Diffuse interstellar bands in RAVE survey spectra
Identifieur interne : 002444 ( PascalFrancis/Corpus ); précédent : 002443; suivant : 002445Diffuse interstellar bands in RAVE survey spectra
Auteurs : U. Munari ; L. Tomasella ; M. Fiorucci ; O. Bienayme ; J. Binney ; J. Bland-Hawthorn ; C. Beeche ; R. Campbell ; K. C. Freeman ; B. Gibson ; G. Gilmore ; E. K. Grebel ; A. Helmi ; J. F. Navarro ; Q. A. Parker ; G. M. Seabroke ; A. Siebert ; A. Siviero ; M. Steinmetz ; F. G. Watson ; M. Williams ; R. F. G. Wyse ; T. ZwitterSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2008.
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Abstract
We have used spectra of hot stars from the RAVE Survey in order to investigate the visibility and properties of five diffuse interstellar bands previously reported in the literature. The RAVE spectroscopic survey for Galactic structure and kinematics records CCD spectra covering the 8400-8800 Å wavelength region at 7500 resolving power. The spectra are obtained with the UK Schmidt at the AAO, equipped with the 6dF multi-fiber positioner. The DIB at 8620.4 Å is by far the strongest and cleanest of all DIBs occurring within the RAVE wavelength range, with no interference by underlying absorption stellar lines in hot stars. It correlates so tightly with reddening that it turns out to be a reliable tool to measure it, following the relation EB-v = 2.72(±0.03) x EW (Å), valid throughout the general interstellar medium of our Galaxy. The presence of a DIB at 8648 Å is confirmed. Its intensity appears unrelated to reddening, in agreement with scanty and preliminary reports available in the literature, and its measurability is strongly compromised by severe blending with underlying stellar He I doublet at 8649 Å. The two weak DIBs at 8531 and 8572 Å do not appear real and should actually be blends of underlying stellar lines. The very weak DIB at 8439 Å cannot be resolved within the profile of the much stronger underlying hydrogen Paschen 18 stellar line.
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| NO : | PASCAL 10-0384234 INIST |
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| ET : | Diffuse interstellar bands in RAVE survey spectra |
| AU : | MUNARI (U.); TOMASELLA (L.); FIORUCCI (M.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); BEECHE (C.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.) |
| AF : | INAF Osservatorio Astronomico di Padova/Asiago/Italie (1 aut., 2 aut., 3 aut., 18 aut.); Observatoire de Strasbourg/Strasbourg/France (4 aut., 17 aut.); Rudolf Pierls Center for Theoretical Physics, University of Oxford/Royaume-Uni (5 aut.); Institute of Astronomy, School of Physics, University of Sydney/Australie (6 aut.); Astrophysikalisches Institut Potsdam/Potsdam/Allemagne (7 aut., 8 aut., 17 aut., 19 aut., 21 aut.); Macquarie University/Sidney/Australie (8 aut., 15 aut.); RSAA Mount Stromlo Observatory/Camberra/Australie (9 aut., 21 aut.); University of Central Lancashire/Preston/Royaume-Uni (10 aut.); Institute of Astronomy, University of Cambridge/Royaume-Uni (11 aut., 16 aut.); Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg/Heidelberg/Allemagne (12 aut.); University of Groningen/Groningen/Pays-Bas (13 aut.); University of Victoria/Victoria/Canada (14 aut.); e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University/Uxbridge/Royaume-Uni (16 aut.); Anglo Australian Observatory/Sydney/Australie (20 aut.); Johns Hopkins University/Baltimore, Maryland/Etats-Unis (22 aut.); Faculty of Mathematics and Physics, University of Ljubljana/Ljubljana/Slovénie (23 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2008; Vol. 488; No. 3; Pp. 969-973; Bibl. 1/4 p. |
| LA : | Anglais |
