AZ Cygni (BD+45 3349) is a large red supergiant (M3 Iab) [3] in the constellation of Cygnus. Located 2,090 parsecs (6,800 ly) from Earth, it has been studied by the CHARA array in order to understand the surface variations of red supergiants. [10]
AZ Cygni (BD+45 3349) is a large red supergiant (M3 Iab) [3] in the constellation of Cygnus. Located 2,090 parsecs (6,800 ly) from Earth, it has been studied by the CHARA array in order to understand the surface variations of red supergiants. [10]
AZ Cygni was first observed in the Bonner Durchmusterung catalogue, published by Friedrich Argelander in 1903. [16] It has since then been included in many star surveys and catalogues, including the Two-Micron Sky Survey, [17] 2MASS, [18] Tycho-2 Catalogue [19] and Gaia (DR2 [13] and DR3 [1] ).
From 2011 to 2016, it was observed using the Michigan Infra-Red Combiner (MIRC) at the six-telescope Center for High Angular Resolution Astronomy Array (CHARA array) [10] [12] [4] to investigate the evolution of surface features on red supergiants. These observations were used to derive the fundamental stellar parameters of the star, reconstruct images of the star and test models of 3D radiative hydrodynamics in red supergiants.
| Year of observation | Angular diameter (mas) | Linear radius (R☉) | Estimation used |
|---|---|---|---|
| Norris (2019) [12] | |||
| 2011 | 3.93±0.01 | 856+20 −14 | LDD |
| 2012 | 4.26±0.02 | 927+21 −15 | LDD |
| 2014 | 4.09±0.01 | 890+21 −15 | LDD |
| 2015 | 4.11±0.01 | 895+21 −15 | LDD |
| 2016 | 4.09±0.01 | 890+21 −15 | LDD |
| Norris (2021) [4] | |||
| – | 3.74 | 814+175 −124 | ? |
| Norris et al. (2021) [10] | |||
| 2011 | 3.82±0.01 | 858+56 −49 [lower-alpha 1] | UD |
| 2011 | 3.93±0.01 | 883+57 −51 [lower-alpha 1] | LDD |
| 2014 | 3.81±0.01 | 856+56 −49 [lower-alpha 1] | UD |
| 2014 | 4.09±0.01 | 919+60 −53 [lower-alpha 1] | LDD |
| 2015 | 3.9±0.01 | 876+57 −50 [lower-alpha 1] | UD |
| 2015 | 4.11±0.01 | 924+59 −53 [lower-alpha 1] | LDD |
| 2016 | 3.99±0.01 | 897+57 −52 [lower-alpha 1] | UD |
| 2016 | 4.09±0.01 | 919+60 −53 [lower-alpha 1] | LDD |
| Average (UD) | 3.85±0.01 | 865+56 −50 [lower-alpha 1] | UD |
| Average (LDD) | 4.05±0.01 | 910+59 −52 [lower-alpha 1] | LDD |
| Model | Teff (K) | Surface gravity (log g) | Radius (R☉) | Luminosity (L☉) | Mass (M☉) | Metallicity [Fe/H] (dex) | E(B – V) |
|---|---|---|---|---|---|---|---|
| Norris (2019) [12] | |||||||
| MARCS | 4,000 | 0.5 | 481 | 53,206 | 15 | 0.0 | 0.76 |
| PHOENIX | 4,100 | 0.0 | 642 | 94,614 | 15 | 0.0 | 0.59 |
| SATLAS | 3,867 | 0.36 | 600 | 110,495 | 30 | 0.0 | 0.89 |
| Average | 3,989±117 | 0.29±0.26 | 574±84 | 82,772±35,173 | 20±9 | 0.0±0.0 | 0.75±0.15 |
| Norris et al. (2021) [10] | |||||||
| MARCS | 4,000 | -0.5 | 1,040 | 249,443 | 15 | 0.0 | 0.56 |
| PHOENIX | 4,000 | 0.0 | 641 | 94,759 | 15 | 0.0 | 0.55 |
| SATLAS | 3,972 | -0.07 | 700 | 109,828 | 15 | 0.0 | 0.54 |
The Gaia DR2 catalogue estimated AZ Cygni's absolute bolometric magnitude at −6.4839±0.6427, corresponding to a luminosity of approximately 30,870+13,790
−24,930 L☉. [20] Although the distance is potentially unreliable due to a very high amount of astrometric noise, rated at a significance of 47.4, anything above a rating of 2 is 'probably significant'. [13] [21]
