MASH‐II: more planetary nebulae from the AAO/UKST Hα survey
Identifieur interne : 001709 ( Istex/Corpus ); précédent : 001708; suivant : 001710MASH‐II: more planetary nebulae from the AAO/UKST Hα survey
Auteurs : Brent Miszalski ; Q. A. Parker ; A. Acker ; J. L. Birkby ; D. J. Frew ; A. KovacevicSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008-02-21.
English descriptors
- KwdEn :
- 2mass, 2mass image, Acker, Angular diameters, Arcmin, Arcsec, Barlow, Blue channels, Bright rims, Bright stars, Cambridge univ, Candidate lists, Candidate selection, Candidate selection criteria, Cent bipolar, Cent round, Central star, Deblending, Detection capability, Discovery techniques, Eld, Frew, Frew parker, Further cuts, Future papers, Galactic, Galactic bulge, Galactic distribution, Galactic latitudes, Galactic plane, Galaxy, Higher latitudes, Journal compilation, Large numbers, Local data base, Macquarie university, Mash, Miszalski, Mnras, Morphology, Mssso, Multiwavelength data, Ndez, Nebula, Object status, Photometric, Photometric data, Photometry, Pixel, Pixel data, Planetary nebulae, Previous surveys, Proc, Quotient, Quotient image, Quotient image search, Quotient images, Same fashion, Search criteria, Separate deblending, Side corner, Small groups, Small number, Star candidates, Stellar, Such images, Surface brightness, Symbiotic stars, Symp, Total number, Ukst supercosmos, Univ, Visualization techniques, Waveband.
- Teeft :
- 2mass, 2mass image, Acker, Angular diameters, Arcmin, Arcsec, Barlow, Blue channels, Bright rims, Bright stars, Cambridge univ, Candidate lists, Candidate selection, Candidate selection criteria, Cent bipolar, Cent round, Central star, Deblending, Detection capability, Discovery techniques, Eld, Frew, Frew parker, Further cuts, Future papers, Galactic, Galactic bulge, Galactic distribution, Galactic latitudes, Galactic plane, Galaxy, Higher latitudes, Journal compilation, Large numbers, Local data base, Macquarie university, Mash, Miszalski, Mnras, Morphology, Mssso, Multiwavelength data, Ndez, Nebula, Object status, Photometric, Photometric data, Photometry, Pixel, Pixel data, Planetary nebulae, Previous surveys, Proc, Quotient, Quotient image, Quotient image search, Quotient images, Same fashion, Search criteria, Separate deblending, Side corner, Small groups, Small number, Star candidates, Stellar, Such images, Surface brightness, Symbiotic stars, Symp, Total number, Ukst supercosmos, Univ, Visualization techniques, Waveband.
Abstract
We present a supplement to the Macquarie/AAO/Strasbourg Hα planetary nebulae (PNe) catalogue (MASH), which we denote MASH‐II. The supplement consists of over 300 true, likely and possible new Galactic PNe found after re‐examination of the entire AAO/UKST Hα survey of the Southern Galactic Plane in digital form. We have spectroscopically confirmed over 240 of these new candidates as bona fide PNe, and we include other high‐quality candidates awaiting spectroscopic confirmation as possible PNe. These latest discoveries largely comprise two distinct groups: small, star like or moderately resolved PNe at one end and mostly large, extremely low surface brightness PNe at the other. Neither group were easy to discover from simple visual scrutiny of the original survey exposures as for MASH but were relatively straightforward to uncover from the digital images via application of semi‐automated discovery techniques. We suspect the few PNe still hidden in the Hα survey will lie outside our search criteria or be difficult to find.
