Astronomy:Stephenson 2-18

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Short description: Possible red supergiant or red hypergiant star in the open cluster Stephenson 2
Stephenson 2-18
Stephenson 2-18 zoomed in, 2MASS survey, 2003.png
Stephenson 2-18 together with its parent cluster Stephenson 2 (upper left), viewed by the Two-Micron All Sky Survey.
Credit: Université de Strasbourg/CNRS (2003)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Scutum
Right ascension  18h 39m 02.3709s[1]
Declination −06° 05′ 10.5357″[1]
Characteristics
Evolutionary stage Red supergiant, possible extreme red hypergiant[2]
Spectral type ~M6[3]
Apparent magnitude (G) 15.2631±0.0092[1]
Apparent magnitude (J) 7.150[4]
Apparent magnitude (H) 4.698[4]
Apparent magnitude (K) 2.9[4]
Astrometry
Radial velocity (Rv)89[5] km/s
Proper motion (μ) RA: −3.045±0.511[1] mas/yr
Dec.: −5.950±0.480[1] mas/yr
Parallax (π)−0.0081 ± 0.3120[1] mas
Distance18,900[6] ly
(5,800[6] pc)
Details
Radius2,150[7][lower-alpha 1] R☉
Luminosity436,516[7] (90,000[8]–630,000[6][lower-alpha 2]) L☉
Temperature3,200[7] K
Other designations
Stephenson 2-18, Stephenson 2 DFK 1, RSGC2-18, 2MASS J18390238-0605106, IRAS 18363-0607, DENIS J183902.4-060510, MSX6C G026.1044-00.0283
Database references
SIMBADdata

Coordinates: Sky map 18h 39m 02.3709s, −06° 05′ 10.5357″ Stephenson 2-18 (abbreviated to St2-18), also known as Stephenson 2 DFK 1 or RSGC2-18, is a red supergiant (RSG) or possible extreme red hypergiant[2] (RHG) star in the constellation of Scutum. It lies near the open cluster Stephenson 2, which is located about 5.8 kiloparsecs (19,000 light-years) away from Earth in the Scutum–Centaurus Arm of the Milky Way galaxy, and is assumed to be one of a group of stars at a similar distance, although some sources consider it to be an unrelated red supergiant.[5][6] It is among the largest known stars, one of the most luminous red supergiants, and one of the most luminous stars in the Milky Way.

Stephenson 2-18 has an estimated radius of around 2,150 solar radii (1.50×109 kilometres; 10.0 astronomical units), which would correspond to a volume nearly 10 billion times that of the Sun. Taking this estimate as correct, it would take nearly 9 hours to travel around its surface at the speed of light, compared to 14.5 seconds for the Sun.[9] If placed at the center of Earth's Solar System, its photosphere would engulf the orbit of Saturn.

Observation history

Comparison of the sizes of selected different stars. From left to right are Cygnus OB2 #12, V382 Carinae, V915 Scorpii, UY Scuti and Stephenson 2-18. Orbits of Saturn and Neptune are also shown for comparison.

The open cluster Stephenson 2 was discovered by American astronomer Charles Bruce Stephenson in 1990 in the data obtained by a deep infrared survey.[2][10] The cluster is also known as RSGC2, one of several massive open clusters in Scutum, each containing multiple red supergiants.[11]

The brightest star in the region of the cluster was given the identifier 1 in the first analysis of cluster member properties. However, it was not considered to be a member of Stephenson 2 due to its outlying position, abnormally high brightness, and slightly atypical proper motion, being categorized as a unrelated red supergiant.[2]

In a later study, the same star was given the number 18 and assigned to an outlying group of stars called Stephenson 2 SW, assumed to be at a similar distance to the core cluster.[8] The designation St2-18 (short for Stephenson 2-18) is often used for the star, following the numbering from Deguchi (2010).[7][8] To avoid confusion from using the same number for different stars and different numbers for the same star, designations from Davies (2007) are often given a prefix of DFK or D,[11] for example Stephenson 2 DFK 1.[5]

In 2012, Stephenson 2-18, along with 56 other red supergiants, was observed in a study regarding the maser emissions from red supergiants across the galaxy. The study derived the properties of those red supergiants using the Australia Telescope Compact Array (ATCA) and the DUSTY model. Stephenson 2-18 was among the red supergiants mentioned.[7]

That same year, it was observed yet again for a study regarding the types of masers on red supergiant stars in clusters. The study identified Stephenson 2-18 as an unrelated star to Stephenson 2, based on its differing radial velocity.[5] During 2013, in a study regarding the red supergiants in Stephenson 2, Stephenson 2-18 (referred to as D1) was observed and had its spectrum taken, with its spectral type identified.[3] In several later studies, the star was described as being a "very late-type red supergiant".[12][6]

