X-Ray Observations of Supernovae as Probes of Stellar Environments

1. X-Ray Observations of Supernovae as Probes of Stellar Environments Stefan Immler Swift Science Center NASA/GSFC/UMCP

2. Stefan Immler / NASA GSFC X-Ray Supernovae • 32 SNe have been detected in X-rays over the past 27 years In the near aftermath (days to years) after their explosions. • X-ray luminosities range from 1034 erg/s (SN 1987A) to some 1041 erg/s (e.g., SNe 1988Z, 1995N, 2002hi) up to 1043 erg/s for GRB/SN (e.g., SN 2006aj/GRB060218). • Approx. half of all detections are from Chandra. • XMM-Newton is very successful in follow-up observations to monitor the long-term X-ray evolution of SNe (see this talk) and to get high quality X-ray spectra. • Due to its rapid response (hrs) and multi-wavelength coverage, Swift is playing an increasingly important role in probing CSM interaction with UV and X-ray observations of young SNe. Golden Age of X-Ray SN Research

3. Stefan Immler / NASA GSFC X-Ray Production Mechanism • Several X-ray production mechanism have been proposed to explain the • observed X-ray emission (among others): • Initial burst of X-rays as the SN shock breaks out of the surface of the star. • Short duration (< 1,000 s), hard X-rays (> 100 keV) plus soft BB continuum • (e.g., SN 2006aj/GRB060218) • Radioactivity of the ejecta (mostly 56Ni decay, e.g., SN 1987A) • Compton scattering of -rays • Inverse Compton scattering of relativistic e– on photospheric UV photons • produced during the explosion (e.g., SN 2002ap) • Pulsar driven X-rays from plerionic SNR • Circumstellar interaction: Interaction of the SN shock with SN environment. • CSM interaction is the most important X-ray production mechanism

4. Stefan Immler / NASA GSFC Circumstellar Interaction Ultraviolet and X-rays emission

5. Stefan Immler / NASA GSFC SN 2006X and SN 1979C in M100 Swift UVOT V, B, U UVOT UVW1, UVW2, UVM2 XRT 0.2–10 keV • SN 2006X (young type Ia) not detected in the UV and in X-rays • SN 1979C (type II) is one of the oldest SN still visible in UV and X-rays

6. Stefan Immler / NASA GSFC SN 1979C in M100 XMM-Newton Swift XRT Chandra ACIS • High X-ray luminosity,Lx = 8  1038 erg/s (0.3–2 keV) at t = 26 years • High and constant mass-loss rate of 1.5  10–4 Myr–1 over • >20,000 yrs in the history of the progenitor

7. Stefan Immler / NASA GSFC SNe 1978K and 1979C • SNe 1979C and 1978K are the oldest known X-ray emitting SNe • Surprisingly similar evolution • Evolution is best described by a t2 rise followed by a t–3 decline

8. Stefan Immler / NASA GSFC SN 2005kd Swift opt/uv Swift X-ray • Type IIn SN at 64 Mpc • High X-ray luminosity,Lx = 1.5  1041 erg/s (0.2–10 keV) • High mass-loss rate of some 10–4 Myr–1 Immler, Pooley & Brown 2007

9. Stefan Immler / NASA GSFC SN 2005ip Swift X-ray Swift UV Swift optical • Type IIn SN at 30 Mpc • High X-ray luminosity,Lx = 1.6  1040 ergs/s (0.2–10 keV) • High mass-loss rate of some 10–4 Myr–1 Immler & Pooley 2007

10. Stefan Immler / NASA GSFC SN 1970G in M101 Chandra 1 Ms X-ray survey of M101 Detection of X-ray emission from SN 1970G 35 years after its explosion Immler & Kuntz 2005

11. Stefan Immler / NASA GSFC SN 1981K in NGC 4258 Lx = 1.2 x 1037 erg/s 20 years after the explosion. Immler, Li, Yang & Wilson 2007

12. Stefan Immler / NASA GSFC SN 2005ke in NGC 1371 XRT X-rays (258 ks) UVOT ultraviolet • First detection of a type Ia SN in X-rays from CSM interaction? • Mass-loss rate of the progenitor’s companion 3  106M yr1 • CSM density 4  107 cm3 at a distance of 3  1015 cm Immler et al. 2006

13. Stefan Immler / NASA GSFC SN 2005ke in NGC 1371 Swift UV lightcurves of type Ia supernovae UV lightcurve shapes of Type Ia supernovae are surprisingly similar … except:

14. Stefan Immler / NASA GSFC SN 2005ke in NGC 1371 • Excess ultraviolet emission detected for SN 2005ke • Caused by the interaction of the supernova shock with dense CSM? • Evidence for a companion star?