Url:
DOI: 10.1111/j.1365-2966.2007.12727.x
Links to Exploration step
ISTEX:7A84A4DAC76872A81BFDABDE5E28449ABF5FDA38Le document en format XML
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The supplement consists of over 300 true, likely and possible new Galactic PNe found after re‐examination of the entire AAO/UKST Hα survey of the Southern Galactic Plane in digital form. We have spectroscopically confirmed over 240 of these new candidates as bona fide PNe, and we include other high‐quality candidates awaiting spectroscopic confirmation as possible PNe. These latest discoveries largely comprise two distinct groups: small, star like or moderately resolved PNe at one end and mostly large, extremely low surface brightness PNe at the other. Neither group were easy to discover from simple visual scrutiny of the original survey exposures as for MASH but were relatively straightforward to uncover from the digital images via application of semi‐automated discovery techniques. We suspect the few PNe still hidden in the Hα survey will lie outside our search criteria or be difficult to find.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>eld</json:string><json:string>quotient</json:string><json:string>nebula</json:string><json:string>mnras</json:string><json:string>mash</json:string><json:string>arcsec</json:string><json:string>frew</json:string><json:string>arcmin</json:string><json:string>journal compilation</json:string><json:string>pixel</json:string><json:string>surface brightness</json:string><json:string>quotient images</json:string><json:string>2mass</json:string><json:string>photometry</json:string><json:string>mssso</json:string><json:string>deblending</json:string><json:string>proc</json:string><json:string>univ</json:string><json:string>galactic</json:string><json:string>ndez</json:string><json:string>miszalski</json:string><json:string>symp</json:string><json:string>cambridge univ</json:string><json:string>planetary nebulae</json:string><json:string>barlow</json:string><json:string>waveband</json:string><json:string>acker</json:string><json:string>photometric</json:string><json:string>small number</json:string><json:string>pixel data</json:string><json:string>central star</json:string><json:string>star candidates</json:string><json:string>quotient image search</json:string><json:string>bright stars</json:string><json:string>large numbers</json:string><json:string>stellar</json:string><json:string>discovery techniques</json:string><json:string>photometric data</json:string><json:string>galactic plane</json:string><json:string>galactic latitudes</json:string><json:string>galactic bulge</json:string><json:string>quotient image</json:string><json:string>frew parker</json:string><json:string>2mass image</json:string><json:string>detection capability</json:string><json:string>candidate selection</json:string><json:string>morphology</json:string><json:string>separate deblending</json:string><json:string>search criteria</json:string><json:string>small groups</json:string><json:string>blue channels</json:string><json:string>such images</json:string><json:string>visualization techniques</json:string><json:string>symbiotic stars</json:string><json:string>candidate selection criteria</json:string><json:string>future papers</json:string><json:string>local data base</json:string><json:string>side corner</json:string><json:string>same fashion</json:string><json:string>object status</json:string><json:string>ukst supercosmos</json:string><json:string>higher latitudes</json:string><json:string>galactic distribution</json:string><json:string>further cuts</json:string><json:string>angular diameters</json:string><json:string>multiwavelength data</json:string><json:string>cent bipolar</json:string><json:string>cent round</json:string><json:string>bright rims</json:string><json:string>candidate lists</json:string><json:string>macquarie university</json:string><json:string>total number</json:string><json:string>previous surveys</json:string><json:string>galaxy</json:string></teeft></keywords><author><json:item><name>Brent Miszalski</name><affiliations><json:string>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia</json:string><json:string>Observatoire Astronomique, Université Louis Pasteur, 67000 Strasbourg, France</json:string><json:string>E-mail: brent@ics.mq.edu.au</json:string></affiliations></json:item><json:item><name>Q. A. Parker</name><affiliations><json:string>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia</json:string><json:string>Anglo‐Australian Observatory, Epping, NSW 1710, Australia</json:string></affiliations></json:item><json:item><name>A. Acker</name><affiliations><json:string>Observatoire Astronomique, Université Louis Pasteur, 67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>J. L. Birkby</name><affiliations><json:string>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA</json:string></affiliations></json:item><json:item><name>D. J. Frew</name><affiliations><json:string>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia</json:string><json:string>Perth Observatory, Bickley, WA 6076, Australia</json:string></affiliations></json:item><json:item><name>A. Kovacevic</name><affiliations><json:string>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>astronomical