It was also mentioned in Humphreys et al. (2020), albeit mistakenly referred to as RSGC1-01, another large and luminous red supergiant in the constellation of Scutum. The study briefly noted its extreme properties, unusual spectral energy distribution and doubtful membership, and calculated a new estimate of Stephenson 2-18's luminosity.[6]

Distance

When the cluster was originally discovered in 1990, Stephenson 2, and therefore Stephenson 2-18, was originally estimated to have a distance of around 30 kiloparsecs (98,000 light-years), much further than the cluster is thought to reside today.[10] This greater distance was calculated by the assumption that the cluster stars were all M-type supergiants, then calculating the distance modulus based on their typical absolute magnitudes.[2]

In 2001, Nakaya et al. estimated the distance of the stars in the cluster to be 1.5 kiloparsecs (4,900 light-years), which is significantly closer than any other distance estimate given for the star and the cluster.[13][2] Alternatively, a study around a similar timeframe gave a further distance of roughly 5.9 kiloparsecs (19,000 light-years).[14][2]

A study in 2007 determined a kinematic distance of 5.83+1.91
−0.78 kiloparsecs (19000+6200
−2500 light-years) from comparison with the cluster's radial velocity, considerably closer than the original distance of 30 kiloparsecs (98,000 light-years) quoted by Stephenson (1990).[2] However, because of Stephenson 2-18's doubtful membership, its distance was not directly estimated. This value was later adopted in a recent study of the cluster.[6]

A similar kinematic distance of 5.5 kiloparsecs (18,000 light-years) was reported in a 2010 study, derived from the average radial velocity of four of the cluster's members (96 kilometers per second) and from an association with a clump of stars near Stephenson 2, Stephenson 2 SW, locating it near the Scutum–Centaurus Arm of the Milky Way.[8] This value was later adopted in a 2012 study, which used the aforementioned distance to calculate the star's luminosity, however noted that the uncertainty in the distance was greater than 50%. Despite this, it is also stated that distances to massive star clusters will be improved in the future.[7]

Verheyen et al. (2013) used the average radial velocity of the cluster (+109.3 ± 0.7 kilometers per second) to derive a kinematic distance of roughly 6 kiloparsecs (20,000 light-years) for the cluster. However, Stephenson 2-18's radial velocity is calculated to be only 89 kilometers per second and therefore, the study states that the star is a field red supergiant not associated with the cluster.[5]

Physical properties

Evolutionary stage

Australia Telescope Compact Array used to derive Stephenson 2-18's 2012 bolometric luminosity and effective temperature estimates

St2-18 shows the traits and properties of a highly luminous red supergiant, with a spectral type of M6, which is unusual for a supergiant star.[3] This makes it one of the most extreme stars in the Milky Way. It occupies the top right corner of the Hertzsprung–Russell diagram, a region characterized for exceptionally large and luminous low-temperature stars.

Stephenson 2-18 is usually classified as a red supergiant, partly due to its broad line profile.[8][2] However, its significant infrared excess (which suggests a possible extreme mass-losing episode) has led the authors of Davies (2007) to state that the star might be a red hypergiant, like VY Canis Majoris. It is also stated that Stephenson 2-18 is on the brink of ejecting its outer layers and evolving into a luminous blue variable (LBV) or Wolf–Rayet star (WR star).[2]

Luminosity

One calculation for finding the bolometric luminosity by fitting the Spectral Energy Distribution (SED) using the DUSTY model gives the star a luminosity of nearly 440,000 L☉.[7]

An alternate but older calculation from 2010, still assuming membership of the Stephenson 2 cluster at 5.5 kpc but based on 12 and 25 μm flux densities, gives a much lower and relatively modest luminosity of 90,000 L☉.[8]

A newer calculation, based on SED integration (based on published fluxes) and assuming a distance of 5.8 kpc, gives a bolometric luminosity of 630,000 L☉. However, it has been noted that its SED is somewhat peculiar, with fluxes that couldn't fit with the accepted range of appropriate temperatures for an RSG, and fluxes that couldn't fit in a standard reddening law. This would suggest a higher extinction, which would make it be even more luminous. Because of this unusually high luminosity, the star's membership to the Stephenson 2 cluster has been considered doubtful, though it is also stated that it cannot necessarily be ruled out yet.[6][lower-alpha 2] As stated in Negueruela et al. (2012), the stellar association is spread over a large area.[15][6]

Temperature

An effective temperature of 3,200 K was calculated in a 2012 study by SED integration using the DUSTY model,[7] which would make it much cooler than the coolest red supergiants predicted by stellar evolutionary theory (typically around 3,500 K).[16]

