Molecular gas associated with RCW 121 and RCW 122

ARNAL,E.M.; DURONEA.N.U.; TESTORI,J.C.

ASTRONOMY AND ASTROPHYSICS

Año: 2008 vol. 486 p. 807 - 818

0004-6361

Aims. We analyse the distribution of the molecular gas towards the region containing the open cluster Havlen-Moffat 1 (HM 1) the Wolf-Rayet stars WR 87, WR 89, and WR 91, and the star forming regions RCW 121 and RCW 122, with the aim of looking for a possible physical relationship among these objects. Methods: We used the carbon monoxide observations carried out at λ ~ 2.6 mm with the 4 m NANTEN radiotelescope; new flux density determinations derived from already existing radio continuum surveys at 2.417, 5, 8.35, and 14.35 GHz; continuum flux density determinations available in the literature; and the Midcourse Space Experiment (MSX) and the Improved Reprocessing of the IRAS Survey (IRIS) databases. Results: Adopting a distance of 5 kpc for RCW 121 and RCW 122, we found a giant molecular cloud (GMC) with a linear extent of ~100 × 20 pc to be associated with galactic star-forming regions. The total mass of this GMC is of the order of 1.2 × 106 solar masses and its mean radial velocity is about -15 km s-1. Within the GMC there are individual molecular gas concentrations, having total molecular masses in the range from 4.6 × 104 M_ȯ (RCW 122 C) to 2.2 × 105 M_ȯ (RCW 122). The CO profiles observed toward the peak of the molecular concentrations are broad, with typical full-width half-maximum around 6 to 7 km s-1, and show line asymmetries and/or double-peaked shape that change with the observed position within a given CO concentration. An analysis of the MSX and IRAS databases show that each CO concentration has a strong IR counterpart. The dust temperature of these concentrations range from 46 K (RCW 121) to 76 K (RCW 122 C). Their infrared luminosity are a few times 105 Lȯ. The new radio continuum flux density determinations are in good agreement with previous determinations at other frequencies, and confirm the thermal nature of RCW 121 and RCW 122. Based on the newly-determined 5 GHz flux density, we found that to power these Hii regions, each of them must harbour a sizable number of O type stars. Under the assumption that all the ionizing stars have a O7 V spectral type, at least ~8 and ~4 of these stars would be needed to ionize RCW 122 and RCW 121, respectively.