Water masers in red supergiants

Pashchenko, M. I.; Rudnitskij, G. M.; Самодуров, В. А.; Толмачев, А. М.

doi:10.1080/10556790601138855

Cited by 4 publications

(2 citation statements)

References 9 publications

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“…We shall note that the intensity of the H 2 O maser line is somewhat weaker than that of three well-known nearby (isolated) RSGs: i.e., VY CMa (1.2 kpc), VX Sgr (1.6 kpc) and NML Cyg (1.6 kpc) exhibit the peak intensities of 199.8 Jy, 167.2 Jy and 18.8 Jy (these flux values are scaled at 3.5 kpc, Pashchenko et al 2006;Choi et al 2008;Zhang et al 2012b), while W 237 and W 26 exhibit 0.72 Jy and 0.73 Jy. Here, we find roughly two order of differences in intensity between the two cases.…”

Section: Results Of the Sio And H 2 O Maser Observationsmentioning

confidence: 88%

Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated With Massive Clusters

Nakashima

Yung

et al. 2012

ApJ

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We report the results of Australia Telescope Compact Array (ATCA) observations of the Westerlund 1 (Wd1) region in the SiO v = 1, J = 1-0 and H 2 O 6 16 -5 23 maser lines, and we also report the analysis of maser properties of red supergiants (RSGs) associated with 6 massive clusters including Wd1. The primary purpose of this research is to explore possibilities of using maser emission for investigating the nature of massive clusters and associated RSGs. The SiO v = 1, J = 1-0 and H 2 O 6 16 -5 23 maser lines are detected toward 2 of 4 known RSGs in Wd1. The large velocity ranges of maser emission are consistent with the RSG status. RSGs with maser emission tend to exhibit redder log(F 21 /F 12 ) and [K-12.13] colors compared to RSGs with no maser emission. The mass-loss rates derived from dust radiative transfer modeling suggest that RSGs with maser emission tend to exhibit larger mass-loss rates compared to RSGs with no maser emission. In an extended sample of 57 RSGs in 6 massive clusters, detections in the SiO line tend to homogeneously distribute in absolute luminosity L, whereas those in the H 2 O line tend to distribute in a region with large L values.

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Section: Results Of the Sio And H 2 O Maser Observationsmentioning

confidence: 88%

Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated With Massive Clusters

Nakashima

Yung

et al. 2012

ApJ

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“…One pertinent example is VY CMa, which has mildly bipolar geometry, with the bulk outflow at 35-40 km/s, but with some faster features up to 70 km/s (Smith 2004;Smith et al 2009a;Decin et al 2016). Another extreme RSG with bipolar geometry seen in water masers is VX Sgr (Berulis et al 1999;Pashchenko et al 2006).…”

Section: Radiative Acceleration or Geometry?mentioning

confidence: 99%

High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation

Smith,

Andrews

2020

Preprint

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SN 2017hcc was remarkable for being a nearby and strongly polarized superluminous Type IIn supernova (SN). We obtained high-resolution echelle spectra that we combine with other spectra to investigate its line profile evolution. All epochs reveal narrow P Cygni components from pre-shock circumstellar material (CSM), indicating an axisymmetric outflow from the progenitor of 40-50 km s −1 . Intermediate-width and broad components exhibit the classic evolution seen in luminous SNe IIn: symmetric Lorentzian profiles from pre-shock CSM lines broadened by electron scattering at early times, transitioning at late times to multi-component, irregular profiles coming from the SN ejecta and post-shock shell. As in many SNe IIn, profiles show a progressively increasing blueshift, with a clear flux deficit in red wings of the intermediate and broad velocity components after day 200. This blueshift develops after the continuum luminosity fades, and in the intermediate-width component, persists at late times even after the SN ejecta fade. In SN 2017hcc, the blueshift cannot be explained as occultation by the SN photosphere, pre-shock acceleration of CSM, or a lopsided explosion or CSM. Instead, the blueshift arises from dust formation in the post-shock shell and in the SN ejecta. The effect has a wavelength dependence characteristic of dust, exhibiting an extinction law consistent with large grains. Thus, SN 2017hcc experienced post-shock dust formation and had a mildly bipolar CSM shell, similar to SN 2010jl. Like other superluminous SNe IIn, the progenitor lost around 10 M ⊙ due to extreme eruptive mass loss in the decade before exploding.

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High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation

Smith

Andrews

2020

Monthly Notices of the Royal Astronomical Society

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SN 2017hcc was remarkable for being a nearby and strongly polarized superluminous Type IIn supernova (SN). We obtained high-resolution echelle spectra that we combine with other spectra to investigate its line profile evolution. All epochs reveal narrow P Cygni components from pre-shock circumstellar material (CSM), indicating an axisymmetric outflow from the progenitor of 40-50 km s−1. Intermediate-width and broad components exhibit the classic evolution seen in luminous SNe IIn: symmetric Lorentzian profiles from pre-shock CSM lines broadened by electron scattering at early times, transitioning at late times to multi-component, irregular profiles coming from the SN ejecta and post-shock shell. As in many SNe IIn, profiles show a progressively increasing blueshift, with a clear flux deficit in red wings of the intermediate and broad velocity components after day 200. This blueshift develops after the continuum luminosity fades, and in the intermediate-width component, persists at late times even after the SN ejecta fade. In SN 2017hcc, the blueshift cannot be explained as occultation by the SN photosphere, pre-shock acceleration of CSM, or a lopsided explosion or CSM. Instead, the blueshift arises from dust formation in the post-shock shell and in the SN ejecta. The effect has a wavelength dependence characteristic of dust, exhibiting an extinction law consistent with large grains. Thus, SN 2017hcc experienced post-shock dust formation and had a mildly bipolar CSM shell, similar to SN 2010jl. Like other superluminous SNe IIn, the progenitor lost around 10 M⊙ due to extreme eruptive mass loss in the decade before exploding.

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Water masers in red supergiants

Cited by 4 publications

References 9 publications

Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated With Massive Clusters

Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated With Massive Clusters

High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation

High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation

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