Optical versus infrared studies of dusty galaxies and active galactic nuclei – I. Nebular emission lines
Identifieur interne : 000818 ( Main/Corpus ); précédent : 000817; suivant : 000819Optical versus infrared studies of dusty galaxies and active galactic nuclei – I. Nebular emission lines
Auteurs : Vivienne Wild ; Brent Groves ; Timothy Heckman ; Paule Sonnentrucker ; Lee Armus ; David Schiminovich ; Benjamin Johnson ; Lucimara Martins ; Stephanie LamassaSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-01-21.
English descriptors
Abstract
Optical nebular emission lines are commonly used to estimate the star formation rate of galaxies and the black hole accretion rate of their central active nuclei. The accuracy of the conversion from line strengths to physical properties depends upon the accuracy to which the lines can be corrected for dust attenuation. For studies of single galaxies with normal amounts of dust, most dust corrections result in the same derived properties within the errors. However, for statistical studies of populations of galaxies, or for studies of galaxies with higher dust contents, such as might be found in some classes of ‘transition’ galaxies, significant uncertainty arises from the dust attenuation correction. In this paper, we compare the strength of the predominantly unobscured mid‐infrared [Ne ii] λ15.5 μ m+[Ne iii] λ12.8 μ m emission lines to the optical Hα emission lines in four samples of galaxies: (i) ordinary star‐forming galaxies (80 galaxies); (ii) optically selected dusty galaxies (11); (iii) ultraluminous infrared galaxies (6); and (iv) Seyfert 2 galaxies (20). We show that a single dust attenuation curve applied to all samples can correct the Hα luminosity for dust attenuation to a factor better than 2. Similarly, we compare [O iv] and [O iii] luminosities to find that [O iii] can be corrected to a factor better than 3. This shows that the total dust attenuation suffered by the active galactic nucleus narrow‐line region is not significantly different from that suffered by the star‐forming H ii regions in the galaxy. We provide explicit dust attenuation corrections, together with errors, for [O ii], [O iii] and Hα. The best‐fitting average attenuation curve is slightly greyer than the Milky Way extinction law, indicating either that external galaxies have slightly different typical dust properties from those of the Milky Way or that there is a significant contribution from scattering. Finally, we uncover an intriguing correlation between silicate absorption and Balmer decrement, two measures of dust in galaxies, which probe entirely different regimes in optical depth.
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DOI: 10.1111/j.1365-2966.2010.17536.x
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The accuracy of the conversion from line strengths to physical properties depends upon the accuracy to which the lines can be corrected for dust attenuation. For studies of single galaxies with normal amounts of dust, most dust corrections result in the same derived properties within the errors. However, for statistical studies of populations of galaxies, or for studies of galaxies with higher dust contents, such as might be found in some classes of ‘transition’ galaxies, significant uncertainty arises from the dust attenuation correction. In this paper, we compare the strength of the predominantly unobscured mid‐infrared [Ne ii] λ15.5 μ m+[Ne iii] λ12.8 μ m emission lines to the optical Hα emission lines in four samples of galaxies: (i) ordinary star‐forming galaxies (80 galaxies); (ii) optically selected dusty galaxies (11); (iii) ultraluminous infrared galaxies (6); and (iv) Seyfert 2 galaxies (20). We show that a single dust attenuation curve applied to all samples can correct the Hα luminosity for dust attenuation to a factor better than 2. Similarly, we compare [O iv] and [O iii] luminosities to find that [O iii] can be corrected to a factor better than 3. This shows that the total dust attenuation suffered by the active galactic nucleus narrow‐line region is not significantly different from that suffered by the star‐forming H ii regions in the galaxy. We provide explicit dust attenuation corrections, together with errors, for [O ii], [O iii] and Hα. The best‐fitting average attenuation curve is slightly greyer than the Milky Way extinction law, indicating either that external galaxies have slightly different typical dust properties from those of the Milky Way or that there is a significant contribution from scattering. 