A catalogue of X-ray emitting WR stars Ada Nebot, C. Motch, and the - PowerPoint PPT Presentation

A catalogue of X-ray emitting WR stars Ada Nebot, C. Motch, and the ARCHES collaboration ARCHES workshop Paris, 30 Novembre - 2 Dicembre 2015

The Galactic science case • What is the XLF of the hard X-ray low to intermediate luminosity sources? - CVs, AB (Sazonov+2006) - OB, WR too!! (Mauerhan+2010, Anderson+2011) • What is the origin of the hard X-ray emission in O,B and WRs? - Intrinsic X-ray emission - Wind accretion onto a compact object - Colliding winds in a binary

How can XMM-Newton help? • Large FOV ~30 min + high sensitivity • 30-100 serendipitous sources/pointing ~133.000 sources with multi-wavelength information • Statistical identification based on different surveys: - Bright flux sample Della Ceca+2004 - Medium flux sample Barcons+2002 - Faint flux sample - Galactic Plane Survey Hands+2004, Motch +2010, Nebot Gómez-Morán+2013 EPIC-pn 0.2-12 keV image of field 3C436

The cross-correlation 2MASS 2MASS EPIC-pn DSS GLIMPSE AllWISE Cross-correlation with optical/infrared catalogues

Wolf-Rayet stars WO 1% WC • The input catalogue: 639 WRs from the catalogue from P . Crowther WN 43% 57%

Wolf-Rayet stars WO 1% WC • The input catalogue: 639 WRs from the catalogue from P . Crowther WN 43% 57% WO 1% WC • The coverage: ~one third within the ARCHES catalogue coverage 39% WN 60%

Wolf-Rayet stars WO 1% WC • The input catalogue: 639 WRs from the catalogue from P . Crowther WN 43% 57% WO 1% WC • The coverage: ~one third within the ARCHES catalogue coverage 39% WN 60% WO 7% WC 21% • The detections: 29 WRs with an entry in the ARCHES catalogue WN 72%

Wolf-Rayet stars: fraction of X-ray active WRs • What is the fraction of active WRs ? Does it depend on the spectral type? - ~17% of the WN (mostly binaries but some single too) - ~8% of the WC (binaries + the single ? WR102-1) - 100% WO (WR 30a binary, WR142 is likely single fast rotator) • But need to correct for detection biases: f = # WRs detected / # WRs covered x detection biases • Detection biases depend on: Lx, Nh, distance, exposure time, sensitivity, … (work in progress)

Using WR as learning sample…

Using WR as learning sample… X-ray and infrared colours • (H-K) estimate on the 1.0 extinction A K Indebetouw et al. (2005) 0.5 HR3 • Modelled the evolution of HR 0 with extinction for different populations: - Young stars (dashed line) (kT1,kT2) = (0.2,0.8)keV -0.5 - Hard WR (solid line) 1: WR kT = 5 keV (e. g. WR 142, Oskinova et al. 2009) 0 0.5 1.0 1.5 2.0 2.5 H-Ks

Using WR as learning sample… X-ray and infrared colours • (H-K) estimate on the 1.0 extinction A K Indebetouw et al. (2005) 0.5 HR3 • Modelled the evolution of HR 0 with extinction for different Hard populations: - Young stars (dashed line) (kT1,kT2) = (0.2,0.8)keV -0.5 Soft - Hard WR (solid line) 1: WR kT = 5 keV (e. g. WR 142, Oskinova et al. 2009) 0 0.5 1.0 1.5 2.0 2.5 H-Ks

Using WR as learning sample… X-ray and infrared colours 1.0 What is the nature of the hard 0.5 X-ray sources with infrared (2MASS & GLIMPSE) HR3 associations? 0 Hard -0.5 Soft Hard X-ray 1: WR 0 0.5 1.0 1.5 2.0 2.5 H-Ks

