The RMS survey : 13CO observations of candidate massive YSOs in the northern Galactic plane
Identifieur interne : 003386 ( PascalFrancis/Corpus ); précédent : 003385; suivant : 003387The RMS survey : 13CO observations of candidate massive YSOs in the northern Galactic plane
Auteurs : J. S. Urquhan ; A. L. Busfield ; M. G. Hoare ; S. L. Lumsden ; R. D. Oudmaijer ; T. J. T. Moore ; A. G. Gibb ; C. R. Purcell ; M. G. Burton ; L. J. L. Marechal ; Z. Jiang ; M. WangSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2008.
Descripteurs français
- Pascal (Inist)
- Objet stellaire jeune, Plan galactique, Couleur, Galaxies, Source ponctuelle, Région H II compacte, Nébuleuse planétaire, Cinématique, Luminosité, Transition rotationnelle, Fréquence transition, Nuage moléculaire, Maser, Multiplicité, Courbe rotation, Vitesse radiale, Formation stellaire, Etoile premier type, Dynamique.
English descriptors
- KwdEn :
Abstract
Context. The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, high-resolution mid-infrared colour-selected sample of massive young stellar objects (MYSOs). We have identified ∼2000 MYSO candidates located within our Galaxy by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. The aim of our follow-up observations is to identify other objects with similar colours such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe) and distinguish between genuine MYSOs and nearby low-mass YSOs. Aims. A critical part of our follow-up programme is to conduct 13CO molecular line observations in order to determine kinematic distances to all of our MYSO candidates. These distances will be used in combination with far-IR and (sub)millimetre fluxes to determine bolometric luminosities which will allow us to identify and remove nearby low-mass YSOs. In addition these molecular line observations will help in identifying evolved stars which are weak CO emitters. Methods. We have used the 15 m James Clerk Maxwell Telescope (JCMT), the 13.7 m telescope of the Purple Mountain Observatory (PMO), the 20 m Onsala telescope and the 22 m Mopra telescope to conduct molecular line observations towards 508 MYSOs candidates located in the 1st and 2nd Quadrants. These observations have been made at the J = 1-0 (Mopra, Onsala and PMO) and J = 2-1 (JCMT) rotational transition frequency of 13CO molecules and have a spatial resolution of ∼20"-55", a sensitivity of T*A ≃ 0.1 K and a velocity resolution of ∼0.2 km s-1. We complement these targeted observations with 13CO spectra extracted from the Galactic Ring Survey (GRS), which have a velocity resolution of ∼0.21 km s-1 and sensitivity T*A ≃ 0.13-0.2 K, towards a further 403 RMS sources. Results. In this paper we present the results and analysis of the 13CO spectra obtained towards 911 MYSO candidates. We detect 13 CO emission towards 780 RMS sources which corresponds to approximately 84% of those observed. A total of 2595 emission components are detected above 3σ level (typically T*A > 0.3 K), with multiple components being observed towards the majority of these sources - 520 sources (∼56%) - with an average of ∼4 molecular clouds detected along each line of sight. These multiple emission features make it difficult to assign a unique kinematic velocity to many of our sample. We have used archival CS (J = 2-1) and maser velocities to resolve the component multiplicity towards 175 sources (∼20%) and have derived a criterion which is used to identify the most likely component for a further 191 multiple component sources. Combined with the single component detections we have obtained unambiguous kinematic velocities for 638 of the 780 MYSOs candidates towards which CO is detected (∼80% of the detections). The 141 sources for which we have not been able to determine the kinematic velocity will require additional line data. Using the rotation curve of Brand and Blitz (1993) and their radial velocities we calculate kinematic distances for all detected components.
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Pour connaître la documentation sur le format Inist Standard.
