On the absence of molecular absorption in high-redshift millimetre-band searches
Identifieur interne : 004593 ( PascalFrancis/Curation ); précédent : 004592; suivant : 004594On 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.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Cosmologie.
English descriptors
- KwdEn :
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).
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Webb</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Murphy, M T" sort="Murphy, M T" uniqKey="Murphy M" first="M. T." last="Murphy">M. T. Murphy</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Centre for Astrophysics and Supercornputing, Swinburne University of Technology, PO Box 218</s1><s2>Hawthorn, VIC 3122</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Wiklind, T" sort="Wiklind, T" uniqKey="Wiklind T" first="T." last="Wiklind">T. Wiklind</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Space Telescope Science Institute</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Onsala Space Observatory</s1><s2>439 92 Onsala</s2><s3>SWE</s3><sZ>9 aut.</sZ></inist:fA14><country>Suède</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Joint ALMA Observatory</s1><s2>Santiago</s2><s3>CHL</s3><sZ>9 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0409599</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0409599 INIST</idno><idno type="RBID">Pascal:11-0409599</idno><idno type="wicri:Area/PascalFrancis/Corpus">001962</idno><idno type="wicri:Area/PascalFrancis/Curation">004593</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">On the absence of molecular absorption in high-redshift millimetre-band searches</title><author><name sortKey="Curran, S J" sort="Curran, S J" uniqKey="Curran S" first="S. J." last="Curran">S. J. Curran</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Whiting, M T" sort="Whiting, M T" uniqKey="Whiting M" first="M. T." last="Whiting">M. T. Whiting</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>CSIRO Australia Telescope National Facility, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>2 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>LERMA, Observatoire de Paris, 77 Avenue Denfert-Rocherecau</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Kuno, N" sort="Kuno, N" uniqKey="Kuno N" first="N." last="Kuno">N. Kuno</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Nobeyama Radio Observatory</s1><s2>Nagano 384-1305</s2><s3>JPN</s3><sZ>4 aut.</sZ></inist:fA14><country>Japon</country></affiliation></author><author><name sortKey="Francis, P" sort="Francis, P" uniqKey="Francis P" first="P." last="Francis">P. Francis</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Australian National University</s1><s2>Canberra</s2><s3>AUS</s3><sZ>5 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Nakai, N" sort="Nakai, N" uniqKey="Nakai N" first="N." last="Nakai">N. Nakai</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Institute of Physics, University of Tsukuba, Ten-noudai</s1><s2>Tsukuba, Ibaraki 305-8571</s2><s3>JPN</s3><sZ>6 aut.</sZ></inist:fA14><country>Japon</country></affiliation></author><author><name sortKey="Webb, J K" sort="Webb, J K" uniqKey="Webb J" first="J. K." last="Webb">J. K. Webb</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Murphy, M T" sort="Murphy, M T" uniqKey="Murphy M" first="M. T." last="Murphy">M. T. Murphy</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Centre for Astrophysics and Supercornputing, Swinburne University of Technology, PO Box 218</s1><s2>Hawthorn, VIC 3122</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Wiklind, T" sort="Wiklind, T" uniqKey="Wiklind T" first="T." last="Wiklind">T. Wiklind</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Space Telescope Science Institute</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Onsala Space Observatory</s1><s2>439 92 Onsala</s2><s3>SWE</s3><sZ>9 aut.</sZ></inist:fA14><country>Suède</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>Joint ALMA Observatory</s1><s2>Santiago</s2><s3>CHL</s3><sZ>9 aut.</sZ></inist:fA14><country>Chili</country></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absorption line</term><term>Abundance</term><term>Active galaxies</term><term>Color</term><term>Continuum</term><term>Cosmic radio sources</term><term>Cosmology</term><term>Excitation</term><term>Luminosity</term><term>Molecular absorption</term><term>Quasars</term><term>Radio galaxies</term><term>Red shift</term><term>Rotational transition</term><term>Temperature zero K</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Absorption moléculaire</term><term>Déplacement vers le rouge</term><term>Transition rotationnelle</term><term>Galaxies actives</term><term>Couleur</term><term>Quasar</term><term>Continuum</term><term>Luminosité</term><term>Excitation</term><term>Température zéro K</term><term>Abondance</term><term>Raie absorption</term><term>Cosmologie</term><term>Radiogalaxies</term><term>Radiosource cosmique</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Cosmologie</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<sup>+</sup> 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) H<sub>2</sub> 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 T<sub>x</sub> = 10 K at z = 0, with the number decreasing with increasing temperatures (to zero detectable at T<sub>x</sub> ? 