The Period–Luminosity Relations of Red Supergiants in M33 and M31

Ren, Yi; Jiang, Biwei; Yang, Ming; Jian, Gao

doi:10.3847/1538-4365/ab0825

Cited by 36 publications

(51 citation statements)

References 68 publications

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“…It is clear that pulsations following a P-L relation are present in most RSGs in the Local Group and that this relation does not depend on the metallicity (Ren et al 2019). In order to consider RSGs "standard candles" (as suggested by Glass 1979), factors like the abundance of irregular variables, mass loss, dust production and the additional sources of long-period variability need to be further explored.…”

Section: Discussionmentioning

confidence: 99%

“…The agreement between the lines and our results is evident. Soraisam et al (2018) found that RSG P-L relation is consistent between the LMC, SMC, Galactic RSGs and the M33 (Yang & Jiang 2011, Yang & Jiang 2012and Soraisam et al 2018, despite the range of metallicities (Ren et al 2019). 0 0.001 0.002 0.003 0.004 0.005 0.006 0.007 0.008 0.009 0.01…”

Section: Red Supergiants In the Lmcmentioning

confidence: 91%

See 1 more Smart Citation

The period–luminosity relation of red supergiants with Gaia DR2

Chatys

Bedding

Murphy

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We revisit the K -band period-luminosity (P-L) relations of Galactic red supergiants using Gaia Data Release 2 parallaxes and up to 70 yr of photometry from AAVSO and ASAS campaigns. In addition, we examine 206 LMC red supergiants using 50 yr of photometric data from the Digitised Harvard Astronomical Plate Collection. We identified periods by computing power spectra and calculated the period-luminosity relations of our samples and compared them with the literature. Newly available data tighten the P-L relations substantially. Identified periods form two groups: one with periods of 300-1000 days, corresponding to pulsations, and another with Long Secondary Periods between 1000 and 8000 days. Among the 48 Galactic objects we find shorter periods in 25 stars and long secondary periods in 23 stars. In the LMC sample we identify 85 and 94 red supergiants with shorter and long secondary periods, respectively. The P-L relation of the Galactic red supergiants is in agreement with the red supergiants in both, the Large Magellanic Cloud and the Andromeda Galaxy. We find no clear continuity between the known red giant period-luminosity sequences, and the red supergiant sequences investigated here.

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Section: Discussionmentioning

confidence: 99%

Section: Red Supergiants In the Lmcmentioning

confidence: 91%

The period–luminosity relation of red supergiants with Gaia DR2

Chatys

Bedding

Murphy

et al. 2019

Monthly Notices of the Royal Astronomical Society

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show abstract

“…The regions of each type of evolved massive star are outlined by the dashed lines with color and magnitude criteria listed in Table 4. Due to the relatively large MLR during the RSG phase, the star could be heavily obscured by the surrounding dust envelope (Smith et al 2001;Massey et al 2005;Levesque et al 2006;Yang et al 2018;Ren et al 2019). Therefore, we also empirically extended the RSG region from the reddest and faintest points of the models to the even redder but not fainter area in order to avoid the contamination from extreme AGBs (x-AGB stars are most likely experiencing a "superwind", where the MLR can increase by a factor of ten, and a thick dust envelope obscures the star at optical wavelengths; van Loon et al 2006;Boyer et al 2011) as shown in the diagrams.…”