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The accuracy of the conversion from line strengths to physical properties depends upon the accuracy to which the lines can be corrected for dust attenuation. For studies of single galaxies with normal amounts of dust, most dust corrections result in the same derived properties within the errors. However, for statistical studies of populations of galaxies, or for studies of galaxies with higher dust contents, such as might be found in some classes of ‘transition’ galaxies, significant uncertainty arises from the dust attenuation correction. In this paper, we compare the strength of the predominantly unobscured mid‐infrared [Ne ii] λ15.5 μ m+[Ne iii] λ12.8 μ m emission lines to the optical Hα emission lines in four samples of galaxies: (i) ordinary star‐forming galaxies (80 galaxies); (ii) optically selected dusty galaxies (11); (iii) ultraluminous infrared galaxies (6); and (iv) Seyfert 2 galaxies (20). We show that a single dust attenuation curve applied to all samples can correct the Hα luminosity for dust attenuation to a factor better than 2. Similarly, we compare [O iv] and [O iii] luminosities to find that [O iii] can be corrected to a factor better than 3. This shows that the total dust attenuation suffered by the active galactic nucleus narrow‐line region is not significantly different from that suffered by the star‐forming H ii regions in the galaxy. We provide explicit dust attenuation corrections, together with errors, for [O ii], [O iii] and Hα. The best‐fitting average attenuation curve is slightly greyer than the Milky Way extinction law, indicating either that external galaxies have slightly different typical dust properties from those of the Milky Way or that there is a significant contribution from scattering. 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The accuracy of the conversion from line strengths to physical properties depends upon the accuracy to which the lines can be corrected for dust attenuation. For studies of single galaxies with normal amounts of dust, most dust corrections result in the same derived properties within the errors. However, for statistical studies of populations of galaxies, or for studies of galaxies with higher dust contents, such as might be found in some classes of ‘transition’ galaxies, significant uncertainty arises from the dust attenuation correction. In this paper, we compare the strength of the predominantly unobscured mid‐infrared [Ne ii] λ15.5 μ m+[Ne iii] λ12.8 μ m emission lines to the optical Hα emission lines in four samples of galaxies: (i) ordinary star‐forming galaxies (80 galaxies); (ii) optically selected dusty galaxies (11); (iii) ultraluminous infrared galaxies (6); and (iv) Seyfert 2 galaxies (20). We show that a single dust attenuation curve applied to all samples can correct the Hα luminosity for dust attenuation to a factor better than 2. Similarly, we compare [O iv] and [O iii] luminosities to find that [O iii] can be corrected to a factor better than 3. This shows that the total dust attenuation suffered by the active galactic nucleus narrow‐line region is not significantly different from that suffered by the star‐forming H ii regions in the galaxy. We provide explicit dust attenuation corrections, together with errors, for [O ii], [O iii] and Hα. The best‐fitting average attenuation curve is slightly greyer than the Milky Way extinction law, indicating either that external galaxies have slightly different typical dust properties from those of the Milky Way or that there is a significant contribution from scattering. 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Journal compilation © 2010 RAS</copyright><eventGroup><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.4.2 mode:FullText" date="2011-01-06"></event><event type="publishedOnlineEarlyUnpaginated" date="2010-10-21"></event><event type="firstOnline" date="2010-10-21"></event><event type="publishedOnlineFinalForm" date="2011-01-06"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-03"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="1593">1593</numbering><numbering type="pageLast" number="1610">1610</numbering></numberingGroup><correspondenceTo> E‐mail: <email>wild@iap.fr</email></correspondenceTo><objectNameGroup><objectName elementName="appendix">Appendices</objectName></objectNameGroup><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR17536.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2010 August 16. Received 2010 August 16; in original form 2010 June 9</unparsedEditorialHistory><countGroup><count type="figureTotal" number="9"></count><count type="tableTotal" number="3"></count><count type="formulaTotal" number="296"></count><count type="referenceTotal" number="77"></count><count type="linksCrossRef" number="206"></count></countGroup><titleGroup><title type="main">Optical versus infrared studies of dusty galaxies and active galactic nuclei – I. Nebular emission lines</title><title type="shortAuthors"><i>V. Wild et al.