The Arecibo Galaxy Environment Survey – II. A H i view of the Abell cluster 1367 and its outskirts
Identifieur interne : 008732 ( Main/Exploration ); précédent : 008731; suivant : 008733The Arecibo Galaxy Environment Survey – II. A H i view of the Abell cluster 1367 and its outskirts
Auteurs : L. Cortese [Royaume-Uni] ; R. F. Minchin [États-Unis] ; R. R. Auld ; J. I. Davies ; B. Catinella [États-Unis, Allemagne] ; E. Momjian [États-Unis] ; J. L. Rosenberg [États-Unis] ; R. Taylor ; G. Gavazzi [Italie] ; K. O'Neil [États-Unis] ; M. Baes [Belgique] ; A. Boselli [France] ; G. Bothun [États-Unis] ; B. Koribalski [Australie] ; S. Schneider [États-Unis] ; W. Van Driel [France]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008-02-01.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
- Abell, Abell cluster, Ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages, Ages cube, Alfa, Alfa survey, Alfalfa, Alfalfa reliability limit, Arcmin, Arecibo, Arecibo galaxy environment survey, Arecibo observatory, Automatic extractor, Baryon, Baryon fraction, Baryon fraction distribution, Baryons, Blind survey, Blind surveys, Blue galaxies, Blue sequence, Boselli, Bottom panel, Cent level, Centre, Cluster, Cluster centre, Cluster contours, Cluster core, Cluster environment, Cluster members, Cluster volume, Colour, Considerable number, Contour levels, Cortese, Cosmic radio sources, Cosmological effects, Cube, Data cubes, Data reduction, Data reduction techniques, Deg2, Deg2 centred, Disc inclination, Dwarf systems, Dynamical, Dynamical mass, Effective surface brightness, Empty circles, Empty circles show, Empty dots, Evolutionary history, Extraction methods, Extragalactic data base, Ftot, Galaxy, Galaxy clusters, Galaxy evolution, Galaxy formation, Gavazzi, Giovanelli, Giovanelli haynes, Good agreement, Great part, Great wall, H function, H lines, Haynes, Haynes giovanelli, Heliocentric velocity, Higher surface brightness, Integration time, Journal compilation, Large amount, Line observations, Local cluster, Local universe, Lower panel, Luminosity, Luminosity function, Mass distribution, Mass distributions, Mass function, Minchin, Mnras, Molecular hydrogen, Moment maps, National science foundation, Negligible fraction, Neutral hydrogen, Noise diode, Optical colours, Optical counterpart, Optical counterpart candidates, Optical counterparts, Optical luminosity function, Optical properties, Optical radius, Optical recessional velocity, Optical redshift, Optical velocity, Outskirts, Peculiar galaxies, Radio galaxies, Recessional, Recessional velocities, Recessional velocity, Red shift, Redshift, Relative error, Same baryon fraction, Sdss, Sdss plates, Selection effects, Sensitivity limit, Sky surveys, Solid line, Source extraction, Source line, Star mass ratio, Starburst galaxy, Stellar, Stellar mass, Surface brightness, Surface brightness galaxies, Turbulent motions, Unbiased view, Upper panel, Velocity range, Velocity resolution, Velocity width, Velocity widths, Wedge diagram, X ray observation.
- Teeft :
- Abell, Abell cluster, Ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages, Ages cube, Alfa, Alfa survey, Alfalfa, Alfalfa reliability limit, Arcmin, Arecibo, Arecibo galaxy environment survey, Arecibo observatory, Automatic extractor, Baryon, Baryon fraction, Baryon fraction distribution, Blind survey, Blind surveys, Blue galaxies, Blue sequence, Boselli, Bottom panel, Cent level, Centre, Cluster, Cluster centre, Cluster contours, Cluster core, Cluster environment, Cluster members, Cluster volume, Colour, Considerable number, Contour levels, Cortese, Cosmological effects, Cube, Data cubes, Data reduction, Data reduction techniques, Deg2, Deg2 centred, Disc inclination, Dwarf systems, Dynamical, Dynamical mass, Effective surface brightness, Empty circles, Empty circles show, Empty dots, Evolutionary history, Extraction methods, Extragalactic data base, Ftot, Galaxy, Galaxy formation, Gavazzi, Giovanelli, Giovanelli haynes, Good agreement, Great part, Great wall, Haynes, Haynes giovanelli, Heliocentric velocity, Higher surface brightness, Integration time, Journal compilation, Large amount, Line observations, Local universe, Lower panel, Luminosity, Mass distribution, Mass distributions, Mass function, Minchin, Mnras, Molecular hydrogen, Moment maps, National science foundation, Negligible fraction, Neutral hydrogen, Noise diode, Optical colours, Optical counterpart, Optical counterpart candidates, Optical counterparts, Optical luminosity function, Optical properties, Optical radius, Optical recessional velocity, Optical redshift, Optical velocity, Outskirts, Recessional, Recessional velocities, Recessional velocity, Redshift, Relative error, Same baryon fraction, Sdss, Sdss plates, Selection effects, Sensitivity limit, Solid line, Source extraction, Source line, Star mass ratio, Starburst galaxy, Stellar, Stellar mass, Surface brightness, Surface brightness galaxies, Turbulent motions, Unbiased view, Upper panel, Velocity range, Velocity resolution, Velocity width, Velocity widths, Wedge diagram.