| EA : | We have used spectra of hot stars from the RAVE Survey in order to investigate the visibility and properties of five diffuse interstellar bands previously reported in the literature. The RAVE spectroscopic survey for Galactic structure and kinematics records CCD spectra covering the 8400-8800 Å wavelength region at 7500 resolving power. The spectra are obtained with the UK Schmidt at the AAO, equipped with the 6dF multi-fiber positioner. The DIB at 8620.4 Å is by far the strongest and cleanest of all DIBs occurring within the RAVE wavelength range, with no interference by underlying absorption stellar lines in hot stars. It correlates so tightly with reddening that it turns out to be a reliable tool to measure it, following the relation EB-v = 2.72(±0.03) x EW (Å), valid throughout the general interstellar medium of our Galaxy. The presence of a DIB at 8648 Å is confirmed. Its intensity appears unrelated to reddening, in agreement with scanty and preliminary reports available in the literature, and its measurability is strongly compromised by severe blending with underlying stellar He I doublet at 8649 Å. The two weak DIBs at 8531 and 8572 Å do not appear real and should actually be blends of underlying stellar lines. The very weak DIB at 8439 Å cannot be resolved within the profile of the much stronger underlying hydrogen Paschen 18 stellar line. |
| CC : | 001E03 |
| FD : | Bande interstellaire diffuse; Etoile chaude; Visibilité; Structure galactique; Cinématique; Raie absorption; Matière interstellaire; Galaxies; Intensité; Raie Paschen; Voie lactée |
| ED : | Diffuse interstellar band; Hot star; Visibility; Galactic structure; Kinematics; Absorption line; Interstellar matter; Galaxies; Intensity; Paschen lines; Milky Way |
| SD : | Banda interestelar difusa; Estrella caliente; Raya absorción; Intensidad |
| LO : | INIST-14176.354000196582860250 |
| ID : | 10-0384234 |
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Bland-Hawthorn</name><affiliation><inist:fA14 i1="04"><s1>Institute of Astronomy, School of Physics, University of Sydney</s1><s3>AUS</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Beeche, C" sort="Beeche, C" uniqKey="Beeche C" first="C." last="Beeche">C. Beeche</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Macquarie University</s1><s2>Sidney</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name><affiliation><inist:fA14 i1="07"><s1>RSAA Mount Stromlo Observatory</s1><s2>Camberra</s2><s3>AUS</s3><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibson, B" sort="Gibson, B" uniqKey="Gibson B" first="B." last="Gibson">B. Gibson</name><affiliation><inist:fA14 i1="08"><s1>University of Central Lancashire</s1><s2>Preston</s2><s3>GBR</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><inist:fA14 i1="09"><s1>Institute of Astronomy, University of Cambridge</s1><s3>GBR</s3><sZ>11 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Grebel, E K" sort="Grebel, E K" uniqKey="Grebel E" first="E. K." last="Grebel">E. K. Grebel</name><affiliation><inist:fA14 i1="10"><s1>Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg</s1><s2>Heidelberg</s2><s3>DEU</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name><affiliation><inist:fA14 i1="11"><s1>University of Groningen</s1><s2>Groningen</s2><s3>NLD</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name><affiliation><inist:fA14 i1="12"><s1>University of Victoria</s1><s2>Victoria</s2><s3>CAN</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><affiliation><inist:fA14 i1="06"><s1>Macquarie University</s1><s2>Sidney</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name><affiliation><inist:fA14 i1="09"><s1>Institute of Astronomy, University of Cambridge</s1><s3>GBR</s3><sZ>11 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="13"><s1>e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University</s1><s2>Uxbridge</s2><s3>GBR</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><inist:fA14 i1="02"><s1>Observatoire de Strasbourg</s1><s2>Strasbourg</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><inist:fA14 i1="01"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>Asiago</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation><inist:fA14 i1="14"><s1>Anglo Australian Observatory</s1><s2>Sydney</s2><s3>AUS</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="07"><s1>RSAA Mount Stromlo Observatory</s1><s2>Camberra</s2><s3>AUS</s3><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wyse, R F G" sort="Wyse, R F G" uniqKey="Wyse R" first="R. F. G." last="Wyse">R. F. G. Wyse</name><affiliation><inist:fA14 i1="15"><s1>Johns Hopkins University</s1><s2>Baltimore, Maryland</s2><s3>USA</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><inist:fA14 