2022A&A...661L...1C


Query : 2022A&A...661L...1C

2022A&A...661L...1C - Astronomy and Astrophysics, volume 661, L1-1 (2022/5-1)

Probing red supergiant dynamics through photo-center displacements measured by Gaia.

CHIAVASSA A., KUDRITZKI R., DAVIES B., FREYTAG B. and DE MINK S.E.

Abstract (from CDS):


Context. Red supergiant (RSGs) are cool massive stars in a late phase of their evolution when the stellar envelope becomes fully convective. They are the brightest stars in the universe at infrared light and can be detected in galaxies far beyond the Local Group, allowing for accurate determination of chemical composition of galaxies. The study of their physical properties is extremely important for various phenomena including the final fate of massive stars as type II supernovae and gravitational wave progenitors.
Aims. We explore the well-studied nearby young stellar cluster χ Per, which contains a relatively large population of RSG stars. Using Gaia EDR3 data, we find the distance of the cluster (d = 2.260 ± 0.020 kpc) from blue main sequence stars and compare with RSG parallax measurements analysing the parallax uncertainties of both groups. We then investigate the variability of the convection-related surface structure as a source for parallax measurement uncertainty.
Methods. We use state-of-the-art three-dimensional radiative hydrodynamics simulations of convection with CO5BOLD and the post-processing radiative transfer code OPTIM3D to compute intensity maps in the GaiaG photometric system. We calculate the variabiltiy, as a function of time, of the intensity-weighted mean (or the photo-center) from the synthetic maps. We then select the RSG stars in the cluster and compare their uncertainty on parallaxes to the predictions of photocentre displacements.
Results. The synthetic maps of RSG show extremely irregular and temporal variable surfaces due to convection-related dynamics. Consequentially, the position of the photo-center varies during Gaia measurements between 0.033 and 0.130 AU (~=1 to ~=5% of the corresponding simulation stellar radius). We argue that the variability of the convection-related surface structures accounts for a substantial part of the Gaia EDR3 parallax error of the RSG sample of χ Per.
Conclusions. We suggest that the variation of the uncertainty on Gaia parallax could be exploited quantitatively using appropriate RHD simulations to extract, in a unique way, important information about the stellar dynamics and parameters of RSG stars.

Abstract Copyright: © A. Chiavassa et al. 2022

Journal keyword(s): stars: atmospheres - astrometry - parallaxes - hydrodynamics - convection

