Journal
ASTRONOMY & ASTROPHYSICS
Volume 487, Issue 1, Pages 253-264Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361:200809415
Keywords
stars : formation; stars : early-type; stars : pre-main sequence; ISM : clouds; ISM : kinematics and dynamics
Categories
Funding
- STFC [PP/E001149/1, ST/F002092/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F002092/1, PP/E001149/1] Funding Source: researchfish
Ask authors/readers for more resources
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 similar to 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 (CO)-C-13 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 (CO)-C-13 molecules and have a spatial resolution of similar to 20 ''-55 '', a sensitivity of T-A* similar or equal to 0.1 K and a velocity resolution of similar to 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 similar to 0.21 km s-1 and sensitivity T-A* similar or equal to 0.13-0.2 K, towards a further 403 RMS sources. Results. In this paper we present the results and analysis of the (CO)-C-13 spectra obtained towards 911 MYSO candidates. We detect (CO)-C-13 emission towards 780 RMS sources which corresponds to approximately 84% of those observed. A total of 2595 emission components are detected above 3 sigma level (typically T-A* = 0.3 K), with multiple components being observed towards the majority of these sources - 520 sources (similar to 56%) - with an average of similar to 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 (similar to 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 (similar to 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.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available