Section: Multiwavelength Time-series Datamentioning

confidence: 99%

Evolved massive stars at low-metallicity

Yang

Bonanos

Jiang

et al. 2019

A&A

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We present a clean, magnitude-limited (IRAC1 or WISE1 ≤ 15.0 mag) multiwavelength source catalog for the Small Magellanic Cloud (SMC) with 45 466 targets in total, with the purpose of building an anchor for future studies, especially for the massive star populations at low-metallicity. The catalog contains data in 50 different bands including 21 optical and 29 infrared bands, retrieved from SEIP, VMC, IRSF, AKARI, HERITAGE, Gaia, SkyMapper, NSC, Massey (2002, ApJS, 141, 81), and GALEX, ranging from the ultraviolet to the far-infrared. Additionally, radial velocities and spectral classifications were collected from the literature, and infrared and optical variability statistics were retrieved from WISE, SAGE-Var, VMC, IRSF, Gaia, NSC, and OGLE. The catalog was essentially built upon a 1″ crossmatching and a 3″ deblending between the Spitzer Enhanced Imaging Products (SEIP) source list and Gaia Data Release 2 (DR2) photometric data. Further constraints on the proper motions and parallaxes from Gaia DR2 allowed us to remove the foreground contamination. We estimate that about 99.5% of the targets in our catalog are most likely genuine members of the SMC. Using the evolutionary tracks and synthetic photometry from MESA Isochrones & Stellar Tracks and the theoretical J − KS color cuts, we identified 1405 red supergiant (RSG), 217 yellow supergiant, and 1369 blue supergiant candidates in the SMC in five different color-magnitude diagrams (CMDs), where attention should also be paid to the incompleteness of our sample. We ranked the candidates based on the intersection of different CMDs. A comparison between the models and observational data shows that the lower limit of initial mass for the RSG population may be as low as 7 or even 6 M⊙ and that the RSG is well separated from the asymptotic giant branch (AGB) population even at faint magnitude, making RSGs a unique population connecting the evolved massive and intermediate stars, since stars with initial mass around 6 to 8 M⊙ are thought to go through a second dredge-up to become AGB stars. We encourage the interested reader to further exploit the potential of our catalog.

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“…Targets without errors are not shown in the CMDs, while the average photometric uncertainties are indicated when available. Due to the relatively large MLR during the RSGs phase, the star could be heavily obscured by the surrounding dust envelope (Smith et al 2001;Massey et al 2005;Levesque et al 2006;Yang et al 2018;Ren et al 2019). Thus, we also empirically extended the RSGs region from the reddest and faintest points of the models to the even redder but not fainter area, in order to avoid the contamination from extreme AGBs (x-AGBs, stars are most likely to be experiencing a "superwind", where the mass-loss rate can increase by a factor of 10, and a thick dust envelope obscures the star at optical wavelengths; van Loon et al 2006;Boyer et al 2011) as shown in the diagrams.…”

Section: Identifying Evolved Massive Star Candidates On the Color-mag...mentioning

confidence: 99%

Evolved Massive Stars at Low-metallicity I. A Source Catalog for the Small Magellanic Cloud

Yang,

Bonanos,

Jiang

et al. 2019

Preprint

Self Cite

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We present a clean, magnitude-limited (IRAC1 or WISE1 ≤ 15.0 mag) multiwavelength source catalog for the Small Magellanic Cloud (SMC) with 45,466 targets in total, with the purpose of building an anchor for future studies, especially for the massive star populations at low-metallicity. The catalog contains data in 50 different bands including 21 optical and 29 infrared bands, retrieved from SEIP, VMC, IRSF, AKARI, HERITAGE, Gaia, SkyMapper, NSC, Massey et al. (2002), and GALEX, ranging from the ultraviolet to the far-infrared. Additionally, radial velocities and spectral classifications were collected from the literature, as well as infrared and optical variability statistics were retrieved from WISE, SAGE-Var, VMC, IRSF, Gaia, NSC, and OGLE. The catalog was essentially built upon a 1 crossmatching and a 3 deblending between the Spitzer Enhanced Imaging Products (SEIP) source list and Gaia Data Release 2 (DR2) photometric data. Further constraints on the proper motions and parallaxes from Gaia DR2 allowed us to remove the foreground contamination. We estimated that about 99.5% of the targets in our catalog were most likely genuine members of the SMC. By using the evolutionary tracks and synthetic photometry from MESA Isochrones & Stellar Tracks and the theoretical J − K S color cuts, we identified 1,405 red supergiant, 217 yellow supergiant and 1,369 blue supergiant candidates in the SMC in five different color-magnitude diagrams (CMDs), where attention should also be paid to the incompleteness of our sample. We ranked the candidates based on the intersection of different CMDs. A comparison between the models and observational data shows that the lower limit of initial mass for the RSGs population may be as low as 7 or even 6 M and the RSG is well separated from the AGB population even at faint magnitude, making RSGs a unique population connecting the evolved massive and intermediate stars, since stars with initial mass around 6 to 8 M are thought to go through a second dredge-up to become asymptotic giant branch stars. We encourage the interested reader to further exploit the potential of our catalog.

show abstract

The Period–Luminosity Relations of Red Supergiants in M33 and M31

Cited by 36 publications

References 68 publications

The period–luminosity relation of red supergiants with Gaia DR2

The period–luminosity relation of red supergiants with Gaia DR2

Evolved massive stars at low-metallicity

Evolved Massive Stars at Low-metallicity I. A Source Catalog for the Small Magellanic Cloud

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