PAMS: The Perseus Arm Molecular Survey–I. Survey description and first results

The external environments surrounding molecular clouds vary widely across galaxies such as the Milky Way, and statistical samples of clouds are required to understand them. We present the Perseus Arm Molecular Survey (PAMS), a James Clerk Maxwell Telescope (JCMT) survey combining new and archival data of molecular-cloud complexes in the outer Perseus spiral arm in ¹²CO, ¹³CO, and C¹⁸O (J = 3–2). With a survey area of ∼8 deg², PAMS covers well-known complexes such as W3, W5, and NGC 7538 with two fields at l ≈ 110^◦ and l ≈ 135^◦. PAMS has an effective resolution of 17 arcsec, and rms sensitivity of T_mb = 0.7–1.0 K in 0.3 km s⁻¹ channels. Here we present a first look at the data, and compare the PAMS regions in the Outer Galaxy with Inner Galaxy regions from the CO Heterodyne Inner Milky Way Plane Survey (CHIMPS). By comparing the various CO data with maps of H₂ column density from Herschel, we calculate representative values for the CO-to-H₂ column-density X-factors, which are X12_{CO (3−2)} = 4.0 × 10²⁰ and X13_{CO (3−2)} = 4.0 × 10²¹ cm⁻² (K km s⁻¹)⁻¹ with a factor of 1.5 uncertainty. We find that the emission profiles, size–linewidth, and mass–radius relationships of ¹³CO-traced structures are similar between the Inner and Outer Galaxy. Although PAMS sources are slightly more massive than their Inner Galaxy counterparts for a given size scale, the discrepancy can be accounted for by the Galactic gradient in gas-to-dust mass ratio, uncertainties in the X-factors, and selection biases. We have made the PAMS data publicly available, complementing other CO surveys targeting different regions of the Galaxy in different isotopologues and transitions.