15. Stefan Immler / NASA GSFC SN 2005ke in NGC 1371

16. Stefan Immler / NASA GSFC SN Ia Systems White Dwarf White Dwarf I) Double degenerate Star White Dwarf Single degenerate II) A thermonuclear (Type Ia) supernova is a white dwarf that accretes matter from a companion star and explodes as it reaches the Chandrasekhar mass (1.4x Sun). Unsolved question: What is the companion objects? Two scenarios how thermonuclear SN (Type Ia) systems could look like

17. Stefan Immler / NASA GSFC SNe 2006dd and 2006mr in NGC 1316

18. Stefan Immler / NASA GSFC SN 2006jc in UGC 4904 Swift optical/UV Chandra X-ray SN 2006jc (24 Mpc) is detected in X-rays with Swift and Chandra t ~ 20–180 d Immler et al. 2007a

19. Stefan Immler / NASA GSFC SN 2006jc in UGC 4904 Brightening in X-rays: dense shell around the site of the explosion? A luminous outburst was observed two years before SN Immler et al. 2007a

20. Stefan Immler / NASA GSFC SN 2006jc in UGC 4904 Outburst 2 years before the SN explosion, leading to ejection of shell Immler et al. 2007a

21. Stefan Immler / NASA GSFC SN 2006bp in NGC 3953 . Swift optical Swift UV Swift X-ray • Type IIP (‘plateau’) SN at d = 14.9 Mpc • Observed with Swift <1 day after the explosion • Detection of X-ray emission <1 day after the explosion • Earliest detection of a SN in X-rays (minus GRB/SN), Lx = 2  1039 ergs/s Immler et al. 2007b

22. Stefan Immler / NASA GSFC SN 2006bp in NGC 3953 • Flexible scheduling with Swift observations allow X-ray timing analysis. • SN would have been missed with any other observatory (XMM, Chandra …). • With Swift we are probing a previously unexplored time domain for SNe. • The SN is fading below the detection threshold within 10 days. • Detection of previously unknown, variable ULX in the host galaxy. Immler et al. 2007b

23. Stefan Immler / NASA GSFC SN X-Ray Light Curves

24. Stefan Immler / NASA GSFC Environments of SN

25. Stefan Immler / NASA GSFC SN 2006bp in NGC 3953 Sequence RSG (IIP) - superwind/LBV (IIn) - post LBV (IIb)

26. Stefan Immler / NASA GSFC Summary X-ray observations of young SNe are uniquely suited to: • Measure key physical parameters of CSM interaction, such as: Mass-loss rates of the progenitors over significant time-scales in the evolution of the progenitor as a function of SN type and progenitor, CSM densities in the environments of SNe out to large radii, • Study the temporal evolution of the forward and reverse shock, • New observations with Swift are used to probe the previously unexplored time domain of the early UV and X-ray emission (< days) and probe links between GRBs/SNe by observing SN related long-duration GRBs. Free Bonus:

27. Stefan Immler / NASA GSFC Swift Mugshots of Supernovae opt UV X-ray opt UV X-ray opt UV X-ray

28. Stefan Immler / NASA GSFC Swift Survey of Galaxies optical+UV X-ray

29. Stefan Immler / NASA GSFC Swift Survey of Galaxies Optical UV X-rays

30. Stefan Immler / NASA GSFC Elliptical Galaxies NGC 1316 V, B, U W1, M2, W2 X-ray

31. Stefan Immler / NASA GSFC Spiral Galaxies NGC 4321 V, B, U W1, M2, W2 X-ray

32. Stefan Immler / NASA GSFC Spiral Galaxies NGC 300 V, B, U W1, M2, W2 X-ray

33. Stefan Immler / NASA GSFC Spiral Galaxies NGC 891 V, B, U W1, M2, W2 X-ray

34. Stefan Immler / NASA GSFC Spiral Galaxies NGC 1365 V, B, U W1, M2, W2 X-ray

35. Stefan Immler / NASA GSFC Spiral Galaxies NGC 4236 V, B, U W1, M2, W2 X-ray

36. Stefan Immler / NASA GSFC Spiral Galaxies NGC 6744 V, B, U W1, M2, W2 X-ray

37. Stefan Immler / NASA GSFC Irregular Galaxies NGC 4449 V, B, U W1, M2, W2 X-ray

38. Stefan Immler / NASA GSFC Irregular Galaxies NGC 1313 V, B, U W1, M2, W2 X-ray

39. Stefan Immler / NASA GSFC Peculiar Galaxies NGC 4649 V, B, U W1, M2, W2 X-ray

40. Stefan Immler / NASA GSFC Groups of Galaxies Arp 224 V, B, U W1, M2, W2 X-ray

41. Stefan Immler / NASA GSFC Groups of Galaxies Arp 319 V, B, U W1, M2, W2 X-ray • Status of the Swift Survey of Nearby Galaxies: • 114 galaxies completed (2007 Sept 1), but more to come! • Demonstrates the capabilities of the instruments on board Swift