2009AJ....137.3558S


C.D.S. - SIMBAD4 rel 1.7 - 2020.03.31CEST15:57:08

2009AJ....137.3558S - Astron. J., 137, 3558-3573 (2009/March-0)

Red supergiants as potential type IIn supernova progenitors: spatially resolved 4.6 µm CO emission around VY CMa and Betelgeuse.

SMITH N., HINKLE K.H. and RYDE N.

Abstract (from CDS):

We present high-resolution 4.6 µm CO spectra of the circumstellar environments of two red supergiants (RSGs) that are potential supernova (SN) progenitors: Betelgeuse and VY Canis Majoris (VY CMa). Around Betelgeuse, 12CO emission within ±3'' (±12 km/s) follows a mildly clumpy but otherwise spherical shell, smaller than its ∼55'' shell in K I λ7699. In stark contrast, 4.6 µm CO emission around VY CMa is coincident with bright K I in its clumpy asymmetric reflection nebula, within ±5'' (±40 km/s) of the star. Our CO data reveal redshifted features not seen in K I spectra of VY CMa, indicating a more isotropic distribution of gas punctuated by randomly distributed asymmetric clumps. The relative CO and K I distribution in Betelgeuse arises from ionization effects within a steady wind, whereas in VY CMa, K I is emitted from skins of CO cloudlets resulting from episodic mass ejections 500-1000 yr ago. In both cases, CO and K I trace potential pre-SN circumstellar matter: we conclude that an extreme RSG like VY CMa might produce a Type IIn event like SN 1988Z if it were to explode in its current state, but Betelgeuse will not. VY CMa demonstrates that luminous blue variables are not necessarily the only progenitors of SNe IIn, but it underscores the requirement that SNe IIn suffer enhanced episodic mass loss shortly before exploding.

Abstract Copyright:

Journal keyword(s): circumstellar matter - stars: evolution - stars: mass loss - stars: winds, outflows

Status at CDS:  

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 [HS53] A s*y 01 32 32.8024103986 +30 30 25.014155970 20.1 19.9 19.1 18.6 17.7 F8Ia 51 0
2 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5084 1
3 * omi Cet Mi* 02 19 20.79210 -02 58 39.4956   7.63 6.53 5.03   M5-9IIIe+DA 1428 0
4 SN 2006gy SN* 03 17 27.06 +41 24 19.5       14.20   SNIIn 281 1
5 SN 1999em SN* 04 41 27.04 -02 51 45.2   13.79 13.7     SNIIP 573 1
6 * bet Ori s*b 05 14 32.27210 -08 12 05.8981 -0.56 0.10 0.13 0.13 0.15 B8Iae 726 0
7 SN 1987A SN* 05 35 28.020 -69 16 11.07   4.75 4.81     SNIIpec 4430 2
8 * 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 1456 0
9 * eps CMa * 06 58 37.54876 -28 58 19.5102 0.36 1.29 1.50 1.59 1.80 B1.5II 458 1
10 V* VY CMa s*r 07 22 58.32877 -25 46 03.2355 12.01 10.19 7.95     M5Iae 989 0
11 LDN 1667 DNe 07 25.1 -25 46           ~ 11 0
12 SN 1988Z SN* 10 51 50.10 +16 00 00.5   16.8       SNIIn 329 1
13 SN 2006tf SN* 12 46 15.81 +11 25 55.4     16.7     SNIIn 89 1
14 * alf Her ** 17 14 38.85818 +14 23 25.2262   4.51 3.06     M5Ib-II+G5III+F2V: 188 0
15 IRC +10420 pA* 19 26 48.0981288433 +11 21 16.756524951   13.98 11.66     F8Ia+e 449 0
16 * P Cyg s*b 20 17 47.2020844 +38 01 58.552724 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1128 1
17 SN 1980K SN* 20 35 30.07 +60 06 23.7   11.6       SNIIL 426 1
18 * rho Cas LP* 23 54 23.0339951270 +57 29 57.766930774 7.00 5.85 4.59 3.63 2.89 G2_0 359 0

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