The sizes and kinematic structure of absorption systems towards the lensed quasar APM08279+5255
Identifieur interne : 005022 ( PascalFrancis/Corpus ); précédent : 005021; suivant : 005023The sizes and kinematic structure of absorption systems towards the lensed quasar APM08279+5255
Auteurs : S. L. Ellison ; R. Ibata ; M. Pettini ; G. F. Lewis ; B. Aracil ; P. Petitjean ; R. SrianandSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2004.
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Abstract
We have obtained spatially resolved spectra of the zem = 3.911 triply imaged QSO APM08279+5255 using the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). We study the line of sight equivalent width (EW) differences and velocity shear of high and low ionization absorbers (including a damped Lyman alpha [DLA] system identified in a spatially unresolved ground based spectrum) in the three lines of sight. The combination of a particularly rich spectrum and three sight-lines allow us to study 27 intervening absorption systems over a redshift range 1.1 < zabs < 3.8, probing proper transverse dimensions of 30 h-170 pc up to 2.7 h-170 kpc. We find that high ionization systems (primarily C IV absorbers) do not exhibit strong EW variations on scales <0.4 h-170 kpc; their fractional EW differences are typically less than 30%. When combined with previous work on other QSO pairs, we find that the fractional variation increases steadily with separation out to at least ∼100 h-170 kpc. Conversely, low ionization systems (primarily Mg II absorbers) show strong variations (often >80%) over kpc scales. A minimum radius for strong (EW > 0.3 Å) Mg II systems of >1.4 h-170 kpc is inferred from absorption coincidences in all lines of sight. For weak Mg II absorbers (EW < 0.3 Å), a maximum likelihood analysis indicates a most probable coherence scale of 2.0 h-170 kpc for a uniform spherical geometry, with 95% confidence limits ranging between 1.5 and 4.4 h-170 kpc. The weak Mg II absorbers may therefore represent a distinct population of smaller galaxies compared with the strong Mg II systems which we know to be associated with luminous galaxies whose halos extend over tens of kpc. Alternatively, the weak systems may reside in the outer parts of larger galaxies, where their filling factor may be lower. By cross-correlating spectra along different lines of sight, we infer shear velocities of typically less than 20 km s-1 for both high and low ionization absorbers. Finally, for systems with weak absorption that can be confidently converted to column densities, we find constant N(C IV)/N(Si IV) across the three lines of sight. Similarly, the [Al/Fe] ratios in the zabs = 2.974 DLA are consistent with solar relative abundances over a transverse distance of ∼0.35 h-170 kpc.
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| ET : | The sizes and kinematic structure of absorption systems towards the lensed quasar APM08279+5255 |
| AU : | ELLISON (S. L.); IBATA (R.); PETTINI (M.); LEWIS (G. F.); ARACIL (B.); PETITJEAN (P.); SRIANAND (R.) |
| AF : | P. Universidad Católica de Chile, Casilla 306/Santiago 22/Chili (1 aut.); European Southern Observatory, Casilla 19001/Santiago 19/Chili (1 aut.); University of Victoria, Department of Physics and Astronomy, Elliott Building, 3800 Finnerty Rd./Victoria, BC, V8P 1A1/Canada (1 aut.); Observatoire de Strasbourg, 11 rue de l'Université/67000, Strasbourg/France (2 aut.); Institute of Astronomy, Madingley Rd/Cambridge, CB3 0HA/Royaume-Uni (3 aut.); Institute of Astronomy, School of Physics, A 29, University of Sydney/NSW 2006/Australie (4 aut.); Institut d'Astrophysique de Paris - CNRS, 98bis boulevard Arago/75014 Paris/France (5 aut., 6 aut.); IUCAA, Post Bag 4, Ganeshkhind/Pune 411 007/Inde (7 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2004; Vol. 414; No. 1; Pp. 79-93; Bibl. 59 ref. |
| LA : | Anglais |
| EA : | We have obtained spatially resolved spectra of the zem = 3.911 triply imaged QSO APM08279+5255 using the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). We study the line of sight equivalent width (EW) differences and velocity shear of high and low ionization absorbers (including a damped Lyman alpha [DLA] system identified in a spatially unresolved ground based spectrum) in the three lines of sight. The combination of a particularly rich spectrum and three sight-lines allow us to study 27 intervening absorption systems over a redshift range 1.1 < zabs < 3.8, probing proper transverse dimensions of 30 h-170 pc up to 2.7 h-170 kpc. We find that high ionization systems (primarily C IV absorbers) do not exhibit strong EW variations on scales <0.4 h-170 kpc; their fractional EW differences are typically less than 30%. When combined with previous work on other QSO pairs, we find