2014A&A...561A..15C


C.D.S. - SIMBAD4 rel 1.7 - 2019.09.22CEST11:17:06

2014A&A...561A..15C - Astronomy and Astrophysics, volume 561A, 15-15 (2014/1-1)

IRAS 18357-0604 - an analogue of the galactic yellow hypergiant IRC +10420?

CLARK J.S., NEGUERUELA I. and GONZALEZ-FERNANDEZ C.

Abstract (from CDS):

Yellow hypergiants represent a short-lived evolutionary episode experienced by massive stars as they transit to and from a red supergiant phase. As such, their properties provide a critical test of stellar evolutionary theory, while recent observations unexpectedly suggest that a subset may explode as Type II supernovae. The galactic yellow hypergiant IRC +10420 is a cornerstone system for understanding this phase since it is the strongest post-RSG candidate known, has demonstrated real-time evolution across the Hertzsprung-Russell diagram and been subject to extensive mass loss. In this paper we report on the discovery of a twin of IRC +10420 - IRAS 18357-0604. Optical and near-IR spectroscopy are used to investigate the physical properties of IRAS 18357-0604 and also provide an estimate of its systemic velocity, while near- to mid-IR photometry probes the nature of its circumstellar environment. These observations reveal pronounced spectral similarities between IRAS 18357-0604 and IRC +10420, suggesting comparable temperatures and wind geometries. IR photometric data reveals a similarly dusty circumstellar environment, although historical mass loss appears to have been heavier in IRC +10420. The systemic velocity implies a distance compatible with the red supergiant-dominated complex at the base of the Scutum Crux arm; the resultant luminosity determination is consistent with a physical association but suggests a lower initial mass than inferred for IRC +10420 (≲20 M versus ∼40 M). Evolutionary predictions for the physical properties of supernova progenitors derived from ∼18-20 M stars - or ∼12-15 M stars that have experienced enhanced mass loss as red supergiants - compare favourably with those of IRAS 18357-0604, which in turn appears to be similar to the the progenitor of SN2011dh; it may therefore provide an important insight into the nature of the apparently H-depleted yellow hypergiant progenitors of some Type IIb SNe.

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Journal keyword(s): stars: emission-line, Be - circumstellar matter - stars: evolution

Simbad objects: 35

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Number of rows : 35

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 LHA 115-S 18 Em* 00 54 09.5415603586 -72 41 43.291670748 12.94 13.48 13.82   12.55 B[e] 72 0
2 HD 8752 * 01 25 20.8969784945 -51 16 35.171619218   9.82 8.60     K1III 6 0
3 HD 269006 s*b 05 02 07.3944119328 -71 20 13.118657760 9.93 10.60 10.55 10.43 10.38 LBV 229 0
4 SN 2009kr SN* 05 12 03.30 -15 41 52.2           SN.II 60 1
5 V* S Dor sg* 05 18 14.3572490675 -69 15 01.148131817 9.08 10.39 10.25 9.74 9.14 A5Iaeq 335 0
6 CPD-69 463 s*y 05 38 51.6167474749 -69 08 07.314653596 11.93 12.45 12.014     F7Ia 77 1
7 * l Pup sg* 07 43 48.4687222 -28 57 17.372015 4.06 4.09 3.93 3.68 3.50 A4Iabe 172 0
8 SN 1993J SN* 09 55 24.77476 +69 01 13.7026   10.8 12.0     SN.IIb 1221 1
9 HD 90177 s*b 10 22 53.8426931454 -59 37 28.361118869 9.16 9.66 8 8.15   LBV 298 0
10 V* AG Car WR* 10 56 11.5779283438 -60 27 12.809532379 7.00 7.57 6.96 7.73   WN11h 578 0
11 NAME Crux-Scutum Spiral Arm reg 12 30 -60.0           ~ 263 0
12 SN 2008cn SN* 12 40 55.66 -40 58 12.1           SN.II 29 1
13 SN 2011dh SN* 13 30 05.10555 +47 10 10.9227           SN.IIb 262 1
14 Cl* Westerlund 1 BKS K *iC 16 47 02.23 -45 50 59.1   22.0 17.575 13.611   F1Ia+ 19 0
15 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 439 0
16 Cl* Westerlund 1 W 16 *iC 16 47 06.6152064188 -45 50 42.171179650   20.5 16.248     A5Ia+ 21 0
17 Cl* Westerlund 1 W 243 s*b 16 47 07.5028508821 -45 52 29.152464693   19.873 15.730     LBV 47 0
18 WRAY 15-1676 pA* 17 19 49.3292317040 -39 10 37.929612963     13.1     ~ 40 1
19 [FMR2006] 15 s?y 18 37 57.7978549989 -06 52 32.002047628           G6I 5 0
20 RSGC 1 OpC 18 37 58 -06 53.0           ~ 83 0
21 IRAS 18357-0604 IR 18 38 23.4057310368 -06 01 26.770155662           ~ 8 0
22 Cl* Stephenson 2 DFK 23 sg* 18 39 01.4761585736 -06 00 59.775921147           M4I 4 0
23 MSX6C G026.1215-00.0345 sg* 18 39 05.586 -06 04 26.58           K4I 6 0
24 2MASS J18390805-0605244 sg* 18 39 08.0430602107 -06 05 24.185408590           M4I 6 0
25 Cl* Stephenson 2 DFK 17 sg* 18 39 15.0508700859 -06 05 19.207376922           K3I 4 0
26 IRC -10447 s*r 18 39 19.6096079321 -06 00 40.761206101           M3I 17 0
27 Cl Stephenson 2 OpC 18 39 20 -06 01.7           ~ 79 0
28 [S90] 10 sg* 18 39 24.6065493239 -06 02 13.905395274     19.91 16.4 12.85 M4I 11 0
29 HD 172806 * 18 42 06.2385389737 +04 02 03.626027625   8.08 8.02     B9V 7 0
30 HD 179821 pA* 19 13 58.6083165753 +00 07 31.934676028 10.81 9.694 8.19     G4_0-Ia 215 0
31 IRC +10420 pA* 19 26 48.0981288433 +11 21 16.756524951   13.98 11.66     F8Ia+e 448 0
32 V* V509 Cas LP* 23 00 05.1007915562 +56 56 43.348681058 8.01 6.68 5.13 3.96 3.11 G4_0 306 0
33 * omi And Be* 23 01 55.2645930 +42 19 33.533383 3.00 3.53 3.62 3.61 3.69 B6IV/V_sh 408 0
34 * 6 Cas sg* 23 48 50.17052 +62 12 52.2577 6.08 6.10 5.43     A3Ia+ 177 0
35 * rho Cas LP* 23 54 23.0339951270 +57 29 57.766930774 7.00 5.85 4.59 3.63 2.89 G2_0 356 0

    Equat.    Gal    SGal    Ecl

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2019.09.22-11:17:06

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