Spectrally resolved C II emission in M 33 (HerM33es)

Physical conditions and kinematics around BCLMP 691^⋆

¹ Univ. Bordeaux, Laboratoire d’Astrophysique de Bordeaux, 33270 Floirac, France
e-mail: braine@obs.u-bordeaux1.fr
² CNRS, LAB, UMR 5804, 33270 Floirac, France
³ IRAM, 300 rue de la Piscine, 38406 St Martin d’Hères, France
⁴ Instituto Radioastronomia Milimetrica (IRAM), Av. Divina Pastora 7, Nucleo Central, 18012 Granada, Spain
⁵ Leiden Observatory, Leiden University, PO Box 9513, NL 2300 RA Leiden, The Netherlands
⁶ SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen, The Netherlands
⁷ Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India
⁸ Laboratoire d’Astrophysique de Marseille – LAM, Université d’Aix-Marseille & CNRS UMR 7326, 38 rue F. Joliot-Curie, 13388 Marseille Cedex 13, France
⁹ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
¹⁰ Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany
¹¹ Astron. Dept., King Abdulaziz University, PO Box 80203, Jeddah, Saudi Arabia

Received: 5 April 2012
Accepted: 15 June 2012

Abstract

This work presents high spectral resolution observations of the [C ii] line at 158 μm, one of the major cooling lines of the interstellar medium, taken with the HIFI heterodyne spectrometer on the Herschel satellite. In BCLMP 691, an H ii region far north (3.3 kpc) in the disk of M 33, the [C ii] and CO line profiles show similar velocities within 0.5 km   s^-1, while the H i line velocities are systematically shifted towards lower rotation velocities by ~5 km   s^-1. Observed at the same 12′′angular resolution, the [C ii] lines are broader than those of CO by about 50% but narrower than the H i lines. The [C ii] line intensities also follow those of CO much better than those of H i. A weak shoulder on the [C ii] line suggests a marginal detection of the [¹³C ii] line, insufficient to constrain the [C ii] optical depth. The velocity coincidence of the CO and [C ii] lines and the morphology at optical/UV wavelengths indicate that the emission is coming from a molecular cloud behind the H ii region. The relative strength of [C ii] with respect to the FIR continuum emission is comparable to that observed in the Magellanic Clouds on similar linear scales but the CO emission relative to [C ii] is stronger in M 33. The [C ii] line to far-infrared continuum ratio suggests a photoelectric heating efficiency of 1.1%. The data, together with published models indicate a UV field G₀ ~ 100 in units of the solar neighborhood value, a gas density n_H~1000 cm^-3, and a gas temperature T ~ 200 K. Adopting these values, we estimate the C⁺ column density to be N_C ⁺  ≈ 1.3×10¹⁷cm^-2. The [C ii] emission comes predominantly from the warm neutral region between the H ii region and the cool molecular cloud behind it. From published abundances, the inferred C⁺ column corresponds to a hydrogen column density of N_H~2×10²¹cm^-2. The CO observations suggest thatN_H=2N_H2~3.2×10²¹cm^-2 and 21 cm measurements, also at 12′′resolution, yield N_H   i≈1.2×10²¹cm^-2 within the [C ii] velocity range. Thus, some H₂ not detected in CO must be present, in agreement with earlier findings based on the SPIRE 250−500 μm emission.