Physical and chemical complexity in high-mass star-forming regions with ALMA - I. Overview and evolutionary trends of physical properties

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Volume 674 (June 2023)

A&A, 674 (2023) A160

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Table 2

Overview of the ALMA 3 mm continuum data products.

Region	Beam		Noise	Peak intensity	Flux density	Field

	θ_maj × θ_min (“×”)	PA (°)	σ_cont (mJy beam⁻¹)	(mJy beam⁻¹)	(mJy)
IRDC G11.11-4	1.0 × 0.8	104	0.033	1.4	15	Field 2
IRDC 18223-3	1.0 × 0.7	108	0.022	2.9	23	Field 3
IRDC 18310-4	1.0 × 0.7	111	0.022	1.2	4.0	Field 3
HMPOIRAS 18089	0.8 × 0.7	101	0.057	24	130	Field 2
HMPOIRAS 18182	1.1 × 0.7	107	0.029	13	90	Field 3
HMPOIRAS 18264	1.0 × 0.7	108	0.031	9.9	130	Field 3
HMC G9.62+0.19	0.9 × 0.7	104	0.049	58	640	Field 2
HMC G10.47+0.03	0.8 × 0.7	100	0.25	340	830	Field 2
HMC G34.26+0.15	0.8 × 0.7	118	1.8	2500	7100	Field 1
UCHII G10.30−0.15	1.0 × 0.8	104	0.041	18	1000	Field 2
UCHII G13.87+0.28	1.0 × 0.8	105	0.065	7.0	1800	Field 2

Notes. The regions are grouped into three fields (Field 1, Field 2, and Field 3) and were observed together during the ALMA observations to reduce off-source calibration time. The flux density is computed considering only areas with S/N > 5 within the full ALMA FOV.

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