The spectrum of the Antares nebula

Swings, J. P.; Preston, George W.

doi:10.1086/155977

Cited by 9 publications

(12 citation statements)

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“…The 24.52 µm line of α Sco shown in Figure 7 is slightly wider than for the other stars (see Table 3), however we find no indication of extended emission. The Antares nebulae is a -16source of rich optical Fe II emission, e.g., Swings & Preston (1978), which is excited by the nearby B star companion (separation of 2.7 ′′ ) (Reimers et al 2008). TEXES observations of this system may be sampling material from a slightly more extended, but still spatially unresolved, region than for the single stars, and this material may have different velocity fields.…”

Section: Detectionsmentioning

confidence: 99%

Texes Observations of M Supergiants: Dynamics and Thermodynamics of Wind Acceleration

Harper

Richter

Ryde³

et al. 2009

ApJ

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We have detected [Fe II] 17.94 µm and 24.52 µm emission from a sample of M supergiants (µ Cep, α Sco, α Ori, CE Tau, AD Per, and α Her) using the Texas Echelon Cross Echelle Spectrograph on NASA's Infrared Telescope Facility. These low opacity emission lines are resolved at R ≃ 50, 000 and provide new diagnostics of the dynamics and thermodynamics of the stellar wind acceleration zone. The [Fe II] lines, from the first excited term (a 4 F ), are sensitive to the warm plasma where energy is deposited into the extended atmosphere to form the chromosphere and wind outflow. These diagnostics complement previous Kuiper Airborne Observatory and Infrared Satellite Observatory observations which were sensitive to the cooler and more extended circumstellar envelopes. The turbulent velocities of V turb ≃ 12 − 13 km s −1 observed in the [Fe II] a 4 F forbidden lines are found to be a common property of our sample, and are less than that derived from the hotter chromospheric C II] 2325Å lines observed in α Ori, where V turb ≃ 17−19km s −1 . For the first time, we have dynamically resolved the motions of the dominant cool atmospheric component discovered in α Ori from multi-wavelength radio interferometry by Lim et al. (1998). Surprisingly, the emission centroids are quite Gaussian and at rest with respect to the M supergiants. These constraints combined with model calculations of the infrared emission line fluxes for α Ori imply that the warm material has a low outflow velocity and is located close to the star. We have also detected narrow [Fe I] 24.04 µm emission that confirms that Fe II is the dominant ionization state in α Ori's extended atmosphere.

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Section: Detectionsmentioning

confidence: 99%

Texes Observations of M Supergiants: Dynamics and Thermodynamics of Wind Acceleration

Harper

Richter

Ryde³

et al. 2009

ApJ

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“…Antares (α Sco A, M 1.5 Iab) and its blue visual companion α Sco B (B 2.5 V) are known to be surrounded by a circumstellar envelope seen in absorption in both components which can be used to determine the mass-loss rate of the M supergiant (Deutsch 1960;Kudritzki & Reimers 1978;Hagen et al 1987;Baade & Reimers 2007). The common envelope has also been known for a long time as an emission nebula with strong [Fe ii] lines (Wilson & Sanford 1937;Struve & Swings 1940;Swings & Preston 1978). The most extensive study was that by Swings & Preston (1978) based on high-resolution long-slit photographic Coudé spectra taken with the Mount Wilson 100 inch and Palomar 200 inch telescopes.…”

Section: Introductionmentioning

confidence: 99%

“…The common envelope has also been known for a long time as an emission nebula with strong [Fe ii] lines (Wilson & Sanford 1937;Struve & Swings 1940;Swings & Preston 1978). The most extensive study was that by Swings & Preston (1978) based on high-resolution long-slit photographic Coudé spectra taken with the Mount Wilson 100 inch and Palomar 200 inch telescopes. They found that the "[Fe ii]-rich nebula" is strong roughly 3.…”

