Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Ishihara, Daisuke; Kaneda, Hidehiro; Onaka, Takashi; Ita, Yoshifusa; Matsuura, M.; Matsunaga, Noriyuki

doi:10.1051/0004-6361/201117626

Cited by 42 publications

(64 citation statements)

References 48 publications

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“…However, the JHK colours of mass-losing O-rich stars are very similar to those of C-stars and these will dominate in the higher metallicity Galactic bulge. Ojha et al (2007) have questioned the Cole & Weinberg interpretation of the 2MASS colours and Ishihara et al (2011) show, from a study of stars with both 2MASS and Akari photometry, that the majority of AGB stars in the direction of the Galactic centre are O-rich. This is confirmed by Uttenthaler et al (2015).…”

Section: Mira Variablesmentioning

confidence: 99%

The age and structure of the Galactic bulge from Mira variables

Catchpole¹,

Whitelock²,

Feast³

et al. 2015

Mon. Not. R. Astron. Soc.

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We report periods and JHKL observations for 648 oxygen-rich Mira variables found in two outer bulge fields at b = −7 o and l = ±8 o and combine these with data on 8057 inner bulge Miras from the OGLE, Macho and 2MASS surveys, which are concentrated closer to the Galactic centre. Distance moduli are estimated for all these stars. Evidence is given showing that the bulge structure is a function of age. The longer period Miras (log P > 2.6, age ∼ 5 Gyr and younger) show clear evidence of a bar structure inclined to the line of sight in both the inner and outer regions. The distribution of the shorter period (metal-rich globular cluster age) Miras, appears spheroidal in the outer bulge. In the inner region these old stars are also distributed differently from the younger ones and possibly suggest a more complex structure. These data suggest a distance to the galactic centre R 0 , of 8.9 kpc with an estimated uncertainty of ∼ 0.4 kpc. The possible effect of helium enrichment on our conclusions is discussed.

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Section: Mira Variablesmentioning

confidence: 99%

The age and structure of the Galactic bulge from Mira variables

Catchpole¹,

Whitelock²,

Feast³

et al. 2015

Mon. Not. R. Astron. Soc.

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show abstract

“…The maximum amplitude is used to limit the number of heavily reddened C-rich Miras in our sample, which have on average larger amplitudes than O-rich Miras with the same period range. While C-rich Miras with low reddening track the O-rich Mira PLR, heavily-reddened C-rich Miras fall below the PLR and would bias our fit (Ishihara et al 2011;Whitelock et al 2003). From our simulations, we find that our amplitudes are well-recovered, with the mean amplitude of the input and recovered Miras within a few 0.01 mag of each other.…”

Section: Recovery Of Mira Parametersmentioning

confidence: 97%

Hubble Space Telescope Observations of Mira Variables in the SN Ia Host NGC 1559: An Alternative Candle to Measure the Hubble Constant

Huang

Riess

Yuan

et al. 2020

ApJ

227

181

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We present year-long, near-infrared Hubble Space Telescope WFC3 observations used to search for Mira variables in NGC 1559, the host galaxy of the Type Ia supernova (SN Ia) 2005df. This is the first dedicated search for Miras, highly-evolved low-mass stars in a SN Ia host and subsequently the first calibration of the SN Ia luminosity using Miras in a role historically played by Cepheids. We identify a sample of 115 O-rich Miras with P < 400 day based on their light curve properties. We find that the scatter in the Mira Period-Luminosity Relation (PLR) is comparable to Cepheid PLRs seen in SN Ia supernova host galaxies. Using a sample of O-rich Miras discovered in NGC 4258 with HST F160W and its maser distance, we measure a distance modulus for NGC 1559 of µ 1559 = 31.41 ± 0.050 (statistical) ±0.052 (systematic) mag. Based on the light curve of the normal, well-observed, low-reddening SN 2005df, we obtain a measurement of the fiducial SN Ia absolute magnitude of M 0 B = −19.27 ± 0.13 mag. With the Hubble diagram of SNe Ia we find H 0 = 72.7 ± 4.5 km s −1 Mpc −1 . Combining the calibration from the NGC 4258 megamaser and the Large Magellanic Cloud detached eclipsing binaries gives a best value of H 0 = 73.3 ± 3.9 km s −1 Mpc −1 . This result is within 1σ of the Hubble constant derived using Cepheids and multiple calibrating SNe Ia. This is the first of four expected calibrations of the SN Ia luminosity from Miras which should reduce the error in H 0 via Miras to ∼ 3%. In light of the present Hubble tension and JWST, Miras have utility in the extragalactic distance scale to check Cepheid distances or calibrate nearby SNe in early-type host galaxies that would be unlikely targets for Cepheid searches.

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“…Alternative diagnostics in selecting O-rich and C-rich from photometry have been explored. Ishihara et al (2011) and Matsunaga et al (2017) have used color-color diagrams of J − K s and AKARI colors to select C-rich stars in the Bulge, and have shown this to be an improvement over the use of single 2MASS color. Lebzelter et al (2018) of 2MASS magnitudes defined as…”

Section: Determining Carbon-and Oxygen-rich Typesmentioning

confidence: 99%

Long-period High-amplitude Red Variables in the KELT Survey

Arnold

McSwain

Pepper

et al. 2020

ApJS

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We present a sample of 4,132 Mira-like variables (red variables with long periods and high amplitudes) in the Kilodegree Extremely Little Telescope (KELT) survey. Of these, 814 are new detections. We used 2MASS colors to identify candidate asymptotic giant branch (AGB) stars. We tested for photometric variability among the sample and used Lomb-Scargle to determine the periodicity of the variable sample. We selected variables with high amplitudes and strong periodic behavior using a Random Forest classifier.Of the sample of 4,132 Mira-like variables, we estimate that 70% are Miras, and 30% are semi-regular (SR) variables. We also adopt the method of using (W RP − W Ks ) vs.

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Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Cited by 42 publications

References 48 publications

The age and structure of the Galactic bulge from Mira variables

The age and structure of the Galactic bulge from Mira variables

Hubble Space Telescope Observations of Mira Variables in the SN Ia Host NGC 1559: An Alternative Candle to Measure the Hubble Constant

Long-period High-amplitude Red Variables in the KELT Survey

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