data bases: miscellaneous</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>catalogues</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>surveys</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>planetary nebulae: general</value></json:item></subject><articleId><json:string>MNR12727</json:string></articleId><arkIstex>ark:/67375/WNG-221J6VNM-F</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We present a supplement to the Macquarie/AAO/Strasbourg Hα planetary nebulae (PNe) catalogue (MASH), which we denote MASH‐II. The supplement consists of over 300 true, likely and possible new Galactic PNe found after re‐examination of the entire AAO/UKST Hα survey of the Southern Galactic Plane in digital form. We have spectroscopically confirmed over 240 of these new candidates as bona fide PNe, and we include other high‐quality candidates awaiting spectroscopic confirmation as possible PNe. These latest discoveries largely comprise two distinct groups: small, star like or moderately resolved PNe at one end and mostly large, extremely low surface brightness PNe at the other. Neither group were easy to discover from simple visual scrutiny of the original survey exposures as for MASH but were relatively straightforward to uncover from the digital images via application of semi‐automated discovery techniques. We suspect the few PNe still hidden in the Hα survey will lie outside our search criteria or be difficult to find.</abstract><qualityIndicators><score>8.896</score><pdfWordCount>6694</pdfWordCount><pdfCharCount>37891</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>10</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>158</abstractWordCount><abstractCharCount>1035</abstractCharCount><keywordCount>4</keywordCount></qualityIndicators><title>MASH‐II: more planetary nebulae from the AAO/UKST Hα survey</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>384</volume><issue>2</issue><pages><first>525</first><last>534</last><total>10</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2007</json:string><json:string>2003</json:string><json:string>2008</json:string></date><geogName></geogName><orgName><json:string>National Science Foundation</json:string><json:string>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB</json:string><json:string>University of Massachusetts</json:string><json:string>California Institute of Technology</json:string><json:string>Macquarie University</json:string><json:string>UK Schmidt Telescope</json:string><json:string>National Aeronautics and Space</json:string><json:string>Australia Astronomique, Universit</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>A. Acker</json:string><json:string>Brent Miszalski</json:string><json:string>D. J. Frew</json:string><json:string>Warren Reid</json:string><json:string>I. Based</json:string><json:string>L. Birkby</json:string><json:string>Kyle DePew</json:string><json:string>Van de Steene</json:string><json:string>Louis Pasteur</json:string><json:string>Francois Ochsenbein</json:string><json:string>A. Parker</json:string><json:string>R. Pretorius</json:string><json:string>A. Kovacevic</json:string></persName><placeName><json:string>Ellipticity</json:string><json:string>Australia</json:string><json:string>Perth</json:string><json:string>Strasbourg</json:string><json:string>France</json:string></placeName><ref_url><json:string>http://vizier.u-strasbg.fr/vizier/MASH</json:string></ref_url><ref_bibl><json:string>Jacoby et al. 2007</json:string><json:string>Tylenda, Acker & Stenholm 1993</json:string><json:string>Harris et al. 2007</json:string><json:string>Corradi et al. 2003</json:string><json:string>Pierce 2005</json:string><json:string>Parker et al. 2006b</json:string><json:string>Gaustad et al. 2001</json:string><json:string>Bond et al. 2001</json:string><json:string>Cohen et al. 2007</json:string><json:string>Hambly et al. 2001</json:string><json:string>Moe & De Marco 2006</json:string><json:string>Parker et al. 2006a</json:string><json:string>Viironen et al. 2006</json:string><json:string>Frew, Parker & Russeil 2006b</json:string><json:string>B. Miszalski et al.</json:string><json:string>Keller et al. 2007</json:string><json:string>Madsen et al. 2006</json:string><json:string>Kronberger et al. 2006</json:string><json:string>Phillips 2001</json:string><json:string>Magrini 2006</json:string><json:string>Zijlstra & Pottasch 1991</json:string><json:string>Mampaso et al. 2006</json:string><json:string>Parker et al. 2005</json:string><json:string>Frew, Madsen & Parker 2006a</json:string><json:string>Drew et al. 2005</json:string><json:string>Frew & Parker 2006</json:string><json:string>Reid & Parker 2006</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-221J6VNM-F</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences biologiques et medicales</json:string><json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string><json:string>4 - biophysique des tissus, organes et