Parallax-based distances to Galactic H II regions: Nearby spiral structure

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Table 2

H II regions with parallax distances based on Gaia DR3.

H II region name	Cl	R	d_⊙	V_LSR	Line	Ref.	d_kin	Group	Note
		(″)	(kpc)	(km s⁻¹)			(kpc)
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
G000.003+00.127	K	206	${2.28}_{- 0.12}^{+ 0.18}$ $2.28_{ - 0.12}^{ + 0.18}$	−5.5	Hα	1	–	I	–
G000.121−00.304	Q	37	${2.51}_{- 0.11}^{+ 0.15}$ $2.51_{ - 0.11}^{ + 0.15}$	–	–	–	–	III	–
G011.662−01.692	K	907	${1.25}_{- 0.02}^{+ 0.02}$ $1.25_{ - 0.02}^{ + 0.02}$	18.3	RRL	2	–	I	maser
G017.315+00.389	C	78	${1.85}_{- 0.05}^{+ 0.05}$ $1.85_{ - 0.05}^{ + 0.05}$	–	–	–	–	III	–
G018.253−00.298	K	205	${3.36}_{- 0.38}^{+ 0.33}$ $3.36_{ - 0.38}^{ + 0.33}$	47.5	H110α	3	${3.60}_{- 0.36}^{+ 0.32}$ $3.60_{ - 0.36}^{ + 0.32}$	I	M22
G018.669−00.298	K	272	${1.95}_{- 0.06}^{+ 0.08}$ $1.95_{ - 0.06}^{ + 0.08}$	27.6	CO(1−0)	4	${2.33}_{- 0.24}^{+ 0.17}$ $2.33_{ - 0.24}^{ + 0.17}$	I	M22
G024.138+00.123	K	88	${2.18}_{- 0.06}^{+ 0.08}$ $2.18_{ - 0.06}^{ + 0.08}$	114.5	H87 + 88/85α	2	${6.61}_{- 0.32}^{+ 0.41}$ $6.61_{ - 0.32}^{ + 0.41}$	III	–
G026.443+01.741	K	201	${2.40}_{- 0.05}^{+ 0.07}$ $2.40_{ - 0.05}^{ + 0.07}$	42.3	CS(2−1)	5	${2.70}_{- 0.22}^{+ 0.22}$ $2.70_{ - 0.22}^{ + 0.22}$	I	M22
G026.802+03.526	K	69	${0.41}_{- 0.01}^{+ 0.01}$ $0.41_{ - 0.01}^{ + 0.01}$	45.3	Hα	6	${2.88}_{- 0.27}^{+ 0.22}$ $2.88_{ - 0.27}^{ + 0.22}$	III	–
G028.200−00.050	K	60	${2.49}_{- 0.11}^{+ 0.14}$ $2.49_{ - 0.11}^{ + 0.14}$	96.8	HCO+	7	${5.50}_{- 0.32}^{+ 0.40}$ $5.50_{ - 0.32}^{ + 0.40}$	I	–
…	…	…	…	…	…	…	…	…	…

Notes. The entire version in a machine-readable format is available at the CDS. Column (1) is the source name. Cols. (2) and (3) are the classification and radius given by the WISE catalogue of H II regions (Anderson et al. 2014). Col. (4) is the parallax-based distance given by this work according to Gaia DR3 (see Sect. 3.2 for detail). Cols. (5), (6), and (7) list the LSR velocity, the observed line(s), and the reference if available in literature: 1: Fich et al. (1990); 2: Lockman (1989); 3: Downes et al. (1980); 4: Blitz et al. (1982); 5: Bronfman et al. (1996); 6: Fich et al. (1990); 7: Sewilo et al. (2004). Col. (8) is the kinematic distance calculated by using the tool of Wenger et al. (2018) and the Galactic rotation model of Reid et al. (2019). Col. (9) is a classification based on the robustness of the estimated parallax distances as discussed in Sect. 3.2. Col. (10) gives a note for those H II regions with determined parallax distances in literature: maser: the distance is determined from the associated HMSFR maser; M22: the distance was given by Méndez-Delgado et al. (2022) based on Gaia DR3.

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