Measuring Star Formation Rate and Far-infrared Color in High-redshift Galaxies Using the CO(7-6) and [N II] 205 µm Lines
Inami, Hanae; Gao, Yu; Liu, Lijie; Díaz-Santos, Tanio; Lu, Nanyao; Schulz, Bernhard; Armus, Lee; Zhao, Yinghe; van der Werf, Paul P.; Sanders, David B.; Xu, C. Kevin; Privon, George C.; Charmandaris, Vassilis; Howell, Justin; Mazzarella, Joseph M.; Lord, Steven D.
United States, China, Chile, Greece, France, Germany, Netherlands
Abstract
To better characterize the global star formation activity in a galaxy, one needs to know not only the star formation rate (SFR) but also the rest-frame, far-infrared color (e.g., the 60-100 μm color, C(60/100)) of the dust emission. The latter probes the average intensity of the dust heating radiation field and scales statistically with the effective SFR surface density in star-forming galaxies including (ultra-)luminous infrared galaxies ((U)LIRGs). To this end, here we exploit a new spectroscopic approach involving only two emission lines: CO(7-6) at 372 μm and [N ii] at 205 μm([N ii]205μm). For local (U)LIRGs, the ratios of the CO(7-6) luminosity (LCO(7-6)) to the total infrared luminosity (LIR; 8-1000 μm) are fairly tightly distributed (to within ∼0.12 dex) and show little dependence on C(60/100). This makes LCO(7-6) a good SFR tracer, which is less contaminated by active galactic nuclei than LIR and may also be much less sensitive to metallicity than LCO(1-0). Furthermore, the logarithmic [N ii]205μm/CO(7-6) luminosity ratio depends fairly strongly (at a slope of ∼ -1.4) on C(60/100), with a modest scatter (∼0.23 dex). This makes it a useful estimator on C(60/100) with an implied uncertainty of ∼0.15 (or ≲4 K in the dust temperature (Tdust) in the case of a graybody emission with Tdust ≳ 30 K and a dust emissivity index β ≥ 1). Our locally calibrated SFR and C(60/100) estimators are shown to be consistent with the published data of (U)LIRGs of z up to ∼6.5.
Based on Herschel observations. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.