1. To a brief summary E. Verroi and G. Naletto

2. The main problem is the instability of count rates in the 4 channels  Bad possibility of pointing the star ( since we are “blind” )  Low focusing control  Great noise contribution for long periods variable objects

3. Why ?

4. First hypothesis... Shape of the beam section on the first lens of the optical train for a well centred source

5. First hypotesis... In this case we would see differences beetween the 4 channels BUT stability in the global countrate (4 ch sum) THERE IS ANOTHER PROBLEM

6. ...Another instrument  Only two stars have been analyzed (gzccnc216-pg0911)  We don’t know the sky conditions for these 2 acquisitions  Neither their positions in the sky A time tagging photon counting array returns data like this:

7. Pg are about 4 times brighter than gz but their noise (thermal + sky ) is about half. Integration of the signal over 20 minutes of acquisition  Gz-kind star and Pg-kind star 

8. Data analysis

9. Pg: x 3.6”--- y 3.9” Gz: x 2,4” --- y 2,5” Gaussian fit FWHM Gaussian fit FWHM Look out !! This is not the seeing !!

10. During the whole acquisition (20 min for each star) an optical system with the aperture of AQuEYE (3 arcsec entrance diameter) would acquire only: 53% 53% for gz 33% 33% for pg

11. In the worst case an 8” pinhole is necessary to collect about 90% of the photons during the acquisition! Fraction of collected photons as function of the pinhole diameter for Pg0911

12. This is the seeing: Binning the data we can simulate the seeing pg0911 with integration time = 0.5 s

13. Pg 3s T-bin Pg 1s T-bin Pg 0.5 s T-bin Pg 0.25s T-bin Gz 8s T-bin Gz 1s T-bin

14. Only a part of the problem is caused by auto guidance system. Centroid position of the star for 8s time bin for pg0911 The auto guide jumps are of the order of 0.5” but also with a “perfect” guide we don’t collect enough photons:

15. Fraction of photons collected as a function of the entrance aperture angular diameter for several measurements of seeing for a perfect guiding and well pointed instrument For this reason we choose to increase the pinhole dimension for IQuEYE as we will see later

16. Simulation of the signal for the four SPADs as AQuEYE would see it...

17. original simulated

18. IQUEYE The Italian Quantum Eye for NTT/TNG Assumptions: Telescope: focal length = 38.5 m; focal plane scale factor = 187 µ m/arcsec; f/10.85 Assumed FoV to be collected: 5 arcsec = 0.935 mm on telescope focus Needed total magnification (100 µ m diameter SPAD): smaller than 1/10

19. IQUEYE Optical Concept It has been considered a focal reducer with two couple of lenses, with a magnification of 1/3.25, and reducing a 5 ” telescope image (935 µ m) to 290 µ m (FWZH). Then, a pyramid splits the beam in four arms, and the following lenses further magnify the spot by 1/3.6, bringing the 5 arcsec spot size to 80 µ m diameter (geometric magnification). Focal reducer Aqueye like single arm

20. IQUEYE Optical Performance

21. The end

23. Summary of preceding episodes... The aim of this activity is to realize a “prototype” of the instrument QuantEYE, proposed for application to the focal plane of OWL. QuantEYE is a very fast photometer, dedicated to the observation of celestial targets in the photon counting regime at 1 GHz max count rate Our resources: 182 cm Ekar telescope in Asiago mounting AFOSC (Asiago Faint Object Spectrograph and Camera ) AFOSC is a focal plane instrument applied to the telescope focus with which the beam is collimated, filtered/dispersed (grism) and refocused (with a 0.58 magnification).

24. Summary of preceding episodes... Owing to the limitations we have on available resources, we decided to subdivide the telescope pupil in only four parts ( instead of the 100 previewed for QuantEYE ) focusing each of them on a dedicated 50  m SPAD detector.

25. Summary of preceding episodes... Specular Pyramid: Couples of Doublets: Focus the beam on the SPAD’s detector S.P.A.D. Single photon avalanche diode Optional Filters AFOSC focus Splits the beam in four parts towards each SPAD

26. Summary of preceding episodes... Our optics send a 180  m spot covering the whole pin-hole in 50  m in the image plane. 50  m is the spad’s detectors diameter To the presentation