Submillimetre observations of galaxy clusters with the BLAST: the star formation activity in Abell 3112
Identifieur interne : 006699 ( Main/Merge ); précédent : 006698; suivant : 006700Submillimetre observations of galaxy clusters with the BLAST: the star formation activity in Abell 3112
Auteurs : Filiberto G. Braglia [Canada] ; Peter A. R. Ade ; James J. Bock [États-Unis] ; Edward L. Chapin [Canada] ; Mark J. Devlin [États-Unis] ; Alastair Edge ; Matthew Griffin ; Joshua O. Gundersen [États-Unis] ; Mark Halpern [Canada] ; Peter C. Hargrave ; David H. Hughes [Mexique] ; Jeff Klein [États-Unis] ; Gaelen Marsden [Canada] ; Philip Mauskopf ; Lorenzo Moncelsi ; Calvin B. Netterfield [Canada] ; Henry Ngo [Canada] ; Luca Olmi [États-Unis, Italie] ; Enzo Pascale ; Guillaume Patanchon [France] ; Kevin A. Pimbblet [Australie] ; Marie Rex [États-Unis] ; Douglas Scott [Canada] ; Christopher Semisch [États-Unis] ; Nicholas Thomas [États-Unis] ; Matthew D. P. Truch [États-Unis] ; Carole Tucker ; Gregory S. Tucker [États-Unis] ; Elisabetta Valiante [Canada] ; Marco P. Viero [États-Unis] ; Donald V. Wiebe [Canada]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-04-01.
English descriptors
- KwdEn :
- Abell, Average ssfr, Biviano, Blast, Blast bands, Blast catalogue, Blast counterparts, Blast data, Blast maps, Blast observations, Blast sources, Blast wavelengths, Blue galaxies, Boxes mark, Braglia, Brightest cluster galaxy, California institute, Central galaxy, Characteristic magnitude, Cluster, Cluster centre, Cluster core, Cluster diagram, Cluster galaxies, Cluster member, Cluster member catalogue, Cluster members, Cluster redshift, Clustercentric, Clustercentric distances, Clustercentric radius, Cold dust, Colour, Colours, Devlin, Distance scale, Dust content, Dust masses, Emission lines, Environmental effects, Flux densities, Galaxy, Galaxy clusters, Galaxy geometry, Global decrease, Good agreement, Haines, Inclination angle, Individual sources, Infall region, Instrumental counts, Instrumental noise, Ira, Iras source, Lamentary structures, Large aperture submillimeter telescope, Large fraction, Large sample, Large spirals, Largest part, Line marks, Lines mark, Luminosity, Mnras, Monthly notices, Normal galaxies, Normal starforming galaxies, Notable drop, Number counts, Optical cluster members, Optical colour, Optical colours, Optical counterparts, Optical spectra, Optical spectroscopy, Optical spectrum, Panels show, Pascale, Photometry, Physics astronomy, Pierini, Porter raychaudhury, Positional uncertainty, Potential cluster members, Previous results, Previous studies, Propulsion laboratory, Radial bins, Radial distribution, Radial peak, Radial trends, Random occurrence, Redshift, Rejection probability, Robust, Same area, Same method, Seds, Sfrs, Solid line, Source catalogue, Source extraction, Spectral region, Spectroscopic, Spectroscopic catalogue, Ssfr, Star formation, Star formation activity, Stellar, Stellar mass, Stellar masses, Stellar population, Submm, Submm emission, Submm wavelengths, Unobscured star formation activity, Upper limit, Vertical lines mark, Wavelength.