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Format Inist (serveur)
| NO : | PASCAL 08-0374788 INIST |
|---|---|
| ET : | The RMS survey : 13CO observations of candidate massive YSOs in the northern Galactic plane |
| AU : | URQUHAN (J. S.); BUSFIELD (A. L.); HOARE (M. G.); LUMSDEN (S. L.); OUDMAIJER (R. D.); MOORE (T. J. T.); GIBB (A. G.); PURCELL (C. R.); BURTON (M. G.); MARECHAL (L. J. L.); JIANG (Z.); WANG (M.) |
| AF : | School of Physics and Astrophysics, University of Leeds/Leeds, LS2 9JT/Royaume-Uni (1 aut., 2 aut., 3 aut., 4 aut., 5 aut.); Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf/Birkenhead, CH41 1LD/Royaume-Uni (6 aut.); Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road/Vancouver, BC, V6T 1Z1/Canada (7 aut.); School of Physics, University of New South Wales/Sydney, NSW 2052/Australie (8 aut., 9 aut.); Jodrell Bank Observatory, University of Manchester/Cheshire, SK11 9DL/Royaume-Uni (8 aut.); École Normale Supérieure, Département de Physique, 24 rue Lhomond/75005, Paris/France (10 aut.); Purple Mountain Observatory/Nanjing/Chine (11 aut., 12 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2008; Vol. 487; No. 1; Pp. 253-264; Bibl. 1/2 p. |
| LA : | Anglais |
| EA : | Context. The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, high-resolution mid-infrared colour-selected sample of massive young stellar objects (MYSOs). We have identified ∼2000 MYSO candidates located within our Galaxy by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. The aim of our follow-up observations is to identify other objects with similar colours such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe) and distinguish between genuine MYSOs and nearby low-mass YSOs. Aims. A critical part of our follow-up programme is to conduct 13CO molecular line observations in order to determine kinematic distances to all of our MYSO candidates. These distances will be used in combination with far-IR and (sub)millimetre fluxes to determine bolometric luminosities which will allow us to identify and remove nearby low-mass YSOs. In addition these molecular line observations will help in identifying evolved stars which are weak CO emitters. Methods. We have used the 15 m James Clerk Maxwell Telescope (JCMT), the 13.7 m telescope of the Purple Mountain Observatory (PMO), the 20 m Onsala telescope and the 22 m Mopra telescope to conduct molecular line observations towards 508 MYSOs candidates located in the 1st and 2nd Quadrants. These observations have been made at the J = 1-0 (Mopra, Onsala and PMO) and J = 2-1 (JCMT) rotational transition frequency of 13CO molecules and have a spatial resolution of ∼20"-55", a sensitivity of T*A ≃ 0.1 K and a velocity resolution of ∼0.2 km s-1. We complement these targeted observations with 13CO spectra extracted from the Galactic Ring Survey (GRS), which have a velocity resolution of ∼0.21 km s-1 and sensitivity T*A ≃ 0.13-0.2 K, towards a further 403 RMS sources. Results. In this paper we present the results and analysis of the 13CO spectra obtained towards 911 MYSO candidates. We detect 13 CO emission towards 780 RMS sources which corresponds to approximately 84% of those observed. A total of 2595 emission components are detected above 3σ level (typically T*A > 0.3 K), with multiple components being observed towards the majority of these sources - 520 sources (∼56%) - with an average of ∼4 molecular clouds detected along each line of sight. These multiple emission features make it difficult to assign a unique kinematic velocity to many of our sample. We have used archival CS (J = 2-1) and maser velocities to resolve the component multiplicity towards 175 sources (∼20%) and have derived a criterion which is used to identify the most likely component for a further 191 multiple component sources. Combined with the single component detections we have obtained unambiguous kinematic velocities for 638 of the 780 MYSOs candidates towards which CO is detected (∼80% of the detections). The 141 sources for which we have not been able to determine the kinematic velocity will require additional line data. Using the rotation curve of Brand and Blitz (1993) and their radial velocities we calculate kinematic distances for all detected components. |
| CC : | 001E03 |
| FD : | Objet stellaire jeune; Plan galactique; Couleur; Galaxies; Source ponctuelle; Région H II compacte; Nébuleuse planétaire; Cinématique; Luminosité; Transition rotationnelle; Fréquence transition; Nuage moléculaire; Maser; Multiplicité; Courbe rotation; Vitesse radiale; Formation stellaire; Etoile premier type; Dynamique |
