HM 1, also known as Havlen-Moffat 1, is an open cluster located in the constellation of Scorpius, close to the galactic plane. It was first observed by R. J. Havlen and A. F. J. Moffat in 1976.[5] HM 1 is thought to be 9,500 to 12,700 light-years (2,900 to 3,900 parsecs) away from the Earth, beyond the Carina–Sagittarius Arm.[2] It is heavily reddened by interstellar extinction, so although it comprises mostly blue-colored stars, it appears brighter for longer-wavelength passbands.[2] It is projected against the H II region known as RCW 121, and appears to be the source of ionization for the nearby regions RCW 122 and RCW 123.[2]
| HM 1 (Havlen-Moffat 1) | |
|---|---|
 Approximate location of HM 1 (circled) | |
| Observation data (J2000 epoch) | |
| Right ascension | 17h 18m 54s[1] |
| Declination | −38° 49′ 01″[1] |
| Distance | 9,500–12,700 ly (2,900–3,900 pc[2]) |
| Apparent dimensions (V) | 5′[3] |
| Physical characteristics | |
| Estimated age | 1-2 Myr[4] 2-4 Myr[2] |
| Star cluster rich in massive stars | |
| Other designations | C 1715-387 |
| Associations | |
| Constellation | Scorpius |
Properties
editThe extinction value for HM 1 is calculated to be EB−V = 1.85 magnitudes, and its distance was first estimated to be around 2.9 ± 0.4 kiloparsecs away.[5] Later estimates put the cluster at around 3.3 kiloparsecs away; this is still one of the more closer massive star clusters.[2]
HM 1 is fairly young for an open cluster; it is estimated to be 1 to 2, or 2 to 4 million years old.[6] This is indicated by the presence of Of stars, which have relatively short lives. However, a red supergiant with a bolometric magnitude of −6.6 and a mass of about 20 M☉ was discovered near the cluster, contradicting the supposed age of the cluster.[7] However, subsequent work showed the star is likely in the foreground.[2]
Composition
editHM 1 is noted for its components, including several Wolf–Rayet stars and Of stars. Both types of stars are fairly rare and very massive, and their coexistence in star clusters was unexpected. The evolution of Wolf–Rayet stars and Of stars in star clusters is currently unclear. Very few Wolf–Rayet stars have been found in star clusters, and a possible explanation is that the formation of these cluster Wolf–Rayet stars requires a binary star system containing two Of stars. Alternatively, cluster Wolf–Rayet stars may simply be rare because they represent a short stage in the evolution of Of stars, whether single or binary.[5]
Many of the stellar components are extremely blue-colored O-type stars that are among some of the most luminous stars known. Some of the candidate members listed have masses of over 20 M☉, making this cluster one of the richest known.[6] Examples include the peculiar star LSS 4067, an O-type supergiant with a spectral type of O4If+.[4] WR 89, another luminous star, is a strong X-ray source and is possibly a colliding-wind binary, based on data from XMM-Newton.[6] In contrast, WR 87 has a high plasma temperature consistent with that of a colliding-wind binary but otherwise appears to be a single star (similar to WR 136).[4]
| Name[note 1] | Teff | MV | Mbol | Mass (M☉) | Spectral type | Ref. |
|---|---|---|---|---|---|---|
| HM 1 1 (WR 89) | 39800 | −7.56 | −11.09 | 87[8] | WN8h | [8] |
| HM 1 2 (LSS 4067) | 47800 | −7.0 | −11.4 | 120 | O4If+ | [4] |
| HM 1 3 (WR 87) | 44700 | −6.95 | −10.79 | 59[8] | WN7h | [8] |
| HM 1 6 | 45000 | −6.5 | −10.7 | 95 | O5If | [4] |
| HM 1 8[note 2] | 41200 + 34500 | −5.2 + −3.7 | −10[4] | 26.8 + <9.7 | O4.5IV(f) + O9.7V | [9] |
| HM 1 9 | 37900 | −5.3 | −8.9 | 38 | [4] | |
| HM 1 12 | 41900 | −5.5 | −9.5 | 50 | O6If | [4] |
| HM 1 13 | 41000 | −5.3 | −9.2 | 44 | O7V((f)) | [4] |
| HM 1 16 | 33100 | −5.4 | −8.7 | 32 | [4] | |
| HM 1 18 | 38100 | −4.4 | −8.1 | 29 | [4] | |
| HM 1 19 | 39300 | −4.1 | −7.8 | 28 | [4] | |
| HM 1 20 | 34700 | −4.1 | −7.4 | 22 | O9.5V | [4] |
Gallery
edit
See also
edit- Cygnus OB2, an OB association containing many massive stars
- List of most massive stars
References
edit- ^ a b Kharchenko, N. V.; Piskunov, A. E.; Schilbach, E.; Röser, S.; Scholz, R.-D. (2013). "Global survey of star clusters in the Milky Way". Astronomy & Astrophysics. 558: A53. arXiv:1308.5822. Bibcode:2013A&A...558A..53K. doi:10.1051/0004-6361/201322302. S2CID 118548517.
