The RMS survey

¹³CO observations of candidate massive YSOs in the southern Galactic plane

¹ School of Physics and Astrophysics, University of Leeds, Leeds LS2 9JT, UK e-mail: jsu@ast.leeds.ac.uk
² Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK
³ Department of Physics and Astronomy, University of British Columbia, 6224 Aricultural Road, Vancouver, BC, V6T 1Z1, Canada
⁴ School of Physics and Astronomy, University of New South Wales, Sydney, NSW 2052, Australia
⁵ Jodrell Bank Observatory, University of Manchester, Cheshire SK11 9DL, UK
⁶ École Normale Supérieure, Département de Physique, 24 rue Lhomond, 75005 Paris, France

Received: 6 June 2007
Accepted: 18 August 2007

Abstract

Context.The Red MSX Source (RMS) survey is an ongoing multi-wavelength observational programme designed to return a large, well-selected sample of massive young stellar objects (MYSOs). We have identified ~2000 MYSOs 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 contaminating objects 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 22 m Mopra telescope, the 15 m JCMT and the 20 m Onsala telescope to conduct molecular line observations towards 854 MYSOs candidates located in the 3rd and 4th quadrants. These observations have been made at the J = 1–0 (Mopra and Onsala) and J = 2–1 (JCMT) rotational transition frequency of ¹³CO molecules and have a spatial resolution of ~20´´-40´´, a sensitivity of   0.1 K and a velocity resolution of ~0.2 km s^-1.

Results.We detect ¹³CO emission towards a total of 752 of the 854 RMS sources observed (~88%). In total 2132 emission components are detected above 3σ level (typically  K). Multiple emission profiles are observed towards the majority of these sources – 461 sources (~60%) – with an average of ~4 molecular clouds detected along the line of sight. These multiple emission features make it difficult to assign a kinematic velocity to many of our sample. We have used archival CS (J = 2–1) and maser velocities to resolve the component multiplicity towards 82 sources and have derived a criterion which is used to identify the most likely component for a further 218 multiple component sources. Combined with the single component detections we have obtained unambiguous kinematic velocities towards 591 sources (~80% of the detections). The 161 sources for which we have not been able to determine the kinematic velocity will require additional line data. Using the rotation curve of Brand & Blitz (1993) and their radial velocities we calculate kinematic distances for all components detected.