A paper in 2019 calculated the luminosity of AZ Cygni using the Gaia distance and a bolometric magnitude of -7.58, which would result in a luminosity of around 84,700 L☉. [22] Another paper in 2019 estimated three luminosity values of 53,206 L☉, 94,416 L☉ and 110,495 L☉ with an average of 82,772±35,173 L☉. [12] According to a 2021 paper, the best fitting atmosphere models would correspond to luminosities of 249,443 L☉, 94,759 L☉ and 109,828 L☉. [10]
The radius of AZ Cygni was first determined to be around 748 R☉ in a 2019 paper based on the Gaia-derived distance, [22] although it is potentially unreliable due to a high amount of astrometric noise. [13]
By using the angular diameter and Gaia parallax-derived distance in the 2019 Mid-infrared stellar Diameters and Fluxes compilation Catalogue (MDFC), a radius between 913 R☉ and 920 R☉ can be derived. [23] Another paper in 2019 estimated five different radii from observations between 2011 and 2016 based on the MDFC angular diameter and Gaia parallax: 856+20
−14 R☉ (2011), 927+21
−15 R☉ (2012), 890+21
−15 R☉ (2014), 895+21
−15 R☉ (2015) and 890+21
−15 R☉ (2016). The same paper also approximated AZ Cygni's radius based on model spectra, in which three values of 481 R☉, 642 R☉ and 600 R☉ were estimated with an average of 574±84 R☉. [12]
The radius of AZ Cygni was again estimated at 814+175
−124 R☉ based on its angular diameter and Gaia parallax in a 2021 study. [4] A separate paper in 2021 calculated a radius of 911+57
−50 R☉, an average value after using the star's angular diameter and Gaia parallaxes. Based on the best fitting atmosphere models, three different radii were calculated: 1,040 R☉, 641 R☉ and 700 R☉. [10]
In a 1989 paper it was estimated that AZ Cygni would have spectral types of between M2Iab and M4Iab. [6] A study in 2000 estimated that the spectral type of AZ Cygni is M3.1Iab. [24] The spectral type of AZ Cygni was estimated at M3 Iab in a 2002 paper. [3]
A paper in 2004 estimated that the effective temperature of AZ Cygni is 3,200 K with a spectral type of M3 Iab. [5] AZ Cygni had 3 different effective temperature estimates in a paper in 2019 derived from model spectra: 4,000 K, 4,100 K and 3,867 K with an average of 3,989±117 K. [12] In another study in 2021 AZ Cygni would have three effective temperature estimates based on the best fitting atmosphere models: 4,000 K, 4,000 K and 3,972 K and also mentions that it is an M2–4.5 Iab star. [10] The RSG and Close Stars Catalog (2024) features an adopted mean spectral type of M3 for AZ Cygni based on previous spectral types. [25] [26]
The mass of AZ Cygni was first determined based on the best fitting model spectra, which would correspond to three mass estimates: 15 M☉, 15 M☉ and 30 M☉ with an average of 20±9 M☉. [12] A paper in 2021 estimated three mass estimates equal to 15 M☉ based on the best fitting atmosphere models. [10]
AZ Cygni has a complex surface, with large and small features that vary over different timescales. Patterns of large convection cells, varying over periods of more than a year, are combined with smaller hot granules of rising gas that vary over shorter timescales. The size of the larger surface features is in line with models of 3D radiative hydrodynamics in red supergiants. [10]
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