On the absence of molecular absorption in high‐redshift millimetre‐band searches
Identifieur interne : 001F06 ( Istex/Curation ); précédent : 001F05; suivant : 001F07On the absence of molecular absorption in high‐redshift millimetre‐band searches
Auteurs : S. J. Curran [Australie] ; M. T. Whiting [Australie] ; F. Combes [France] ; N. Kuno [Japon] ; P. Francis [Australie] ; N. Nakai [Japon] ; J. K. Webb [Australie] ; M. T. Murphy [Australie] ; T. Wiklind [États-Unis, Suède, Chili]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-09-21.
English descriptors
- KwdEn :
- Absorber, Carilli, Colour, Colour depth, Column densities, Column density, Column density limits, Combes, Curran, Curran whiting, Decimetre, Drinkwater, Emission redshift, Excitation, Excitation temperature, Excitation temperatures, Fwhm, Galaxy, Host galaxy, Iram, Luminosity, Millimetre, Millimetre absorbers, Millimetre absorption, Mnras, Molecular absorption, Molecular fractions, Monthly notices, Optical depth, Previous surveys, Prochaska, Quasar, Reddening, Redshift, Spectral scans, Total column density, Ultraviolet luminosities, Webb, Whiting, Wiklind, Wiklind combes.
- Teeft :
- Absorber, Carilli, Colour, Colour depth, Column densities, Column density, Column density limits, Combes, Curran, Curran whiting, Decimetre, Drinkwater, Emission redshift, Excitation, Excitation temperature, Excitation temperatures, Fwhm, Galaxy, Host galaxy, Iram, Luminosity, Millimetre, Millimetre absorbers, Millimetre absorption, Mnras, Molecular absorption, Molecular fractions, Monthly notices, Optical depth, Previous surveys, Prochaska, Quasar, Reddening, Redshift, Spectral scans, Total column density, Ultraviolet luminosities, Webb, Whiting, Wiklind, Wiklind combes.
Abstract
We have undertaken a search for millimetre‐waveband absorption (through the CO and HCO+ rotational transitions) in the host galaxies of reddened radio sources (z= 0.405–1.802). Despite the colour selection (optical–near‐infrared colours of V−K≳ 5 in all but one source), no absorption was found in any of the eight quasars for which the background continuum flux was detected. On the basis of the previous (mostly intervening) H2 and OH detections, the limits reached here and in some previous surveys should be deep enough to detect molecular absorption according to their V−K colours. However, our survey makes the assumption that the reddening is associated with dust close to the emission redshift of the quasar and that the narrow millimetre component of this emission is intercepted by the compact molecular cores. By using the known millimetre absorbers to define the colour depth and comparing this with the ultraviolet luminosities of the sources, we find that, even if these assumptions are valid, only 12 of the 40 objects (mainly from this work) are potentially detectable. This is assuming an excitation temperature of Tx= 10 K at z= 0, with the number decreasing with increasing temperatures (to zero detectable at Tx≳ 100 K).
Url:
DOI: 10.1111/j.1365-2966.2011.19193.x
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J." last="Curran">S. J. Curran</name><affiliation wicri:level="1"><mods:affiliation>School of Physics, University of New South Wales, Sydney, NSW 2052, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>School of Physics, University of New South Wales, Sydney, NSW 2052</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>E-mail: sjc@phys.unsw.edu.au</mods:affiliation><country wicri:rule="url">Australie</country></affiliation></author><author><name sortKey="Whiting, M T" sort="Whiting, M T" uniqKey="Whiting M" first="M. T." last="Whiting">M. T. 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Francis</name><affiliation wicri:level="1"><mods:affiliation>Australian National University, Canberra, Australia</mods:affiliation><country xml:lang="fr">Australie</country><wicri:regionArea>Australian National University, Canberra</wicri:regionArea></affiliation></author><author><name sortKey="Nakai, N" sort="Nakai, N" uniqKey="Nakai N" first="N." last="Nakai">N. Nakai</name><affiliation wicri:level="1"><mods:affiliation>Institute of Physics, University of Tsukuba, Ten‐noudai, Tsukuba, Ibaraki 305‐8571, Japan</mods:affiliation><country xml:lang="fr">Japon</country><wicri:regionArea>Institute of Physics, University of Tsukuba, Ten‐noudai, Tsukuba, Ibaraki 305‐8571</wicri:regionArea></affiliation></author><author><name sortKey="Webb, J K" sort="Webb, J K" uniqKey="Webb J" first="J. K." last="Webb">J. K. 