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distance</term><term>Cluster mass</term><term>Cluster member</term><term>Cluster membership</term><term>Cluster stars</term><term>Cspn</term><term>Cspn magnitude</term><term>Ctio</term><term>Discovery images</term><term>Distance estimates</term><term>Emission lines</term><term>Excellent agreement</term><term>Excitation class</term><term>Frew</term><term>Frew parker</term><term>Frinchaboy</term><term>Galactic</term><term>Galactic disc</term><term>Galactic longitude</term><term>Galactic scaleheight arguments</term><term>Globular cluster</term><term>Good agreement</term><term>Host cluster</term><term>Ifmr</term><term>Independent distance estimate</term><term>Initial discovery</term><term>Janes</term><term>Janes phelps</term><term>Kingsburgh barlow</term><term>Large distances</term><term>Luminosity</term><term>Macquarie university</term><term>Mash</term><term>Metallicity</term><term>Middle panel</term><term>Miszalski</term><term>Mnras</term><term>Monoceros stream</term><term>Monthly notices</term><term>Morphology</term><term>Nebula</term><term>Open cluster</term><term>Open cluster velocity dispersions</term><term>Open clusters</term><term>Optical spectra</term><term>Phelps</term><term>Photometry</term><term>Physical association</term><term>Physics astronomy</term><term>Planetary nebula</term><term>Planetary nebula project</term><term>Planetary nebulae</term><term>Possible type</term><term>Preliminary estimates</term><term>Progenitor</term><term>Progenitor mass</term><term>Progenitor star</term><term>Quotient image</term><term>Radial velocities</term><term>Radial velocity</term><term>Reddening</term><term>Reddening estimates</term><term>Reid parker</term><term>Saao</term><term>Saao spectrum</term><term>Same area</term><term>Schmidt plates</term><term>Sight line</term><term>Spatial coincidences</term><term>Spectral observations</term><term>Symbiotic stars</term><term>Total dirbe reddening estimate</term><term>Uxes</term><term>Velocity agreement</term><term>Zanstra temperature</term><term>Zanstra temperatures</term><term>Zijlstra</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 narrow‐band 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><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>France</li><li>États-Unis</li></country><region><li>Alsace (région administrative)</li><li>Grand Est</li><li>Texas</li></region><settlement><li>Illkirch–Graffenstaden</li></settlement></list><tree><country name="Australie"><noRegion><name sortKey="Parker, Quentin A" sort="Parker, Quentin A" uniqKey="Parker Q" first="Quentin A." last="Parker">Quentin A. Parker</name></noRegion><name sortKey="Dobbie, Paul D" sort="Dobbie, Paul D" uniqKey="Dobbie P" first="Paul D." last="Dobbie">Paul D. Dobbie</name><name sortKey="Frew, David J" sort="Frew, David J" uniqKey="Frew D" first="David J." last="Frew">David J. Frew</name><name sortKey="Kovacevic, Anna V" sort="Kovacevic, Anna V" uniqKey="Kovacevic A" first="Anna V." last="Kovacevic">Anna V. Kovacevic</name><name sortKey="Miszalski, Brent" sort="Miszalski, Brent" uniqKey="Miszalski B" first="Brent" last="Miszalski">Brent Miszalski</name><name sortKey="Parker, Quentin A" sort="Parker, Quentin A" uniqKey="Parker Q" first="Quentin A." last="Parker">Quentin A. Parker</name><name sortKey="Parker, Quentin A" sort="Parker, Quentin A" uniqKey="Parker Q" first="Quentin A." last="Parker">Quentin A. Parker</name></country><country name="France"><noRegion><name sortKey="Miszalski, Brent" sort="Miszalski, Brent" uniqKey="Miszalski B" first="Brent" last="Miszalski">Brent Miszalski</name></noRegion><name sortKey="Koppen, Joachim" sort="Koppen, Joachim" uniqKey="Koppen J" first="Joachim" last="Köppen">Joachim Köppen</name><name sortKey="Koppen, Joachim" sort="Koppen, Joachim" uniqKey="Koppen J" first="Joachim" last="Köppen">Joachim Köppen</name></country><country name="États-Unis"><region name="Texas"><name sortKey="Frinchaboy, Peter M" sort="Frinchaboy, Peter M" uniqKey="Frinchaboy P" first="Peter M." last="Frinchaboy">Peter M. Frinchaboy</name></region></country><country name="Allemagne"><noRegion><name sortKey="Koppen, Joachim" sort="Koppen, Joachim" uniqKey="Koppen J" first="Joachim" last="Köppen">Joachim Köppen</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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