Credit: ESO/VPHAS+ Survey/N. Wright
|Observation data (J2000 epoch)|
|Right ascension||16h 47m 04.0s|
|Declination||−45° 51′ 04.9″|
|Distance||12.1±2.0 (3.7±0.6 kpc)|
|Estimated age||3.50 Myr|
|Other designations||Ara Cluster, Westerlund 1, ESO 277-12, C 1644-457, VDBH 197|
Westerlund 1 (abbreviated Wd1, sometimes called Ara Cluster) is a compact young super star cluster in the Milky Way galaxy, about 3.5–5 kpc away from Earth. It is one of the most massive young star clusters in the Milky Way, and was discovered by Bengt Westerlund in 1961 but remained largely unstudied for many years due to high interstellar absorption in its direction. In the future, it will probably evolve into a globular cluster.
The cluster contains a large number of rare, evolved, high-mass stars, including: 6 yellow hypergiants, 4 red supergiants including Westerlund 1-26, one of the largest known stars, 24 Wolf-Rayet stars, a luminous blue variable, many OB supergiants, and an unusual supergiant sgB[e] star which has been proposed to be the remnant of a recent stellar merger. In addition, X-ray observations have revealed the presence of the anomalous X-ray pulsar CXO J164710.2-455216, a slow rotating neutron star that must have formed from a high-mass progenitor star. Westerlund 1 is believed to have formed in a single burst of star formation, implying the constituent stars have similar ages and compositions.
Aside from hosting some of the most massive and least-understood stars in our galaxy, Westerlund 1 is useful as a relatively nearby, easy to observe super star cluster that can help astronomers determine what occurs within extragalactic super star clusters.
The brightest O7-8V main sequence stars in Wd1 have V-band photometric magnitudes around 20.5, and therefore at visual wavelengths Wd1 is dominated by highly luminous post-Main Sequence stars (V-band magnitudes of 14.5–18, absolute magnitudes −7 to −10), along with less-luminous post-Main Sequence stars of luminosity class Ib and II (V-band magnitudes of 18–20). Due to the extremely high interstellar reddening towards Wd1, it is very difficult to observe in the U- and B-bands, and most observations are made in the R- or I-bands at the red end of the spectrum or in the infra red. Stars in the cluster are generally named using a classification introduced by Westerlund, although a separate naming convention is often used for the Wolf-Rayet stars.
At X-ray wavelengths, Wd1 shows diffuse emission from interstellar gas and point emission from both high-mass, post-Main Sequence and low mass, pre-Main Sequence stars. The Westerlund 1 magnetar is the most luminous X-ray point source in the cluster, with the sgB[e] star W9, the (presumed) binary W30a and the Wolf–Rayet stars WR A and WR B all strong X-ray sources. Approximately 50 other X-ray point sources are associated with luminous optical counterparts. Finally, at radio wavelengths the sgB[e] star W9 and red supergiants W20 and W26 are strong radio sources, while the majority of the cool hypergiants and a few OB supergiants and Wolf–Rayet stars are also detected.
Distance and location
Wd1 has been too remote for direct measurement of the distance via parallax measurements, but the Gaia space mission is expected to provide such a measurement in 2018. In the meantime, the distance to Wd1 must be estimated from the expected absolute magnitude of the stars and estimates of the extinction towards the cluster. This has been done for both the yellow hypergiant and Wolf–Rayet populations, yielding estimates around 5 kpc in both cases, while a determination from the main-sequence population suggests 3.6 kpc. These estimates all place Wd1 near the outer edge of the Galactic bar, which may be significant in determining how such a massive cluster formed.
The detection of only a limited number of Wolf–Rayet stars at radio wavelengths provides a lower limit on the distance of 2 kpc; while a few Wolf–Rayet stars are detected, these are believed to be colliding-wind binaries with correspondingly enhanced radio emission.
Age and evolutionary state
The age of Wd1 is estimated at 4–5 Myr from comparison of the population of evolved stars with models of stellar evolution. The presence of significant numbers of both Wolf–Rayet stars and red and yellow supergiants in Wd1 represents a strong constraint on the age: theory suggests that red supergiants will not form until around 4 Myr as the most massive stars do not go through a red supergiant phase, while the Wolf–Rayet population declines sharply after 5 Myr. This range of ages is broadly consistent with infra-red observations of Wd1 that reveal the presence of late-O main sequence stars, although a lower age of around 3.5 Myr has been suggested from observations of lower-mass stars in Wd1.
If Wd1 formed stars with a typical initial mass function then the cluster would have originally contained a significant number of very massive stars, such as those currently observed in the younger Arches cluster. Current estimates of the age of Wd1 are greater than the lifetimes of these stars, and stellar evolution models suggest that there would already have been 50–150 supernovae in Wd1, with a supernova rate of approximately one per 10,000 years over the last million years. However, to date only one definitive supernova remnant has been detected—the Westerlund 1 magnetar—and the lack of other compact objects and high-mass X-ray binaries is puzzling. A number of suggestions have been put forward, including high supernova kick velocities that disrupt binary systems, the formation of slowly accreting (and therefore undetectable) stellar mass black holes, or binary systems in which both objects are now compact objects, but the problem has yet to be resolved.
As the stars in Westerlund 1 have the same age, composition and distance, the cluster represents an ideal environment for understanding the evolution of massive stars. The simultaneous presence of stars evolving on to and off of the Main Sequence presents a robust test for stellar evolution models, which are also currently unable to correctly predict the observed distribution of Wolf–Rayet subtypes in Westerlund 1.