Spectral type

Negueruela et al. (2013) identified Stephenson 2-18's spectral type to be around M6, which is unusual for even a red supergiant star, based on its spectrum and some spectral features. The features on Stephenson 2-18's spectrum include titanium oxide (TiO) spectral lines.[3]

Size

Stephenson 2-18 compared to the Sun

A radius of 2,150 R☉ (1.50×109 km; 10.0 astronomical unit|au; 930,000,000 mi) was derived from a bolometric luminosity of nearly 440,000 L☉ and an estimated effective temperature of 3,200 K, which is considerably larger than theoretical models of the largest red supergiants predicted by stellar evolutionary theory (around 1,500 R☉).[16][7] Assuming this value is correct, this would make it larger than other famous red supergiants, such as Antares A, Betelgeuse, VY Canis Majoris and UY Scuti.

Mass loss

Stephenson 2-18 has been estimated to have a mass loss rate of roughly 1.35×10−5 M☉ per year,[7] which is among the highest known for any red supergiant star. It is possible that Stephenson 2-18 underwent an extreme mass loss episode recently, due to its significant infrared excess.[2]

In 2013, an article describing the red supergiants in Stephenson 2 stated that Stephenson 2-18 (referred to as D1) and D2 (another member of Stephenson 2) have maser emissions, indicating that they have the highest mass loss in the cluster. Only the stars with the highest bolometric luminosity in the cluster seem to present maser emissions.[3] Stephenson 2-18 displays strong silicate emission, especially at wavelengths of 10 μm and 18 μm.[8] Water masers were detected in the star as well.[7]

Membership

Stephenson 2-18 seen by Pan-STARRS DR1

It has been debated for a while if this star is actually part of its supposed cluster. Due to its radial velocity being below the other cluster stars but with some spectrum-derived indications showing signs of membership, some sources state that the star is unlikely to be a foreground giant;[2][3] however, more recent papers considered the star an unlikely member due to its extreme and inconsistent properties.[6] Using radial velocities determined from SiO maser emission and IR CO absorption, a study of red supergiant masers in massive clusters considered Stephenson 2-18 as a field red supergiant, unrelated to Stephenson 2 due to its lower radial velocity that is significantly different compared to other stars from Stephenson 2.[5] Unfortunately, Stephenson 2-18's membership cannot be ruled out yet.[6]

Another possibility is that Stephenson 2-18 is actually a member, because its radial velocity is offset by an expanding optically thick envelope. After all, the velocity difference between this star’s radial velocity and Stephenson 2 itself (20 kilometers per second) is a typical outflow speed for red supergiants.[2] Another study says that Stephenson 2-18 is part of a cluster related to Stephenson 2, Stephenson 2 SW, which is assumed to be at the same distance as the core cluster itself and also contains several massive stars and red supergiants.[8]

Uncertainty

The distance of Stephenson 2-18 has been stated to have a relative uncertainty greater than 50%,[7] and the radius of 2,150 R☉ could possibly be an overestimation because the largest stellar radii predicted by stellar evolutionary theory is estimated to only be roughly 1,500 R☉.[16] Luminosity estimates for the star are uncertain as well, as another estimate of the luminosity gave a value of 90,000 L☉.[8]

The star's doubtful membership, uncertain distance and differing radial velocities compared to the rest of the stars in Stephenson 2 have caused some authors to consider the star as a red supergiant unrelated to Stephenson 2 or any of the red supergiant clusters at the base of the Scutum–Centaurus Arm.[5][6]

Evolution

Based on current stellar models and theories on stellar evolution, Stephenson 2-18 is said to be on the edge of shedding its outer layers, in which it will then evolve blueward into a luminous blue variable or a Wolf–Rayet star.[2]

