1. Ljubljana fiber fed fast photometer Andrej Čadež Bojan Dintinjana Anja Lautar Dejan Paradiž Dušan Ponikvar Bled, March.2008

2. Steps toward timing the Crab pulsar - hardware Telescope with robotic guiding system Off- axis fiber pickup in the image plane Photon counting detector Event time tagging device (CAEN) GPS clock The inevitable computer

3. Optics

4. Focal plane optics

5. Pointing errors (error-signal)

6. Focusing on the fiber with a flat mirror A rough focus is obtained, sufficient to start finding fiber position with respect to CCD field of view.

7. Guiding on the fiber 1: find the star in the field of the camera 2: choose it and by clicking it, send it to initial position (still in the field of camera) 3: check initial position and send it to the fiber – a new blue image indicates the field of view with star on fiber 4: new picture is taken in blue – the expected image turns red 5: choose blue and corresponding red stars to calculate corrections to guide the telescope

9. Fine tuning: Autocollimator focus needs to be fine tuned on stars. This is done by scanning the signal with respect to the position of guiding stars on the CCD image. After the centroid is found, the telescope focusing is adjusted to highest fiber signal. The new position of the fiber plane is calculated and the fiber plane repositioned to align the fiber focal plane with CCD focal plane. Focusing is completed when the ratio star count rate/sky count rate is the same as in the CCD image. Image distortion must be taken into account when positions of off axis guide stars are used with respect to positions of guide stars in the original image with the object in the field of view. Image distortion moves the position of a star by up to 10arc seconds at the edge of the field (15arc min off axis). Image distortion errors were handled in two steps: 1) CCD was displaced off axis to bring fiber position closer to optical axis ; 2) Focal plane field distortion is determined by comparing image and catalogue position data using Fitsblink software.

10. Focusing on fiber – fiber plane scan

11. Scan - focusing

12. Field distortion

13. Field distortion correction

14. 10 th magnitude star signal

15. First Crab observation (March 2 nd 2008) (before field distortion correction)

16. Conclusions The Ljubljana fiber fast photometer performs as expected: the SPAD count rate is comparable to the photon count rate determined from CCD images, thus no appreciable light losses in the fiber have been detected. A need to compare the signal with Asiago. Telescope pointing errors are appr. 0.3 arc sec rms with autoguding correction arriving every 30sec. Some excursions up to 1.5 arc seconds, are due to loss of autoguider correction signal. Field distortion correction is expected to fix the problem. CAEN electronics performs as specified, the maximum count rate is not a limiting factor for stars fainter then 8 th magnitude (for VEGA). Outstanding problems: the 50  m fiber has an 1.7 arc seconds diameter receiving area. This area must be increased to 3 arc seconds diameter (100  m). Optical coupling to a larger fiber was tested, but losses were unacceptable. Other solutions under consideration: a) tapered fiber coupling b) focal reducer lens before the fiber c) use a SPAD with a 100  m fiber input.

17. Observing Crab with a fast photometer – why it might be interesting? Karpov et al., Astrophys Space Sci 2007 it is the brightest pulsar seen in optical, it is nearby and young one of the main properties of the Crab emission is the very high stability of its optical pulse shape despite the secular decrease of the luminosity, related to the spin rate decrease (Pacini 1971; Nasuti et al. 1996) at the same time pulsars in general and Crab itself are unstable it has been found early that the variations of the Crab optical light curve, in contrast with the radio ones, are governed by Poissonian statistics (Kristian et al. 1970) a number of observations show the absence of non-stationary effects in the structure, intensity and the duration of the Crab optical pulses, and the restrictions on the regular and stochastic fine structure of its pulse on the time scales from 3 μs to 500 μs (Beskin et al. 1983; Percival et al. 1993), the fluctuations of the pulse intensity (Kristian et al. 1970) small changes of the optical pulse intensity, synchronous with the giant radio pulses, have been detected (Shearer et al. 2003) the evidence for the short time scale precession of the pulsar has been detected by studying its optical light curve (Čadez et al. 2001)

18. Optical spectrum of pulsar is pure power law Carramiñana, Čadež & Zwitter (2000) Stroboscope adapted to LFOSC at 2.1m. The two pulses have same spectrum: index  = 0.2  0.1 for 5000-7500Å. No absorption feature at 5900Å. The underlying nebular spectrum.

19. Nebular emission lines are excited by leptons generated at the pulsar and moving along the magnetic field lines Movie outside Powerpoint

20. Pulsations in slow motion (Vidrih, Carraminana, Čadež 2002)

21. Pulse shapes (HST – Dolan, Galičič, Kitt Peak – Fordham et al.)

22. Changing pulse shapes? (Karpov et al. 2007) Pulse shape is exhibiting changes on a few microsecond scale in a few days

23. Timing noise (Karpov et al. 2007) Timing noise of a few  s on a time scale of ~1h and ~100  s on a time scale of days has been measured

24. Does the pulsar free-precess? (Čadež, Calvani, Carraminana, Galičič,Vidrih 1996-2003) Pulsar stroboscopic phase photometry and HST data (over 10 years of data span) show evidence of enhanced phase noise at 0.01711 and 0.0133 Hz