A Decade of Short-duration Gamma-ray Burst Afterglows

Transcription

1 A Decade of Short-duration Gamma-ray Burst Afterglows Wen-fai Fong University of Arizona! in collaboration with: Raffaella Margutti, Edo Berger, B. Ashley Zauderer! Einstein Fellows Symposium,

2 Motivation Gamma-rays X-ray Optical Near-IR Radio Central engine Prompt emission Afterglow Figure adapted from Gehrels et al. 2007

3 Motivation Gamma-rays X-ray Optical Near-IR Radio Central engine Prompt emission Afterglow Figure adapted from Gehrels et al. 2007

4 Motivation Gamma-rays X-ray Optical Near-IR Radio Central engine Characterize short GRBs on parsec scales: kinetic energy density opening angle Prompt emission Afterglow Figure adapted from Gehrels et al. 2007

5 Outline Background Afterglow census Explosion properties Application to gravitational waves

6 One decade ago November 20, 2004

7 One decade ago October 27, 2004

8 One decade ago Rapid slewing Multi-wavelength Precise localization

9 Two populations of bursts SHORT, t < 2 sec Counts per second LONG, t > 2 sec Credit: NASA Time since Trigger (s)

10 Two populations of bursts SHORT, t < 2 sec Counts per second LONG, t > 2 sec Credit: NASA Time since Trigger (s)

11 Two populations of bursts Counts per second SHORT, t < 2 sec LONG, t > 2 sec 10% 90% Credit: NASA Time since Trigger (s)

12 The first short GRB afterglows GRB Fox et al Hubble Space Telescope ΔT < 48 hours

13 The first short GRB afterglows GRB Fox et al Hubble Space Telescope ΔT < 48 hours ~23 10 hr after burst discovery

14 The multi-wavelength Target-of-Opportunity afterglow chase Chandra XMM-Newton

15 The multi-wavelength Target-of-Opportunity afterglow chase Chandra Magellan (Chile) MMTO (Arizona) LBT (Arizona) XMM-Newton

16 The multi-wavelength Target-of-Opportunity afterglow chase Chandra Magellan (Chile) MMTO (Arizona) LBT (Arizona) UKIRT (Hawaii) XMM-Newton

17 The multi-wavelength Target-of-Opportunity afterglow chase Chandra Magellan (Chile) MMTO (Arizona) LBT (Arizona) UKIRT (Hawaii) VLA (New Mexico) XMM-Newton

18 Afterglow census

19 Why do we need multi-wavelength? log(flux) log(frequency)

20 Why do we need multi-wavelength? log(flux) E K,iso, n E K,iso, n E K,iso log(frequency)

21 Short GRB X-ray afterglows

22 Short GRB X-ray afterglows 60/78 detections

23 Short GRB optical afterglows Optical

24 Short GRB optical afterglows Optical

25 Short GRB optical afterglows Optical 6-10 m 26/72 detections

26 Short GRB radio afterglows 10 3 Detection 3 upper limit Radio Radio Flux Density (µjy) Time after Burst t (days)

27 Short GRB radio afterglows 10 3 Detection 3 upper limit Radio Radio Flux Density (µjy) Time after Burst t (days)

28 Short GRB radio afterglows 10 3 Detection 3 upper limit Radio Radio Flux Density (µjy) /50 detections Time after Burst t (days)

29 Afterglow census log(flux) log(frequency)

30 Afterglow census log(flux) Radio Optical Near-IR X-ray # Detected # Observed E K,iso, n E K,iso, n E K,iso log(frequency)

31 What can the lack of afterglow detections tell us about their Explosion Properties?

32 What can the lack of afterglow detections tell us about their Explosion Properties?

33 An example: GRB A X-ray and optical afterglows, radio non-detection F ν

34 An example: GRB A X-ray and optical afterglows, radio non-detection F X-ray ν

35 An example: GRB A X-ray and optical afterglows, radio non-detection F Optical Near-IR X-ray ν

36 An example: GRB A X-ray and optical afterglows, radio non-detection F Radio Optical Near-IR X-ray ν

37 An example: GRB A X-ray and optical afterglows, radio non-detection F Radio Optical Near-IR X-ray ν

38 An example: GRB A X-ray and optical afterglows, radio non-detection +0.3 E K,iso = x erg! +3.1 n = x 10-3 cm -3 F Radio Optical Near-IR X-ray ν

39 Each burst has its own story...

40 Population explosion properties DENSITY long GRBs <n> = 4.1 x 10-3 cm -3 95% is <1 cm -3

41 Population explosion properties DENSITY KINETIC ENERGY long GRBs long GRBs <n> = 4.1 x 10-3 cm -3 <E K,iso > = 1.7 x erg 95% is <1 cm -3!! No trend with elliptical vs. star-forming host

42 highly collimated spherical

43 Fong et al. 2012; 2014

44 Fong et al. 2012; 2014 if θ jet ~ 10 deg, E true ~ erg R true ~ 1000 Gpc -3 yr -1

45 Application to gravitational wave counterparts

46

47 For a compact object merger at 200 Mpc!!

48 For a compact object merger at 200 Mpc!! for an observer angle of twice the opening angle of the jet

49 For a compact object merger at 200 Mpc!! with typical inputs from observed short GRBs n~10-3 cm -3, E~10 49 erg!!! for an observer angle of twice the opening angle of the jet

50 For a compact object merger at 200 Mpc!! with typical inputs from observed short GRBs n~10-3 cm -3, E~10 49 erg!!! the optical light curve will peak at 24.5 mag (10 40 erg s -1 ). for an observer angle of twice the opening angle of the jet

51 For a compact object merger at 200 Mpc!! with typical inputs from observed short GRBs n~10-3 cm -3, E~10 49 erg!!! the optical light curve will peak at 24.5 mag (10 40 erg s -1 ). Yikes. for an observer angle of twice the opening angle of the jet

52

53 Trends with host properties?

54 Trends with host properties? δr

55 Trends with host properties? δr Star-forming Elliptical

56 Trends with host properties? δr Star-forming Elliptical