Clump formation in ram-pressure stripped galaxies: Evidence from mass function

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Volume 696 (April 2025)

A&A, 696 (2025) A228

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Table 1.

Main properties of our target galaxies and of their clusters.

ID_P16	RA	Dec	M_*	R_e	z_gal	Cluster	z_clus	σ_clus	References
	(J2000)	(J2000)	[× 10¹⁰ M_⊙]	[kpc]				[km/s]
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)
JO175	20:51:17.593	–52:49:22.34	3.2 ± 0.5	$3 . 24_{- 0.34}^{+ 0.37}$ $3.24^{+0.37}_{-0.34}$	0.0468	A3716	0.0457	$753_{- 38}^{+ 36}$ $753^{+36}_{-38}$	(4,10,14)
JO201	00:41:30.295	–09:15:45.98	6.2 ± 0.8	$7 . 73_{- 0.79}^{+ 0.60}$ $7.73^{+0.60}_{-0.79}$	0.0446	A85	0.0559	$859_{- 44}^{+ 42}$ $859^{+42}_{-44}$	(3,4,5,6,8,9,10,
									13,14,15,16,18)
JO204	10:13:46.842	–00:54:51.27	4.1 ± 0.6	$4 . 58_{- 0.26}^{+ 0.22}$ $4.58^{+0.22}_{-0.26}$	0.0424	A957	0.0451	$631_{- 40}^{+ 43}$ $631^{+43}_{-40}$	(2,4,6,12,18)
JO206	21:13:47.410	+02:28:35.50	9.1 ± 0.9	$8 . 94_{- 1.14}^{+ 1.08}$ $8.94^{+1.08}_{-1.14}$	0.0513	IIZW108	0.0486	$575_{- 31}^{+ 33}$ $575^{+33}_{-31}$	(1,4,6,10,13,18,19)
JW39	13:04:07.719	+19:12:38.41	17.0 ± 3.0	$10 . 16_{- 1.34}^{+ 1.23}$ $10.16^{+1.23}_{-1.34}$	0.0650	A1668	0.0634	654 ^(a)	(14,18,19,21,22)
JW100	23:36:25.054	+21:09:02.64	29.0 ± 7.0	$7 . 35_{- 0.74}^{+ 0.43}$ $7.35^{+0.43}_{-0.74}$	0.0602	A2626	0.0548	$650_{- 49}^{+ 53}$ $650^{+53}_{-49}$	(4,6,7,10,11,
									15,17,18,19,20)

Notes. Columns are: GASP ID of the galaxy as in Poggianti et al. (2016) (1); RA and Dec of the galaxy (2 and 3); galaxy stellar mass with 1σ uncertainties (4); effective radius with 1σ uncertainties (5); galaxy redshift (6); ID of the host cluster (7); cluster redshift (8); cluster velocity dispersion with 68% upper and lower uncertainties (9); references (10). Masses are from Vulcani et al. (2018) and derived with our spectrophotometric code SINOPSIS (Fritz et al. 2017). Effective radii are computed as the half-light radii by fitting I-band (computed integrating MUSE data) isophotes to ellipses and taken from Franchetto et al. (2020) and converted to kiloparecs. Cluster redshifts and velocity dispersions are computed from the spectroscopic redshifts of the cluster members and are from Biviano et al. (2017) and Cava et al. (2009).

(1) Poggianti et al. (2017b), (2) Gullieuszik et al. (2017), (3) Bellhouse et al. (2017), (4) Poggianti et al. (2017a), (5) George et al. (2018), (6) Moretti et al. (2018), (7) Poggianti et al. (2019a), (8) Bellhouse et al. (2019), (9) George et al. (2019), (10) Radovich et al. (2019), (11) Moretti et al. (2020), (12) Deb et al. (2020), (13) Ramatsoku et al. (2020), (14) Bellhouse et al. (2021), (15) Tomičić et al. (2021a), (16) Campitiello et al. (2021), (17) Ignesti et al. (2022a), (18) Tomičić et al. (2021b), (19) Ignesti et al. (2022b), (20) Sun et al. (2021), (21) Peluso et al. (2022), (22) George et al. (2023).

^(a)

Uncertainties not available.

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