1 ISM Studies Towards Magnetars (An Update) Magnetar Visualisation, credit ESO Jarryd Hawkes In collaboration with G. Rowell, B. Dawson, M. Burton, Y. Fukui Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
2 ● Background ● Survey purpose and outline ● Results so far ...Since last time: – Bad 7mm data retaken (1647, 1708, 0526) – 12mm data taken and processed Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
3 What are they? Previously made up of two classes of object – AXPs and SGRs ● Exhibit both persistant and bursting/flaring x-ray emission – Period 2-12 seconds, 10 -12 - 10 -10 s/s ˙ – P Luminosities in soft and hard X-rays are greater than their ● rotational energy loss Thought to be powered by – their intense magnetic field (>10 14 G) Black dots - radio pulsars, red symbols - all known magnetars From N. Rea et al. 2012 ApJ 754 27 Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
4 Why look at them? Search for link between magnetars and TeV gamma-ray emission and ● investigate their emission mechanisms and energetics Unknown whether magnetars are able to accelerate particles to TeV ● energies. Spin down power of magnetars ~10 32-34 erg/s, but magnetic dissipation effects – may yield luminosity of ~10 35-36 erg/s (Zhang 2003, In Proc) Look for evidence of the impact of magnetars on the ISM ● As high energy objects with extreme B fields, we expect high energy outflows – High energy emission traced by disturbance of the ISM – ● Emission from shocked and disrupted gas Dense gas / TeV associations ● Discrimination between hadronic / leptonic – origin of gamma-rays Clues to the acceleration processes in – the region Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
5 Why look at them? Understand the environment & ways in which these objects are ● formed Magnetars thought to be born to high mass progenitors, many found in – massive stellar clusters High spin-down rates of magnetars – CXOU J171405.7-381031 imply they are young objects (<10 5 yrs) ● Currently 8 of 25 magnetars found towards visible SNRs So, look for evidence of star – formation towards magnetars in the ISM Dense gas/magnetar associations may – allow for precise distance estimates ● Better luminosity and age estimates γ-ray excess, MGPS contours From Aharonian et al. (2008) A&A, 486, 829 Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
6 Targeted Campaign Utilizing the Mopra radio telescope ● Deep pointings towards each magnetar in the 7mm and 12mm ● bands 1x30 min On/Off pointing – Tracers targeted: – ● CS, NH3, ... -> Cold, dense gas (density, optical depth, temperature) ● SiO, CH3OH, H2O, ... -> Star formation, outflows, shocked gas ● RRLs -> Ionised Gas (HII regions) Follow-up mapping of sources with ● Credit ATNF emission to reveal gas morphology and any relation to nearby objects Also looking at molecular/atomic ● carbon data from the Nanten, MopraCO and HEAT CI surveys Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
7 Catalogue / Observed Emission ● 25 (known + candidates) Source Name Emission Association Nearby TeV region SGR1801-23 CS ... HESS J1800-240B /W28 SGR1806-20 CS W31, MC 13A, massive star cluster HESS J1808-204 XTEJ1810-197 ... HESS J1809-193 AXJ1818.8-1559 ... SNR G15.4+0.1 SGRJ1822.3-1606 CS M17 (HII region) LS 5039/HESS J1825-137 SGRJ1834.9-0846 CS, NH3(1,1),(3,3), C2S, H2O SNR W41 HESS J1834-087 SGR1833-0832 CS ... HESS J1834-087 1E1841-045 CS HESS J1841-055 SNR Kes 73 AXJ1845-0258 SNR G29.6+0.1 HESS J1848-018 SGR1900+14 massive star cluster HESS J1912+101 SGR2013+34 W58 (giant HII complex) ... 1E2259+586 SNR CTB 109 Cassiopeia A 4U0142+61 ... ... SGR0418+5729 ... ... SGR0501+4516 SNR HB9 ... SGR0526-66 LMC, SNR N49, SL 463 N157B? 1E1048.1-5937 GSH 288.3-0.5-2.8 (stellar wind bubble) HESS J1026-582 CXOUJ010043.1-721134 SMC ... 1E1547.0-5408 SNR G327.24-0.13 HESS J1614-518 PSRJ1622-4950 SNR G333.9+0.0 HESS J1626-490 SGR1627-41 CS, NH3(1,1),(2,2),(3,3), CTB 33 (radio complex), MC -71, HESS J1634-472 H2O, C2S? H69a? SNR G337.0-0.1 CXOJ164710.2-455216 CS Westerlund 1 (massive star cluster) Westerlund 1 HESS J1646-458 1RXSJ170849.0-400910 ... HESS J1708-410 CXOUJ171405.7-381031 SNR CTB 37B, HESS J1713-381 CTB 37B SGRJ1745-2900 Galactic Center, Sgr A* Galactic Centre Purple: Candidate Magnetars Grey: Unobservable from the southern hemisphere Source: McGill Online Magnetar Catalogue www.physics.mcgill.ca/~pulsar/magnetar/main.html Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