that the fractional variation increases steadily with separation out to at least ∼100 h-170 kpc. Conversely, low ionization systems (primarily Mg II absorbers) show strong variations (often >80%) over kpc scales. A minimum radius for strong (EW > 0.3 Å) Mg II systems of >1.4 h-170 kpc is inferred from absorption coincidences in all lines of sight. For weak Mg II absorbers (EW < 0.3 Å), a maximum likelihood analysis indicates a most probable coherence scale of 2.0 h-170 kpc for a uniform spherical geometry, with 95% confidence limits ranging between 1.5 and 4.4 h-170 kpc. The weak Mg II absorbers may therefore represent a distinct population of smaller galaxies compared with the strong Mg II systems which we know to be associated with luminous galaxies whose halos extend over tens of kpc. Alternatively, the weak systems may reside in the outer parts of larger galaxies, where their filling factor may be lower. By cross-correlating spectra along different lines of sight, we infer shear velocities of typically less than 20 km s-1 for both high and low ionization absorbers. Finally, for systems with weak absorption that can be confidently converted to column densities, we find constant N(C IV)/N(Si IV) across the three lines of sight. Similarly, the [Al/Fe] ratios in the zabs = 2.974 DLA are consistent with solar relative abundances over a transverse distance of ∼0.35 h-170 kpc. |
| CC : | 001E03D54A; 001E03D62R |
| FD : | Cinématique; Quasar; Largeur équivalente; Ionisation; Maximum vraisemblance; Limite confiance; Densité colonne; Abondance solaire; Distance; Raie absorption; Dynamique; Mirage gravitationnel; Quasar triple; Cisaillement vitesse |
| ED : | Kinematics; Quasars; Equivalent width; Ionization; Maximum likelihood; Confidence limit; Column density; Solar abundance; Distances; Absorption line; Dynamics; Gravitational lensing; Triple quasar; Velocity shear |
| SD : | Anchura equivalente; Maxima verosimilitud; Límite confianza; Densidad columna; Abundancia solar; Raya absorción; Espejismo gravitacional; Quásar triple; Cizallamiento velocidad |
| LO : | INIST-14176.354000115931010110 |
| ID : | 04-0135231 |
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Universidad Católica de Chile, Casilla 306</s1><s2>Santiago 22</s2><s3>CHL</s3><sZ>1 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>European Southern Observatory, Casilla 19001</s1><s2>Santiago 19</s2><s3>CHL</s3><sZ>1 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="03"><s1>University of Victoria, Department of Physics and Astronomy, Elliott Building, 3800 Finnerty Rd.</s1><s2>Victoria, BC, V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ibata, R" sort="Ibata, R" uniqKey="Ibata R" first="R." last="Ibata">R. Ibata</name><affiliation><inist:fA14 i1="04"><s1>Observatoire de Strasbourg, 11 rue de l'Université</s1><s2>67000, Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Pettini, M" sort="Pettini, M" uniqKey="Pettini M" first="M." last="Pettini">M. Pettini</name><affiliation><inist:fA14 i1="05"><s1>Institute of Astronomy, Madingley Rd</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>3 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lewis, G F" sort="Lewis, G F" uniqKey="Lewis G" first="G. F." last="Lewis">G. F. Lewis</name><affiliation><inist:fA14 i1="06"><s1>Institute of Astronomy, School of Physics, A 29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Aracil, B" sort="Aracil, B" uniqKey="Aracil B" first="B." last="Aracil">B. Aracil</name><affiliation><inist:fA14 i1="07"><s1>Institut d'Astrophysique de Paris - CNRS, 98bis boulevard Arago</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Petitjean, P" sort="Petitjean, P" uniqKey="Petitjean P" first="P." last="Petitjean">P. Petitjean</name><affiliation><inist:fA14 i1="07"><s1>Institut d'Astrophysique de Paris - CNRS, 98bis boulevard Arago</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>5 aut.</sZ><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Srianand, R" sort="Srianand, R" uniqKey="Srianand R" first="R." last="Srianand">R. Srianand</name><affiliation><inist:fA14 i1="08"><s1>IUCAA, Post Bag 4, Ganeshkhind</s1><s2>Pune 411 007</s2><s3>IND</s3><sZ>7 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2004">2004</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absorption line</term><term>Column density</term><term>Confidence limit</term><term>Distances</term><term>Dynamics</term><term>Equivalent width</term><term>Gravitational lensing</term><term>Ionization</term><term>Kinematics</term><term>Maximum likelihood</term><term>Quasars</term><term>Solar abundance</term><term>Triple quasar</term><term>Velocity shear</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Cinématique</term><term>Quasar</term><term>Largeur équivalente</term><term>Ionisation</term><term>Maximum