| ED : | Young stellar object; Galactic planes; Color; Galaxies; Point sources; Compact H II region; Planetary nebulae; Kinematics; Luminosity; Rotational transition; Transition frequency; Molecular clouds; Masers; Multiplicity; Rotation curve; Radial velocity; Star formation; Early type stars; Dynamics |
| SD : | Objeto estelar joven; Región H II compacta; Transición rotacional; Frecuencia transición; Curva rotación |
| LO : | INIST-14176.354000197356960270 |
| ID : | 08-0374788 |
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Moore</name><affiliation><inist:fA14 i1="02"><s1>Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf</s1><s2>Birkenhead, CH41 1LD</s2><s3>GBR</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibb, A G" sort="Gibb, A G" uniqKey="Gibb A" first="A. G." last="Gibb">A. G. Gibb</name><affiliation><inist:fA14 i1="03"><s1>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road</s1><s2>Vancouver, BC, V6T 1Z1</s2><s3>CAN</s3><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Purcell, C R" sort="Purcell, C R" uniqKey="Purcell C" first="C. R." last="Purcell">C. R. 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Marechal</name><affiliation><inist:fA14 i1="06"><s1>École Normale Supérieure, Département de Physique, 24 rue Lhomond</s1><s2>75005, Paris</s2><s3>FRA</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jiang, Z" sort="Jiang, Z" uniqKey="Jiang Z" first="Z." last="Jiang">Z. Jiang</name><affiliation><inist:fA14 i1="07"><s1>Purple Mountain Observatory</s1><s2>Nanjing</s2><s3>CHN</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wang, M" sort="Wang, M" uniqKey="Wang M" first="M." last="Wang">M. Wang</name><affiliation><inist:fA14 i1="07"><s1>Purple Mountain Observatory</s1><s2>Nanjing</s2><s3>CHN</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">08-0374788</idno><date when="2008">2008</date><idno type="stanalyst">PASCAL 08-0374788 INIST</idno><idno type="RBID">Pascal:08-0374788</idno><idno type="wicri:Area/PascalFrancis/Corpus">003386</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">The RMS survey : <sup>13</sup>CO observations of candidate massive YSOs in the northern Galactic plane</title><author><name sortKey="Urquhan, J S" sort="Urquhan, J S" uniqKey="Urquhan J" first="J. S." last="Urquhan">J. S. Urquhan</name><affiliation><inist:fA14 i1="01"><s1>School of Physics and Astrophysics, University of Leeds</s1><s2>Leeds, LS2 9JT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Busfield, A L" sort="Busfield, A L" uniqKey="Busfield A" first="A. L." last="Busfield">A. L. Busfield</name><affiliation><inist:fA14 i1="01"><s1>School of Physics and Astrophysics, University of Leeds</s1><s2>Leeds, LS2 9JT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Hoare, M G" sort="Hoare, M G" uniqKey="Hoare M" first="M. G." last="Hoare">M. G. Hoare</name><affiliation><inist:fA14 i1="01"><s1>School of Physics and Astrophysics, University of Leeds</s1><s2>Leeds, LS2 9JT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lumsden, S L" sort="Lumsden, S L" uniqKey="Lumsden S" first="S. L." last="Lumsden">S. L. Lumsden</name><affiliation><inist:fA14 i1="01"><s1>School of Physics and Astrophysics, University of Leeds</s1><s2>Leeds, LS2 9JT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Oudmaijer, R D" sort="Oudmaijer, R D" uniqKey="Oudmaijer R" first="R. D." last="Oudmaijer">R. D. Oudmaijer</name><affiliation><inist:fA14 i1="01"><s1>School of Physics and Astrophysics, University of Leeds</s1><s2>Leeds, LS2 9JT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Moore, T J T" sort="Moore, T J T" uniqKey="Moore T" first="T. J. T." last="Moore">T. J. T. Moore</name><affiliation><inist:fA14 i1="02"><s1>Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf</s1><s2>Birkenhead, CH41 1LD</s2><s3>GBR</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibb, A G" sort="Gibb, A G" uniqKey="Gibb A" first="A. G." last="Gibb">A. G. Gibb</name><affiliation><inist:fA14 i1="03"><s1>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road</s1><s2>Vancouver, BC, V6T 1Z1</s2><s3>CAN</s3><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Purcell, C R" sort="Purcell, C R" uniqKey="Purcell C" first="C. R." last="Purcell">C. R. Purcell</name><affiliation><inist:fA14 i1="04"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Jodrell Bank Observatory, University of Manchester</s1><s2>Cheshire, SK11 9DL</s2><s3>GBR</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Burton, M G" sort="Burton, M G" uniqKey="Burton M" first="M. G." last="Burton">M. G. Burton</name><affiliation><inist:fA14 i1="04"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Marechal, L J L" sort="Marechal, L J L" uniqKey="Marechal L" first="L. J. L." last="Marechal">L. J. L. Marechal</name><affiliation><inist:fA14 i1="06"><s1>École Normale Supérieure, Département de Physique, 24 rue Lhomond</s1><s2>75005, Paris</s2><s3>FRA</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Jiang, Z" sort="Jiang, Z" uniqKey="Jiang Z" first="Z." last="Jiang">Z. Jiang</name><affiliation><inist:fA14 i1="07"><s1>Purple Mountain Observatory</s1><s2>Nanjing</s2><s3>CHN</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Wang, M" sort="Wang, M" uniqKey="Wang M" first="M." last="Wang">M. Wang</name><affiliation><inist:fA14 i1="07"><s1>Purple Mountain Observatory</s1><s2>Nanjing</s2><s3>CHN</s3><sZ>11 aut.