The MeerKAT Fornax Survey - VI. The collapse of the galaxy H I Mass Function in Fornax

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Table A.1.

H I detected galaxies.

Name	FCC Number	log(M_HI/M_⊙)	v_sys	w₂₀	M_r
			(km s⁻¹)	(km s⁻¹)	(mag)
(1)	(2)	(3)	(4)	(5)	(6)
ESO 358-015	113	8.2 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1388	98	−17.03
ESO 358-016	115	8.1 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1700	95	−15.43
ESO 358-051	263	8.4 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1724	142	−18.33
ESO 358-063	312	9.3 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1929	311	−20.02
ESO 358-064	B1899	7.7 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1465	127	−16.20
ESO 359-002	335	7.3 $\begin{matrix} + 0.05 \\ - 0.05 \end{matrix}$ $\substack{+0.05 \\ -0.05}$	1447	95	−18.18
FCC 057	57	7.2 $\begin{matrix} + 0.05 \\ - 0.05 \end{matrix}$ $\substack{+0.05 \\ -0.05}$	1442	59	−14.37
FCC 090	90	7.7 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1825	79	−17.60
FCC 102	102	8.0 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1640	59	−15.80
FCC 120	120	8.0 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	846	45	−15.72
FCC 128	128	7.1 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1543	50	−15.50
FCC 134	134	6.4 $\begin{matrix} + 0.06 \\ - 0.07 \end{matrix}$ $\substack{+0.06 \\ -0.07}$	1395	35	−14.65
FCC 207	207	6.1 $\begin{matrix} + 0.07 \\ - 0.08 \end{matrix}$ $\substack{+0.07 \\ -0.08}$	1420	43	−16.55
FCC 248	248	6.1 $\begin{matrix} + 0.07 \\ - 0.09 \end{matrix}$ $\substack{+0.07 \\ -0.09}$	1859	15	−13.44
FCC 261	261	7.2 $\begin{matrix} + 0.05 \\ - 0.05 \end{matrix}$ $\substack{+0.05 \\ -0.05}$	1665	62	−16.44
FCC 267	267	7.2 $\begin{matrix} + 0.05 \\ - 0.05 \end{matrix}$ $\substack{+0.05 \\ -0.05}$	833	50	−16.16
FCC 282	282	7.1 $\begin{matrix} + 0.05 \\ - 0.05 \end{matrix}$ $\substack{+0.05 \\ -0.05}$	1260	69	−17.79
FCC 299	299	7.5 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	2100	104	−15.18
FCC 306	306	8.3 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04\\ -0.05}$	884	130	−16.00
FCC 323	323	7.6 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1499	47	−14.41
FCC 332	332	7.2 $\begin{matrix} + 0.05 \\ - 0.05 \end{matrix}$ $\substack{+0.05 \\ -0.05}$	1325	118	−14.41
FCCB 0507	B507	7.8 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1149	74	−13.87
FCCB 0905	B905	7.7 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1246	70	−15.12
FCCB 1461	B1461	7.1 $\begin{matrix} + 0.05 \\ - 0.05 \end{matrix}$ $\substack{+0.05 \\ -0.05}$	799	34	−13.58
FDS6 DWARF 100b	–	7.1 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1983	36	−13.06
FDS14 DWARF 011	–	6.5 $\begin{matrix} + 0.10 \\ - 0.12 \end{matrix}$ $\substack{+0.10 \\ -0.12}$	1430	48	−12.73
NGC 1351A	67	8.8 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1347	221	−18.48
NGC 1365	121	10.2 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1636	400	−22.46
NGC 1386	179	7.7 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	868	48	−20.67
NGC 1387	184	6.6 $\begin{matrix} + 0.07 \\ - 0.08 \end{matrix}$ $\substack{+0.07 \\ -0.08}$	1302	155	−21.32
NGC 1427	276	7.6 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1390	110	−21.05
NGC 1427A	235	9.4 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	2036	120	−18.75
NGC 1436	290	8.3 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1395	225	−20.23
NGC 1437A	285	8.8 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	886	93	−18.02
NGC 1437B	308	8.5 $\begin{matrix} + 0.04 \\ - 0.05 \end{matrix}$ $\substack{+0.04 \\ -0.05}$	1510	142	−18.67

Notes. (1) Galaxy name. (2) FCC number. (3) M_HI and its uncertainty, as measured from the 41″ resolution image. (4) Systemic velocity measured in the optical definition. (5) Width of the H I profile at 20% of the peak flux from the SoFiA parametrisation. (6) Absolute r-band magnitude derived from aperture photometry from Su et al. (2021), assuming a distance of 20 Mpc.

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