i1="16"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>23 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">10-0384234</idno><date when="2008">2008</date><idno type="stanalyst">PASCAL 10-0384234 INIST</idno><idno type="RBID">Pascal:10-0384234</idno><idno type="wicri:Area/PascalFrancis/Corpus">002444</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Diffuse interstellar bands in RAVE survey spectra</title><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation><inist:fA14 i1="01"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>Asiago</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Tomasella, L" sort="Tomasella, L" uniqKey="Tomasella L" first="L." last="Tomasella">L. Tomasella</name><affiliation><inist:fA14 i1="01"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>Asiago</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Fiorucci, M" sort="Fiorucci, M" uniqKey="Fiorucci M" first="M." last="Fiorucci">M. Fiorucci</name><affiliation><inist:fA14 i1="01"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>Asiago</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienayme">O. Bienayme</name><affiliation><inist:fA14 i1="02"><s1>Observatoire de Strasbourg</s1><s2>Strasbourg</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation><inist:fA14 i1="03"><s1>Rudolf Pierls Center for Theoretical Physics, University of Oxford</s1><s3>GBR</s3><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bland Hawthorn, J" sort="Bland Hawthorn, J" uniqKey="Bland Hawthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><affiliation><inist:fA14 i1="04"><s1>Institute of Astronomy, School of Physics, University of Sydney</s1><s3>AUS</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Beeche, C" sort="Beeche, C" uniqKey="Beeche C" first="C." last="Beeche">C. Beeche</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Macquarie University</s1><s2>Sidney</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name><affiliation><inist:fA14 i1="07"><s1>RSAA Mount Stromlo Observatory</s1><s2>Camberra</s2><s3>AUS</s3><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibson, B" sort="Gibson, B" uniqKey="Gibson B" first="B." last="Gibson">B. Gibson</name><affiliation><inist:fA14 i1="08"><s1>University of Central Lancashire</s1><s2>Preston</s2><s3>GBR</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><inist:fA14 i1="09"><s1>Institute of Astronomy, University of Cambridge</s1><s3>GBR</s3><sZ>11 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Grebel, E K" sort="Grebel, E K" uniqKey="Grebel E" first="E. K." last="Grebel">E. K. Grebel</name><affiliation><inist:fA14 i1="10"><s1>Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg</s1><s2>Heidelberg</s2><s3>DEU</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name><affiliation><inist:fA14 i1="11"><s1>University of Groningen</s1><s2>Groningen</s2><s3>NLD</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name><affiliation><inist:fA14 i1="12"><s1>University of Victoria</s1><s2>Victoria</s2><s3>CAN</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><affiliation><inist:fA14 i1="06"><s1>Macquarie University</s1><s2>Sidney</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name><affiliation><inist:fA14 i1="09"><s1>Institute of Astronomy, University of Cambridge</s1><s3>GBR</s3><sZ>11 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="13"><s1>e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University</s1><s2>Uxbridge</s2><s3>GBR</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><inist:fA14 i1="02"><s1>Observatoire de Strasbourg</s1><s2>Strasbourg</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><inist:fA14 i1="01"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>Asiago</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation><inist:fA14 i1="14"><s1>Anglo Australian Observatory</s1><s2>Sydney</s2><s3>AUS</s3><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation><inist:fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="07"><s1>RSAA Mount Stromlo Observatory</s1><s2>Camberra</s2><s3>AUS</s3><sZ>9 aut.