</sZ><sZ>12 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>Color</term><term>Compact H II region</term><term>Dynamics</term><term>Early type stars</term><term>Galactic planes</term><term>Galaxies</term><term>Kinematics</term><term>Luminosity</term><term>Masers</term><term>Molecular clouds</term><term>Multiplicity</term><term>Planetary nebulae</term><term>Point sources</term><term>Radial velocity</term><term>Rotation curve</term><term>Rotational transition</term><term>Star formation</term><term>Transition frequency</term><term>Young stellar object</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Objet stellaire jeune</term><term>Plan galactique</term><term>Couleur</term><term>Galaxies</term><term>Source ponctuelle</term><term>Région H II compacte</term><term>Nébuleuse planétaire</term><term>Cinématique</term><term>Luminosité</term><term>Transition rotationnelle</term><term>Fréquence transition</term><term>Nuage moléculaire</term><term>Maser</term><term>Multiplicité</term><term>Courbe rotation</term><term>Vitesse radiale</term><term>Formation stellaire</term><term>Etoile premier type</term><term>Dynamique</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, high-resolution mid-infrared colour-selected sample of massive young stellar objects (MYSOs). We have identified ∼2000 MYSO candidates located within our Galaxy by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. The aim of our follow-up observations is to identify other objects with similar colours such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe) and distinguish between genuine MYSOs and nearby low-mass YSOs. Aims. A critical part of our follow-up programme is to conduct <sup>13</sup>CO molecular line observations in order to determine kinematic distances to all of our MYSO candidates. These distances will be used in combination with far-IR and (sub)millimetre fluxes to determine bolometric luminosities which will allow us to identify and remove nearby low-mass YSOs. In addition these molecular line observations will help in identifying evolved stars which are weak CO emitters. Methods. We have used the 15 m James Clerk Maxwell Telescope (JCMT), the 13.7 m telescope of the Purple Mountain Observatory (PMO), the 20 m Onsala telescope and the 22 m Mopra telescope to conduct molecular line observations towards 508 MYSOs candidates located in the 1st and 2nd Quadrants. These observations have been made at the J = 1-0 (Mopra, Onsala and PMO) and J = 2-1 (JCMT) rotational transition frequency of <sup>13</sup>CO molecules and have a spatial resolution of ∼20"-55", a sensitivity of T*<sub>A</sub> ≃ 0.1 K and a velocity resolution of ∼0.2 km s<sup>-1</sup>. We complement these targeted observations with <sup>13</sup>CO spectra extracted from the Galactic Ring Survey (GRS), which have a velocity resolution of ∼0.21 km s<sup>-1</sup> and sensitivity T*<sub>A</sub> ≃ 0.13-0.2 K, towards a further 403 RMS sources. Results. In this paper we present the results and analysis of the <sup>13</sup>CO spectra obtained towards 911 MYSO candidates. We detect <sup>13</sup> CO emission towards 780 RMS sources which corresponds to approximately 84% of those observed. A total of 2595 emission components are detected above 3σ level (typically T*<sub>A</sub> > 0.3 K), with multiple components being observed towards the majority of these sources - 520 sources (∼56%) - with an average of ∼4 molecular clouds detected along each line of sight. These multiple emission features make it difficult to assign a unique kinematic velocity to many of our sample. We have used archival CS (J = 2-1) and maser velocities to resolve the component multiplicity towards 175 sources (∼20%) and have derived a criterion which is used to identify the most likely component for a further 191 multiple component sources. Combined with the single component detections we have obtained unambiguous kinematic velocities for 638 of the 780 MYSOs candidates towards which CO is detected (∼80% of the detections). The 141 sources for which we have not been able to determine the kinematic velocity will require additional line data. Using the rotation curve of Brand and Blitz (1993) and their radial velocities we calculate kinematic distances for all detected components.