Table 2.
Subsample of LSBs at the distance of Virgo detected in H I by ALFALFA (Haynes et al. 2018).
| ID | AGC ID | c z⊙ | W50 | log MHI | Offset |
|---|---|---|---|---|---|
| (km s−1) | (km s−1) | (M⊙) | (arcmin) | ||
| (1) | (2) | (3) | (4) | (5) | (6) |
| 186 | 220 258 | 2219 | 24 ± 3 | 8.8 ± 0.1 | 0.4 |
| 261 | 7307 | 1183 | 52 ± 3 | 8.6 ± 0.1 | 0.2 |
| 1405 | 7547 | 1100 | 71 ± 3 | 9.1 ± 0.1 | 0.1 |
| 1424 | 220 597 | 1860 | 48 ± 2 | 7.7 ± 0.1 | 1.3 (a) |
| 1968 | 227 874 | 473 | 30 ± 10 | 7.9 ± 0.2 | 2.8 (b) |
Notes. (1) Name of the source; (2) Arecibo General Catalogue (AGC) ID; (3) Heliocentric velocity of the H I line profile midpoint; (4) Velocity width of the H I line profile at 50% of the peak (W50); (5) H I mass; (6) Offset of the ALFALFA beam centroid with respect to the NGVS coordinate of the source.
The ALFALFA beam includes also the bright galaxy VCC 963 to which the H I detection is probably associated.
H I detection is between our diffuse galaxy and the elliptical galaxy M 49 (Sancisi et al. 1987; Patterson & Thuan 1992; Henning et al. 1993; Arrigoni Battaia et al. 2012).
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