Simbad objects: 42

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Number of rows : 42
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NGC 869 859 * 02 18 49.5437025648 +57 07 18.909925248 10.71 11.080 10.7850   10.3895 B2.0V 23 0
2 NGC 869 869 * 02 18 49.7450665584 +57 06 48.093233256 12.16 12.364 12.071   11.622 B2.0V 21 0
3 V* BU Per LP* 02 18 53.2915355976 +57 25 16.763048652 15.53 12.87 10.40     M4Ib 91 0
4 BD+56 515 Be* 02 18 53.8611376104 +57 08 22.236580968 9.33 9.87 8.5262   8.0645 B2.0V 39 0
5 BD+56 517 * 02 18 55.7271815616 +57 09 06.625290312 10.26 10.77 10.4410   9.6640 B1.5III 40 0
6 NGC 869 963 V* 02 18 57.6823349688 +57 08 17.992912128 10.84 11.320 11.0730     B2V 26 1
7 BD+56 519 * 02 18 58.9757073576 +57 08 42.317905524 9.54 10.00 9.7460     B2.0III 27 0
8 BD+56 518 * 02 18 58.9988006448 +57 09 26.631548388 10.53 10.97 10.6840   9.8608 B2.0III 44 0
9 NGC 869 982 * 02 18 59.0902792560 +57 07 27.743569212   14.332 13.9805 13.90 13.4131 B9 15 0
10 BD+56 520 bC* 02 19 00.2068359360 +57 08 44.320290036 9.71 10.20 10.0010     B1.5IV 26 0
11 BD+56 521 * 02 19 01.7289279528 +57 10 43.146699744 10.73 10.844 10.3051   9.8469 B8V 31 0
12 BD+56 523 * 02 19 04.9811102952 +56 57 31.057209684   10.65 10.5140     B1.5III 15 0
13 NGC 869 1085 * 02 19 06.9682189560 +57 09 04.462023780 10.27 10.766 10.4700     B2.0III 25 0
14 BD+56 526 * 02 19 10.3112286744 +57 07 37.584599556 8.99 9.384 9.0380     B1.0III 32 0
15 BD+56 528 Pu* 02 19 10.6810880568 +57 01 29.855395740   9.99 9.8700   8.6622 B0.5I 19 0
16 BD+56 529 Be* 02 19 13.6735270416 +57 07 43.570965000 10.24 10.59 10.2290   8.6693 B1Ve 40 0
17 NGC 869 1181 * 02 19 15.1494676536 +57 08 12.593592168   13.05 12.6917   12.1583 B3.0V 16 0
18 NGC 869 1187 * 02 19 16.5714069168 +57 10 59.249964180 10.8 11.21 10.8430   10.1438 B1.0V 32 0
19 BD+56 533 * 02 19 26.1704691240 +57 06 52.412750856   10.3 10.3520     B1.0III 12 0
20 HD 14162 Be* 02 19 27.4668283440 +57 08 17.649813192 9.26 9.605 8.4634 9.42 7.8474 B0.5V 54 0
21 HD 14210 ** 02 19 56.1338931384 +57 19 05.147228568   8.48 8.25   7.3179 B9III 25 0
22 V* AD Per s*r 02 20 29.0035384536 +56 59 35.239755912 12.70 10.16 7.8490   7.1111 M3Iab 125 1
23 BD+56 548 Be* 02 20 39.0482294904 +57 18 42.699355092 9.2 9.8 9.811   11.4514 B1.5IIIe 47 0
24 HD 14321 EB* 02 20 52.8798668952 +56 55 32.717424432 8.98 9.52 8.6406   8.0964 B2.0III 46 0
25 V* FZ Per s*r 02 20 59.6455018656 +57 09 29.964294288 12.75 10.20 7.9620   6.7185 M1Iab 112 0
26 HD 14357 bC* 02 21 10.4369424696 +56 51 56.340040320 8.31 8.83 8.4988 8.21 8.0630 B2.0I 74 0
27 BD+56 563 Be* 02 21 43.3997996592 +57 07 32.801871180 9.12 9.77 8.4704   7.9688 B1IIIe 63 0
28 NGC 884 2133 * 02 21 49.1434658088 +57 07 44.717638800 12.944 12.54 12.220   11.806 B3.0III 15 0
29 NGC 884 2139 V* 02 21 49.6554884280 +57 08 21.528438180 11.941 11.65 11.3379   11.0050 B2V 36 0
30 NGC 884 2185 V* 02 21 55.5656144184 +57 05 58.650880308 11.711 11.25 10.9157   10.5988 B2IV 31 0
31 NGC 884 2196 * 02 21 57.6768397848 +57 09 25.701599376 12.177 11.89 11.579   11.149 B2.0III 35 0
32 NGC 884 2232 EB* 02 22 00.8186090784 +57 07 31.992222324 11.500 11.36 11.0850     B3.0V 34 0
33 BD+56 571 Pu* 02 22 00.9422546280 +57 08 14.317119744 9.14 9.69 8.4004   7.9314 B1V 41 0
34 V* SU Per s*r 02 22 06.8948309496 +56 36 14.893650072 13.86 11.57 9.40     M3-M4Iab 142 0
35 NGC 884 OpC 02 22 20 +57 08.9           ~ 473 0
36 V* RS Per s*r 02 22 24.2955658080 +57 06 34.102933812 12.37 10.09 8.7680     M3.5IabFe-1 140 0
37 V* V439 Per s*r 02 23 11.0656487832 +57 11 57.984565452 12.81 10.41 8.1650   6.8612 M0.5Iab 78 0
38 V* V403 Per s*r 02 23 24.1101297168 +57 12 43.045313724 13.32 10.81 8.4020 6.67 5.21 M0Iab 68 0
39 V* V441 Per s*r 02 25 21.8607402192 +57 26 14.130487320 13.07 10.61 8.22 6.09 4.29 M3Iab 79 0
40 * alf Ori s*r 05 55 10.30536 +07 24 25.4304 4.38 2.27 0.42 -1.17 -2.45 M1-M2Ia-Iab 1585 0
41 * alf Sco s*r 16 29 24.45970 -26 25 55.2094 4.08 2.75 0.91 -0.64 -1.87 M1.5Iab+B2Vn 730 0
42 NAME Local Group GrG ~ ~           ~ 7848 0

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2022.12.08-17:42:17

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