Red Supergiant Stars in the Large Magellanic Cloud. I. The Period-Luminosity Relation

Yang, Ming; Jiang, Biwei

doi:10.1088/0004-637x/727/1/53

Cited by 53 publications

(71 citation statements)

References 65 publications

(128 reference statements)

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“…Kiss et al (2006) and Percy & Khatu (2014) identified periods of a few hundred to a few thousand days with varying stellar lightcurve morphology for RSGs in the AAVSO International Database. Such pulsations have also been observed occurring in RSGs within the Small and Large Magellanic Clouds (Feast et al 1980;Ita et al 2004;Szczygie l et al 2010;Yang & Jiang 2011;Yang & Jiang 2012;Yang et al 2018), M31 and M33 (Soraisam et al 2018;Ren et al 2019), M51 (Conroy et al 2018), M101 (Jurcevic et al 2000), within HST archival data of NGC 1326A, NGC 1425, and NGC 4548 (Spetsieri et al 2019), and within the GAIA DR2 RSG sample (Chatys et al 2019). These works identify these RSG pulsations Corresponding author: J.…”

Section: Introductionmentioning

confidence: 69%

A Massive Star’s Dying Breaths: Pulsating Red Supergiants and Their Resulting Type IIP Supernovae

Goldberg

Bildsten

Paxton

2020

ApJ

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Massive stars undergo fundamental-mode and first-overtone radial pulsations with periods of 100-1000 days as Red Supergiants (RSGs). At large amplitudes, these pulsations substantially modify the outer envelope's density structure encountered by the outgoing shock wave from the eventual core collapse of these M > 9M stars. Using Modules for Experiments in Stellar Astrophysics (MESA), we model the effects of fundamental-mode and first-overtone pulsations in the RSG envelopes, and the resulting Type IIP supernovae (SNe) using MESA+STELLA. We find that, in the case of fundamental mode pulsations, SN plateau observables such as the luminosity at day 50, L 50 , time-integrated shock energy ET , and plateau duration t p are consistent with radial scalings derived considering explosions of non-pulsating stars. Namely, most of the effect of the pulsation is consistent with the behavior expected for a star of a different size at the time of explosion. However, in the case of overtone pulsations, the Lagrangian displacement is not monotonic. Therefore, in such cases, excessively bright or faint SN emission at different times reflects the underdense or overdense structure of the emitting region near the SN photosphere.

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Section: Introductionmentioning

confidence: 69%

A Massive Star’s Dying Breaths: Pulsating Red Supergiants and Their Resulting Type IIP Supernovae

Goldberg

Bildsten

Paxton

2020

ApJ

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“…To explore the relation between photometric and spectral variations in both MCs, we have used the works of Yang & Jiang (2011, 2012. They studied the photometric variability of a large number of RSGs taken mainly from the same source as our sample (Massey 2003).…”

Section: Spectral Variabilitymentioning

confidence: 99%

Spectral type, temperature, and evolutionary stage in cool supergiants

Dorda

Negueruela

González-Fernández

et al. 2016

A&A

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Context. In recent years, our understanding of red supergiants has been questioned by strong disagreements between stellar atmospheric parameters derived with different techniques. Temperature scales have been disputed, and the possibility that spectral types do not depend primarily on temperature has been raised. Aims. We explore the relations between different observed parameters, and we explore the ability to derive accurate intrinsic stellar parameters from these relations through the analysis of the largest spectroscopic sample of red supergiants to date. Methods. We obtained intermediate-resolution spectra of a sample of about 500 red supergiants in the Large and the Small Magellanic Cloud. From these spectra, we derive spectral types and measure a large set of photospheric atomic lines. We explore possible correlations between different observational parameters, also making use of near-and mid-infrared colours and literature on photometric variability.Results. Direct comparison between the behaviour of atomic lines (Fe i, Ti i, and Ca ii) in the observed spectra and a comprehensive set of synthetic atmospheric models provides compelling evidence that effective temperature is the prime underlying variable driving the spectral-type sequence between early G and M2 for supergiants. In spite of this, there is a clear correlation between spectral type and luminosity, with later spectral types tending to correspond to more luminous stars with heavier mass loss. This trend is much more marked in the LMC than in the SMC. The population of red supergiants in the SMC is characterised by a higher degree of spectral variability, early spectral types (centred on type K1) and low mass-loss rates (as measured by dust-sensitive mid-infrared colours). The population in the LMC displays less spectroscopic variability and later spectral types. The distribution of spectral types is not single-peaked. Instead, the brightest supergiants have a significantly different distribution from less luminous objects, presenting mostly M subtypes (centred on M2), and increasing mass-loss rates for later types. In this regard, the behaviour of red supergiants in the LMC is not very different from that of Milky Way objects. Conclusions. The observed properties of red supergiants in the SMC and the LMC cannot be described correctly by standard evolutionary models. The very strong correlation between spectral type and bolometric luminosity, supported by all data from the Milky Way, cannot be reproduced at all by current evolutionary tracks.

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“…HII regions can be isolated by their much redder K s −A colors, while measurements in the four IRAC bands distinguish between RSGs, O-rich and C-rich AGBs. Yang & Jiang (2011) revised the pulsation properties of RSGs in the LMC using a comprehensive list of 191 RSGs (Buchanan et al 2009). Only 24% of RSGs show regular pulsation (Yang & Jiang 2011 So far, little work has been done on Galactic evolved stars based on GLIMPSE data.…”

Section: Introductionmentioning

confidence: 99%

“…Yang & Jiang (2011) revised the pulsation properties of RSGs in the LMC using a comprehensive list of 191 RSGs (Buchanan et al 2009). Only 24% of RSGs show regular pulsation (Yang & Jiang 2011 So far, little work has been done on Galactic evolved stars based on GLIMPSE data. WRs have an infrared excess, due to free-free emission from dense stellar winds (Cohen et al 1975).…”

Section: Introductionmentioning

confidence: 99%

Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

Messineo

Menten

Churchwell

et al. 2011

A&A

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Context. Mass-loss from evolved stars chemically enriches the interstellar medium (ISM). Stellar winds from massive stars and their explosions as supernovae shape the ISM and trigger star formation. Studying evolved stars is fundamental for understanding galaxy formation and evolution at any redshift. Aims. We aim to establish a photometric classification scheme for Galactic mass-losing evolved stars (e.g., WR, RSG, and AGB stars) with the goal of identifying new ones, and subsequently to use these samples as tracers of Galactic structure. Methods. We searched for counterparts of known Galactic WR, LBV, RSG, and O-rich AGB stars in the 2MASS, GLIMPSE, and MSX catalogs, and we analyzed their properties with near-and mid-infrared color-color diagrams. Results. We used the Q1 parameter, which is a measure of the deviation from the interstellar reddening vector in the J − H versus H−K s diagram, and we defined a new parameter, Q2, which is a measure of the deviation from the interstellar reddening vector in the Conclusions. The GLIMPSE catalog is a powerful tool for photometric classification of Galactic mass-losing evolved stars. Our new criteria will yield many new RSGs and WRs.

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Red Supergiant Stars in the Large Magellanic Cloud. I. The Period-Luminosity Relation

Cited by 53 publications

References 65 publications

A Massive Star’s Dying Breaths: Pulsating Red Supergiants and Their Resulting Type IIP Supernovae

A Massive Star’s Dying Breaths: Pulsating Red Supergiants and Their Resulting Type IIP Supernovae

Spectral type, temperature, and evolutionary stage in cool supergiants

Near- and mid-infrared colors of evolved stars in the Galactic plane. TheQ1 andQ2 parameters

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