</i></title><title type="short"><i>Nebular emission from dusty galaxies</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Vivienne</givenNames><familyName>Wild</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>Brent</givenNames><familyName>Groves</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a3"><personName><givenNames>Timothy</givenNames><familyName>Heckman</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a3"><personName><givenNames>Paule</givenNames><familyName>Sonnentrucker</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a4"><personName><givenNames>Lee</givenNames><familyName>Armus</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a5"><personName><givenNames>David</givenNames><familyName>Schiminovich</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a6"><personName><givenNames>Benjamin</givenNames><familyName>Johnson</familyName></personName></creator><creator creatorRole="author" xml:id="cr8" affiliationRef="#a7"><personName><givenNames>Lucimara</givenNames><familyName>Martins</familyName></personName></creator><creator creatorRole="author" xml:id="cr9" affiliationRef="#a3"><personName><givenNames>Stephanie</givenNames><familyName>LaMassa</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="FR"><unparsedAffiliation>Institut d'Astrophysique de Paris, CNRS, Université Pierre & Marie Curie, UMR 7095, 98bis bd Arago, 75014 Paris, France</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="NL"><unparsedAffiliation>Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, the Netherlands</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="US"><unparsedAffiliation>Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="US"><unparsedAffiliation>Caltech, Spitzer Science Center, MS 314‐6, Pasadena, CA 91125, USA</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="US"><unparsedAffiliation>Department of Astronomy, Columbia University, New York, NY 10027, USA</unparsedAffiliation></affiliation><affiliation xml:id="a6"><unparsedAffiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="BR"><unparsedAffiliation>NAT‐Universidade Cruzeirodo Sul, Sao Paulo, Brazil</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">dust, extinction</keyword><keyword xml:id="k2">galaxies: ISM</keyword><keyword xml:id="k3">galaxies: star formation</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>Optical nebular emission lines are commonly used to estimate the star formation rate of galaxies and the black hole accretion rate of their central active nuclei. The accuracy of the conversion from line strengths to physical properties depends upon the accuracy to which the lines can be corrected for dust attenuation. For studies of single galaxies with normal amounts of dust, most dust corrections result in the same derived properties within the errors. However, for statistical studies of populations of galaxies, or for studies of galaxies with higher dust contents, such as might be found in some classes of ‘transition’ galaxies, significant uncertainty arises from the dust attenuation correction. In this paper, we compare the strength of the predominantly unobscured mid‐infrared [Ne <sc>ii</sc>] <span type="mathematics">λ15.5 μ m</span>+[Ne <sc>iii</sc>] <span type="mathematics">λ12.8 μ m</span> emission lines to the optical H<span type="mathematics">α</span> emission lines in four samples of galaxies: (i) ordinary star‐forming galaxies (80 galaxies); (ii) optically selected dusty galaxies (11); (iii) ultraluminous infrared galaxies (6); and (iv) Seyfert 2 galaxies (20). We show that a single dust attenuation curve applied to all samples can correct the H<span type="mathematics">α</span> luminosity for dust attenuation to a factor better than 2. Similarly, we compare [O <sc>iv</sc>] and [O <sc>iii</sc>] luminosities to find that [O <sc>iii</sc>] can be corrected to a factor better than 3. This shows that the total dust attenuation suffered by the active galactic nucleus narrow‐line region is not significantly different from that suffered by the star‐forming H <sc>ii</sc> regions in the galaxy. We provide explicit dust attenuation corrections, together with errors, for [O <sc>ii</sc>], [O <sc>iii</sc>] and H<span type="mathematics">α</span>. The best‐fitting average attenuation curve is slightly greyer than the Milky Way extinction law, indicating either that external galaxies have slightly different typical dust properties from those of the Milky Way or that there is a significant contribution from scattering. Finally, we uncover an intriguing correlation between silicate absorption and Balmer decrement, two measures of dust in galaxies, which probe entirely different regimes in optical depth.