100 K).</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>416</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>On the absence of molecular absorption in high-redshift millimetre-band searches</s1></fA08><fA11 i1="01" i2="1"><s1>CURRAN (S. J.)</s1></fA11><fA11 i1="02" i2="1"><s1>WHITING (M. T.)</s1></fA11><fA11 i1="03" i2="1"><s1>COMBES (F.)</s1></fA11><fA11 i1="04" i2="1"><s1>KUNO (N.)</s1></fA11><fA11 i1="05" i2="1"><s1>FRANCIS (P.)</s1></fA11><fA11 i1="06" i2="1"><s1>NAKAI (N.)</s1></fA11><fA11 i1="07" i2="1"><s1>WEBB (J. K.)</s1></fA11><fA11 i1="08" i2="1"><s1>MURPHY (M. T.)</s1></fA11><fA11 i1="09" i2="1"><s1>WIKLIND (T.)</s1></fA11><fA14 i1="01"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>7 aut.</sZ><sZ>8 aut.</sZ></fA14><fA14 i1="02"><s1>CSIRO Australia Telescope National Facility, PO Box 76</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>2 aut.</sZ></fA14><fA14 i1="03"><s1>LERMA, Observatoire de Paris, 77 Avenue Denfert-Rocherecau</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Nobeyama Radio Observatory</s1><s2>Nagano 384-1305</s2><s3>JPN</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Australian National University</s1><s2>Canberra</s2><s3>AUS</s3><sZ>5 aut.</sZ></fA14><fA14 i1="06"><s1>Institute of Physics, University of Tsukuba, Ten-noudai</s1><s2>Tsukuba, Ibaraki 305-8571</s2><s3>JPN</s3><sZ>6 aut.</sZ></fA14><fA14 i1="07"><s1>Centre for Astrophysics and Supercornputing, Swinburne University of Technology, PO Box 218</s1><s2>Hawthorn, VIC 3122</s2><s3>AUS</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>Space Telescope Science Institute</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ></fA14><fA14 i1="09"><s1>Onsala Space Observatory</s1><s2>439 92 Onsala</s2><s3>SWE</s3><sZ>9 aut.</sZ></fA14><fA14 i1="10"><s1>Joint ALMA Observatory</s1><s2>Santiago</s2><s3>CHL</s3><sZ>9 aut.</sZ></fA14><fA20><s1>2143-2153</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000509103310400</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0409599</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>USA</s0></fA66><fC01 i1="01" l="ENG"><s0>We have undertaken a search for millimetre-waveband absorption (through the CO and HCO<sup>+</sup> 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) H<sub>2</sub> 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 T<sub>x</sub> = 10 K at z = 0, with the number decreasing with increasing temperatures (to zero detectable at T<sub>x</sub> ? 100 K).</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Absorption moléculaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Molecular absorption</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Absorción molecular</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Déplacement vers le rouge</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Red shift</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Transition rotationnelle</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Rotational transition</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Transición rotacional</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Galaxies actives</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Active galaxies</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Couleur</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Color</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Quasar</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Quasars</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Continuum</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Continuum</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Continuo</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Luminosité</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Luminosity</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Excitation</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Excitation</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Température zéro K</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Temperature zero K</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Abondance</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Abundance</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Raie absorption</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>Absorption line</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Raya absorción</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Cosmologie</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Cosmology</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Radiogalaxies</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Radio galaxies</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Radiosource cosmique</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Cosmic radio sources</s0><s5>40</s5></fC03><fN21><s1>283</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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|wiki= Wicri/Asie
|area= AustralieFrV1
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|étape= Curation
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|clé= Pascal:11-0409599
|texte= On the absence of molecular absorption in high-redshift millimetre-band searches
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