The macquarie/AAO/Strasbourg Hα planetary nebula catalogue : MASH
Identifieur interne : 002038 ( PascalFrancis/Curation ); précédent : 002037; suivant : 002039The macquarie/AAO/Strasbourg Hα planetary nebula catalogue : MASH
Auteurs : Quentin A. Parker [Australie] ; A. Acker [France] ; D. J. Frew [Australie] ; M. Hartley [Australie] ; A. E. J. Peyaud [Australie, France] ; F. Ochsenbein [France] ; S. Phillipps [Royaume-Uni] ; D. Russeil [France] ; S. F. Beaulieu [Canada] ; M. Cohen [États-Unis] ; J. Köppen [France] ; B. Miszalski [Australie] ; D. H. Morgan [Royaume-Uni] ; R. A. H. Morris [Royaume-Uni] ; M. J. Pierce [Australie, Royaume-Uni] ; A. E. Vaughan [Australie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2006.
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- topic : Spectrométrie.
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Abstract
We present the Macquarie/AAO/Strasbourg Ha Planetary Nebula Catalogue (MASH) of over 900 true, likely and possible new Galactic planetary nebulae (PNe) discovered from the AAO/UKST Ha survey of the southern Galactic plane. The combination of depth, resolution, uniformity and areal coverage of the Hα survey has opened up a hitherto unexplored region of parameter space permitting the detection of this significant new PN sample. Away from the Galactic bulge the new PNe are typically more evolved, of larger angular extent, of lower surface brightness and more obscured (i.e. extinguished) than those in most previous surveys. We have also doubled the number of PNe in the Galactic bulge itself and although most are compact, we have also found more evolved examples. The MASH catalogue represents the culmination of a seven-year programme of identification and confirmatory spectroscopy. A key strength is that the entire sample has been derived from the same, uniform observational data. The 60 per cent increase in known Galactic PNe represents the largest ever incremental sample of such discoveries and will have a significant impact on many aspects of PN research. This is especially important for studies at the faint end of the PN luminosity function which was previously poorly represented.
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Cohen</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Radio Astronomy Laboratory, University of California</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Koppen, J" sort="Koppen, J" uniqKey="Koppen J" first="J." last="Köppen">J. Köppen</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Observatoire Astronomique, Vniversité Louis Pasteur</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Miszalski, B" sort="Miszalski, B" uniqKey="Miszalski B" first="B." last="Miszalski">B. Miszalski</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Morgan, D H" sort="Morgan, D H" uniqKey="Morgan D" first="D. H." last="Morgan">D. H. Morgan</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Institute for Astronomy, School of Physics, University of Edinburgh</s1><s2>Edinburgh EH8 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Morris, R A H" sort="Morris, R A H" uniqKey="Morris R" first="R. A. H." last="Morris">R. A. H. Morris</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Astrophysics Group, University of Bristol, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Pierce, M J" sort="Pierce, M J" uniqKey="Pierce M" first="M. J." last="Pierce">M. J. Pierce</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Astrophysics Group, University of Bristol, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Vaughan, A E" sort="Vaughan, A E" uniqKey="Vaughan A" first="A. E." last="Vaughan">A. E. Vaughan</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">06-0519139</idno><date when="2006">2006</date><idno type="stanalyst">PASCAL 06-0519139 INIST</idno><idno type="RBID">Pascal:06-0519139</idno><idno type="wicri:Area/PascalFrancis/Corpus">004057</idno><idno type="wicri:Area/PascalFrancis/Curation">002038</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">The macquarie/AAO/Strasbourg Hα planetary nebula catalogue : MASH</title><author><name sortKey="Parker, Quentin A" sort="Parker, Quentin A" uniqKey="Parker Q" first="Quentin A." last="Parker">Quentin A. Parker</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Anglo-Australian Observatory</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>1 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Acker, A" sort="Acker, A" uniqKey="Acker A" first="A." last="Acker">A. Acker</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Observatoire Astronomique, Vniversité Louis Pasteur</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Frew, D J" sort="Frew, D J" uniqKey="Frew D" first="D. J." last="Frew">D. J. Frew</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Hartley, M" sort="Hartley, M" uniqKey="Hartley M" first="M." last="Hartley">M. Hartley</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>UK Schmidt Telescope, Anglo-Australian Observatory</s1><s2>Siding Spring, 2357 NSW</s2><s3>AUS</s3><sZ>4 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Peyaud, A E J" sort="Peyaud, A E J" uniqKey="Peyaud A" first="A. E. J." last="Peyaud">A. E. J. Peyaud</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Observatoire