Radio continuum tails in ram pressure-stripped spiral galaxies: Experimenting with a semi-empirical model in Abell 2255

Open Access

Table 4.

Parameters describing the galaxies motion in the cluster as inferred from our analysis.

ID	V_sky	V_los	V_tot	n_e	P_Ram
	[km s⁻¹]	[km s⁻¹]	[km s⁻¹]	[×10⁻³ cm⁻³]	[×10⁻¹¹ erg cm⁻³]
1	429 ± 83	–935	1029 ± 34	0.07 ± 0.01	0.14 ± 0.01
3	215 ± 32	–1355	1372 ± 5	0.81 ± 0.03	2.91 ± 0.1
4	325 ± 38	–64	331 ± 37	0.99 ± 0.04	0.21 ± 0.05
6	160 ± 32	–961	975 ± 5	0.19 ± 0.01	0.34 ± 0.01
7	251 ± 44	–928	962 ± 11	0.31 ± 0.01	0.56 ± 0.02

Notes. From left to right: Galaxy ID (see Table 2); best-fit V_sky; V_los derived from galaxy redshift (see Table 2); total velocity computed as ; electron density at the projected clustercentric distance (Fig. 6); ram pressure computed as .

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.