vraisemblance</term><term>Limite confiance</term><term>Densité colonne</term><term>Abondance solaire</term><term>Distance</term><term>Raie absorption</term><term>Dynamique</term><term>Mirage gravitationnel</term><term>Quasar triple</term><term>Cisaillement vitesse</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have obtained spatially resolved spectra of the z<sub>em</sub> = 3.911 triply imaged QSO APM08279+5255 using the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). We study the line of sight equivalent width (EW) differences and velocity shear of high and low ionization absorbers (including a damped Lyman alpha [DLA] system identified in a spatially unresolved ground based spectrum) in the three lines of sight. The combination of a particularly rich spectrum and three sight-lines allow us to study 27 intervening absorption systems over a redshift range 1.1 < z<sub>abs</sub> < 3.8, probing proper transverse dimensions of 30 h<sup>-1</sup>70 pc up to 2.7 h<sup>-1</sup>70 kpc. We find that high ionization systems (primarily C IV absorbers) do not exhibit strong EW variations on scales <0.4 h<sup>-1</sup>70 kpc; their fractional EW differences are typically less than 30%. When combined with previous work on other QSO pairs, we find that the fractional variation increases steadily with separation out to at least ∼100 h<sup>-1</sup>70 kpc. Conversely, low ionization systems (primarily Mg II absorbers) show strong variations (often >80%) over kpc scales. A minimum radius for strong (EW > 0.3 Å) Mg II systems of >1.4 h<sup>-1</sup>70 kpc is inferred from absorption coincidences in all lines of sight. For weak Mg II absorbers (EW < 0.3 Å), a maximum likelihood analysis indicates a most probable coherence scale of 2.0 h<sup>-1</sup>70 kpc for a uniform spherical geometry, with 95% confidence limits ranging between 1.5 and 4.4 h<sup>-1</sup>70 kpc. The weak Mg II absorbers may therefore represent a distinct population of smaller galaxies compared with the strong Mg II systems which we know to be associated with luminous galaxies whose halos extend over tens of kpc. Alternatively, the weak systems may reside in the outer parts of larger galaxies, where their filling factor may be lower. By cross-correlating spectra along different lines of sight, we infer shear velocities of typically less than 20 km s<sup>-1</sup> for both high and low ionization absorbers. Finally, for systems with weak absorption that can be confidently converted to column densities, we find constant N(C IV)/N(Si IV) across the three lines of sight. Similarly, the [Al/Fe] ratios in the z<sub>abs</sub> = 2.974 DLA are consistent with solar relative abundances over a transverse distance of ∼0.35 h<sup>-1</sup>70 kpc.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>414</s2></fA05><fA06><s2>1</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The sizes and kinematic structure of absorption systems towards the lensed quasar APM08279+5255</s1></fA08><fA11 i1="01" i2="1"><s1>ELLISON (S. L.)</s1></fA11><fA11 i1="02" i2="1"><s1>IBATA (R.)</s1></fA11><fA11 i1="03" i2="1"><s1>PETTINI (M.)</s1></fA11><fA11 i1="04" i2="1"><s1>LEWIS (G. F.)</s1></fA11><fA11 i1="05" i2="1"><s1>ARACIL (B.)</s1></fA11><fA11 i1="06" i2="1"><s1>PETITJEAN (P.)</s1></fA11><fA11 i1="07" i2="1"><s1>SRIANAND (R.)</s1></fA11><fA14 i1="01"><s1>P. Universidad Católica de Chile, Casilla 306</s1><s2>Santiago 22</s2><s3>CHL</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>European Southern Observatory, Casilla 19001</s1><s2>Santiago 19</s2><s3>CHL</s3><sZ>1 aut.</sZ></fA14><fA14 i1="03"><s1>University of Victoria, Department of Physics and Astronomy, Elliott Building, 3800 Finnerty Rd.</s1><s2>Victoria, BC, V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ></fA14><fA14 i1="04"><s1>Observatoire de Strasbourg, 11 rue de l'Université</s1><s2>67000, Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ></fA14><fA14 i1="05"><s1>Institute of Astronomy, Madingley Rd</s1><s2>Cambridge, CB3 0HA</s2><s3>GBR</s3><sZ>3 aut.</sZ></fA14><fA14 i1="06"><s1>Institute of Astronomy, School of Physics, A 29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>4 aut.</sZ></fA14><fA14 i1="07"><s1>Institut d'Astrophysique de Paris - CNRS, 98bis boulevard Arago</s1><s2>75014 Paris</s2><s3>FRA</s3><sZ>5 aut.</sZ><sZ>6 aut.</sZ></fA14><fA14 i1="08"><s1>IUCAA, Post Bag 4, Ganeshkhind</s1><s2>Pune 411 007</s2><s3>IND</s3><sZ>7 aut.</sZ></fA14><fA20><s1>79-93</s1></fA20><fA21><s1>2004</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000115931010110</s5></fA43><fA44><s0>0000</s0><s1>© 2004 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>59 ref.