Abstract
We present 21 cm H i line observations of 5 × 1 deg2 centred on the local Abell cluster 1367 obtained as part of the Arecibo Galaxy Environment Survey. One hundred sources are detected (79 new H i measurements and 50 new redshifts), more than half belonging to the cluster core and its infalling region. Combining the H i data with Sloan Digital Sky Survey (SDSS) optical imaging, we show that our H i selected sample follows scaling relations similar to the ones usually observed in optically selected samples. Interestingly, all galaxies in our sample appear to have nearly the same baryon fraction independently of their size, surface brightness and luminosity. The most striking difference between H i and optically selected samples resides in their large‐scale distribution: whereas optical and X‐ray observations trace the cluster core very well, in H i there is almost no evidence of the presence of the cluster. Some implications on the determination of the cluster luminosity function and H i distribution for samples selected at different wavelength are also discussed.
Url:
- https://api.istex.fr/document/422586F1E6E70034C5EDD72DE36D2C41845187C0/fulltext/pdf
- https://api.istex.fr/document/FDF6FBFD793BB40965F85FCAD11D635949393266/fulltext/pdf
DOI: 10.1111/j.1365-2966.2007.12664.x
Affiliations:
- Allemagne, Australie, Belgique, France, Italie, Royaume-Uni, États-Unis
- Massachusetts, Nouveau-Mexique, Oregon, Provence-Alpes-Côte d'Azur, Province de Flandre-Orientale, Région flamande, Virginie-Occidentale, Île-de-France
- Amherst (Massachusetts), Gand, Marseille, Meudon
- Université de Gand, Université du Massachusetts
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Le document en format XML
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observation</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Amas galaxies</term><term>Amas local</term><term>Baryon</term><term>Brillance surface</term><term>Déplacement vers le rouge</term><term>Etude ciel</term><term>Evolution galaxies</term><term>Fonction H</term><term>Fonction luminosité</term><term>Galaxies particulières</term><term>Luminosité</term><term>Observation RX</term><term>Radiogalaxies</term><term>Radiosource cosmique</term><term>Raie H</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Abell</term><term>Abell cluster</term><term>Ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages ages</term><term>Ages cube</term><term>Alfa</term><term>Alfa survey</term><term>Alfalfa</term><term>Alfalfa reliability limit</term><term>Arcmin</term><term>Arecibo</term><term>Arecibo galaxy environment survey</term><term>Arecibo observatory</term><term>Automatic extractor</term><term>Baryon</term><term>Baryon fraction</term><term>Baryon fraction distribution</term><term>Blind survey</term><term>Blind surveys</term><term>Blue galaxies</term><term>Blue sequence</term><term>Boselli</term><term>Bottom panel</term><term>Cent level</term><term>Centre</term><term>Cluster</term><term>Cluster centre</term><term>Cluster contours</term><term>Cluster core</term><term>Cluster environment</term><term>Cluster members</term><term>Cluster volume</term><term>Colour</term><term>Considerable number</term><term>Contour levels</term><term>Cortese</term><term>Cosmological effects</term><term>Cube</term><term>Data cubes</term><term>Data reduction</term><term>Data reduction techniques</term><term>Deg2</term><term>Deg2 centred</term><term>Disc inclination</term><term>Dwarf systems</term><term>Dynamical</term><term>Dynamical mass</term><term>Effective surface brightness</term><term>Empty circles</term><term>Empty circles show</term><term>Empty dots</term><term>Evolutionary history</term><term>Extraction methods</term><term>Extragalactic data base</term><term>Ftot</term><term>Galaxy</term><term>Galaxy formation</term><term>Gavazzi</term><term>Giovanelli</term><term>Giovanelli haynes</term><term>Good agreement</term><term>Great part</term><term>Great wall</term><term>Haynes</term><term>Haynes giovanelli</term><term>Heliocentric velocity</term><term>Higher surface brightness</term><term>Integration time</term><term>Journal compilation</term><term>Large amount</term><term>Line observations</term><term>Local universe</term><term>Lower panel</term><term>Luminosity</term><term>Mass distribution</term><term>Mass distributions</term><term>Mass function</term><term>Minchin</term><term>Mnras</term><term>Molecular hydrogen</term><term>Moment maps</term><term>National science foundation</term><term>Negligible fraction</term><term>Neutral hydrogen</term><term>Noise diode</term><term>Optical colours</term><term>Optical counterpart</term><term>Optical counterpart candidates</term><term>Optical counterparts</term><term>Optical luminosity function</term><term>Optical properties</term><term>Optical radius</term><term>Optical recessional velocity</term><term>Optical redshift</term><term>Optical velocity</term><term>Outskirts</term><term>Recessional</term><term>Recessional