- ^ a b c d e f g Vázquez, R. A.; Baume, G. (2001). "The open cluster Havlen-Moffat No. 1 revisited". Astronomy and Astrophysics. 371 (3): 908–920. Bibcode:2001A&A...371..908V. doi:10.1051/0004-6361:20010410.
- ^ Morales, Esteban F. E.; Wyrowski, Friedrich; Schuller, Frederic; Menten, Karl M. (2013). "Stellar clusters in the inner Galaxy and their correlation with cold dust emission". Astronomy & Astrophysics. 560: A76. arXiv:1310.2612. Bibcode:2013A&A...560A..76M. doi:10.1051/0004-6361/201321626. S2CID 118422539.
- ^ a b c d e f g h i j k l m Massey, P.; Degioia-Eastwood, K.; Waterhouse, E. (2001). "The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. II. Results from 12 Galactic Clusters and OB Associations". The Astronomical Journal. 121 (2): 1050–1070. arXiv:astro-ph/0010654. Bibcode:2001AJ....121.1050M. doi:10.1086/318769. S2CID 53345173.
- ^ a b c Havlen, R. J.; Moffat, A. F. J. (1977). "A new cluster containing 2 Wolf-Rayet-stars and 2 Of-stars". Astronomy and Astrophysics. 58 (3): 351–356. Bibcode:1977A&A....58..351H.
- ^ a b c Nazé, Y.; Rauw, G.; Sana, H.; Corcoran, M. F. (2013). "X-ray properties of the young open clusters HM1 and IC 2944/2948". Astronomy & Astrophysics. 555: A83. arXiv:1305.5105. Bibcode:2013A&A...555A..83N. doi:10.1051/0004-6361/201321099. S2CID 119231082.
- ^ The, P. S.; Arens, M.; van der Hucht, K. A. (1982). "An investigation of the Scorpius open cluster C1715-387 containing two WN7, two Of and one red supergiant members". Astrophysical Letters. 22: 109. Bibcode:1982ApL....22..109T.
- ^ a b c d Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters". Astronomy & Astrophysics. A57: 625. arXiv:1904.04687. Bibcode:2019A&A...625A..57H. doi:10.1051/0004-6361/201834850. S2CID 104292503.
- ^ Rodríguez, C. N.; Ferrero, G. A.; Benvenuto, O. G.; Gamen, R.; Morrell, N. I.; Barbá, R. H.; Arias, J.; Massey, P. (2021). "Fundamental parameters of the massive eclipsing binary HM1 8". Monthly Notices of the Royal Astronomical Society. 508 (2): 2179–2193. arXiv:2109.13054. doi:10.1093/mnras/stab2699.
Notes
edit- ^ These numbers are not the same as the ones used in SIMBAD. For example, HM 1 6 (WR 87) is [NRS2013] HM1 6, not Cl HM 1 6.
- ^ This is a binary star system. Parameters, if two are provided, refer to the primary and secondary, respectively.