1. Producing Science with the Palomar Transient Factory Branimir Sesar (MPIA, formerly Caltech)

2. Producing Science with the Palomar Transient Factory Branimir Sesar (MPIA, formerly Caltech)

3. Survey Goals & Key Projects (Law et al. 2009, Rau et al. 2009) Goal: to study the transient and variable sky Extragalactic Transients in nearby galaxies, CC SNe, TDE, Hα Sky Survey, search for eLIGO/EM counterparts Galactic AM CVn systems (H + He WD), CVs, RR Lyrae stars to map the Milky Way structure and dynamics Solar System: KBOs, small NEAs/PHAs (prospect for growth → asteroid retrieval mission)

4. P48 wide-field imager → Discovery engine P200 Spec. followup P60 Photo. followup

5. P48 wide-field imager → Discovery engine P200 Spec. followup P60 Photo. followup Fast spectroscopic typing with SED Machine (R~100, PI: Nick Konidaris, Caltech) R~100 spectra of various transients and variables → important spectral features are still discernible R~100 spectra of various transients and variables → important spectral features are still discernible

6. P48 Overview 7.26 deg 2 field-of-view → will be upgraded to 47 deg 2 for ZTF (2015-2016) 1” / pixel resolution → barely sampled at median 2” seeing → PSF photometry possible Robotic telescope & scheduler → automatic selection of fields → time & money saver g', R, and 2 Hα filters ~250 images / night CFHT12k camera (well-defined cosmetics)

7. PTF Image Differencing Engine (PTFIDE; Frank Masci, IPAC) Real-time Pipeline (transients)

8. Time from exposure to alert: 20 – 40 min 0.3% contamination, 0.7% of real transients missed

9. IPAC Pipeline (variables & light curves) Repeatability of < 0.01 mag R-band 5σ limit @ 20.6 mag (aperture), 20.9 mag (PSF) 12,000 deg 2 with >30 epochs 1 st PTF/iPTF data release (M81, M44, M42, Cas A, Kepler) http://www.ptf.caltech.edu/page/first_data_release http://www.ptf.caltech.edu/page/first_data_release Public release of PTF, iPTF and ZTF data (w/ NSF funding) coverage of the Galactic plane (|b| < 5 deg)

10. Science 2,254 spectroscopically confirmed SNe 88 publications (5 in Nature) Finding dSphs with PTF SN Ia in M101 (PTF11kly; Nugent et al. 2011, Li et al. 2011)

11. Hundreds of low-luminosity dSph galaxies orbiting the MW? Low-luminosity dSph Tollerud et al. (2008) Estimated number of observable faint MW satellites LSST should be able to observe ~300 low- luminosity dSphs About 50 low-luminosity dSphs in ~10,000 sq. deg and between 60 - 100 kpc

12. Segue I (M V = -1.5, D = 23 kpc, r h = 30 pc) MSTO RR Lyrae BHB Only 6 RGB stars! Seg RGB → orange Seg MS → blue

13. “Segue I”-like dSph at 60 kpc (M V = -1.5) dSph RGB → orange foreground → white

14. Segue I (M V = -1.5, D = 23 kpc, r h = 30 pc) MSTO RR Lyrae BHB Only 6 RGB stars! Seg RGB → orange Seg MS → blue

15. Table 4 of Boettcher, Willman et al. (2013) Boo III 1 -2.0 (Sesar, submitted to ApJ) Boo II 1? ? (within 1.5' of Boo II @ 33 kpc) Almost every dSph has at least one RR Lyrae star → use distant RR Lyrae stars as tracers of low-luminosity dSphs

16. ~180 RRab stars between 60 and 100 kpc Orange – Sgr?

17. “Segue I”-like dSph at 60 kpc dSph is still invisible in the color- magnitude diagram

18. “Segue I”-like dSph at 60 kpc dSph RGB → orange foreground → white

19. Pick a distant RR Lyrae star D = 60 kpc

20. Select stars that may be at the distance of the RR Lyrae star M92 isochrone at 60 kpc

21. Plot angular coordinates with respect to the coordinates of the RR Lyrae star

22. Convert angular to projected distances

23. Repeat for a different RR Lyrae star (i.e., sightline) and add onto the same plot

25. Overdensity of sources when f dSph = 1.0... Note: This is just for visualization

26. ...when f dSph = 0.2

27. … when f = 0 (i.e., just the background)

28. Sensitivity of the detection method Black pixels: parameter space where detection is possible at 3-sigma level 19 27 37 49 74 98 123 Minimum number of dSphs needed for a detection

29. What is observed in SDSS

30. Constraining the luminosity function of dSph galaxies r h = 120 pc r h = 30 pc

31. PanSTARRS1 S82 light curve PS1 light curve PS1 is deeper than PTF, and covers more area → repeat search

32. RR Lyrae Stars Old, evolved stars (> 9 Gyr) → trace old populations of stars Standard candles → identify them → know their distance (with ~6% uncertainty) Bright (V ~ 21 at 110 kpc) Variable stars (P ~ 0.6 day) with distinct light curves ( ~1 mag amplitude) → easily identifiable Repeated observations (~30 or more) are needed Light curve of an RR Lyrae type ab

33. Death throes - An outburst from a massive star 40 days before a supernova explosion (Ofek+ 2013) No detection @ -60 & -50 days Outburst! Explosion!

34. Localization of an optical afterglow in 71 deg 2 (Singer et al. 2013) ZTF will cover this area with ~2 images Optical afterglow

35. GRB 130702A to iPTF13bxl Timeline 00:05 Fermi GMB trigger (UT July 2 nd ) 01:05 position refined by human (GBM group) 03:08 Sun sets at Palomar 04:17 PTF starts observations (10 fields, 2x60-s per field; 72 square degrees) 4214 "candidates": 44 were known asteroids, 1744 were coincident with stars (r<21) → 43 viable candidates Human inspection reduced this to 6 excellent candidates iPTF13bxh core of a bright galaxy, iPTF13bxr known quasar, iPTF13bxt was close to a star in SDSS Remaining candidates: iPTFbxl(RB2=0.86), iPTFbxk (RB2=0.83) and iPTFbxj (RB2=0.49) Sunrise in California

36. GRB 130702A to iPTF13bxl Timeline 00:50 Swift observations for iPTF13bxl requested (UT July 3 rd ) → X-ray source detected 04:10 Robotic observations of these candidates at P60 → iPTFbxl showed decline relative to first P48 observation (!) 04:24 Spectral observations on the Palomar 200-inch → spectrum is featureless (!!) 08:24 Announced iPTF13bxl as afterglow (ATEL, GCN) 17:34 LAT localization (3.2 square degrees) 19:03 IPN announces annulus of width 0.9 degrees 23:17 Magellan observations led to z=0.145

37. Small, but potentially hazardous asteroids Adam Waszczak (grad student @ Caltech) NEA 2014 JG55 (diameter: 10 m, closest approach: ¼ Earth-Moon distance)

38. RR Lyrae stars in SDSS Stripe 82 (Sesar, Ivezić+ 2010) “Smooth” inner halo ends at 30 kpc → only streams and dSphs beyond 30 kpc?

39. Be Aware of the Contamination Sesar et al. (2007): Smaller number of epochs in SDSS Stripe 82 Could not properly remove non-RR Lyrae stars ~30% contamination in our RR Lyrae sample Detection of false halo substructures Psc