- Teeft :
- Abell, Average ssfr, Biviano, Blast, Blast bands, Blast catalogue, Blast counterparts, Blast data, Blast maps, Blast observations, Blast sources, Blast wavelengths, Blue galaxies, Boxes mark, Braglia, Brightest cluster galaxy, California institute, Central galaxy, Characteristic magnitude, Cluster, Cluster centre, Cluster core, Cluster diagram, Cluster galaxies, Cluster member, Cluster member catalogue, Cluster members, Cluster redshift, Clustercentric, Clustercentric distances, Clustercentric radius, Cold dust, Colour, Colours, Devlin, Distance scale, Dust content, Dust masses, Emission lines, Environmental effects, Flux densities, Galaxy, Galaxy clusters, Galaxy geometry, Global decrease, Good agreement, Haines, Inclination angle, Individual sources, Infall region, Instrumental counts, Instrumental noise, Ira, Iras source, Lamentary structures, Large aperture submillimeter telescope, Large fraction, Large sample, Large spirals, Largest part, Line marks, Lines mark, Luminosity, Mnras, Monthly notices, Normal galaxies, Normal starforming galaxies, Notable drop, Number counts, Optical cluster members, Optical colour, Optical colours, Optical counterparts, Optical spectra, Optical spectroscopy, Optical spectrum, Panels show, Pascale, Photometry, Physics astronomy, Pierini, Porter raychaudhury, Positional uncertainty, Potential cluster members, Previous results, Previous studies, Propulsion laboratory, Radial bins, Radial distribution, Radial peak, Radial trends, Random occurrence, Redshift, Rejection probability, Robust, Same area, Same method, Seds, Sfrs, Solid line, Source catalogue, Source extraction, Spectral region, Spectroscopic, Spectroscopic catalogue, Ssfr, Star formation, Star formation activity, Stellar, Stellar mass, Stellar masses, Stellar population, Submm, Submm emission, Submm wavelengths, Unobscured star formation activity, Upper limit, Vertical lines mark, Wavelength.
Abstract
We present observations at 250, 350 and 500 μm of the nearby galaxy cluster Abell 3112 (z= 0.075) carried out with the Balloon‐borne Large Aperture Submillimeter Telescope. Five cluster members are individually detected as bright submillimetre (submm) sources. Their far‐infrared spectral energy distributions and optical colours identify them as normal star‐forming galaxies of high mass, with globally evolved stellar populations. They all have (B−R) colours of 1.38 ± 0.08, transitional between the blue, active population and the red, evolved galaxies that dominate the cluster core. We stack to estimate the mean submm emission from all cluster members, which is determined to be 16.6 ± 2.5, 6.1 ± 1.9 and 1.5 ± 1.3 mJy at 250, 350 and 500 μm, respectively. Stacking analyses of the submm emission of cluster members reveal trends in the mean far‐infrared luminosity with respect to clustercentric radius and KS‐band magnitude. We find that a large fraction of submm emission comes from the boundary of the inner, virialized region of the cluster, at clustercentric distances around R500. Stacking also shows that the bulk of the submm emission arises in intermediate‐mass galaxies with KS magnitude ∼1 mag fainter than the characteristic magnitude . The results and constraints obtained in this work will provide a useful reference for the forthcoming surveys to be conducted on galaxy clusters by Herschel.
