NGC 5045
(MWSC 2096)
0.57
UTI
0.48
CN
0.48
Cdens
0.38
CC3
0.75
Clit
1.0
Cdup
Radius (P>50% members)
7.7 [arcmin]
- CN 0.48 Poorly populated
- Cdens 0.48 Loose
- CC3 0.38 Low quality
- Clit 0.75 Well-studied
- Cdup 1.0 Unique
Overview
NGC 5045 is a poorly populated, loose object of low C3 quality. Its parallax locates it at a moderate* distance, near the mid-plane, affected by moderate extinction. It is catalogued as a near-solar metallicity, very young cluster (see Parameters). It is well-studied in the literature.
(*): The parallax distance estimate (~2.00 kpc) differs significantly from the median photometric distance (~1.50 kpc).
Relatively close
Moderate extinction
Near-solar metallicity
Very young
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | â | 198.69 | -63.547 | 0.5 | -4.279 | -2.375 | 6.29 |
| Hunt & Reffert | 2024 | 198.723 | -63.572 | 0.495 | -4.283 | -2.378 | -4.308 |
| Cavallo et al. | 2024 | 198.607 | -63.554 | 0.495 | â | â | â |
| Hunt & Reffert | 2023 | 198.723 | -63.572 | 0.495 | -4.283 | -2.378 | -4.308 |
| Just et al. | 2023 | 198.619 | -63.416 | â | â | â | â |
| Kharchenko et al. | 2016 | 198.619 | -63.416 | â | â | â | â |
| Dias et al. | 2014 | 198.542 | -63.39 | â | -3.0 | -2.86 | â |
| Kharchenko et al. | 2013 | 198.63 | -63.42 | â | -7.0 | -0.31 | -16.8 |
| Gozha et al. | 2012 | 198.542 | -63.39 | â | â | â | â |
| Piskunov et al. | 2008 | 198.533 | -63.39 | â | â | â | â |
| Kharchenko et al. | 2007 | 199.26 | -63.41 | â | 0.38 | â | -16.76 |
| Piskunov et al. | 2007 | 198.533 | -63.39 | â | â | â | â |
| Kharchenko et al. | 2005 | 198.54 | -63.39 | â | -5.9 | -2.05 | -16.76 |
| Dias et al. | 2002 | 198.542 | -63.39 | â | -3.0 | -2.86 | -7.35 |
đĄ Note: The UCC values are estimated from its identified members.
| Reference | Year | Dist [kpc] | Av [mag] | DAv [mag] | Age [Myr] | [Fe/H] [dex] | Mass [Msun] | Bfr | BSS |
|---|---|---|---|---|---|---|---|---|---|
| Hunt & Reffert | 2024 | â | â | â | â | â | 218* | â | â |
| Cavallo et al. | 2024 | 1.53 | 0.89 | â | 46 | 0.020 | â | â | â |
| Hunt & Reffert | 2023 | 1.91 | 1.42 | 1.52 | 20 | â | â | â | â |
| Just et al. | 2023 | â | â | â | 90 | â | 721 | â | â |
| Kharchenko et al. | 2016 | 1.66 | 1.42 | â | 90 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.66 | 1.42 | â | 90 | â | â | â | â |
| Gozha et al. | 2012 | 1.50 | â | â | 13 | â | 6457 | â | â |
| Piskunov et al. | 2008 | 1.50 | 1.15 | â | 13 | â | 1538* | â | â |
| Piskunov et al. | 2007 | 1.50 | 1.15 | â | 13 | â | 322 | â | â |
| Kharchenko et al. | 2005 | 1.50 | 1.15 | â | 13 | â | â | â | â |
| Dias et al. | 2002 | 1.50 | 1.15 | â | 13 | â | â | â | â |
(*): Indicates that this parameter is assigned more than one value in the corresponding reference.


Cavallo et al. (2024)
Silver sample.
Dias et al. (2002)
Asterism (Archinal, B. A. & Hynes, S. J. 2003)