1. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 1 The Darkest GRBs of the Swift Era Daniel Perley (Hubble Fellow, Caltech) Brad Cenko Nial Tanvir Andrew Levan Joshua Bloom Jens Hjorth Johan Fynbo Daniele Malesani Thomas Krühler Adam Morgan Nat Butler Maryam Modjaz

2. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 2 Dark Gamma-Ray Bursts X-ray Groot+1998 Generically: Events with surprisingly faint (generally, undetected) optical afterglows. optical

3. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 3 Dark Gamma-Ray Bursts Jakobsson+2004: use β ox If flatter than synchrotron permits (β ox <0.5), burst is absorbed (or nonsynchrotron). Van der Holst+ 2009: βox<βx-0.5 (but typical βx~1.0; very similar in practice) Frequency → Flux f ν → optical X-ray

4. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 4 The Origins of Dark GRBs Intrinsic causes: Low-luminosity afterglow Extrinsic causes: Obscured by dust in host Obscured by IGM at z > 6 All appear to contribute to some degree: need a uniform, complete sample to quantify frequencies!

5. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 5 The Origins of Dark GRBs Intrinsic causes: Low-luminosity afterglow Extrinsic causes: Obscured by dust in host Obscured by IGM at z > 6 All appear to contribute to some degree: need a uniform, complete sample to quantify frequencies! + P60 GROND Cenko+ 2009 Perley+ 2009 Greiner+ 2011 Kruhler+ 2011 Swift

6. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 6 Origins of Dark Bursts P60 extinction histogramP60 redshift histogram

7. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 7 Origins of Dark Bursts Mostly moderately (Av = 0.5-1.5) dust-obscured at moderate-z.

8. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 8 Origins of Dark Bursts Fewer very highly obscured events. Very few high-z events.

9. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 9 Origins of Dark Bursts Mostly moderately (Av = 0.5-1.5) dust-obscured at moderate-z. 2005-2012: 53/55 at z<5.5 54/55 at z<7 2005-2012: 5/55 at Av<2 ~10% “very” heavily obscured ~2% high-z

10. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 10 Origins of Dark Bursts Mostly moderately (Av = 0.5-1.5) dust-obscured at moderate-z. 2005-2012: 53/55 at z<5.5 54/55 at z<7 2005-2012: 5/55 at Av<2 ~10% “very” heavily obscured ~2% high-z Only a handful in single-telescope samples. How to find more?

11. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 11 Finding the Darkest Bursts Search through GCN circulars and published literature for reports of events with... No optical detection (1m+ class at early times, 4m+ class at late times) Unusually faint optical or NIR detection Bright NIR detection, fainter optical detection Reports of red color … etc. Many of these aren't (very) dark!

12. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 12 Limitations of βox Defined for R-band only (arbitrary) but extinction is extremely wavelength (and therefore redshift) dependent – e.g. J-band limit “worth” more than V-band, and colors are clinching! Fairly dusty events can have “normal” βox (if at low-z and/or β intrinsic ~ 1) Very mild obscuration can easily produce βox < 0.5 at moderate-z Minimum condition only: says little about degree of extinction opt NIR opt UV XRT

13. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 13 Identifying and Ranking the Darkest Bursts Most dark bursts are dusty: treat as an extinction fitting problem (even with limited data). Construct “minimum coeval SED” and fit with extinction.

14. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 14 Many very dusty Swift GRBs 40 with Av > 1.0 found so far (likely several others from qualitative afterglow reports)

15. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 15 High-z Bursts If photo-z from afterglow is not available, still separable from dusty events with X-ray N H and deep host follow-up. N H excess < 5 × 10 20 GRB 100205A: Very likely at z ~ 10 No host detected with Keck to R > 27

16. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 16 High-z Bursts If photo-z from afterglow is not available, still separable from dusty events with X-ray N H and deep host follow-up. GRB 100205A: Very likely at z ~ 9 No host detected with HST/WFC3 to H AB > 26.5 N H excess < 5 × 10 20

17. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 17 High-z Bursts If photo-z from afterglow is not available, still separable from dusty events with X-ray N H and deep host follow-up. GRB 100205A: Very likely at z ~ 9 No host detected with HST/WFC3 to H AB > 26.5 N H excess < 5 × 10 20 ~5 such events in entire Swift sample to date.

18. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 18 Rates of the Darkest Bursts 643 Swift GRBs (by end 2011) ~ 40 observed Av > 1 ~ 5 observed z > 7 (likely) >5% heavily obscured (P60: 7-20%) >~1% very high-z (P60: 0.2-5%)

19. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 19 Conclusions Moderately dusty (Av ~ 0.5 mag) events are quite common (~25%), and explain most β OX dark bursts. (Not a qualitatively different distribution from optically-bright bursts.) Extremely obscured events (Av ~ 2-10 mag) are also present, but in small numbers (~10%). Thanks to Swift, the sample of these events is now quite large. (~40+) High-z events remain extremely rare (~1-2%) (Part I)

20. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 20 Where are the dusty, luminous, massive hosts? GRB 990123, a “typical” (non-dark) host galaxy: z = 1.60 SFR = 5 M o /yr Mass = 2 × 10 9 M o Av < 0.5 mag

21. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 21 Where are the dusty, luminous, massive hosts? Shapley et al. 2012

22. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 22 990123 Where are the dusty, luminous, massive hosts? Shapley et al. 2012 GRBs from Savaglio et al. 2009

23. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 23 Pre-Swift GRB Colors

24. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 24 Dark GRB Host Campaign Observe every Av >~ 1.5 mag event we can find. 2005-2009 sample 30 dark host fields (29 30 detected!) 19 with spectroscopic redshift 2 with photometric redshift

25. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 25 Dramatic difference in optical-NIR colors

26. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 26 Dramatic difference in optical-NIR colors

27. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 27 Modeling host galaxy properties

28. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 28 Modeling host galaxy properties

29. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 29 Extinction → Redshift → SFR →Mass → Differences in every parameter

30. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 30 Dark GRB hosts are... More massive More rapidly star-forming Redder and dustier Extinction → Redshift → SFR →Mass → Redshift → Differences in every parameter

31. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 31 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr SFR vs. stellar mass

32. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 32 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr SFR vs. stellar mass (z>1)

33. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 33 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr Plenty of overlap, but: SFR vs. stellar mass (z>1)

34. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 34 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr “No” dark GRBs in dwarfs SFR vs. stellar mass (z>1)

35. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 35 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr New class #1: Dusty starbursts SFR vs. stellar mass (z>1)

36. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 36 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr New class #2: Very massive, steadily-growing galaxies SFR vs. stellar mass (z>1) New class #1: Dusty starbursts

37. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 37 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr SFR vs. stellar mass (z>1)

38. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 38 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr SFR vs. stellar mass

39. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 39 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr SFR vs. stellar mass

40. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 40 Dark bursts are a minority

41. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 41 10-20% Dark bursts are a minority

42. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 42 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr Luminous, red hosts have been found, but...

43. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 43 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr … there still aren't many.

44. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 44 Jakobsson+2011 & Hjorth talk … there still aren't many.

45. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 45 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr … there still aren't many.

46. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 46 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr ULIRGs LIRGs Normal galaxies … and there still aren't enough.

47. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 47 1/sSFR = 10 Myr 1/sSFR = 100 Myr 1/sSFR = 1 Gyr 1/sSFR = 10 Gyr ULIRGs LIRGs Normal galaxies 20-30% 20-30% 40-60% expected … and there still aren't enough. Perez-Gonzales et al. 2008, Shapley et al. 2012

48. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 48 1/sSFR = 1 Gyr 1/sSFR = 10 Myr 1/sSFR = 10 Gyr 1/sSFR = 100 Myr 1/sSFR = 10 Gyr ULIRGs LIRGs Normal galaxies 20-30% 20-30% 40-60% ~5% ~15% ~80% expected actual … and there still aren't enough. Perez-Gonzales et al. 2008, Shapley et al. 2012

49. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 49 R(GRB) = ??? × R(SFR) const? GRBs form in all galaxy environments after all! Implications

50. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 50 R(GRB) = ??? × R(SFR) const? GRBs form in all galaxy environments after all! … but not at the relative rates you would expect. Implications

51. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 51 R(GRB) = ??? × R(SFR) const? GRBs form in all galaxy environments after all! … but not at the relative rates you would expect. … and long-wavelength observations do not change this. Implications

52. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 52 1. Dark GRB hosts are different: systematically higher mass, SFR, and reddening. → No obscured GRBs from ultra-faint dwarfs (SMCs) so far. → No unobscured GRBs from very massive/luminous galaxies. → Optical extinction is galaxy- wide (nonlocal), with few exceptions. 2. GRBs form in all star-forming galaxies at z>1, but not at uniform rates. → Complex connection to metallicity (or other factor): no obvious “cutoff” Conclusions (Part II)

53. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 53

54. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 54 One Criterion is Not Enough! No optical detections at all βox < 0.5

55. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 55 One Criterion is Not Enough! No optical detections at all Afterglow reddened βox < 0.5 z > 6

56. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 56 One Criterion is Not Enough! No optical detections at all Afterglow reddened βox < 0.5 Mildly obscured, moderate-z, low β Dusty but intrinsically UV- luminous X-ray faint Mildly obscured and X-ray faint Dusty but intrinsically luminous Dusty and not luminous or low-z, or very very dusty z > 6

57. 2012-06-18 Daniel Perley The Darkest Swift Gamma-Ray Bursts Liverpool GRB Conference 57 One Criterion is Not Enough! No optical detections at all Afterglow reddened βox < 0.5 Mildly obscured, moderate-z, low β Dusty but intrinsically UV- luminous X-ray faint Mildly obscured and X-ray faint Dusty but intrinsically luminous Dusty and not luminous or low-z, or very very dusty z > 6