</s0></fA45><fA47 i1="01" i2="1"><s0>04-0135231</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>We have obtained spatially resolved spectra of the z<sub>em</sub> = 3.911 triply imaged QSO APM08279+5255 using the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). We study the line of sight equivalent width (EW) differences and velocity shear of high and low ionization absorbers (including a damped Lyman alpha [DLA] system identified in a spatially unresolved ground based spectrum) in the three lines of sight. The combination of a particularly rich spectrum and three sight-lines allow us to study 27 intervening absorption systems over a redshift range 1.1 < z<sub>abs</sub> < 3.8, probing proper transverse dimensions of 30 h<sup>-1</sup>70 pc up to 2.7 h<sup>-1</sup>70 kpc. We find that high ionization systems (primarily C IV absorbers) do not exhibit strong EW variations on scales <0.4 h<sup>-1</sup>70 kpc; their fractional EW differences are typically less than 30%. When combined with previous work on other QSO pairs, we find that the fractional variation increases steadily with separation out to at least ∼100 h<sup>-1</sup>70 kpc. Conversely, low ionization systems (primarily Mg II absorbers) show strong variations (often >80%) over kpc scales. A minimum radius for strong (EW > 0.3 Å) Mg II systems of >1.4 h<sup>-1</sup>70 kpc is inferred from absorption coincidences in all lines of sight. For weak Mg II absorbers (EW < 0.3 Å), a maximum likelihood analysis indicates a most probable coherence scale of 2.0 h<sup>-1</sup>70 kpc for a uniform spherical geometry, with 95% confidence limits ranging between 1.5 and 4.4 h<sup>-1</sup>70 kpc. The weak Mg II absorbers may therefore represent a distinct population of smaller galaxies compared with the strong Mg II systems which we know to be associated with luminous galaxies whose halos extend over tens of kpc. Alternatively, the weak systems may reside in the outer parts of larger galaxies, where their filling factor may be lower. By cross-correlating spectra along different lines of sight, we infer shear velocities of typically less than 20 km s<sup>-1</sup> for both high and low ionization absorbers. Finally, for systems with weak absorption that can be confidently converted to column densities, we find constant N(C IV)/N(Si IV) across the three lines of sight. Similarly, the [Al/Fe] ratios in the z<sub>abs</sub> = 2.974 DLA are consistent with solar relative abundances over a transverse distance of ∼0.35 h<sup>-1</sup>70 kpc.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03D54A</s0></fC02><fC02 i1="02" i2="3"><s0>001E03D62R</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Cinématique</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Kinematics</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Quasar</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Quasars</s0><s5>27</s5></fC03><fC03 i1="03" i2="X" l="FRE"><s0>Largeur équivalente</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="ENG"><s0>Equivalent width</s0><s5>28</s5></fC03><fC03 i1="03" i2="X" l="SPA"><s0>Anchura equivalente</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Ionisation</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Ionization</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Maximum vraisemblance</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Maximum likelihood</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Maxima verosimilitud</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Limite confiance</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Confidence limit</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Límite confianza</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Densité colonne</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Column density</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Densidad columna</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Abondance solaire</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Solar abundance</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Abundancia solar</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Distance</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Distances</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Raie absorption</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Absorption line</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Raya absorción</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Dynamique</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Dynamics</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Mirage gravitationnel</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>Gravitational lensing</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Espejismo gravitacional</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Quasar triple</s0><s5>40</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Triple quasar</s0><s5>40</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Quásar triple</s0><s5>40</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Cisaillement vitesse</s0><s5>41</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Velocity shear</s0><s5>41</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Cizallamiento velocidad</s0><s5>41</s5></fC03><fN21><s1>089</s1></fN21><fN82><s1>PSI</s1></fN82></pA></standard><server><NO>PASCAL 04-0135231 INIST</NO><ET>The sizes and kinematic structure of absorption systems towards the lensed quasar APM08279+5255</ET><AU>ELLISON (S. L.); IBATA (R.); PETTINI (M.); LEWIS (G. F.); ARACIL (B.); PETITJEAN (P.); SRIANAND (R.)