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Home , Luminous blue variable, Magnetar, OB star, Super star cluster

PoS(INTEGRAL 2010)091

e birth. We http://pos.sissa.it Licence. Licence. rse” rse” massive star young cluster our in , 4710.2-455216. isWhile this the collapsed only ion ion arguments are employed to derive a progenitor e properties of W243 they and how pertain to the University University cal Sciences, DCU r motion directedr motion away thefrom region, er of a former binary.massive

Black Holes. We identify a candidate former 10² Supernovae have occurredmay on the basis of th

, just , progenitorwithin the range mass for reative Commons Commons reative Attribution-NonCommercial-ShareAlike

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1 Besides carrying distinctionthe of being the most [email protected] [email protected] [email protected] Speaker 1 Copyright owned by the author(s)of the owned terms by Copyrightthe C under

 A candidate former companion star to the Magnetar Magnetar the to star companion former candidate A Galactic massive the in J164710.2-455216 CXOU 1 Westerlund cluster L. Norci Schoolof Physical Sciences and NCPST, Dublin City contains the notable Magnetar CXOU J16 stellar remnant known for this cluster, a further ~ Initialcluster Mass Function, possibly all leaving P.J. Kavanagh Glasnevin, Dublin 9, Ireland E-mail: Meurs E.J.A. Schoolof Cosmic Physics, DIAS, and Schoolof Physi Glasnevin, Dublin 9, Ireland E-mail: companion to the Magnetar in of view its high prope 8th INTEGRAL Workshop “The Gamma-rayRestless Unive Dublin, Ireland September 27-30,2010 Schoolof Physical Sciences and NCPST, Dublin City Glasnevin, Dublin 9, Ireland E-mail: viz. the W243. th We discuss also draw attention to another candidate to be memb former Magnetar companion hypothesis. Binary evolut mass for Magnetarthe of 24-25

PoS(INTEGRAL 2010)091

cal cal ay from from ay ar is a is ar ed binary binary ed P. Kavanagh e for Wd1 a Wd1e for n in Wd1. n inWd1. ter Supernova ter uliarities and uliarities (Brandner et al. al. et (Brandner en part of a binary a binary of part en uster dimensions. dimensions. uster rds unity, W243 rds unity, k et al. 2008; Belczynski Belczynski 2008; al. et k ion indicates that some 10² that some indicates ion al. 2006).

y imagey (right) of Westerlund 1, latterthe with 2

). V A , an age of 3.6 Myr and a distance of 3.6 kpc. Piatti et al. (1998) found a found (1998) al.et Piatti kpc. 3.6 of distance and a Myr 3.6 of , an age M 4 10 Figure 1. VLT optical (left) and image Chandra X-ra Magnetar position indicated. (NASA/CXC/UCLA/Muno et companion W243 2. Candidate star former This st the Magnetar. from far not found is Wd1 in W243 supergiant The A-type pec displays spectral It A2Iab. spectrum with (LBV), Variable Blue Luminous aw directed 2003), al. et Zacharias UCAC2, km/s; (222 motion proper a high possesses 2). (Figure Magnetar the towa (q) ratios mass with in binaries, are born massive most As be have to Magnetar, the to companion former candidate as a itself presents a disrupt Indeed, progenitor. Magnetar the explosion of the Supernova after disrupted (Clar Magnetar the for possibility as a previously mentioned has been 2008). Taam & 1 Westerlund 1. Cl Star Super almost of cluster star a Galactic is (Wd1) 1 Westerlund estimat (2008) al. et Brandner study, photometric a comprehensive of theOn basis of ~4.5 mass an opti without (Figure 1), J164710.2-455216 CXOU Magnetar, a harbours cluster The know object collapsed only This the is al. et 2006). (Muno counterpart or Near-IR af remnant Star a Neutron stellar yielding still mass on the maximum Depending Funct Mass Initial likely cluster’s of the extrapolation an explosion, Magnetar the preceded have could Hole remnants Black leaving Supernovae 2008). al. et 2008; Clark large obscuration of 12.9 magn ( magn 12.9 of large obscuration Candidate former Magnetar companion in Wd1 PoS(INTEGRAL 2010)091 n n erg/s.

r) hasr) r 34 (based (based ical al. (2008) (2008) al. 10 P. Kavanagh Sun a and find no find a and M the large large the tem with low tem stimate a stimate he H atmosphere atmosphere H he t & Maeder 2000), 2000), Maeder t & nosity of > ~35-36 ssive stars would be X- would be stars ssive aving used too large a too used aving for the progenitor (Ritchie et et (Ritchie the for progenitor Sun q² (which is customary), and (iii) customary), is q² (which . M ∝ Sun M > 40 initial left) andleft) Palomar Observatory Sky Survey IR rrow inrrow rightthe panel represents the proper motio