A number of lines of evidence point to a high binary fraction amongst the high-mass stars in Wd1. Some massive binaries are detected directly through photometry and radial velocity observations, while many others are inferred through secondary characteristics (such as high X-ray luminosity, non-thermal radio spectra and excess infra-red emission) that are typical of colliding-wind binaries or dust-forming Wolf–Rayet stars. Overall binary fractions of 70% for the Wolf–Rayet population and in excess of 40% for the OB supergiants are currently estimated, although both may be incomplete.
This section needs expansion. You can help by adding to it. (March 2018)
|Designation||Right ascension||Declination||Object type||Spectral type||Luminosity (L☉)||Temperature (K)|
|W2a||16h 46m 59.7s||−45° 50′ 51.1″||Blue supergiant||O9.5 Ia - B0.5 Ia|
|W4||16h 47m 01.42s||−45° 50′ 37.1″||Yellow hypergiant||G0 Ia+ - F2 Ia+|
|W6a||16h 47m 04.0s||−45° 50′ 21.0″||Blue supergiant|
|W7||16h 46m 03.62s||−45° 50′ 14.2″||Blue hypergiant|
|W8a||16h 47m 04.79s||−45° 50′ 24.9″||Yellow hypergiant|
|W8b||16h 47m 04.95s||−45° 50′ 26.7″||Blue supergiant||B1-5Ia|
|W9||16h 47m 04.14s||−45° 50′ 31.1″||B[e] star||sgB[e]|
|W12a||16h 47m 02.21s||−45° 50′ 58.8″||Yellow hypergiant|
|W13||16h 47m 06.45s||−45° 50′ 26.0″||Eclipsing binary||B0.5 Ia+, OB|
|W16a||16h 47m 06.61s||−45° 50′ 42.1″||Yellow hypergiant|
|W20||16h 47m 04.70s||−45° 51′ 23.8″||Red supergiant||126,000||3,500|
|W26||16h 47m 05.40s||−45° 50′ 36.5″||Red hypergiant||M2-6Ia||320,000 - 1,100,000||3,600 - 3,700|
|W32||16h 47m 03.67s||−45° 50′ 43.5″||Yellow hypergiant|
|W33||16h 47m 04.12s||−45° 50′ 48.3″||Blue hypergiant|
|W75||16h 47m 08.93s||−45° 49′ 58.4″||Red supergiant||68,000||3,600|
|W237||16h 47m 03.09s||−45° 52′ 18.8″||Red supergiant||230,000||3,600|
|W243||16h 47m 07.55s||−45° 52′ 28.5″||Luminous blue variable||LBV|
|W265||16h 47m 06.26s||−45° 49′ 23.7″||Yellow hypergiant|
|WR 77a||16h 46m 55.4s||−45° 51′ 34″||Wolf–Rayet star||WN6-7|
|WR 77aa||16h 46m 46.3s||−45° 47′ 58″||Wolf–Rayet star||WC9d|
|WR 77b||16h 46m 59.9s||−45° 55′ 26″||Wolf–Rayet star||WC8|
|WR 77c||16h 47m 00.89s||−45° 51′ 20.9″||Wolf–Rayet star||WNL|
|WR 77d, W57c||16h 47m 01.5s||−45° 51′ 45″||Wolf–Rayet star||WN8|
|WR 77e||16h 47m 01.67s||−45° 51′ 19.9″||Wolf–Rayet star||WN6-8|
|WR 77f, W5||16h 47m 02.97s||−45° 50′ 19.5″||Wolf–Rayet star||WNVL|
|WR 77g||16h 47m 03.1s||−45° 50′ 43″||Wolf–Rayet star||WC7|
|WR 77h, W66||16h 47m 04.0s||−45° 51′ 37.5″||Wolf–Rayet star||WC9|
|WR 77i||16h 47m 04.02s||−45° 51′ 25.2″||Wolf–Rayet star||WN6-8|
|WR 77j, W44||16h 47m 04.20s||−45° 51′ 07.0″||Wolf–Rayet star||WN9|
|WR 77k||16h 47m 04.1s||−45° 51′ 20.0″||Wolf–Rayet star||WC9|
|WR 77l||16h 47m 04.40s||−45° 51′ 03.8″||Wolf–Rayet star||WC8.5|
|WR 77m, W239||16h 47m 05.21s||−45° 52′ 25.0″||Wolf–Rayet star||WC9|
|WR 77n||16h 47m 05.35s||−45° 51′ 05.0″||Wolf–Rayet star||WN8 (uncertain)|
|WR 77o, W14c||16h 47m 06.0s||−45° 15′ 22″||Wolf–Rayet star||WN7o|
|WR 77p, W241||16h 47m 06.06s||−45° 52′ 08.3″||Wolf–Rayet star||WC9|
|WR 77q||16h 47m 06.24s||−45° 51′ 26.5″||Wolf–Rayet star||WN6-8|
|WR 77r||16h 47m 07.6s||−45° 52′ 36″||Wolf–Rayet star||WN6|
|WR 77s, W72||16h 47m 08.32s||−45° 50′ 45.5″||Wolf–Rayet star||earlier than WN7|
|CXOU J164710.2-455216||16h 47m 10.18s||−45° 52′ 16.7″||anomalous X-ray pulsar|
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- SIMBAD, CXOU J164710.2-455216
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