The effects of an active galactic nucleus on host galaxy colour and morphology measurements
Identifieur interne : 000072 ( Main/Exploration ); précédent : 000071; suivant : 000073The effects of an active galactic nucleus on host galaxy colour and morphology measurements
Auteurs : C. M. Pierce [États-Unis] ; J. M. Lotz [États-Unis] ; J. R. Primack [États-Unis] ; D. J. V. Rosario [États-Unis] ; R. L. Griffith [États-Unis] ; C. J. Conselice ; S. M. Faber [États-Unis] ; D. C. Koo [États-Unis] ; A. L. Coil [États-Unis] ; S. Salim [États-Unis] ; A. M. Koekemoer [États-Unis] ; E. S. Laird ; R. J. Ivison ; R. Yan [Canada]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-06-21.
English descriptors
Abstract
We assess the effects of simulated active galactic nuclei (AGN) on the colour and morphology measurements of their host galaxies. To test the morphology measurements, we select a sample of galaxies not known to host AGN and add a series of point sources scaled to represent specified fractions of the observed V‐band light detected from the resulting systems; we then compare morphology measurements of the simulated systems to measurements of the original galaxies. AGN contributions >rsim 20 per cent bias most of the morphology measurements tested, though the extent of the apparent bias depends on the morphological characteristics of the original galaxies. We test colour measurements by adding to non‐AGN galaxy spectra a quasar spectrum scaled to contribute specified fractions of the rest‐frame B‐band light detected from the resulting systems. A quasar fraction of 5 per cent can move the NUV −r colour of an elliptical galaxy from the ultraviolet–optical red sequence to the green valley, and 20 per cent can move it into the blue cloud. Combining the colour and morphology results, we find that a galaxy/AGN system with an AGN contribution >rsim 20 per cent may appear bluer and more bulge dominated than the underlying galaxy. We conclude that (1) bulge‐dominated, E/S0/Sa, and early‐type morphology classifications are accurate for red AGN host galaxies and may be accurate for blue host galaxies, unless the AGN manifests itself as a well‐defined point source and (2) although highly unobscured AGN, such as the quasar used for our experiments, can significantly bias the measured colours of AGN host galaxies, it is possible to identify such systems by examining optical images of the hosts for the presence of a point source and/or measuring the level of nuclear obscuration.
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DOI: 10.1111/j.1365-2966.2010.16502.x
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Yan</name><affiliation wicri:level="4"><country xml:lang="fr">Canada</country><wicri:regionArea>Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4</wicri:regionArea><orgName type="university">Université de Toronto</orgName><placeName><settlement type="city">Toronto</settlement><region type="state">Ontario</region></placeName></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2010-06-21">2010-06-21</date><biblScope unit="volume">405</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="718">718</biblScope><biblScope unit="page" to="734">734</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">DC86C484065AEA1DA07182A6E6C667EEFC2C0303</idno><idno type="DOI">10.1111/j.1365-2966.2010.16502.x</idno><idno type="ArticleID">MNR16502</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>galaxies: active</term><term>galaxies: fundamental parameters</term><term>galaxies: nuclei</term><term>galaxies: structure</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We assess the effects of simulated active galactic nuclei (AGN) on the colour and morphology measurements of their host galaxies. To test the morphology measurements, we select a sample of galaxies not known to host AGN and add a series of point sources scaled to represent specified fractions of the observed V‐band light detected from the resulting systems; we then compare morphology measurements of the simulated systems to measurements of the original galaxies. AGN contributions >rsim 20 per cent bias most of the morphology measurements tested, though the extent of the apparent bias depends on the morphological characteristics of the original galaxies. We test colour measurements by adding to non‐AGN galaxy spectra a quasar spectrum scaled to contribute specified fractions of the rest‐frame B‐band light detected from the resulting systems. A quasar fraction of 5 per cent can move the NUV −r colour of an elliptical galaxy from the ultraviolet–optical red sequence to the green valley, and 20 per cent can move it into the blue cloud. Combining the colour and morphology results, we find that a galaxy/AGN system with an AGN contribution >rsim 20 per cent may appear bluer and more bulge dominated than the underlying galaxy. We conclude that (1) bulge‐dominated, E/S0/Sa, and early‐type morphology classifications are accurate for red AGN host galaxies and may be accurate for blue host galaxies, unless the AGN manifests itself as a well‐defined point source and (2) although highly unobscured AGN, such as the quasar used for our experiments, can significantly bias the measured colours of AGN host galaxies, it is possible to identify such systems by examining optical images of the hosts for the presence of a point source and/or measuring the level of nuclear obscuration.</div></front></TEI><affiliations><list><country><li>Canada</li><li>États-Unis</li></country><region><li>Ontario</li></region><settlement><li>Toronto</li></settlement><orgName><li>Université de Toronto</li></orgName></list><tree><noCountry><name sortKey="Conselice, C J" sort="Conselice, C J" uniqKey="Conselice C" first="C. J." last="Conselice">C. J. Conselice</name><name sortKey="Ivison, R J" sort="Ivison, R J" uniqKey="Ivison R" first="R. J." last="Ivison">R. J. Ivison</name><name sortKey="Laird, E S" sort="Laird, E S" uniqKey="Laird E" first="E. S." last="Laird">E. S. Laird</name></noCountry><country name="États-Unis"><noRegion><name sortKey="Pierce, C M" sort="Pierce, C M" uniqKey="Pierce C" first="C. M." last="Pierce">C. M. Pierce</name></noRegion><name sortKey="Coil, A L" sort="Coil, A L" uniqKey="Coil A" first="A. L." last="Coil">A. L. Coil</name><name sortKey="Faber, S M" sort="Faber, S M" uniqKey="Faber S" first="S. M." last="Faber">S. M. Faber</name><name sortKey="Griffith, R L" sort="Griffith, R L" uniqKey="Griffith R" first="R. L." last="Griffith">R. L. Griffith</name><name sortKey="Koekemoer, A M" sort="Koekemoer, A M" uniqKey="Koekemoer A" first="A. M." last="Koekemoer">A. M. Koekemoer</name><name sortKey="Koo, D C" sort="Koo, D C" uniqKey="Koo D" first="D. C." last="Koo">D. C. Koo</name><name sortKey="Lotz, J M" sort="Lotz, J M" uniqKey="Lotz J" first="J. M." last="Lotz">J. M. Lotz</name><name sortKey="Lotz, J M" sort="Lotz, J M" uniqKey="Lotz J" first="J. M." last="Lotz">J. M. Lotz</name><name sortKey="Pierce, C M" sort="Pierce, C M" uniqKey="Pierce C" first="C. M." last="Pierce">C. M. Pierce</name><name sortKey="Pierce, C M" sort="Pierce, C M" uniqKey="Pierce C" first="C. M." last="Pierce">C. M. Pierce</name><name sortKey="Primack, J R" sort="Primack, J R" uniqKey="Primack J" first="J. R." last="Primack">J. R. Primack</name><name sortKey="Rosario, D J V" sort="Rosario, D J V" uniqKey="Rosario D" first="D. J. V." last="Rosario">D. J. V. Rosario</name><name sortKey="Salim, S" sort="Salim, S" uniqKey="Salim S" first="S." last="Salim">S. Salim</name></country><country name="Canada"><region name="Ontario"><name sortKey="Yan, R" sort="Yan, R" uniqKey="Yan R" first="R." last="Yan">R. Yan</name></region></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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