Using WR as learning sample… X-ray and infrared colours 1.0 What is the nature of the hard 0.5 X-ray sources with infrared (2MASS & GLIMPSE) HR3 associations? 0 Hard Hard X-ray 1: WR -0.5 Soft 7: HMXB 7: Be 0 0.5 1.0 1.5 2.0 2.5 H-Ks

Using WR as learning sample… X-ray and infrared colours 1.0 What is the nature of the hard 0.5 X-ray sources with infrared (2MASS & GLIMPSE) HR3 associations? 0 Hard Pilot Survey: Hard X-ray Awarded 1/2 night at the WHT 1: WR -0.5 Soft 7: HMXB 7: Be 0 0.5 1.0 1.5 2.0 2.5 H-Ks

0.2-12 keV, XMM 8 µm, GLIMPSE 24 µm, MIPSGAL WN8h 0.2-12 keV, XMM 5.6 µm, GLIMPSE 1.4 GHz, VLA Ofpe/WN9 0.2-12 keV, XMM 24 µm, MIPSGAL 1.4 GHz, VLA 0.2-12 keV, XMM 8 µm, GLIMPSE 24 µm, MIPSGAL Be 0.2-12 keV, XMM 8 µm, GLIMPSE 24 µm, MIPSGAL Nebot Gómez-Morán et al 2015 (astro-ph XXX)

Investigating multi-wavelength properties…

Investigating multi-wavelength properties… X-ray-to-infrared flux ratio 1 4 1 2 What is the nature of the hard X-ray sources with infrared 1 0 (2MASS & GLIMPSE) associations? Ks 8 6 Unidentified log (fx/fk) < -2 — WR γ -Cas Be log (fx/fk) ~ -2.5 — γ -Cas analogs HMXB 4 log (fx/fk) > -3 — HMXBs W R 2 - 5 - 4 - 3 - 2 - 1 0 log10(fx/fk) Nebot Gómez-Morán et al 2015

Lx versus Period Preliminary results… Distance known for 24 of these 31 WRs, and period for 12 binaries Computed mean Lx in three bands: T otal (0.2-12 keV), soft (0.2-2 keV), hard (2-12keV) Lx in 0.2-12 keV a WN 34.0 Lx (0.2-12keV) [ergs/s] 33.5 133 33.0 32.5 139 4 6 141 4 7 138 32.0 - 1 0 1 2 3 4 log (Period [days])

Lx versus Period Preliminary results… Distance known for 24 of these 31 WRs, and period for 12 binaries Computed mean Lx in three bands: T otal (0.2-12 keV), soft (0.2-2 keV), hard (2-12keV) Lx in 0.2-12 keV a WO 140 34.0 a WC a WN Lx (0.2-12keV) [ergs/s] 33.5 133 33.0 4 8 30a 32.5 139 4 6 141 4 7 138 1 1 32.0 7 9 - 1 0 1 2 3 4 log (Period [days])

Lx versus Period Preliminary results… Distance known for 24 of these 31 WRs, and period for 12 binaries Computed mean Lx in three bands: T otal (0.2-12 keV), soft (0.2-2 keV), hard (2-12keV) 0.2-2 keV 2-12 keV 34.0 a WO 133 a WO 140 4 8 140 a WC a WC a WN a WN 32.5 33.5 Lx (0.2-2keV) [ergs/s] Lx (2-12keV) [ergs/s] 4 6 138 32.0 33.0 30a 30a 139 133 4 7 31.5 32.5 4 8 141 139 1 1 4 7 32.0 4 6 31.0 1 1 7 9 141 7 9 138 - 1 0 1 2 3 4 - 1 0 1 2 3 4 log (Period [days]) log (Period [days])

Summary • The WR catalogue will provide SED for at least 31 WRs (WN, WC and WO) detected in X-rays. • Hard X-ray sources with log(fx/fk) < -3 are dominated by WR stars • We have WR candidates and we plan to take more spectra to confirm their nature. • and…