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Optical versus infrared studies of dusty galaxies and active galactic nuclei – I. Nebular emission lines</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Nebular emission from dusty galaxies</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Optical versus infrared studies of dusty galaxies and active galactic nuclei – I. Nebular emission lines</title></titleInfo><name type="personal"><namePart type="given">Vivienne</namePart><namePart type="family">Wild</namePart><affiliation>Institut d'Astrophysique de Paris, CNRS, Université Pierre & Marie Curie, UMR 7095, 98bis bd Arago, 75014 Paris, France</affiliation><description>Correspondence: E‐mail: </description><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Brent</namePart><namePart type="family">Groves</namePart><affiliation>Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Timothy</namePart><namePart type="family">Heckman</namePart><affiliation>Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Paule</namePart><namePart type="family">Sonnentrucker</namePart><affiliation>Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Lee</namePart><namePart type="family">Armus</namePart><affiliation>Caltech, Spitzer Science Center, MS 314‐6, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">David</namePart><namePart type="family">Schiminovich</namePart><affiliation>Department of Astronomy, Columbia University, New York, NY 10027, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Benjamin</namePart><namePart type="family">Johnson</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Lucimara</namePart><namePart type="family">Martins</namePart><affiliation>NAT‐Universidade Cruzeirodo Sul, Sao Paulo, Brazil</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Stephanie</namePart><namePart type="family">LaMassa</namePart><affiliation>Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2011-01-21</dateIssued><edition>Accepted 2010 August 16. Received 2010 August 16; in original form 2010 June 9</edition><copyrightDate encoding="w3cdtf">2011</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType><extent unit="figures">9</extent><extent unit="tables">3</extent><extent unit="formulas">296</extent><extent unit="references">77</extent></physicalDescription><abstract lang="en">Optical nebular emission lines are commonly used to estimate the star formation rate of galaxies and the black hole accretion rate of their central active nuclei. The accuracy of the conversion from line strengths to physical properties depends upon the accuracy to which the lines can be corrected for dust attenuation. For studies of single galaxies with normal amounts of dust, most dust corrections result in the same derived properties within the errors. However, for statistical studies of populations of galaxies, or for studies of galaxies with higher dust contents, such as might be found in some classes of ‘transition’ galaxies, significant uncertainty arises from the dust attenuation correction. In this paper, we compare the strength of the predominantly unobscured mid‐infrared [Ne ii] λ15.5 μ m+[Ne iii] λ12.8 μ m emission lines to the optical Hα emission lines in four samples of galaxies: (i) ordinary star‐forming galaxies (80 galaxies); (ii) optically selected dusty galaxies (11); (iii) ultraluminous infrared galaxies (6); and (iv) Seyfert 2 galaxies (20). We show that a single dust attenuation curve applied to all samples can correct the Hα luminosity for dust attenuation to a factor better than 2. Similarly, we compare [O iv] and [O iii] luminosities to find that [O iii] can be corrected to a factor better than 3. This shows that the total dust attenuation suffered by the active galactic nucleus narrow‐line region is not significantly different from that suffered by the star‐forming H ii regions in the galaxy. We provide explicit dust attenuation corrections, together with errors, for [O ii], [O iii] and Hα. The best‐fitting average attenuation curve is slightly greyer than the Milky Way extinction law, indicating either that external galaxies have slightly different typical dust properties from those of the Milky Way or that there is a significant contribution from scattering. Finally, we uncover an intriguing correlation between silicate absorption and Balmer decrement, two measures of dust in galaxies, which probe entirely different regimes in optical depth.</abstract><subject lang="en"><genre>keywords</genre><topic>dust, extinction</topic><topic>galaxies: ISM</topic><topic>galaxies: star formation</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2011</date><detail type="volume"><caption>vol.</caption><number>410</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>1593</start><end>1610</end><total>18</total></extent></part></relatedItem><identifier type="istex">3F8CBF933A4D69927EF939190E35057DC9DD96B0</identifier><identifier type="DOI">10.1111/j.1365-2966.2010.17536.x</identifier><identifier type="ArticleID">MNR17536</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2010 The Authors. 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