Url:
DOI: 10.1111/j.1365-2966.2010.17973.x
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<author><name sortKey="Marsden, Gaelen" sort="Marsden, Gaelen" uniqKey="Marsden G" first="Gaelen" last="Marsden">Gaelen Marsden</name>
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<affiliation wicri:level="1"><country xml:lang="fr">Italie</country>
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</author>
<author><name sortKey="Rex, Marie" sort="Rex, Marie" uniqKey="Rex M" first="Marie" last="Rex">Marie Rex</name>
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<wicri:regionArea>Steward Observatory, University of Arizona, 933 N. Chery Ave, Tucson, AZ 85721</wicri:regionArea>
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<author><name sortKey="Scott, Douglas" sort="Scott, Douglas" uniqKey="Scott D" first="Douglas" last="Scott">Douglas Scott</name>
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<author><name sortKey="Semisch, Christopher" sort="Semisch, Christopher" uniqKey="Semisch C" first="Christopher" last="Semisch">Christopher Semisch</name>
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<wicri:regionArea>Department of Physics & Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104</wicri:regionArea>
<placeName><region type="state">Pennsylvanie</region>
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<author><name sortKey="Thomas, Nicholas" sort="Thomas, Nicholas" uniqKey="Thomas N" first="Nicholas" last="Thomas">Nicholas Thomas</name>
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<wicri:regionArea>Department of Physics, University of Miami, 1320 Campo Sano Drive, Coral Gables, FL 33146</wicri:regionArea>
<placeName><region type="state">Floride</region>
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<author><name sortKey="Truch, Matthew D P" sort="Truch, Matthew D P" uniqKey="Truch M" first="Matthew D. P." last="Truch">Matthew D. P. Truch</name>
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<wicri:regionArea>Department of Physics & Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104</wicri:regionArea>
<placeName><region type="state">Pennsylvanie</region>
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<author><name sortKey="Tucker, Carole" sort="Tucker, Carole" uniqKey="Tucker C" first="Carole" last="Tucker">Carole Tucker</name>
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<wicri:regionArea>Department of Physics, Brown University, 182 Hope Street, Providence, RI 02912</wicri:regionArea>
<placeName><region type="state">Rhode Island</region>
<settlement type="city">Providence (Rhode Island)</settlement>
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<orgName type="university">Université Brown</orgName>
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<author><name sortKey="Valiante, Elisabetta" sort="Valiante, Elisabetta" uniqKey="Valiante E" first="Elisabetta" last="Valiante">Elisabetta Valiante</name>
<affiliation wicri:level="1"><country xml:lang="fr">Canada</country>
<wicri:regionArea>Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1</wicri:regionArea>
<wicri:noRegion>BC V6T 1Z1</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Viero, Marco P" sort="Viero, Marco P" uniqKey="Viero M" first="Marco P." last="Viero">Marco P. Viero</name>
<affiliation wicri:level="2"><country xml:lang="fr">États-Unis</country>
<wicri:regionArea>California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125</wicri:regionArea>
<placeName><region type="state">Californie</region>
</placeName>
</affiliation>
</author>
<author><name sortKey="Wiebe, Donald V" sort="Wiebe, Donald V" uniqKey="Wiebe D" first="Donald V." last="Wiebe">Donald V. Wiebe</name>
<affiliation wicri:level="1"><country xml:lang="fr">Canada</country>
<wicri:regionArea>Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1</wicri:regionArea>
<wicri:noRegion>BC V6T 1Z1</wicri:noRegion>
</affiliation>
</author>
</analytic>
<monogr></monogr>
<series><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="ISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<imprint><biblScope unit="vol">412</biblScope>
<biblScope unit="issue">2</biblScope>
<biblScope unit="page" from="1187">1187</biblScope>
<biblScope unit="page" to="1202">1202</biblScope>