velocities</term><term>Recessional velocity</term><term>Redshift</term><term>Relative error</term><term>Same baryon fraction</term><term>Sdss</term><term>Sdss plates</term><term>Selection effects</term><term>Sensitivity limit</term><term>Solid line</term><term>Source extraction</term><term>Source line</term><term>Star mass ratio</term><term>Starburst galaxy</term><term>Stellar</term><term>Stellar mass</term><term>Surface brightness</term><term>Surface brightness galaxies</term><term>Turbulent motions</term><term>Unbiased view</term><term>Upper panel</term><term>Velocity range</term><term>Velocity resolution</term><term>Velocity width</term><term>Velocity widths</term><term>Wedge diagram</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present 21 cm H i line observations of 5 × 1 deg2 centred on the local Abell cluster 1367 obtained as part of the Arecibo Galaxy Environment Survey. One hundred sources are detected (79 new H i measurements and 50 new redshifts), more than half belonging to the cluster core and its infalling region. Combining the H i data with Sloan Digital Sky Survey (SDSS) optical imaging, we show that our H i selected sample follows scaling relations similar to the ones usually observed in optically selected samples. Interestingly, all galaxies in our sample appear to have nearly the same baryon fraction independently of their size, surface brightness and luminosity. The most striking difference between H i and optically selected samples resides in their large‐scale distribution: whereas optical and X‐ray observations trace the cluster core very well, in H i there is almost no evidence of the presence of the cluster. Some implications on the determination of the cluster luminosity function and H i distribution for samples selected at different wavelength are also discussed.</div></front></TEI><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>Belgique</li><li>France</li><li>Italie</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Massachusetts</li><li>Nouveau-Mexique</li><li>Oregon</li><li>Provence-Alpes-Côte d'Azur</li><li>Province de Flandre-Orientale</li><li>Région flamande</li><li>Virginie-Occidentale</li><li>Île-de-France</li></region><settlement><li>Amherst (Massachusetts)</li><li>Gand</li><li>Marseille</li><li>Meudon</li></settlement><orgName><li>Université de Gand</li><li>Université du Massachusetts</li></orgName></list><tree><noCountry><name sortKey="Auld, R R" sort="Auld, R R" uniqKey="Auld R" first="R. R." last="Auld">R. R. Auld</name><name sortKey="Davies, J I" sort="Davies, J I" uniqKey="Davies J" first="J. I." last="Davies">J. I. Davies</name><name sortKey="Taylor, R" sort="Taylor, R" uniqKey="Taylor R" first="R." last="Taylor">R. Taylor</name></noCountry><country name="Royaume-Uni"><noRegion><name sortKey="Cortese, L" sort="Cortese, L" uniqKey="Cortese L" first="L." last="Cortese">L. Cortese</name></noRegion></country><country name="États-Unis"><noRegion><name sortKey="Minchin, R F" sort="Minchin, R F" uniqKey="Minchin R" first="R. F." last="Minchin">R. F. Minchin</name></noRegion><name sortKey="Bothun, G" sort="Bothun, G" uniqKey="Bothun G" first="G." last="Bothun">G. Bothun</name><name sortKey="Catinella, B" sort="Catinella, B" uniqKey="Catinella B" first="B." last="Catinella">B. Catinella</name><name sortKey="Momjian, E" sort="Momjian, E" uniqKey="Momjian E" first="E." last="Momjian">E. Momjian</name><name sortKey="Momjian, E" sort="Momjian, E" uniqKey="Momjian E" first="E." last="Momjian">E. Momjian</name><name sortKey="O Neil, K" sort="O Neil, K" uniqKey="O Neil K" first="K." last="O'Neil">K. O'Neil</name><name sortKey="Rosenberg, J L" sort="Rosenberg, J L" uniqKey="Rosenberg J" first="J. L." last="Rosenberg">J. L. Rosenberg</name><name sortKey="Schneider, S" sort="Schneider, S" uniqKey="Schneider S" first="S." last="Schneider">S. Schneider</name></country><country name="Allemagne"><noRegion><name sortKey="Catinella, B" sort="Catinella, B" uniqKey="Catinella B" first="B." last="Catinella">B. Catinella</name></noRegion></country><country name="Italie"><noRegion><name sortKey="Gavazzi, G" sort="Gavazzi, G" uniqKey="Gavazzi G" first="G." last="Gavazzi">G. Gavazzi</name></noRegion></country><country name="Belgique"><region name="Région flamande"><name sortKey="Baes, M" sort="Baes, M" uniqKey="Baes M" first="M." last="Baes">M. Baes</name></region></country><country name="France"><region name="Provence-Alpes-Côte d'Azur"><name sortKey="Boselli, A" sort="Boselli, A" uniqKey="Boselli A" first="A." last="Boselli">A. Boselli</name></region><name sortKey="Driel, W Van" sort="Driel, W Van" uniqKey="Driel W" first="W. Van" last="Driel">W. Van Driel</name></country><country name="Australie"><noRegion><name sortKey="Koribalski, B" sort="Koribalski, B" uniqKey="Koribalski B" first="B." last="Koribalski">B. Koribalski</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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