Astronomique, Vniversité Louis Pasteur</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Ochsenbein, F" sort="Ochsenbein, F" uniqKey="Ochsenbein F" first="F." last="Ochsenbein">F. Ochsenbein</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Observatoire Astronomique, Vniversité Louis Pasteur</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Phillipps, S" sort="Phillipps, S" uniqKey="Phillipps S" first="S." last="Phillipps">S. Phillipps</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Astrophysics Group, University of Bristol, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Russeil, D" sort="Russeil, D" uniqKey="Russeil D" first="D." last="Russeil">D. Russeil</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Laboiatoire d'Astrophysique de Marseille, 2 Place Le Verrier</s1><s2>13248 Marseille</s2><s3>FRA</s3><sZ>8 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Beaulieu, S F" sort="Beaulieu, S F" uniqKey="Beaulieu S" first="S. F." last="Beaulieu">S. F. Beaulieu</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Département de Physique, et Obseryatoire du mont Mégantic, Université Laval</s1><s2>Québec, QC, G1K 7P4</s2><s3>CAN</s3><sZ>9 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Cohen, M" sort="Cohen, M" uniqKey="Cohen M" first="M." last="Cohen">M. Cohen</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Radio Astronomy Laboratory, University of California</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>10 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Koppen, J" sort="Koppen, J" uniqKey="Koppen J" first="J." last="Köppen">J. Köppen</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Observatoire Astronomique, Vniversité Louis Pasteur</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Miszalski, B" sort="Miszalski, B" uniqKey="Miszalski B" first="B." last="Miszalski">B. Miszalski</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Morgan, D H" sort="Morgan, D H" uniqKey="Morgan D" first="D. H." last="Morgan">D. H. Morgan</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Institute for Astronomy, School of Physics, University of Edinburgh</s1><s2>Edinburgh EH8 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Morris, R A H" sort="Morris, R A H" uniqKey="Morris R" first="R. A. H." last="Morris">R. A. H. Morris</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Astrophysics Group, University of Bristol, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Pierce, M J" sort="Pierce, M J" uniqKey="Pierce M" first="M. J." last="Pierce">M. J. Pierce</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Astrophysics Group, University of Bristol, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Vaughan, A E" sort="Vaughan, A E" uniqKey="Vaughan A" first="A. E." last="Vaughan">A. E. Vaughan</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Australie</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="2006">2006</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>Astronomical catalogues</term><term>Galactic bulge</term><term>Galactic nebulae</term><term>Galactic planes</term><term>Luminosity function</term><term>Milky Way</term><term>Planetary nebulae</term><term>Spectroscopy</term><term>Surface brightness</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Nébuleuse planétaire</term><term>Catalogue astronomique</term><term>Nébuleuse galactique</term><term>Plan galactique</term><term>Bulbe galactique</term><term>Brillance surface</term><term>Spectrométrie</term><term>Fonction luminosité</term><term>Voie lactée</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 the Macquarie/AAO/Strasbourg Ha Planetary Nebula Catalogue (MASH) of over 900 true, likely and possible new Galactic planetary nebulae (PNe) discovered from the AAO/UKST Ha survey of the southern Galactic plane. The combination of depth, resolution, uniformity and areal coverage of the Hα survey has opened up a hitherto unexplored region of parameter space permitting the detection of this significant new PN sample. Away from the Galactic bulge the new PNe are typically more evolved, of larger angular extent, of lower surface brightness and more obscured (i.e. extinguished) than those in most previous surveys. We have also doubled the number of PNe in the Galactic bulge itself and although most are compact, we have also found more evolved examples. The MASH catalogue represents the culmination of a seven-year programme of identification and confirmatory spectroscopy. A key strength is that the entire sample has been derived from the same, uniform observational data. The 60 per cent increase in known Galactic PNe represents the largest ever incremental sample of such discoveries and will have a significant impact on many aspects of PN research. This is especially important for studies at the faint end of the PN luminosity function which was previously poorly represented.</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>373</s2></fA05><fA06><s2>1</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The macquarie/AAO/Strasbourg Hα planetary nebula catalogue : MASH</s1></fA08><fA11 i1="01" i2="1"><s1>PARKER (Quentin A.)</s1></fA11><fA11 i1="02" i2="1"><s1>ACKER (A.)</s1></fA11><fA11 i1="03" i2="1"><s1>FREW (D. J.)</s1></fA11><fA11 i1="04" i2="1"><s1>HARTLEY (M.)