Section: Introductionmentioning

confidence: 99%

The Antares emission nebula and mass loss of $\sf \alpha$ Scorpii A

Reimers

Hagen

Baade

et al. 2008

A&A

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Aims. The Antares nebula is a peculiar emission nebula seen in numerous [Fe ii] lines and in radio free-free emission, probably associated with the H ii region caused by α Sco B in the wind of α Sco A. High-resolution spectra with spatial resolution were used to study the emission line spectrum, the physical nature of the nebula and to determine the mass-loss rate of the M supergiant α Sco A. Methods. The Antares nebula was mapped with long-slit (10 ) and high-resolution (R = 80 000) spectra using UVES at the VLT. The resulting 2-D images were used to reconstruct a 3-D picture of the H ii region and its absolute location in space relative to α Sco A. Results. We found that the Antares nebula shows, in addition to numerous [Fe ii] lines, the Balmer line recombination spectrum H α , H β up to H 10 , and [N ii] 6583/6548 Å, H α and [N ii] with the same extent as seen in cm radio free-free emission. Combining velocity information from optical and GHRS/HST spectra with H α velocities, the H ii region is found to be located ∼215 AU behind the plane of the sky of α Sco A. From the H α /[N ii] intensity ratio and the non-visibility of the [O ii] 3726/3729 Å lines we estimate a low mean electron temperature of T e = 4900 K and an N abundance enhanced by a factor of ∼3 due to the CNO cycle in α Sco A. The shape and size of the H ii region yield a mean mass-loss rate of (1.05 ± 0.3) × 10 −6 M yr −1 . The [Fe ii] lines originate predominantly at the edges (rear and front) of the H ii region. UV continuum pumping as well as collisional excitation seem to be responsible for the observed iron lines.

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“…The companion was classified as B3 one century ago (Adams & Joy 1921), and subsequent authors classified it as B4 V (Stone & Struve 1954), B2.5 V (Garrison 1967), and B3 V (Corbally 1984 reflect real spectral variations, but are rather a consequence of the difficulty that exists in eliminating the light from the much brighter primary less than 3 away. The B star has not received much attention in the past decades other than the study of its associated emission nebula, which is rich in [Fe ii] lines (Swings & Preston 1978;Reimers et al 2008). The magnitude difference between the two components is highly dependent on the band used (see below), as is expected for a pair composed of a red and a blue star (this pair is a favourite object among amateur astronomers who wish to separate visual binaries of extreme colors and small separations, the first author still remembers his excite-ment when he was able to separate Antares through an eyepiece for the first time 34 years ago).…”

Section: α Sco Ab the Nearest Rsg+b Systemmentioning

confidence: 99%

Lucky spectroscopy, an equivalent technique to lucky imaging

Apellániz

Barbá

Fariña

et al. 2021

A&A

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Context. Many massive stars have nearby companions. These hamper a characterization of massive stars through spectroscopy. Aims. We continue to obtain spatially resolved spectroscopy of close massive visual binaries to derive their spectral types. Methods. We used the lucky spectroscopy technique to obtain a large number of short long-slit spectroscopic exposures of 19 close visual binaries under good seeing conditions. We selected those with the best characteristics, extracted the spectra using multipleprofile fitting, and combined the results to derive spatially separated spectra. The results were analyzed in combination with data from lucky imaging, regular intermediate-resolution single-order spectroscopy, andéchelle high-resolution spectroscopy. Results. The new application of lucky spectroscopy has allowed us (among other results) to [a] spatially disentangle two O stars (FN CMa B and 6 Cas B) with brighter BA supergiant companions for the first time; [b] determine that two B stars (α Sco B and HD 164 492 B) with close and more massive companions are fast rotators (in the second case, solving a case of mistaken identity); [c] extend the technique to cases with extreme magnitude differences (the previous two cases plus CS Cam A,B), shorter separations (HD 193 443 A,B), and fainter primary magnitudes down to B = 11 (HD 219 460 A,B); [d] spatially disentangle the spectra of stars with companions as diverse as an A supergiant (6 Cas A), a Wolf-Rayet star (HD 219 460 B = WR 157), and an M supergiant (α Sco A); [e] discover the unexpected identity of some targets such as two previously unknown bright O stars (HD 51 756 B and BD +60 544) and a new member of the rare OC category (HD 8768 A); and [f] identify and classify (in some cases for the first time) which of the components of four visual binaries (

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The spectrum of the Antares nebula

Cited by 9 publications

References 0 publications

Texes Observations of M Supergiants: Dynamics and Thermodynamics of Wind Acceleration

Texes Observations of M Supergiants: Dynamics and Thermodynamics of Wind Acceleration

The Antares emission nebula and mass loss of $\sf \alpha$ Scorpii A

Lucky spectroscopy, an equivalent technique to lucky imaging

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