Evolution of massive protostars: the IRAS 18151–1208 region ^*,**

¹ Université Bordeaux 1, Laboratoire d'Astrophysique de Bordeaux, 2 rue de l'Observatoire, 33270 Bordeaux, France e-mail: [marseille;bontemps;herpin]@obs.u-bordeaux1.fr
² CNRS/INSU, UMR 5804, BP 89, 33270 Floirac, France
³ SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen, The Netherlands e-mail: vdtak@sron.nl
⁴ University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL, UK e-mail: Cormac.Purcell@manchester.ac.uk

Received: 18 March 2008
Accepted: 3 June 2008

Abstract

Context. The study of physical and chemical properties of massive protostars is critical for better understanding the evolutionary sequence that leads to the formation of high-mass stars.

Aims. IRAS 18151–1208 is a nearby massive region ( kpc, L ~ 2 10⁴ ) that splits into three cores: MM1, MM2, and MM3 (separated by 1´–2´). We aim at (1) studying the physical and chemical properties of the individual MM1, MM2, and MM3 cores; (2) deriving their evolutionary stages; (3) using these results to improve our view of the evolutionary sequence of massive cores.

Methods. The region was observed in the CS, C³⁴S, H₂CO, HCO⁺, H¹³CO⁺, and N₂H⁺ lines at mm wavelengths with the IRAM 30 m and Mopra telescopes. We use 1D and 2D modeling of the dust continuum to derive the density and temperature distributions, which are then used in the RATRAN code to model the lines and constrain the abundances of the observed species.

Results. All the lines were detected in MM1 and MM2. MM3 shows weaker emission, or is even undetected in HCO⁺ and all isotopic species. MM2 is driving a newly discovered CO outflow and hosts a mid-IR-quiet massive protostar. The abundance of CS is significantly greater in MM1 than in MM2, but smaller than in a reference massive protostar such as AFGL 2591. In contrast, the N₂H⁺ abundance decreases from MM2 to MM1, and is larger than in AFGL 2591.

Conclusions. Both MM1 and MM2 host an early-phase massive protostar, but MM2 (and mid-IR-quiet sources in general) is younger and dominated more by the host protostar than MM1 (mid-IR-bright). The MM3 core is probably in a pre-stellar phase. We find that the N₂H⁺/C³⁴S ratio varies systematically with age in the massive protostars for which the data are available. It can be used to identify young massive protostars.