</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>487</s2></fA05><fA06><s2>1</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The RMS survey : <sup>13</sup>CO observations of candidate massive YSOs in the northern Galactic plane</s1></fA08><fA11 i1="01" i2="1"><s1>URQUHAN (J. S.)</s1></fA11><fA11 i1="02" i2="1"><s1>BUSFIELD (A. L.)</s1></fA11><fA11 i1="03" i2="1"><s1>HOARE (M. G.)</s1></fA11><fA11 i1="04" i2="1"><s1>LUMSDEN (S. L.)</s1></fA11><fA11 i1="05" i2="1"><s1>OUDMAIJER (R. D.)</s1></fA11><fA11 i1="06" i2="1"><s1>MOORE (T. J. T.)</s1></fA11><fA11 i1="07" i2="1"><s1>GIBB (A. G.)</s1></fA11><fA11 i1="08" i2="1"><s1>PURCELL (C. R.)</s1></fA11><fA11 i1="09" i2="1"><s1>BURTON (M. G.)</s1></fA11><fA11 i1="10" i2="1"><s1>MARECHAL (L. J. L.)</s1></fA11><fA11 i1="11" i2="1"><s1>JIANG (Z.)</s1></fA11><fA11 i1="12" i2="1"><s1>WANG (M.)</s1></fA11><fA14 i1="01"><s1>School of Physics and Astrophysics, University of Leeds</s1><s2>Leeds, LS2 9JT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>3 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></fA14><fA14 i1="02"><s1>Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf</s1><s2>Birkenhead, CH41 1LD</s2><s3>GBR</s3><sZ>6 aut.</sZ></fA14><fA14 i1="03"><s1>Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road</s1><s2>Vancouver, BC, V6T 1Z1</s2><s3>CAN</s3><sZ>7 aut.</sZ></fA14><fA14 i1="04"><s1>School of Physics, University of New South Wales</s1><s2>Sydney, NSW 2052</s2><s3>AUS</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="05"><s1>Jodrell Bank Observatory, University of Manchester</s1><s2>Cheshire, SK11 9DL</s2><s3>GBR</s3><sZ>8 aut.</sZ></fA14><fA14 i1="06"><s1>École Normale Supérieure, Département de Physique, 24 rue Lhomond</s1><s2>75005, Paris</s2><s3>FRA</s3><sZ>10 aut.</sZ></fA14><fA14 i1="07"><s1>Purple Mountain Observatory</s1><s2>Nanjing</s2><s3>CHN</s3><sZ>11 aut.</sZ><sZ>12 aut.</sZ></fA14><fA20><s1>253-264</s1></fA20><fA21><s1>2008</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000197356960270</s5></fA43><fA44><s0>0000</s0><s1>© 2008 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>08-0374788</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>Context. The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, high-resolution mid-infrared colour-selected sample of massive young stellar objects (MYSOs). We have identified ∼2000 MYSO candidates located within our Galaxy by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. The aim of our follow-up observations is to identify other objects with similar colours such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe) and distinguish between genuine MYSOs and nearby low-mass YSOs. Aims. A critical part of our follow-up programme is to conduct <sup>13</sup>CO molecular line observations in order to determine kinematic distances to all of our MYSO candidates. These distances will be used in combination with far-IR and (sub)millimetre fluxes to determine bolometric luminosities which will allow us to identify and remove nearby low-mass YSOs. In addition these molecular line observations will help in identifying evolved stars which are weak CO emitters. Methods. We have used the 15 m James Clerk Maxwell Telescope (JCMT), the 13.7 m telescope of the Purple Mountain Observatory (PMO), the 20 m Onsala telescope and the 22 m Mopra telescope to conduct molecular line observations towards 508 MYSOs candidates located in the 1st and 2nd Quadrants. These observations have been made at the J = 1-0 (Mopra, Onsala and PMO) and J = 2-1 (JCMT) rotational transition frequency of <sup>13</sup>CO molecules and have a spatial resolution of ∼20"-55", a sensitivity of T*<sub>A</sub> ≃ 0.1 K and a velocity resolution of ∼0.2 km s<sup>-1</sup>. We complement these targeted observations with <sup>13</sup>CO spectra extracted from the Galactic Ring Survey (GRS), which have a velocity resolution of ∼0.21 km s<sup>-1</sup> and sensitivity T*<sub>A</sub> ≃ 0.13-0.2 K, towards a further 403 RMS sources. Results. In this paper we present the results and analysis of the <sup>13</sup>CO spectra obtained towards 911 MYSO candidates. We detect <sup>13</sup> CO emission towards 780 RMS sources which corresponds to approximately 84% of those observed. A total of 2595 emission components are detected above 3σ level (typically T*<sub>A</sub> > 0.3 K), with