Spectral line survey of the ultracompact HII region Monoceros R2^⋆

¹ Observatorio Astronómico Nacional (OAN), Apdo 112, 28800 Alcalá de Henares, Madrid, Spain
e-mail: davidginard@gmail.com
² Instituto de Radio Astronomía Milimétrica (IRAM), Avenida Divina Pastora 7, Local 20, 18012 Granada, Spain
³ Centro de Astrobiología, CSIC-INTA, Crta M-108, km. 4, 28850 Torrejón de Ardoz, Spain
⁴ LERMA, Observatoire de Paris, 61 Av. de l’Observatoire, 75014 Paris, France
⁵ I. Physikalisches Institut der Universität zu Köln, Zülpicher Straße 77, 50937 Köln, Germany
⁶ SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands
⁷ Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, 38406 Saint Martin d’ Hères, France
⁸ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
⁹ Université de Toulouse, UPS-OMP, IRAP, Toulouse, France
¹⁰ CNRS, IRAP, 9 Av. Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France

Received: 27 October 2011
Accepted: 15 March 2012

Abstract

Context. Ultracompact (UC) Hii regions constitute one of the earliest phases in the formation of a massive star and are characterized by extreme physical conditions (G₀ > 10⁵ Habing field and n > 10⁶ cm^-3). The UC Hii Mon R2 is the closest example and an excellent target to study the chemistry in these complex regions.

Aims. Our goal is to investigate the chemistry of the molecular gas around UC Hii Mon R2 and the variations caused by the different local physical conditions.

Methods. We carried out 3 mm and 1 mm spectral surveys using the IRAM 30-m telescope towards three positions that represent different physical environments in Mon R2: (i) the ionization front (IF) at (0″, 0″), and two peaks in the molecular cloud; (ii) molecular Peak 1 (hereafter MP1) at the offset (+15″,  −15″); and (iii) molecular Peak 2 (hereafter MP2) at the farther offset (0″, 40″). In addition, we carried out extensive modeling to explain the chemical differences between the three observed regions.

Results. We detected more than 30 different species (including isotopologues and deuterated compounds). In particular, we detected SO⁺ and C₄H confirming that ultraviolet (UV) radiation plays an important role in the molecular chemistry of this region. In agreement with this interpretation, we detected the typical photo-dissociation region (PDR) molecules CN, HCN, HCO, C₂H, and c-C₃H₂. There are chemical differences between the observed positions. While the IF and the MP1 have a chemistry similar to that found in high UV field and dense PDRs such as the Orion Bar, the MP2 is similar to lower UV/density PDRs such as the Horsehead nebula. Our chemical modeling supports this interpretation.

In addition to the PDR-like species, we detected complex molecules such as CH₃CN, H₂CO, HC₃N, CH₃OH, and CH₃C₂H that are not usually found in PDRs. The sulfur compounds CS, HCS⁺, C₂S, H₂CS, SO, and SO₂ and the deuterated species DCN and C₂D were also identified. The origin of these complex species requires further study. The observed deuteration fractionations, [DCN]/[HCN]  ~  0.03 and [C₂D]/[C₂H]  ~  0.05, are among the highest in warm regions.

Conclusions. Our results show that the high UV/dense PDRs have a different chemistry from the low UV case. Some abundance ratios such as [CO⁺]/[HCO⁺] or [HCO]/[HCO⁺] are good diagnostics for differentiating between them. In Mon R2, we have the two classes of PDRs, a high UV PDR towards the IF and the adjacent molecular bar, and a low-UV PDR, which extends towards the north-west following the border of the cloud.