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Figure 2. image 2MASS of Westerlund 1 core region ( e can we W243), as is secondary, evolved (for an q ~ 0.89 ratio mass an initial of mass W243 transfer mass a post For Magnetar. the for mass progenitor in Meyne models stellar rotating for tracks evolutionary with on comparison ~24-25 of a mass progenitor Magnetar the for find we image of W243 and surrounding region (right). The a of of W243. 3. On binarity the of W243 sta(OB companion hot an unseen W243, of features spectral of the of some view In opt from found was period no However, al.et 2009). (Ritchie W243 for been suggested 2007). (Bonanos star the of monitoring spectr VLT-UVES 2 epochs of employing spectro-astrometry out carried We a hot indeed 3). If (Figure separation binary a 25 AU beyond companion of a evidence the ma of winds stellar colliding the this separation, within is companion sys an LBV for (2002) al. et Zwart Portegies the of model bright. Assuming ray lumi X-ray an exhibits system a binary such loss, mass winds and velocity cluste the of observations XMM-Newton or in Chandra seen is source luminous such No star. runaway single be a W243 to assume we Thus, et 2008). al. (Clark 4. Binary history of Magnetar t transfer stripping (i)mass assuming et (2005), al. O’Maoileidigh in As efficiency transfer mass (ii) a progenitor, Magnetar of the of suggestion a recent than This lower is h authors these to due largely is this value with difference The al. 2010). et Brandner by determined accurately more been has which ~5 kpc, Wd1, to distance to due overestimated been had masses stellar and Thus, as 3.6 kpc. distances. Candidate former Magnetar companion in Wd1 PoS(INTEGRAL 2010)091 ed hows hows ars ars er hand, er hand, to have have to P. Kavanagh

. 2003). Thus, Thus, . 2003). mbling W243. Its W243. Its mbling e two stars are two e Supernova event as event Supernova faster evolving evolving faster n Sequence turn-off turn-off n Sequence y be obtained by a by be obtained y a little lower, like like lower, little a s constraints on on s constraints d expect a significant es the upper initial mass initial mass the upper es (B0.5V stars). stars). (B0.5V Sun M , for formation from single from formation Star Neutron , for he bottom bottom two panelshe show the variation the in Sun progenitor for the Magnetar is right at the the at right is Magnetar the for progenitor M nge for each twoof the observations, thewith dott

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line. line in W243the VLT-UVES spectra. The top panel s α α (Schmidt-Kaler 1982). However, from the analysis of Brandner et al. al. et Brandner the of analysis from However, 1982). (Schmidt-Kaler Sun error. aIf binary companion presentwere one woul σ M (Fryer et al. 2002). Thus, the Magnetar could indeed be the first Neutron Star Neutron first be the indeed could Magnetar Thus, the al.et 2002). (Fryer region of the spectrum obtained on 6 Sept. 2004.T Sun α M W243-like case in5. Another Wd1? rese closely star, W16a, runaway another is of Wd1 centre the Just of NE thes J of magnitudes and V the B, and A5Ia+) (or possibly is A2Ia+ spectrum al et Zacharias (UCAC2, 188 km/s is W16a of motion The similar. proper very its after disrupted that was a binary of been part have similarly could W16a oth the Hole. On a Black leaving presumably event, a Supernova underwent companion H the be could as a Supernova exploding after Star a Neutron leaving starfor a 22 a stars undergo mass lower and lower as Holes) Black Wd1 (after in formed mas current estimated challenging without time, with evolves the cluster ma picture of this Confirmation 2010). al. et (cf. Richie birth Star Neutron Mai that the We note Magnetar. the for measurement motion future proper O8V st where 2006), al. et (Muno O7V-O8V types spectral be around Wd1 may ofpoint ~23 of masses have 15 around mass, turn-off lower astill follow would (2008) continuum continuum centroid (in acrossAU) the wavelength ra of a 24-25 the possibility Interestingly, binari For value. the Solar exceeding much not forstars, Candidate former Magnetar companion in Wd1 Figure 3. Spectro-photometric plot H of the representinglines the 1 deviation in centroid,the offset across H the 25 (2003), et al. Heger by limit determined upper PoS(INTEGRAL 2010)091 A A P. Kavanagh s from thes from 0 (1982) 0 (1982) Intermediate to Intermediate f-Farhad, f-Farhad, he Magnetar. Again, Again, Magnetar. he , 1597 (2009) (2009) , 1597 How Massive single stars single Massive How 507 , L41 (2006) (2006) , L41 , 591 (2005) , 591 (2005) 636 Spectroscopic monitoring of the of monitoring Spectroscopic 10 , A&A , A&A , ApJ , ApJ A VLT/FLAMES survey for massive massive for survey VLT/FLAMES A