<biblScope unit="page-count">16</biblScope>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2011-04-01">2011-04-01</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>Abell</term>
<term>Average ssfr</term>
<term>Biviano</term>
<term>Blast</term>
<term>Blast bands</term>
<term>Blast catalogue</term>
<term>Blast counterparts</term>
<term>Blast data</term>
<term>Blast maps</term>
<term>Blast observations</term>
<term>Blast sources</term>
<term>Blast wavelengths</term>
<term>Blue galaxies</term>
<term>Boxes mark</term>
<term>Braglia</term>
<term>Brightest cluster galaxy</term>
<term>California institute</term>
<term>Central galaxy</term>
<term>Characteristic magnitude</term>
<term>Cluster</term>
<term>Cluster centre</term>
<term>Cluster core</term>
<term>Cluster diagram</term>
<term>Cluster galaxies</term>
<term>Cluster member</term>
<term>Cluster member catalogue</term>
<term>Cluster members</term>
<term>Cluster redshift</term>
<term>Clustercentric</term>
<term>Clustercentric distances</term>
<term>Clustercentric radius</term>
<term>Cold dust</term>
<term>Colour</term>
<term>Colours</term>
<term>Devlin</term>
<term>Distance scale</term>
<term>Dust content</term>
<term>Dust masses</term>
<term>Emission lines</term>
<term>Environmental effects</term>
<term>Flux densities</term>
<term>Galaxy</term>
<term>Galaxy clusters</term>
<term>Galaxy geometry</term>
<term>Global decrease</term>
<term>Good agreement</term>
<term>Haines</term>
<term>Inclination angle</term>
<term>Individual sources</term>
<term>Infall region</term>
<term>Instrumental counts</term>
<term>Instrumental noise</term>
<term>Ira</term>
<term>Iras source</term>
<term>Lamentary structures</term>
<term>Large aperture submillimeter telescope</term>
<term>Large fraction</term>
<term>Large sample</term>
<term>Large spirals</term>
<term>Largest part</term>
<term>Line marks</term>
<term>Lines mark</term>
<term>Luminosity</term>
<term>Mnras</term>
<term>Monthly notices</term>
<term>Normal galaxies</term>
<term>Normal starforming galaxies</term>
<term>Notable drop</term>
<term>Number counts</term>
<term>Optical cluster members</term>
<term>Optical colour</term>
<term>Optical colours</term>
<term>Optical counterparts</term>
<term>Optical spectra</term>
<term>Optical spectroscopy</term>
<term>Optical spectrum</term>
<term>Panels show</term>
<term>Pascale</term>
<term>Photometry</term>
<term>Physics astronomy</term>
<term>Pierini</term>
<term>Porter raychaudhury</term>
<term>Positional uncertainty</term>
<term>Potential cluster members</term>
<term>Previous results</term>
<term>Previous studies</term>
<term>Propulsion laboratory</term>
<term>Radial bins</term>
<term>Radial distribution</term>
<term>Radial peak</term>
<term>Radial trends</term>
<term>Random occurrence</term>
<term>Redshift</term>
<term>Rejection probability</term>
<term>Robust</term>
<term>Same area</term>
<term>Same method</term>
<term>Seds</term>
<term>Sfrs</term>
<term>Solid line</term>
<term>Source catalogue</term>
<term>Source extraction</term>
<term>Spectral region</term>
<term>Spectroscopic</term>
<term>Spectroscopic catalogue</term>
<term>Ssfr</term>
<term>Star formation</term>
<term>Star formation activity</term>
<term>Stellar</term>
<term>Stellar mass</term>
<term>Stellar masses</term>
<term>Stellar population</term>
<term>Submm</term>
<term>Submm emission</term>
<term>Submm wavelengths</term>
<term>Unobscured star formation activity</term>
<term>Upper limit</term>
<term>Vertical lines mark</term>
<term>Wavelength</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en"><term>Abell</term>
<term>Average ssfr</term>
<term>Biviano</term>
<term>Blast</term>
<term>Blast bands</term>
<term>Blast catalogue</term>
<term>Blast counterparts</term>
<term>Blast data</term>
<term>Blast maps</term>
<term>Blast observations</term>
<term>Blast sources</term>
<term>Blast wavelengths</term>
<term>Blue galaxies</term>
<term>Boxes mark</term>
<term>Braglia</term>
<term>Brightest cluster galaxy</term>
<term>California institute</term>
<term>Central galaxy</term>
<term>Characteristic magnitude</term>
<term>Cluster</term>
<term>Cluster centre</term>
<term>Cluster core</term>
<term>Cluster diagram</term>
<term>Cluster galaxies</term>