See also

Notes

  1. ↑ Applying the Stefan-Boltzmann law with a nominal solar effective temperature of 5,772 K:
    [math]\displaystyle{ \sqrt{\biggl(\frac{5,772}{3,200}\biggr)^4 \cdot 10^{5.64}} = 2,149.58\ R_\odot }[/math].
  2. ↑ 2.0 2.1 Mistakenly referred to as RSGC1-F01.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.00 2.01 2.02 2.03 2.04 2.05 2.06 2.07 2.08 2.09 2.10 2.11 2.12 2.13 Davies, B.; Figer, D. F.; Kudritzki, R. P.; MacKenty, J.; Najarro, F.; Herrero, A. (2007). "A Massive Cluster of Red Supergiants at the Base of the Scutum‐Crux Arm". The Astrophysical Journal 671 (1): 781–801. doi:10.1086/522224. Bibcode: 2007ApJ...671..781D. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Negueruela, I.; González-Fernández, C.; Dorda, R.; Marco, A.; Clark, J. S. (2013). "The population of M-type supergiants in the starburst cluster Stephenson 2". Eas Publications Series 60: 279. doi:10.1051/eas/1360032. Bibcode: 2013EAS....60..279N. 
  4. ↑ 4.0 4.1 4.2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E. et al. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues 2246: II/246. Bibcode: 2003yCat.2246....0C. http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 Verheyen, L.; Messineo, M.; Menten, K. M. (2012). "SiO maser emission from red supergiants across the Galaxy . I. Targets in massive star clusters". Astronomy & Astrophysics 541: A36. doi:10.1051/0004-6361/201118265. Bibcode: 2012A&A...541A..36V. 
  6. ↑ 6.00 6.01 6.02 6.03 6.04 6.05 6.06 6.07 6.08 6.09 6.10 6.11 Humphreys, Roberta M.; Helmel, Greta; Jones, Terry J.; Gordon, Michael S. (2020). "Exploring the Mass Loss Histories of the Red Supergiants". The Astronomical Journal 160 (3): 145. doi:10.3847/1538-3881/abab15. Bibcode: 2020AJ....160..145H. 
  7. ↑ 7.00 7.01 7.02 7.03 7.04 7.05 7.06 7.07 7.08 7.09 7.10 7.11 Fok, Thomas K. T; Nakashima, Jun-ichi; Yung, Bosco H. K; Hsia, Chih-Hao; Deguchi, Shuji (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal 760 (1): 65. doi:10.1088/0004-637X/760/1/65. Bibcode: 2012ApJ...760...65F. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 8.6 8.7 8.8 Deguchi, Shuji; Nakashima, Jun-Ichi; Zhang, Yong; Chong, Selina S. N.; Koike, Kazutaka; Kwok, Sun (2010). "SiO and H2O Maser Observations of Red Supergiants in Star Clusters Embedded in the Galactic Disk". Publications of the Astronomical Society of Japan 62 (2): 391–407. doi:10.1093/pasj/62.2.391. Bibcode: 2010PASJ...62..391D. 
  9. ↑ "Solar System Exploration: Planets: Sun: Facts & Figures". NASA. http://solarsystem.nasa.gov/planets/profile.cfm?Object=Sun&Display=Facts&System=Metric. 
  10. ↑ 10.0 10.1 Stephenson, C. B. (1990). "A possible new and very remote galactic cluster". The Astronomical Journal 99: 1867. doi:10.1086/115464. Bibcode: 1990AJ.....99.1867S. 
  11. ↑ 11.0 11.1 Negueruela, I.; González-Fernández, C.; Marco, A.; Clark, J. S.; Martínez-Núñez, S. (2010). "Another cluster of red supergiants close to RSGC1". Astronomy and Astrophysics 513: A74. doi:10.1051/0004-6361/200913373. Bibcode: 2010A&A...513A..74N. 
  12. ↑ Negueruela, Ignacio (2016). "Clusters rich in red supergiants". Astronomy in Focus, as presented at the IAU XXIX General Assembly, 2015. 29B: 461-463. doi:10.1017/S1743921316005858. https://ui.adsabs.https://ui.adsabs.harvard.edu/abs/2016IAUFM..29B.461N. Retrieved April 6, 2022. 
  13. ↑ Nakaya, H.; Watanabe, M.; Ando, M.; Nagata, T.; Sato, S. (2001). "A Highly Reddened Star Cluster Embedded in the Galactic Plane". The Astronomical Journal 122: 876-884. doi:10.1086/321178. 
  14. ↑ Ortolani, S.; Bica, E.; Barbuy, B.; Momany, Y. (2002). "The very reddened open clusters Pismis 23 (Lyngå 10) and Stephenson 2". Astronomy and Astrophysics 390: 931-935. doi:10.1051/0004-6361:20020716. Bibcode: 2002A&A...390..931O. 
  15. ↑ Negueruela, I.; Marco, A.; González-Fernández, C.; Jiménez-Esteban, F.; Clark, J. S.; Garcia, M.; Solano, E. (2012). "Red supergiants around the obscured open cluster Stephenson 2". Astronomy & Astrophysics 547: A15. doi:10.1051/0004-6361/201219540. Bibcode: 2012A&A...547A..15N. 
  16. ↑ 16.0 16.1 16.2 Emily M. Levesque; Philip Massey; K. A. G. Olsen; Bertrand Plez et al. (August 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal 628 (2): 973–985. doi:10.1086/430901. Bibcode: 2005ApJ...628..973L. 




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