multiple components being observed towards the majority of these sources - 520 sources (∼56%) - with an average of ∼4 molecular clouds detected along each line of sight. These multiple emission features make it difficult to assign a unique kinematic velocity to many of our sample. We have used archival CS (J = 2-1) and maser velocities to resolve the component multiplicity towards 175 sources (∼20%) and have derived a criterion which is used to identify the most likely component for a further 191 multiple component sources. Combined with the single component detections we have obtained unambiguous kinematic velocities for 638 of the 780 MYSOs candidates towards which CO is detected (∼80% of the detections). The 141 sources for which we have not been able to determine the kinematic velocity will require additional line data. Using the rotation curve of Brand and Blitz (1993) and their radial velocities we calculate kinematic distances for all detected components.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Objet stellaire jeune</s0><s2>NO</s2><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Young stellar object</s0><s2>NO</s2><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Objeto estelar joven</s0><s2>NO</s2><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Plan galactique</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Galactic planes</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Couleur</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Color</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Galaxies</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Galaxies</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Source ponctuelle</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Point sources</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Région H II compacte</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Compact H II region</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Región H II compacta</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Nébuleuse planétaire</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Planetary nebulae</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Cinématique</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Kinematics</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Luminosité</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Luminosity</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Transition rotationnelle</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Rotational transition</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Transición rotacional</s0><s5>35</s5></fC03><fC03 i1="11" i2="X" l="FRE"><s0>Fréquence transition</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="ENG"><s0>Transition frequency</s0><s5>36</s5></fC03><fC03 i1="11" i2="X" l="SPA"><s0>Frecuencia transición</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Nuage moléculaire</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Molecular clouds</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Maser</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Masers</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Multiplicité</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>Multiplicity</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Courbe rotation</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Rotation curve</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Curva rotación</s0><s5>40</s5></fC03><fC03 i1="16" i2="3" l="FRE"><s0>Vitesse radiale</s0><s5>41</s5></fC03><fC03 i1="16" i2="3" l="ENG"><s0>Radial velocity</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>Star formation</s0><s5>42</s5></fC03><fC03 i1="18" i2="3" l="FRE"><s0>Etoile premier type</s0><s5>43</s5></fC03><fC03 i1="18" i2="3" l="ENG"><s0>Early type stars</s0><s5>43</s5></fC03><fC03 i1="19" i2="3" l="FRE"><s0>Dynamique</s0><s5>44</s5></fC03><fC03 i1="19" i2="3" l="ENG"><s0>Dynamics</s0><s5>44</s5></fC03><fN21><s1>238</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 08-0374788 INIST</NO><ET>The RMS survey : <sup>13</sup>CO observations of candidate massive YSOs in the northern Galactic plane</ET><AU>URQUHAN (J. S.); BUSFIELD (A. L.); HOARE (M. G.); LUMSDEN (S. L.); OUDMAIJER (R. D.); MOORE (T. J. T.); GIBB (A. G.); PURCELL (C. R.); BURTON (M. G.); MARECHAL (L. J. L.); JIANG (Z.); WANG (M.)