organismes</json:string></inist></categories><publicationDate>2008</publicationDate><copyrightDate>2008</copyrightDate><doi><json:string>10.1111/j.1365-2966.2007.12727.x</json:string></doi><id>7A84A4DAC76872A81BFDABDE5E28449ABF5FDA38</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/7A84A4DAC76872A81BFDABDE5E28449ABF5FDA38/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/7A84A4DAC76872A81BFDABDE5E28449ABF5FDA38/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/7A84A4DAC76872A81BFDABDE5E28449ABF5FDA38/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">MASH‐II: more planetary nebulae from the AAO/UKST Hα survey</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2008 The Authors</licence></availability><date type="published" when="2008-02-21"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">MASH‐II: more planetary nebulae from the AAO/UKST Hα survey</title><title level="a" type="short">MASH‐II</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">Brent</forename><surname>Miszalski</surname></persName><affiliation>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation><affiliation>Observatoire Astronomique, Université Louis Pasteur, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation><affiliation>E‐mail: brent@ics.mq.edu.au</affiliation></author><author xml:id="author-0001"><persName><forename type="first">Q. A.</forename><surname>Parker</surname></persName><affiliation>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation><affiliation>Anglo‐Australian Observatory, Epping, NSW 1710, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">A.</forename><surname>Acker</surname></persName><affiliation>Observatoire Astronomique, Université Louis Pasteur, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">J. L.</forename><surname>Birkby</surname></persName><affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA</affiliation></author><author xml:id="author-0004"><persName><forename type="first">D. J.</forename><surname>Frew</surname></persName><affiliation>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation><affiliation>Perth Observatory, Bickley, WA 6076, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">A.</forename><surname>Kovacevic</surname></persName><affiliation>Department of Physics, Macquarie University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation></author><idno type="istex">7A84A4DAC76872A81BFDABDE5E28449ABF5FDA38</idno><idno type="ark">ark:/67375/WNG-221J6VNM-F</idno><idno type="DOI">10.1111/j.1365-2966.2007.12727.x</idno><idno type="unit">MNR12727</idno><idno type="toTypesetVersion">file:MNR.MNR12727.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2008.384.issue-2</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">384</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="525">525</biblScope><biblScope unit="page" to="534">534</biblScope><biblScope unit="page-count">10</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2008-02-21"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>We present a supplement to the Macquarie/AAO/Strasbourg Hα planetary nebulae (PNe) catalogue (MASH), which we denote MASH‐II. 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The supplement consists of over 300 true, likely and possible new Galactic PNe found after re‐examination of the entire AAO/UKST Hα survey of the Southern Galactic Plane in digital form. We have spectroscopically confirmed over 240 of these new candidates as bona fide PNe, and we include other high‐quality candidates awaiting spectroscopic confirmation as possible PNe. These latest discoveries largely comprise two distinct groups: small, star like or moderately resolved PNe at one end and mostly large, extremely low surface brightness PNe at the other. Neither group were easy to discover from simple visual scrutiny of the original survey exposures as for MASH but were relatively straightforward to uncover from the digital images via application of semi‐automated discovery techniques. 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Received 2007 November 15; in original form 2007 October 9</edition><copyrightDate encoding="w3cdtf">2008</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">8</extent><extent unit="tables">3</extent><extent unit="formulas">16</extent><extent unit="references">33</extent><extent unit="linksCrossRef">97</extent></physicalDescription><abstract lang="en">We present a supplement to the Macquarie/AAO/Strasbourg Hα planetary nebulae (PNe) catalogue (MASH), which we denote MASH‐II. The supplement consists of over 300 true, likely and possible new Galactic PNe found after re‐examination of the entire AAO/UKST Hα survey of the Southern Galactic Plane in digital form. We have spectroscopically confirmed over 240 of these new candidates as bona fide PNe, and we include other high‐quality candidates awaiting spectroscopic confirmation as possible PNe. These latest discoveries largely comprise two distinct groups: small, star like or moderately resolved PNe at one end and mostly large, extremely low surface brightness PNe at the other. Neither group were easy to discover from simple visual scrutiny of the original survey exposures as for MASH but were relatively straightforward to uncover from the digital images via application of semi‐automated discovery techniques. 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