</sZ><sZ>21 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wyse, R F G" sort="Wyse, R F G" uniqKey="Wyse R" first="R. F. G." last="Wyse">R. F. G. Wyse</name><affiliation><inist:fA14 i1="15"><s1>Johns Hopkins University</s1><s2>Baltimore, Maryland</s2><s3>USA</s3><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><inist:fA14 i1="16"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>23 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="2008">2008</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>Diffuse interstellar band</term><term>Galactic structure</term><term>Galaxies</term><term>Hot star</term><term>Intensity</term><term>Interstellar matter</term><term>Kinematics</term><term>Milky Way</term><term>Paschen lines</term><term>Visibility</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Bande interstellaire diffuse</term><term>Etoile chaude</term><term>Visibilité</term><term>Structure galactique</term><term>Cinématique</term><term>Raie absorption</term><term>Matière interstellaire</term><term>Galaxies</term><term>Intensité</term><term>Raie Paschen</term><term>Voie lactée</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We have used spectra of hot stars from the RAVE Survey in order to investigate the visibility and properties of five diffuse interstellar bands previously reported in the literature. The RAVE spectroscopic survey for Galactic structure and kinematics records CCD spectra covering the 8400-8800 Å wavelength region at 7500 resolving power. The spectra are obtained with the UK Schmidt at the AAO, equipped with the 6dF multi-fiber positioner. The DIB at 8620.4 Å is by far the strongest and cleanest of all DIBs occurring within the RAVE wavelength range, with no interference by underlying absorption stellar lines in hot stars. It correlates so tightly with reddening that it turns out to be a reliable tool to measure it, following the relation EB-v = 2.72(±0.03) x EW (Å), valid throughout the general interstellar medium of our Galaxy. The presence of a DIB at 8648 Å is confirmed. Its intensity appears unrelated to reddening, in agreement with scanty and preliminary reports available in the literature, and its measurability is strongly compromised by severe blending with underlying stellar He I doublet at 8649 Å. The two weak DIBs at 8531 and 8572 Å do not appear real and should actually be blends of underlying stellar lines. The very weak DIB at 8439 Å cannot be resolved within the profile of the much stronger underlying hydrogen Paschen 18 stellar line.</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>488</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Diffuse interstellar bands in RAVE survey spectra</s1></fA08><fA11 i1="01" i2="1"><s1>MUNARI (U.)</s1></fA11><fA11 i1="02" i2="1"><s1>TOMASELLA (L.)</s1></fA11><fA11 i1="03" i2="1"><s1>FIORUCCI (M.)</s1></fA11><fA11 i1="04" i2="1"><s1>BIENAYME (O.)</s1></fA11><fA11 i1="05" i2="1"><s1>BINNEY (J.)</s1></fA11><fA11 i1="06" i2="1"><s1>BLAND-HAWTHORN (J.)</s1></fA11><fA11 i1="07" i2="1"><s1>BEECHE (C.)</s1></fA11><fA11 i1="08" i2="1"><s1>CAMPBELL (R.)</s1></fA11><fA11 i1="09" i2="1"><s1>FREEMAN (K. C.)</s1></fA11><fA11 i1="10" i2="1"><s1>GIBSON (B.)</s1></fA11><fA11 i1="11" i2="1"><s1>GILMORE (G.)</s1></fA11><fA11 i1="12" i2="1"><s1>GREBEL (E. K.)</s1></fA11><fA11 i1="13" i2="1"><s1>HELMI (A.)</s1></fA11><fA11 i1="14" i2="1"><s1>NAVARRO (J. F.)</s1></fA11><fA11 i1="15" i2="1"><s1>PARKER (Q. A.)</s1></fA11><fA11 i1="16" i2="1"><s1>SEABROKE (G. M.)</s1></fA11><fA11 i1="17" i2="1"><s1>SIEBERT (A.)</s1></fA11><fA11 i1="18" i2="1"><s1>SIVIERO (A.)</s1></fA11><fA11 i1="19" i2="1"><s1>STEINMETZ (M.)</s1></fA11><fA11 i1="20" i2="1"><s1>WATSON (F. G.)</s1></fA11><fA11 i1="21" i2="1"><s1>WILLIAMS (M.)</s1></fA11><fA11 i1="22" i2="1"><s1>WYSE (R. F. G.)</s1></fA11><fA11 i1="23" i2="1"><s1>ZWITTER (T.)</s1></fA11><fA14 i1="01"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>Asiago</s2><s3>ITA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>18 aut.</sZ></fA14><fA14 i1="02"><s1>Observatoire de Strasbourg</s1><s2>Strasbourg</s2><s3>FRA</s3><sZ>4 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="03"><s1>Rudolf Pierls Center for Theoretical Physics, University of Oxford</s1><s3>GBR</s3><sZ>5 aut.</sZ></fA14><fA14 i1="04"><s1>Institute of Astronomy, School of Physics, University of Sydney</s1><s3>AUS</s3><sZ>6 aut.