</AU><AF>School of Physics and Astrophysics, University of Leeds/Leeds, LS2 9JT/Royaume-Uni (1 aut., 2 aut., 3 aut., 4 aut., 5 aut.); Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf/Birkenhead, CH41 1LD/Royaume-Uni (6 aut.); Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road/Vancouver, BC, V6T 1Z1/Canada (7 aut.); School of Physics, University of New South Wales/Sydney, NSW 2052/Australie (8 aut., 9 aut.); Jodrell Bank Observatory, University of Manchester/Cheshire, SK11 9DL/Royaume-Uni (8 aut.); École Normale Supérieure, Département de Physique, 24 rue Lhomond/75005, Paris/France (10 aut.); Purple Mountain Observatory/Nanjing/Chine (11 aut., 12 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2008; Vol. 487; No. 1; Pp. 253-264; Bibl. 1/2 p.</SO><LA>Anglais</LA><EA>Context. The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, high-resolution mid-infrared colour-selected sample of massive young stellar objects (MYSOs). We have identified ∼2000 MYSO candidates located within our Galaxy by comparing the colours of MSX and 2MASS point sources to those of known MYSOs. The aim of our follow-up observations is to identify other objects with similar colours such as ultra compact (UC) HII regions, evolved stars and planetary nebulae (PNe) and distinguish between genuine MYSOs and nearby low-mass YSOs. Aims. A critical part of our follow-up programme is to conduct <sup>13</sup>CO molecular line observations in order to determine kinematic distances to all of our MYSO candidates. These distances will be used in combination with far-IR and (sub)millimetre fluxes to determine bolometric luminosities which will allow us to identify and remove nearby low-mass YSOs. In addition these molecular line observations will help in identifying evolved stars which are weak CO emitters. Methods. We have used the 15 m James Clerk Maxwell Telescope (JCMT), the 13.7 m telescope of the Purple Mountain Observatory (PMO), the 20 m Onsala telescope and the 22 m Mopra telescope to conduct molecular line observations towards 508 MYSOs candidates located in the 1st and 2nd Quadrants. These observations have been made at the J = 1-0 (Mopra, Onsala and PMO) and J = 2-1 (JCMT) rotational transition frequency of <sup>13</sup>CO molecules and have a spatial resolution of ∼20"-55", a sensitivity of T*<sub>A</sub> ≃ 0.1 K and a velocity resolution of ∼0.2 km s<sup>-1</sup>. We complement these targeted observations with <sup>13</sup>CO spectra extracted from the Galactic Ring Survey (GRS), which have a velocity resolution of ∼0.21 km s<sup>-1</sup> and sensitivity T*<sub>A</sub> ≃ 0.13-0.2 K, towards a further 403 RMS sources. Results. In this paper we present the results and analysis of the <sup>13</sup>CO spectra obtained towards 911 MYSO candidates. We detect <sup>13</sup> CO emission towards 780 RMS sources which corresponds to approximately 84% of those observed. A total of 2595 emission components are detected above 3σ level (typically T*<sub>A</sub> > 0.3 K), with multiple components being observed towards the majority of these sources - 520 sources (∼56%) - with an average of ∼4 molecular clouds detected along each line of sight. These multiple emission features make it difficult to assign a unique kinematic velocity to many of our sample. We have used archival CS (J = 2-1) and maser velocities to resolve the component multiplicity towards 175 sources (∼20%) and have derived a criterion which is used to identify the most likely component for a further 191 multiple component sources. Combined with the single component detections we have obtained unambiguous kinematic velocities for 638 of the 780 MYSOs candidates towards which CO is detected (∼80% of the detections). The 141 sources for which we have not been able to determine the kinematic velocity will require additional line data. Using the rotation curve of Brand and Blitz (1993) and their radial velocities we calculate kinematic distances for all detected components.</EA><CC>001E03</CC><FD>Objet stellaire jeune; Plan galactique; Couleur; Galaxies; Source ponctuelle; Région H II compacte; Nébuleuse planétaire; Cinématique; Luminosité; Transition rotationnelle; Fréquence transition; Nuage moléculaire; Maser; Multiplicité; Courbe rotation; Vitesse radiale; Formation stellaire; Etoile premier type; Dynamique</FD><ED>Young stellar object; Galactic planes; Color; Galaxies; Point sources; Compact H II region; Planetary nebulae; Kinematics; Luminosity; Rotational transition; Transition frequency; Molecular clouds; Masers; Multiplicity; Rotation curve; Radial velocity; Star formation; Early type stars; Dynamics</ED><SD>Objeto estelar joven; Región H II compacta; Transición rotacional; Frecuencia transición; Curva rotación</SD><LO>INIST-14176.354000197356960270</LO><ID>08-0374788</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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