1. First results from The Palomar Transient Factory Eran Ofek Einstein fellow CALTECH

2. Talk Layout PTF goals System overview Capabilities and products What have we found so far? Next Generation Transients Factory

3. PTF collaboration PI: S. R. Kulkarni Caltech, LCOGT, Berkeley, LBL, IPAC, Columbia, Oxford, Weizmann

4. PTF goals To study the transient and variable sky Core collapse SNe Calibrating SN Ia for cosmology Explore new regions of transients parameter space Stellar variability: RR Lyr, AM CVn,… Solar system: Asteroid rotations Law et al., Rau et al.

5. PTF system overview 48” Oschin Schmidt camera (Palomar obs.) 7.2 deg 2 FOV (92 Mpix) Scale: 1”/pix, lim. mag ~21 Robotic telescope & scheduler Full automatic operation Auto. Selection of science targets

6. PTF system overview 60s exposure + 35s readout ~510,000 deg 2 yr -1 Filters: g, R, H  + Real time image Subtraction and Transient classification

7. PTF system overview Real time transient classification Galaxy zoo transient

8. PTF observing strategy Observing strategy 40% : 3-day cadence 40% : 1-day cadence 10% : All sky H  survey 10% : Monitoring of star formation regions

9. PTF followup

10. What did we observe so far? Log 10 (N images )

11. Abs. photometry Abs. photometry calibration good to 2-3% Using SDSS stars as standard stars to calibrate fields outside SDSS footprint (photometric nights) CCD 4

12. Relative photometry Relative photometry ~3-5mmag

13. Deep coadd Deep sky: ~10 images lim. mag. ~22.5 ~100 images lim. mag. ~24

14. Data Release First public data release: 2011

15. Galactic What have we found? Galactic: 51 dwarf novae 3 AM CVn Planet candidates around M-dwarfs PTF 10nvg: enhanced accretion and outflow in Class-I protostar New FU Ori star Levitan et al., in prep. Law et al., in prep. Covey et al., 1011.2565 Miller et al., 1011.2063

16. AM CVn Primary background noise for LISA PTF 09hpk Levitan et al., in prep.

17. FU Ori and other PTF10qpf: new FU Ori star Miller et al., 1011.2063

18. Planets around M-dwarfs Only 16 planetary systems detected around M-dwarfs Possible to find planets in the habitable zone… Calibrating the mass-radius relation of M-dwarfs Law et al., in prep.

19. Planets around M-dwarfs Some eclipsing M-dwarfs we found…

20. Planets around M-dwarfs Consistent with secondary radius ~ 1.5-2.0 R J Law et al., in prep.

21. Planets around M-dwarfs Law et al., in prep.

22. Planets around M-dwarfs Law et al., in prep.

23. Asteroids rotation Poolishok et al., in prep.

24. Asteroids rotation Poolishok et al., in prep.

25. Extragalactic What have we found? Since March 2009: >5,000 transient candidates 1036 spectroscopically confirmed SNe 692 Ia 49 Ibc 257 II ~3% of these “SNe” are weird and hard to classify into existing scheme: e.g., faint and fast, Ca rich, luminous, etc. Kasliwal et al., 1005.1455 Kasliwal et al., ApJ 723, 98

26. HST UV spectra of Ia SNe PTF Can find SN Ia early PI: R. Ellis

27. HST UV spectra of Ia SNe The first dozen… Cooke et al., 1010.2211

28. HST UV spectra of Ia SNe Cooke et al., 1010.2211 The mean UV spectrum of the z~0 and z~0.5 agree, but some differences in metallic absorptions

29. The hosts of CC SNe Arcavi et al., ApJ 721, 777 M R <-18M R >-18 Ic-BL and IIb are more common in dwarf hosts, Stripped CC (Ic) are not seen in dwarf hosts. Probably because in lower metallicity hosts, Metallicity-driven mass loss is reduced.

30. The SN2005E family >23 kpc from NGC 1032 No host: M R >-7 Spec: He burning products Ca reach Possibilities: Acc. Induced Collapse.Ia May solve puzzles: 44 Ca in Solar System 44 Ti-> 44 Ca via b decay Positrons annihilation in Galactic bulge Perets et al. Nature 465, 322

31. The SN2005E family: 09dav  40kpc from putative spiral host  Abs R mag ~-15  Fast: 1 mag in 10 day  Very red, g-r = 1.2  Similar to SN1991bg but with He  Hydrogen in nebular phase Kasliwal et al., in prep. Sullivan et al., in prep.

32. The SN2005E family: 10iuv  37 kpc from putative host  Abs R. mag ~ -15.  Fast: 1 mag in 10 days  Intriguing Nebular Spectra Kasliwal et al., in prep.

33. Luminous supernovae Galactic: 51 dwarf novae; 2 AM CVn;…

34. Luminous supernovae Quimby et al., 0910.0059

35. Luminous supernovae Quimby et al., 0910.0059

36. Shock breakout / PTF PTF detects SNe early -> can detect shock breakout (but still limited by cadence). GALEX + PTF synergy PTF + rapid follow up with Swift /UVOT/XRT

37. Shock breakout / PTF Ofek et al., Apj in press PTF 09uj

38. Shock breakout / PTF Ofek et al., Apj in press PTF 09uj

39. Shock breakout / PTF PTF 09uj Ofek et al., Apj in press

40. Shock breakout / PTF PTF 09dah

41. NGTF Thinking about the next project… PTF-2 will have a ~30-40 deg 2 camera Mounted on the 48” schmidt telescope Simple scheduling – one day cadence objective: find them young ~8000 deg 2 day -1 Scheduled for 2014

42. End Thank you!

43. Shock breakout / Intro Photons first emerge from SN (breakout) when they diffuse ahead of the shock faster than the shock propogates Happens at optical depth:  =c/v duration: ~r/c Decay time: ~r/v

44. Fast supernovae: 10bhp Kasliwal et al., ApJ 723, 98 Very fast: decay ~5 days, M R ~-17 (e.g., similar to SN200bj, [Poznanski+10])

45. Fast supernovae: 10bhp Kasliwal et al., ApJ 723, 98 If powered by 56 Ni then Ni mass ~0.02 M sun and SN quickly becomes optically thin to  -rays. AIC (?).Ia (?)

46. Luminous red nova PTF 10fqs in M99 Kasliwal et al., 1005.1455 Faint/slow event in M99: M R ~-11

47. PTF 10fqs Kasliwal et al., 1005.1455 ~10,000 km/s (?)

48. Search for SB in Chandra archive with Mike Muno Downloaded the entire Chandra archive Search for transients and highly variable Objects (on short time scale) First pass completed: complete for events brighter than 40 counts No SN 2008D-like events (Soderberg et al. 2008) Next: calc. efficiency and extend to faint sources

49. Relative photometry Solution using linear least squares m ij – instrumental mag i-star (1..p), j-image (1..q) Solving per field (overlap between fields not guaranteed)  ij – instrumental mag err

50. Relative photometry Using linear least squares H (“design matrix”) Observations Free parameters

51. Relative photometry Solution using linear least squares We need to solve (in the presence of errors):

52. Relative photometry Simultaneous absolute calibration H is (pq)x(p+q) matrix However, rank is p+q-1 Adding calibration block

53. Relative photometry Additional de-trending We can add more columns to H and P. For example: Airmass x color term Positional terms Multiple CCDs (i.e, overlap)