</sZ></fA14><fA14 i1="05"><s1>Astrophysikalisches Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>7 aut.</sZ><sZ>8 aut.</sZ><sZ>17 aut.</sZ><sZ>19 aut.</sZ><sZ>21 aut.</sZ></fA14><fA14 i1="06"><s1>Macquarie University</s1><s2>Sidney</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="07"><s1>RSAA Mount Stromlo Observatory</s1><s2>Camberra</s2><s3>AUS</s3><sZ>9 aut.</sZ><sZ>21 aut.</sZ></fA14><fA14 i1="08"><s1>University of Central Lancashire</s1><s2>Preston</s2><s3>GBR</s3><sZ>10 aut.</sZ></fA14><fA14 i1="09"><s1>Institute of Astronomy, University of Cambridge</s1><s3>GBR</s3><sZ>11 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="10"><s1>Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg</s1><s2>Heidelberg</s2><s3>DEU</s3><sZ>12 aut.</sZ></fA14><fA14 i1="11"><s1>University of Groningen</s1><s2>Groningen</s2><s3>NLD</s3><sZ>13 aut.</sZ></fA14><fA14 i1="12"><s1>University of Victoria</s1><s2>Victoria</s2><s3>CAN</s3><sZ>14 aut.</sZ></fA14><fA14 i1="13"><s1>e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University</s1><s2>Uxbridge</s2><s3>GBR</s3><sZ>16 aut.</sZ></fA14><fA14 i1="14"><s1>Anglo Australian Observatory</s1><s2>Sydney</s2><s3>AUS</s3><sZ>20 aut.</sZ></fA14><fA14 i1="15"><s1>Johns Hopkins University</s1><s2>Baltimore, Maryland</s2><s3>USA</s3><sZ>22 aut.</sZ></fA14><fA14 i1="16"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>23 aut.</sZ></fA14><fA20><s1>969-973</s1></fA20><fA21><s1>2008</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000196582860250</s5></fA43><fA44><s0>0000</s0><s1>© 2010 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>10-0384234</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 used spectra of hot stars from the RAVE Survey in order to investigate the visibility and properties of five diffuse interstellar bands previously reported in the literature. The RAVE spectroscopic survey for Galactic structure and kinematics records CCD spectra covering the 8400-8800 Å wavelength region at 7500 resolving power. The spectra are obtained with the UK Schmidt at the AAO, equipped with the 6dF multi-fiber positioner. The DIB at 8620.4 Å is by far the strongest and cleanest of all DIBs occurring within the RAVE wavelength range, with no interference by underlying absorption stellar lines in hot stars. It correlates so tightly with reddening that it turns out to be a reliable tool to measure it, following the relation EB-v = 2.72(±0.03) x EW (Å), valid throughout the general interstellar medium of our Galaxy. The presence of a DIB at 8648 Å is confirmed. Its intensity appears unrelated to reddening, in agreement with scanty and preliminary reports available in the literature, and its measurability is strongly compromised by severe blending with underlying stellar He I doublet at 8649 Å. The two weak DIBs at 8531 and 8572 Å do not appear real and should actually be blends of underlying stellar lines. The very weak DIB at 8439 Å cannot be resolved within the profile of the much stronger underlying hydrogen Paschen 18 stellar line.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Bande interstellaire diffuse</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Diffuse interstellar band</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Banda interestelar difusa</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Etoile chaude</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Hot star</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Estrella caliente</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Visibilité</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Visibility</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Structure galactique</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Galactic structure</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Cinématique</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Kinematics</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Raie absorption</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Absorption line</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Raya absorción</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Matière interstellaire</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Interstellar