2010A&A...520A..48R


Query : 2010A&A...520A..48R

2010A&A...520A..48R - Astronomy and Astrophysics, volume 520, A48-48 (2010/9-2)

A VLT/FLAMES survey for massive binaries in Westerlund 1. II. Dynamical constraints on magnetar progenitor masses from the eclipsing binary W13.

RITCHIE B.W., CLARK J.S., NEGUERUELA I. and LANGER N.

Abstract (from CDS):

Westerlund 1 is a young, massive Galactic starburst cluster that contains a rich coeval population of Wolf-Rayet stars, hot- and cool-phase transitional supergiants, and a magnetar. We use spectroscopic and photometric observations of the eclipsing double-lined binary W13 to derive dynamical masses for the two components, in order to determine limits for the progenitor masses of the magnetar CXOU J164710.2-455216 and the population of evolved stars in Wd1. We use eleven epochs of high-resolution VLT/FLAMES spectroscopy to construct a radial velocity curve for W13. R-band photometry is used to constrain the inclination of the system. W13 has an orbital period of 9.2709±0.0015 days and near-contact configuration. The shallow photometric eclipse rules out an inclination greater than 65°, leading to lower limits for the masses of the emission-line optical primary and supergiant optical secondary of 21.4±2.6M and 32.8±4.0M respectively, rising to 23.2+3.3–3.0M and 35.4+5.0–4.6M for our best-fit inclination 62+3–4 degrees. Comparison with theoretical models of Wolf-Rayet binary evolution suggest the emission-line object had an initial mass in excess of ∼35M, with the most likely model featuring highly non-conservative late-Case A/Case B mass transfer and an initial mass in excess of 40M. This result confirms the high progenitor mass of the magnetar CXOU J164710.2-455216 inferred from its membership in Wd1, and represents the first dynamical constraint on the progenitor mass of any magnetar. The red supergiants in Wd1 must have similar progenitor masses to W13 and are therefore amongst the most massive stars to undergo a red supergiant phase, representing a challenge for population models that suggest stars in this mass range end their redwards evolution as yellow hypergiants.

Abstract Copyright:

Journal keyword(s): stars: evolution - supergiants - stars: individual: W13 - stars: magnetars - binaries: general

CDS comments: In ref list Bibby et al. 2008, MNRAS, 385, 544 is a misprint for Bibby et al. 2008, MNRAS, 386, L23.

Simbad objects: 30

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Number of rows : 30
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 [HS53] A s*y 01 32 32.8025598888 +30 30 25.003726668 20.1 19.9 19.1 18.6 17.7 F8Ia 52 0
2 HD 269858 s*b 05 36 43.6936418088 -69 29 47.451149232   10.24 10.15 9.95 9.05 LBV 276 2
3 HD 90657 WR* 10 26 31.4087563344 -58 38 26.182481568 9.53 10.07 9.65 9.84   WN5+O4-6 156 0
4 2E 2336 HXB 10 50 08.93 -59 53 19.9           Be 394 0
5 V* BP Cru HXB 12 26 37.5605188992 -62 46 13.261044684   12.70 10.66     B1.5Iaeq 635 0
6 HD 149404 s*b 16 36 22.5628499784 -42 51 31.902127776 5.23 5.88 5.52 6.90   O8.5Iab(f)p 237 1
7 Cl* Westerlund 1 BKS H * 16 47 01.4269856784 -45 50 37.248841536   18.781 14.47     F3Ia+ 26 0
8 WR 77f WR* 16 47 02.9772955944 -45 50 19.713734556   21.552 17.792 15.035 12.508 WN10-11h 29 0
9 Cl* Westerlund 1 W 42 * 16 47 03.2521856424 -45 50 52.195013052         10.764 B9Ia+ 16 0
10 Cl* Westerlund 1 W 43 * 16 47 03.56 -45 50 57.6   22.8 18.05 15.378 12.647 O9.5B0.5Ia 15 0
11 Hen 3-1250 Em* 16 47 03.6281794392 -45 50 14.365482036   20.0 15.972     B5Ia+ 25 0
12 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 507 0
13 Cl* Westerlund 1 W 33 * 16 47 04.1256274968 -45 50 48.488202564   20.090 15.61 12.803   B5Ia+ 20 0
14 WR 77k WR* 16 47 04.2072122904 -45 51 07.177760892   22.6 18.86 15.61 12.52 WN7 24 0
15 2MASS J16470540-4550367 LP? 16 47 05.4076906176 -45 50 36.617071668   22.1 16.79     M5-6Ia 32 0
16 Cl* Westerlund 1 W 265 * 16 47 06.2785465416 -45 49 23.774098692   22.0 17.739   10.54 F1-5Ia+ 22 0
17 Cl* Westerlund 1 W 13 EB* 16 47 06.4540771320 -45 50 26.072579796   21.1 17.19 14.63 12.06 BIa+ 31 0
18 Cl* Westerlund 1 W 16 * 16 47 06.6158603112 -45 50 42.186706944   20.5 16.248     A5Ia+ 25 0
19 Cl* Westerlund 1 W 15 * 16 47 06.6306037464 -45 50 29.723762580   22.8 18.96 16.38 13.75 O9.2Ia 24 0
20 Cl* Westerlund 1 W 243 s*b 16 47 07.5040736160 -45 52 29.123491188   19.873 15.730     LBV 56 0
21 PSR J1647-4552 Psr 16 47 10.18 -45 52 16.7           ~ 189 1
22 Cl* Westerlund 1 W 3003 V* 16 47 11.6073210840 -45 49 22.478619972       16.211 13.314 B0Ib 7 0
23 HD 153919 HXB 17 03 56.7725629224 -37 50 38.913331452 6.06 6.78 6.51 6.08 5.90 O6Iafcp 781 1
24 NAME 1806-20 Star Cluster OpC 18 08 39.0 -20 24 39           ~ 33 1
25 PSR J1808-2024 Psr 18 08 39.32 -20 24 40.1           ~ 1172 2
26 W 26 Rad 18 10 -08.8           ~ 6 0
27 GBS 1900+14 gB 19 07 13 +09 19.6           ~ 817 0
28 IRC +10420 pA* 19 26 48.0979492536 +11 21 16.758531216   13.98 11.66     F8Ia+e 463 0
29 HD 228766 WR* 20 17 29.7041883216 +37 18 31.128288048 9.42 9.79 9.14     O4If+O8:II: 112 0
30 BD+40 4220 SB* 20 32 22.4238075360 +41 18 18.942475932 11.32 10.79 9.185     O6.5:Iafe 383 0

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2022.05.25-22:37:11

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