, NewA NewA , , 137 (2008) (2008) , 137 The limiting stellar initial mass for Black mass initial stellar limiting The , 335 (2002) (2002) , 335 478

On the feasibility of detection of neutron star star of neutron of detection feasibility the On 5 578

, in Landolt-Börnstein: Numerical Data and Data Numerical in Landolt-Börnstein: , The Second Naval Observatory U.S. CCD , A&A , A&A , 423 (1998) , 423 (1998) , ApJ , ApJ 127 Fundamental parameters of the highly reddened young open young open reddened highly the of parameters Fundamental , 1289,0 (2003) yCat , A48 (2010) (2010) , A48 , 147 (2008) (2008) , 147 , 101 (2000) (2000) , 101 Unveiling the X-ray point source population of the Young Massive Massive Young the of population source point X-ray the Unveiling 520 477 , A&AS , A&AS 361 with rotation. V. Changes in all the outputs of of outputs the all in Changes V. rotation. with evolution Stellar Basic Stellar Data Stellar Basic , 288 (2003) (2003) , 288 , 2696 (2007) (2007) , 2696 , A&A , A&A , A&A , A&A , A&A , A&A Variability of Young Massive Stars in the Galactic Super Cluster Star Super the in Galactic Stars Massive Young of Variability 591 133 AJ AJ , ApJ , ApJ luminous blue variable Westerlund1-243 from 2002 to 2009 to from 2002 Westerlund1-243 variable blue luminous Langer, N. Negueruela, I. J.S. Clark, Ritchie, [11] B.W. masse progenitor magnetar on constraints Dynamical II. 1. in Westerlund binaries W13 binary eclipsing p. 3 VI/2b, Series, Bd New - Technology and in Relationships Functional M.I. G.L. M.E. Hall, D.M. S.E.Zacharias, Wycoff, Urban, [13] Zacharias, N. E.R. Holdenried, Winter, Germain, L. Astrograph Catalog (UCAC2) [10] B.W. Ritchie, J.S. Clark, J. S., I. Negueruela, F. Najarro, F. Negueruela, J. I. S., J.S. Clark, Ritchie, [10] B.W. Schmidt-Kaler, T. [12] [9] A.E. Piatti, E. Bica, J.J. Claria, J.J. Bica, E. [9]Piatti, A.E. 2 1 and Westerlund clusters massive star models star massive [7] G. Meynet, A. Maeder, A. Meynet, [7] G. S.L.W. Law, C. de Grijs, R. Dougherty, S.M. Crowther, P.A. J.S. Clark, M.P. Muno, [8] Yuse F. Zwart, Portegies S. Pooley, D. Negueruela, I. Morris, M.R. McMillan, 1 in Westerlund Progenitor Massive a with Star Neutron Hole formation in close binary systems binary in close Hole formation Hartmann, D.H. Langer, N. Woosley, S.E. Fryer, C.L. [5] Heger, A. life end their astrometry Gaia using runaways to OB companions [6] C. O’Maoileidigh, E.J.A. Meurs, L. Norci, Norci, L. Meurs, E.J.A. [6] O’Maoileidigh, C. [3] Clark, J. S.; Muno, M. P.; Negueruela, I.; Dougherty, S. M.; Crowther, P. A.; A.; P. M.; S. Crowther, Dougherty, I.; P.; Negueruela, M. J. Muno, S.; [3] Clark, R., de Grijs, P.; S. Goodwin, 1 Cluster Westerlund Wellstein, S. Langer, N. Heger, A. [4] Fryer, C.L. this star could also be an alternative candidate for a former companion to t to companion former a for candidate alternative an be also could this star here. decide to helpful be will Magnetar the of motion the proper References Bonanos, [1] A.Z. 1, Westerlund 1 Westerlund of content stellar low-mass [2] W. Brandner, J.S. Clark, A. Stolte, R. Waters, I. Negueruela, S.P. Goodwin, Goodwin, S.P. Negueruela, I. Waters, Stolte, R. A. J.S. Clark, W. Brandner, [2] Candidate former Magnetar companion in Wd1