8 Results So Far Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
9 SGR 1627-41 SGR 1627-41 Located nearby to extended TeV gamma-ray regions HESS – J1632-478 / HESS J1634-472 and associated with HII complex CTB 33 at 11.0 kpc (Corbel et al. 1999, ApJ, 526, 29) CS at -119 & -75 – km/s -> 6.8/8.9 & 4.8/10.9 kpc (near/far) Preliminary Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
10 SGR 1627-41 NH3 seen at the same velocities – Broad NH3 (~16 km/s) at -75 km/s gives – column density ~8.0E-21 cm -3 , T kin ~ 26 K NH3 at -119 km/s gives column density ~ – 7.7E-21 cm -3 , T kin ~ 20 K Determine relationship – between magnetar & gas/HII region & TeV emission Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
11 SGR 1806-20 Lies towards TeV region HESS J1808-204, together with massive – stellar cluster C1 1806-20. The cluster includes LBV 1806-20, which may power coincident radio nebula G10.3-0.3 (Gaensler et al., 2001, ApJ, 559, 963) TeV luminosity of 1.2x10 34 erg/s can be accounted for by the – energetics of the stellar winds from the cluster or LBV 1806-20 alone, or magnetic energy from SGR 1806-20 (Rowell et al., 2012, AIP Conf Proc, 1505, 273) Range of distance estimates – From Rowell et al., AIP Conference Proceedings, 1505, 273 (2012) Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
12 SGR 1806-20 70 km/s cloud in Nanten 12 CO data covers the TeV emission, peaks – towards its centre and is a good morphological match ● Candidate for hadronic gamma-ray production Obtain gas parameters, use ages of objects and extent of TeV – emission to perform particle diffusion analysis ● Determine hadronic/leptonic gamma-ray production, origin of gamma-rays Nanten 12 CO From 70 – 82 km/s Preliminary Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
13 Swift J1834.9-0846 Possible association with SNR W41 and/or HESS J1834-087 (Kargaltsev 2012, ApJ, 748, 26) ● Origin of TeV emission again ambiguous (PWN/SNR-MC interaction/Magnetar) X-ray and radio image from Kargaltsev et al. (2012) Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
14 Swift J1834.9-0846 CS emission at the same velocity as 13 CO associated with – the SNR (Leahy and Tain, 2008, AJ, 135, 167) CS cloud (radius 2.3') to the south west – of the SGR, within the TeV region ● Virial mass of cloud 3 – 11 x10 3 solar masses (at 4.2 kpc) Mopra CS(J=1-0) From 74 – 78 km/s Preliminary Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
15 Swift J1834.9-0846 NH3(1,1) and C2S indicates dense >10 4 cm -3 ● molecular gas -NH3 same width and profile as CS Possible NH3(3,3) ● H2O maser emission star formation → ● Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
16 1E1841-045 1E1841-045 Associated with SNR Kes 73 – Distance currently estimated from HI absorption features at 7.5-9.4 – kpc (Tian, W. and Leahy, D., 2008, ApJ, 677, 292) If the narrow CS emission at 98 km/s is associated with the – AXP/SNR, we constrain the distance to the object at 9.3 +- 0.1 kpc, which allows for more precise age and luminosity estimates 1E1841-045 Chandra Image, from H. S. Kumar et al. (2013), PotIAU, 9, pp 235-238 Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
17 1E1547.0-5408 Distance of ~9 kpc based on DM (Camilo et al. 2007, ApJ, 666, 93) Association with SNR G327.24-0.13 – HI absorption / RRL measurements to radio sources in the – same star forming region places it at ~4 kpc (Gelfand & Gaensler, 2007, ApJ, 667, 1111) CS at -57 km/s -> 3.7/10.7 kpc – Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
18 CXO J164710.2-455216 Part of massive stellar cluster Westerlund 1 ● Magnetar a possibility for origin of TeV emission seen towards the – cluster (HESS J1646–458) Distance 4.3 kpc based on HI line emission – CS seen at -32 km/s 2.5/11.8 kpc (near/far) → ● Jarryd Hawkes Adelaide University ISM Studies Towards Magnetars Nanten2 Workshop 2015
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