The anatomy of the Orion B Giant Molecular Cloud: A local template for studies of nearby galaxies (1611.04037v1)

Abstract: We aim to develop the Orion B Giant Molecular Cloud (GMC) as a local template for interpreting extra-galactic molecular line observations. We use the wide-band receiver at the IRAM-30m to spatially and spectrally resolve the Orion B GMC. The observations cover almost 1 square degree at 26" resolution with a bandwidth of 32 GHz from 84 to 116 GHz in only two tunings. Among the mapped spectral lines are the 12CO, 13CO, C18O, C17O, HCN, HNC, 12CN, CCH, HCO+, N2H+ (1-0), and 12CS, 32SO, SiO, c-C3H2, CH3OH (2-1) transitions. We introduce the molecular anatomy of the Orion B GMC, including relations between line intensities and gas column density or far-UV radiation fields, and correlations between selected line and line ratios. We also obtain a dust-traced gas mass that is less than about one third the CO-traced mass, using the standard Xco conversion factor. The presence of overluminous CO can be traced back to the dependence of the CO intensity on UV illumination. In fact, while most lines show some dependence on the UV radiation field, CN and CCH are the most sensitive. Moreover dense cloud cores are almost exclusively traced by N2H+. Other traditional high density tracers, such as HCN (1-0), are also easily detected in extended translucent regions at a typical density of about 500 H2 cm-3. In general, we find no straightforward relation between line critical density and the fraction of the line luminosity coming from dense gas regions. Our initial findings demonstrate that the relations between line (ratio) intensities and environment in GMCs are more complicated than often assumed. Sensitivity (i.e., the molecular column density), excitation, and above all chemistry contribute to the observed line intensity distributions. They must be considered together when developing the next generation of extra-galactic molecular line diagnostics of mass, density, temperature and radiation field.

The Molecular Anatomy of Orion B: Implications for Extragalactic Studies

The paper presents a comprehensive analysis of Orion B, a Giant Molecular Cloud (GMC), aiming to establish it as a template for interpreting extragalactic molecular line observations. The focus is on understanding the relations between molecular line intensities, gas column density, far-UV radiation fields, and the subsequent implications for measuring gas mass, density, temperature, and radiation exposure in nearby galaxies.

Observational Methodology

Using the IRAM-30m telescope, the paper maps almost 1 square degree of Orion B with a 26" resolution. Observations covered a bandwidth from 84 to 116 GHz with two tunings, capturing lines such as ^{12}CO, ^{13}CO, C^{18}O, HCN, and HCO^{+}. The paper outlines that, under typical galactic conditions akin to Orion B, only the brightest lines, such as ^{12}CO and ^{13}CO, would readily be detected by single-dish telescopes due to their high intensity. Fainter lines require significantly improved sensitivity to be observed in extragalactic settings.

Key Findings

1. Mass Estimations:
   • The CO-traced mass is about three times higher than the dust-traced mass due to the intense UV illumination in Orion B. This UV exposure causes CO to be over-luminous, highlighting discrepancies when using the CO-to-H_2 conversion factor (X-factor) under non-standard conditions.
   • Virial mass calculations suggest values between the CO and dust-traced masses, indicating that the standard mass determination methods need adjustments considering factors like UV illumination and molecular line optical depth.
2. Line Emission and Density Correlations:
   • Lines like ^{12}CO, often assumed to trace molecular mass, show saturation effects in dense regions, while rarer isotopologues like C^{18}O correlate more directly with visual extinction due to their reduced optical depths.
   • Traditional dense gas tracers like HCO^{+} and HCN, while having high critical densities, emit significantly from lower-density regions. This emission is linked to a different radiative regime that allows their detection in less dense environments, challenging their reliability as high-density tracers without additional context.
3. Chemical and Radiative Influence:
   • CN and C_{2} emerge as sensitive tracers to UV radiation fields, showing high intensity where the UV field is strong. In contrast, N_{2}H^{+} remains a robust tracer for dense regions due to its chemical pathway and reduced presence in UV-illuminated environments.
   • The paper underscores the importance of chemical knowledge in interpreting line ratios, showing how environmental factors distinctly influence molecular abundance and line emitivity.
4. Line Ratio Analysis:
   • By comparing with extragalactic data, the paper finds that line ratios like HCN/HCO^{+} should be interpreted carefully, as factors like UV illumination and chemical pumping can bias their efficacy as tracers of star formation efficiency.
   • Ratios involving C_{2} with traditional tracers like ^{13}CO are promising indicators of UV exposure and star-forming regions.

Implications for Extragalactic Studies

The results stress the necessity of detailed calibration studies of Galactic GMCs before translating findings to external galaxies. Understanding the environmental and chemical context of molecular line emission is crucial for developing reliable gas mass and star formation rate tracers. The paper suggests that factors like UV radiation must be accounted for to avoid biases in mass determination via CO luminosity, particularly in actively star-forming regions of galaxies.

Future directions should include expanding Orion B's mapping to encompass higher-density regions and refining molecular excitation models to include non-standard conditions found in diverse galactic environments. The insights gained underline the complexity of molecular clouds' internal structure and the vital role of such detailed studies in enhancing the precision of extragalactic molecular diagnostics.