</AU><AF>P. Universidad Católica de Chile, Casilla 306/Santiago 22/Chili (1 aut.); European Southern Observatory, Casilla 19001/Santiago 19/Chili (1 aut.); University of Victoria, Department of Physics and Astronomy, Elliott Building, 3800 Finnerty Rd./Victoria, BC, V8P 1A1/Canada (1 aut.); Observatoire de Strasbourg, 11 rue de l'Université/67000, Strasbourg/France (2 aut.); Institute of Astronomy, Madingley Rd/Cambridge, CB3 0HA/Royaume-Uni (3 aut.); Institute of Astronomy, School of Physics, A 29, University of Sydney/NSW 2006/Australie (4 aut.); Institut d'Astrophysique de Paris - CNRS, 98bis boulevard Arago/75014 Paris/France (5 aut., 6 aut.); IUCAA, Post Bag 4, Ganeshkhind/Pune 411 007/Inde (7 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2004; Vol. 414; No. 1; Pp. 79-93; Bibl. 59 ref.</SO><LA>Anglais</LA><EA>We have obtained spatially resolved spectra of the z<sub>em</sub> = 3.911 triply imaged QSO APM08279+5255 using the Space Telescope Imaging Spectrograph (STIS) on board the Hubble Space Telescope (HST). We study the line of sight equivalent width (EW) differences and velocity shear of high and low ionization absorbers (including a damped Lyman alpha [DLA] system identified in a spatially unresolved ground based spectrum) in the three lines of sight. The combination of a particularly rich spectrum and three sight-lines allow us to study 27 intervening absorption systems over a redshift range 1.1 < z<sub>abs</sub> < 3.8, probing proper transverse dimensions of 30 h<sup>-1</sup>70 pc up to 2.7 h<sup>-1</sup>70 kpc. We find that high ionization systems (primarily C IV absorbers) do not exhibit strong EW variations on scales <0.4 h<sup>-1</sup>70 kpc; their fractional EW differences are typically less than 30%. When combined with previous work on other QSO pairs, we find that the fractional variation increases steadily with separation out to at least ∼100 h<sup>-1</sup>70 kpc. Conversely, low ionization systems (primarily Mg II absorbers) show strong variations (often >80%) over kpc scales. A minimum radius for strong (EW > 0.3 Å) Mg II systems of >1.4 h<sup>-1</sup>70 kpc is inferred from absorption coincidences in all lines of sight. For weak Mg II absorbers (EW < 0.3 Å), a maximum likelihood analysis indicates a most probable coherence scale of 2.0 h<sup>-1</sup>70 kpc for a uniform spherical geometry, with 95% confidence limits ranging between 1.5 and 4.4 h<sup>-1</sup>70 kpc. The weak Mg II absorbers may therefore represent a distinct population of smaller galaxies compared with the strong Mg II systems which we know to be associated with luminous galaxies whose halos extend over tens of kpc. Alternatively, the weak systems may reside in the outer parts of larger galaxies, where their filling factor may be lower. By cross-correlating spectra along different lines of sight, we infer shear velocities of typically less than 20 km s<sup>-1</sup> for both high and low ionization absorbers. Finally, for systems with weak absorption that can be confidently converted to column densities, we find constant N(C IV)/N(Si IV) across the three lines of sight. Similarly, the [Al/Fe] ratios in the z<sub>abs</sub> = 2.974 DLA are consistent with solar relative abundances over a transverse distance of ∼0.35 h<sup>-1</sup>70 kpc.</EA><CC>001E03D54A; 001E03D62R</CC><FD>Cinématique; Quasar; Largeur équivalente; Ionisation; Maximum vraisemblance; Limite confiance; Densité colonne; Abondance solaire; Distance; Raie absorption; Dynamique; Mirage gravitationnel; Quasar triple; Cisaillement vitesse</FD><ED>Kinematics; Quasars; Equivalent width; Ionization; Maximum likelihood; Confidence limit; Column density; Solar abundance; Distances; Absorption line; Dynamics; Gravitational lensing; Triple quasar; Velocity shear</ED><SD>Anchura equivalente; Maxima verosimilitud; Límite confianza; Densidad columna; Abundancia solar; Raya absorción; Espejismo gravitacional; Quásar triple; Cizallamiento velocidad</SD><LO>INIST-14176.354000115931010110</LO><ID>04-0135231</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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