matter</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Galaxies</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Galaxies</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Intensité</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Intensity</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Intensidad</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Raie Paschen</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Paschen lines</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Voie lactée</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Milky Way</s0><s5>36</s5></fC03><fN21><s1>249</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 10-0384234 INIST</NO><ET>Diffuse interstellar bands in RAVE survey spectra</ET><AU>MUNARI (U.); TOMASELLA (L.); FIORUCCI (M.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); BEECHE (C.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.)</AU><AF>INAF Osservatorio Astronomico di Padova/Asiago/Italie (1 aut., 2 aut., 3 aut., 18 aut.); Observatoire de Strasbourg/Strasbourg/France (4 aut., 17 aut.); Rudolf Pierls Center for Theoretical Physics, University of Oxford/Royaume-Uni (5 aut.); Institute of Astronomy, School of Physics, University of Sydney/Australie (6 aut.); Astrophysikalisches Institut Potsdam/Potsdam/Allemagne (7 aut., 8 aut., 17 aut., 19 aut., 21 aut.); Macquarie University/Sidney/Australie (8 aut., 15 aut.); RSAA Mount Stromlo Observatory/Camberra/Australie (9 aut., 21 aut.); University of Central Lancashire/Preston/Royaume-Uni (10 aut.); Institute of Astronomy, University of Cambridge/Royaume-Uni (11 aut., 16 aut.); Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg/Heidelberg/Allemagne (12 aut.); University of Groningen/Groningen/Pays-Bas (13 aut.); University of Victoria/Victoria/Canada (14 aut.); e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University/Uxbridge/Royaume-Uni (16 aut.); Anglo Australian Observatory/Sydney/Australie (20 aut.); Johns Hopkins University/Baltimore, Maryland/Etats-Unis (22 aut.); Faculty of Mathematics and Physics, University of Ljubljana/Ljubljana/Slovénie (23 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2008; Vol. 488; No. 3; Pp. 969-973; Bibl. 1/4 p.</SO><LA>Anglais</LA><EA>We have used spectra of hot stars from the RAVE Survey in order to investigate the visibility and properties of five diffuse interstellar bands previously reported in the literature. The RAVE spectroscopic survey for Galactic structure and kinematics records CCD spectra covering the 8400-8800 Å wavelength region at 7500 resolving power. The spectra are obtained with the UK Schmidt at the AAO, equipped with the 6dF multi-fiber positioner. The DIB at 8620.4 Å is by far the strongest and cleanest of all DIBs occurring within the RAVE wavelength range, with no interference by underlying absorption stellar lines in hot stars. It correlates so tightly with reddening that it turns out to be a reliable tool to measure it, following the relation EB-v = 2.72(±0.03) x EW (Å), valid throughout the general interstellar medium of our Galaxy. The presence of a DIB at 8648 Å is confirmed. Its intensity appears unrelated to reddening, in agreement with scanty and preliminary reports available in the literature, and its measurability is strongly compromised by severe blending with underlying stellar He I doublet at 8649 Å. The two weak DIBs at 8531 and 8572 Å do not appear real and should actually be blends of underlying stellar lines. The very weak DIB at 8439 Å cannot be resolved within the profile of the much stronger underlying hydrogen Paschen 18 stellar line.</EA><CC>001E03</CC><FD>Bande interstellaire diffuse; Etoile chaude; Visibilité; Structure galactique; Cinématique; Raie absorption; Matière interstellaire; Galaxies; Intensité; Raie Paschen; Voie lactée</FD><ED>Diffuse interstellar band; Hot star; Visibility; Galactic structure; Kinematics; Absorption line; Interstellar matter; Galaxies; Intensity; Paschen lines; Milky Way</ED><SD>Banda interestelar difusa; Estrella caliente; Raya absorción; Intensidad</SD><LO>INIST-14176.354000196582860250</LO><ID>10-0384234</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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