<term>Cluster member</term>
<term>Cluster member catalogue</term>
<term>Cluster members</term>
<term>Cluster redshift</term>
<term>Clustercentric</term>
<term>Clustercentric distances</term>
<term>Clustercentric radius</term>
<term>Cold dust</term>
<term>Colour</term>
<term>Colours</term>
<term>Devlin</term>
<term>Distance scale</term>
<term>Dust content</term>
<term>Dust masses</term>
<term>Emission lines</term>
<term>Environmental effects</term>
<term>Flux densities</term>
<term>Galaxy</term>
<term>Galaxy clusters</term>
<term>Galaxy geometry</term>
<term>Global decrease</term>
<term>Good agreement</term>
<term>Haines</term>
<term>Inclination angle</term>
<term>Individual sources</term>
<term>Infall region</term>
<term>Instrumental counts</term>
<term>Instrumental noise</term>
<term>Ira</term>
<term>Iras source</term>
<term>Lamentary structures</term>
<term>Large aperture submillimeter telescope</term>
<term>Large fraction</term>
<term>Large sample</term>
<term>Large spirals</term>
<term>Largest part</term>
<term>Line marks</term>
<term>Lines mark</term>
<term>Luminosity</term>
<term>Mnras</term>
<term>Monthly notices</term>
<term>Normal galaxies</term>
<term>Normal starforming galaxies</term>
<term>Notable drop</term>
<term>Number counts</term>
<term>Optical cluster members</term>
<term>Optical colour</term>
<term>Optical colours</term>
<term>Optical counterparts</term>
<term>Optical spectra</term>
<term>Optical spectroscopy</term>
<term>Optical spectrum</term>
<term>Panels show</term>
<term>Pascale</term>
<term>Photometry</term>
<term>Physics astronomy</term>
<term>Pierini</term>
<term>Porter raychaudhury</term>
<term>Positional uncertainty</term>
<term>Potential cluster members</term>
<term>Previous results</term>
<term>Previous studies</term>
<term>Propulsion laboratory</term>
<term>Radial bins</term>
<term>Radial distribution</term>
<term>Radial peak</term>
<term>Radial trends</term>
<term>Random occurrence</term>
<term>Redshift</term>
<term>Rejection probability</term>
<term>Robust</term>
<term>Same area</term>
<term>Same method</term>
<term>Seds</term>
<term>Sfrs</term>
<term>Solid line</term>
<term>Source catalogue</term>
<term>Source extraction</term>
<term>Spectral region</term>
<term>Spectroscopic</term>
<term>Spectroscopic catalogue</term>
<term>Ssfr</term>
<term>Star formation</term>
<term>Star formation activity</term>
<term>Stellar</term>
<term>Stellar mass</term>
<term>Stellar masses</term>
<term>Stellar population</term>
<term>Submm</term>
<term>Submm emission</term>
<term>Submm wavelengths</term>
<term>Unobscured star formation activity</term>
<term>Upper limit</term>
<term>Vertical lines mark</term>
<term>Wavelength</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We present observations at 250, 350 and 500 μm of the nearby galaxy cluster Abell 3112 (z= 0.075) carried out with the Balloon‐borne Large Aperture Submillimeter Telescope. Five cluster members are individually detected as bright submillimetre (submm) sources. Their far‐infrared spectral energy distributions and optical colours identify them as normal star‐forming galaxies of high mass, with globally evolved stellar populations. They all have (B−R) colours of 1.38 ± 0.08, transitional between the blue, active population and the red, evolved galaxies that dominate the cluster core. We stack to estimate the mean submm emission from all cluster members, which is determined to be 16.6 ± 2.5, 6.1 ± 1.9 and 1.5 ± 1.3 mJy at 250, 350 and 500 μm, respectively. Stacking analyses of the submm emission of cluster members reveal trends in the mean far‐infrared luminosity with respect to clustercentric radius and KS‐band magnitude. We find that a large fraction of submm emission comes from the boundary of the inner, virialized region of the cluster, at clustercentric distances around R500. Stacking also shows that the bulk of the submm emission arises in intermediate‐mass galaxies with KS magnitude ∼1 mag fainter than the characteristic magnitude . The results and constraints obtained in this work will provide a useful reference for the forthcoming surveys to be conducted on galaxy clusters by Herschel.</div>
</front>
</TEI>
</record>
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