List of Quenched, Isolated Dwarf Galaxies
Since there are still relatively few candidate quenched, isolated dwarf galaxies known, this is a way to keep track and easily compare their properties.
Please look at the references linked in the table for extended discussion of these galaxies and their properties. The physical and chemical parameters listed here are derived in a different ways from different data, so though every effort is made to show values consistently, rigorous one-to-one comparison will require understanding the nuance of each individual measurement and approach to analysis.
As addressed in greater detail in Polzin et al. (2021), the non-backsplash quiescent field dwarfs share common characteristics including young (~ 1 Gyr) stellar populations and low (106 - 107 M⊙) stellar masses, pointing to similar physical mechanisms informing the cessation of star formation in each case.
| Name | RA/Dec | Distance (Mpc) | Mstar (M⊙) | Age (Gyr) | [M/H] | Reff (kpc) | sSFR (yr-1) | MHI (M⊙) | Environment | References |
|---|---|---|---|---|---|---|---|---|---|---|
| Cetus | 00:26:11.0 -11:02:40 | 0.775 | -1.9 | likely backsplash (Teyssier et al. 2012; Buck et al. 2019) | Whiting et al (1999) | |||||
| Tucana | likely backsplash (Teyssier et al. 2012) | Lavery 1990 | ||||||||
| KKR 25 | 16:13:47.6 +54:22:16 | 1.93 | ~107 | ~1 | ~-1.5 | ~0.6 | ~2x10-11 | 8x104 | isolated | Makarov et al. 2012 |
| KKs 3 | 02:24:44.4 -73:30:51 | 2.12 | 2.3x107 | ~1 | ~-1.6 | 0.725 | 1.1x105 | isolated | Karachentsev et al. 2015; Sharina et al. 2018 | |
| COSMOS-dw1 | 10:00:30.03 +02:08:59.47 | 22 | 2.38x106 | 0.9 | -1.577 | 0.45 | < 1.5x10-12 | no detection | isolated | Polzin et al. (2021) |
| dw0910+7326 (Blobby) | 09:10:13.45 +73:26:19.15 | 3.21 | 9.5x106 | 10 | -1.2 | 0.790 | < 3x10-10 | backsplash | Casey et al. (2023) | |
| PEARLSDG | 12:12:18 +27:35:24 | 31.2 | 4.4x107 | 1 | -1.49 | 0.56 | 2x10-12 | < 4x105 | isolated | Carleton et al. (2024) |
| UGC 5205 | 09:44:07.2 -00:39:30 | ~21 | 3x108 | 0.1-0.3 | ~-1 (MZR) | -1.9 | ≲ 3x10-11 | 3.5x108 | dwarf-dwarf interaction | Kado-Fong et al. (2024) |
Quenched, now-isolated dwarfs that are likely backsplash galaxies or experiencing dwarf-dwarf interactions are listed in italics. Though they are not isolated by every definition, they are isolated by some definitions (generally those that are concerned primarily with current proximity to massive neighbors).
Additional candidates not included in the table due to large uncertainties/necessary follow-up:
- APPLES I (Pasquali et al. 2005)
- Penny et al. (2018)
- Prole et al. (2021)
- Tucana B (Sands et al. 2022)
Some of these candidates are potentially higher mass and subject to AGN feedback and other processes not as readily seen in low mass dwarfs.