</s1></fA11><fA11 i1="05" i2="1"><s1>PEYAUD (A. E. J.)</s1></fA11><fA11 i1="06" i2="1"><s1>OCHSENBEIN (F.)</s1></fA11><fA11 i1="07" i2="1"><s1>PHILLIPPS (S.)</s1></fA11><fA11 i1="08" i2="1"><s1>RUSSEIL (D.)</s1></fA11><fA11 i1="09" i2="1"><s1>BEAULIEU (S. F.)</s1></fA11><fA11 i1="10" i2="1"><s1>COHEN (M.)</s1></fA11><fA11 i1="11" i2="1"><s1>KÖPPEN (J.)</s1></fA11><fA11 i1="12" i2="1"><s1>MISZALSKI (B.)</s1></fA11><fA11 i1="13" i2="1"><s1>MORGAN (D. H.)</s1></fA11><fA11 i1="14" i2="1"><s1>MORRIS (R. A. H.)</s1></fA11><fA11 i1="15" i2="1"><s1>PIERCE (M. J.)</s1></fA11><fA11 i1="16" i2="1"><s1>VAUGHAN (A. E.)</s1></fA11><fA14 i1="01"><s1>Department of Physics, Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>5 aut.</sZ><sZ>12 aut.</sZ><sZ>15 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="02"><s1>Anglo-Australian Observatory</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>1 aut.</sZ></fA14><fA14 i1="03"><s1>Observatoire Astronomique, Vniversité Louis Pasteur</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ><sZ>5 aut.</sZ><sZ>6 aut.</sZ><sZ>11 aut.</sZ></fA14><fA14 i1="04"><s1>UK Schmidt Telescope, Anglo-Australian Observatory</s1><s2>Siding Spring, 2357 NSW</s2><s3>AUS</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Astrophysics Group, University of Bristol, Tyndall Avenue</s1><s2>Bristol BS8 1TL</s2><s3>GBR</s3><sZ>7 aut.</sZ><sZ>14 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="06"><s1>Laboiatoire d'Astrophysique de Marseille, 2 Place Le Verrier</s1><s2>13248 Marseille</s2><s3>FRA</s3><sZ>8 aut.</sZ></fA14><fA14 i1="07"><s1>Département de Physique, et Obseryatoire du mont Mégantic, Université Laval</s1><s2>Québec, QC, G1K 7P4</s2><s3>CAN</s3><sZ>9 aut.</sZ></fA14><fA14 i1="08"><s1>Radio Astronomy Laboratory, University of California</s1><s2>Berkeley, CA 94720</s2><s3>USA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="09"><s1>Institute for Astronomy, School of Physics, University of Edinburgh</s1><s2>Edinburgh EH8 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ></fA14><fA20><s1>79-94</s1></fA20><fA21><s1>2006</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000143074830060</s5></fA43><fA44><s0>0000</s0><s1>© 2006 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.1/4</s0></fA45><fA47 i1="01" i2="1"><s0>06-0519139</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>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We present the Macquarie/AAO/Strasbourg Ha Planetary Nebula Catalogue (MASH) of over 900 true, likely and possible new Galactic planetary nebulae (PNe) discovered from the AAO/UKST Ha survey of the southern Galactic plane. The combination of depth, resolution, uniformity and areal coverage of the Hα survey has opened up a hitherto unexplored region of parameter space permitting the detection of this significant new PN sample. Away from the Galactic bulge the new PNe are typically more evolved, of larger angular extent, of lower surface brightness and more obscured (i.e. extinguished) than those in most previous surveys. We have also doubled the number of PNe in the Galactic bulge itself and although most are compact, we have also found more evolved examples. The MASH catalogue represents the culmination of a seven-year programme of identification and confirmatory spectroscopy. A key strength is that the entire sample has been derived from the same, uniform observational data. The 60 per cent increase in known Galactic PNe represents the largest ever incremental sample of such discoveries and will have a significant impact on many aspects of PN research. This is especially important for studies at the faint end of the PN luminosity function which was previously poorly represented.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Nébuleuse planétaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Planetary nebulae</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Catalogue astronomique</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Astronomical catalogues</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Nébuleuse galactique</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Galactic nebulae</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Plan galactique</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Galactic planes</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Bulbe galactique</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Galactic bulge</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Bulbo galáctico</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Brillance surface</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Surface brightness</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Brillantez superficie</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Spectrométrie</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Spectroscopy</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Fonction luminosité</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Luminosity function</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Voie lactée</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Milky Way</s0><s5>34</s5></fC03><fN21><s1>338</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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