Table 6
Quenching parameters derived using other techniques for some HRS galaxies in the Virgo cluster.
| HRS | NGC/IC | Vel | QA | QF |
|
Age | Ref. | Method |
| km s-1 | Myr | Myr | ||||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) |
|
|
||||||||
| 102 | 4254 | 175 | 129 ± 478 | –0.06 ± 0.36 | 3.14 | 280 | 8 | dyn |
| 124 | 4330 | 120 | 172 ± 50 | 0.89 ± 0.04 | 1.09 | –100 | 3 | dyn |
| 124 | 4330 | 120 | 172 ± 50 | 0.89 ± 0.04 | 1.09 | 200–400 | 11 | phot |
| 144 | 4388 | 180 | 61 ± 25 | 0.74 ± 0.06 | 1.00 | 225 ± 100 | 6 | spec |
| 144 | 4388 | 180 | 61 ± 25 | 0.74 ± 0.06 | 1.00 | 120 | 9 | dyn |
| 149 | 4402 | 120 | 1302 ± 320 | 0.90 ± 0.04 | 3.23 | 200a | 6 | spec |
| 156 | 4419 | 95 | 1610 ± 75 | 0.95 ± 0.05 | 6.15 | 500 ± 150 | 6 | spec |
| 159 | 4424 | 32 | 501 ± 25 | 0.95 ± 0.05 | 2.81 | 275 ± 75 | 6 | spec |
| 163 | 4438 | 130 | 576 ± 250 | 0.95 ± 0.05 | 3.66 | 100 | 4 | dyn |
| 172 | IC3392 | 100 | 299 ± 15 | 1.0 ± 0.05 | 2.90 | 500 ± 100 | 6 | spec |
| 190 | 4501 | 290 | 77 ± 135 | 0.81 ± 0.09 | 2.88 | –250 | 7 | dyn |
| 197 | 4522 | 105 | 64 ± 101 | 0.80 ± 0.04 | 3.01 | 50 | 5 | dyn |
| 197 | 4522 | 105 | 64 ± 101 | 0.80 ± 0.04 | 3.01 | 100 ± 50 | 6 | spec |
| 217 | 4569 | 220 | 288 ± 23 | 0.90 ± 0.05 | 1.84 | 100 | 1 | model |
| 217 | 4569 | 220 | 288 ± 23 | 0.90 ± 0.05 | 1.84 | 300 | 2 | dyn |
| 217 | 4569 | 220 | 288 ± 23 | 0.90 ± 0.05 | 1.84 | 300 ± 50 | 6 | spec |
| 221 | 4580 | 105 | 646 ± 101 | 0.95 ± 0.05 | 1.52 | 475 ± 100 | 6 | spec |
| 247 | 4654 | 175 | 645 ± 804 | 0.40 ± 0.21 | 2.39 | 500a | 10 | dyn |
Notes. Column 1: HRS name; Col. 2: NGC/IC name; Col. 3: rotational velocity used in the CIGALE fit; Col. 4: QA and error derived using CIGALE; Col. 5: QF and error derived using CIGALE; Col. 6: reduced ; Col. 7: age of the interaction derived in the literature; Col. 8: references coded as: 1: Boselli et al. (2006); 2: Vollmer et al. (2004); 3: Vollmer et al. (2012); 4: Vollmer et al. (2009); 5: Vollmer et al. (2006); 6: Crowl & Kenney (2008); 7: Vollmer et al. (2008a); 8: Vollmer et al. (2005); 9: Vollmer & Huchtmeier (2003); 10: Vollmer (2003); 11: Abramson et al. (2011); Col. 9: method used to derive the age of the interaction: “dyn” stands for dynamical models based on the HI and/or CO data; “spec” for IFU spectroscopy of the outer stellar disc; “model” for multizone-chemospectrophotometric models of galaxy evolution; “phot” derived using UV-to-optical photometry.
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.