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Wiklind</name><affiliation wicri:level="1"><mods:affiliation>Space Telescope Science Institute, Baltimore, MD 21218, USA</mods:affiliation><country xml:lang="fr">États-Unis</country><wicri:regionArea>Space Telescope Science Institute, Baltimore, MD 21218</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>Onsala Space Observatory, S‐439 92 Onsala, Sweden</mods:affiliation><country xml:lang="fr">Suède</country><wicri:regionArea>Onsala Space Observatory, S‐439 92 Onsala</wicri:regionArea></affiliation><affiliation wicri:level="1"><mods:affiliation>Joint ALMA Observatory, Santiago, Chile</mods:affiliation><country xml:lang="fr">Chili</country><wicri:regionArea>Joint ALMA Observatory, Santiago</wicri:regionArea></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">416</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="2143">2143</biblScope><biblScope unit="page" to="2153">2153</biblScope><biblScope unit="page-count">11</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-09-21">2011-09-21</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>Absorber</term><term>Carilli</term><term>Colour</term><term>Colour depth</term><term>Column densities</term><term>Column density</term><term>Column density limits</term><term>Combes</term><term>Curran</term><term>Curran whiting</term><term>Decimetre</term><term>Drinkwater</term><term>Emission redshift</term><term>Excitation</term><term>Excitation temperature</term><term>Excitation temperatures</term><term>Fwhm</term><term>Galaxy</term><term>Host galaxy</term><term>Iram</term><term>Luminosity</term><term>Millimetre</term><term>Millimetre absorbers</term><term>Millimetre absorption</term><term>Mnras</term><term>Molecular absorption</term><term>Molecular fractions</term><term>Monthly notices</term><term>Optical depth</term><term>Previous surveys</term><term>Prochaska</term><term>Quasar</term><term>Reddening</term><term>Redshift</term><term>Spectral scans</term><term>Total column density</term><term>Ultraviolet luminosities</term><term>Webb</term><term>Whiting</term><term>Wiklind</term><term>Wiklind combes</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Absorber</term><term>Carilli</term><term>Colour</term><term>Colour depth</term><term>Column densities</term><term>Column density</term><term>Column density limits</term><term>Combes</term><term>Curran</term><term>Curran whiting</term><term>Decimetre</term><term>Drinkwater</term><term>Emission redshift</term><term>Excitation</term><term>Excitation temperature</term><term>Excitation temperatures</term><term>Fwhm</term><term>Galaxy</term><term>Host galaxy</term><term>Iram</term><term>Luminosity</term><term>Millimetre</term><term>Millimetre absorbers</term><term>Millimetre absorption</term><term>Mnras</term><term>Molecular absorption</term><term>Molecular fractions</term><term>Monthly notices</term><term>Optical depth</term><term>Previous surveys</term><term>Prochaska</term><term>Quasar</term><term>Reddening</term><term>Redshift</term><term>Spectral scans</term><term>Total column density</term><term>Ultraviolet luminosities</term><term>Webb</term><term>Whiting</term><term>Wiklind</term><term>Wiklind combes</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have undertaken a search for millimetre‐waveband absorption (through the CO and HCO+ rotational transitions) in the host galaxies of reddened radio sources (z= 0.405–1.802). Despite the colour selection (optical–near‐infrared colours of V−K≳ 5 in all but one source), no absorption was found in any of the eight quasars for which the background continuum flux was detected. On the basis of the previous (mostly intervening) H2 and OH detections, the limits reached here and in some previous surveys should be deep enough to detect molecular absorption according to their V−K colours. However, our survey makes the assumption that the reddening is associated with dust close to the emission redshift of the quasar and that the narrow millimetre component of this emission is intercepted by the compact molecular cores. By using the known millimetre absorbers to define the colour depth and comparing this with the ultraviolet luminosities of the sources, we find that, even if these assumptions are valid, only 12 of the 40 objects (mainly from this work) are potentially detectable. This is assuming an excitation temperature of Tx= 10 K at z= 0, with the number decreasing with increasing temperatures (to zero detectable at Tx≳ 100 K).</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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