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Annual Report International Time Proposal Report Programme title: Observations of Fermi Pulsars Reference number: ITP02 Information on the team PI : Dr Andy Shearer, Centre for Astronomy, NUI, Galway [email protected] +353 49 3114 CoI : Dr. Gottfried Kanbach : MPE Prof Vik Dhillon : University of Sheffield Dr Roberto Mignani : Mullard Space Science Laboratory, Dr Aga Słowikowska: Institute of Astronomy, University of Zielona Gora, Poland Introduction This programme was intended to carryout CCD imaging observations of pulsars detected by the Fermi telescope. These would then be followed by observations with one of three high time resolution cameras which would be able to make definitive observations on the basis of timing. Under this round of the ITP programme we started the CCD imaging of Fermi pulsars and had time for one run using a time sensitive camera - Optima on the NOT. Sadly the Optima run was blighted by very poor weather. This report is a preliminary statement of where we are in our observations. We are about 60% complete on the basis of the allocations we have been given and 30% completed on the basis of the requirements to complete the programme. Time allocation received (give breakdown of telescopes and dates allocated) Summary of Observations and Allocations Dates Telescope Weather Moon Comments 2009 Aug 1-3 INT/WFC Reasonable Bright Good run - see below 2009 Aug 1-3 TNG/ Dolores Good Dark Good run - see below 2009 Dec 1-3 NOT/ Optima Very bad Dark No observations possible Mixed Dark/ Grey Good run of observations some weather (transparency) and technical problems 2010 Jan 14-18 INT/WFC 2010 Mar 25-27 WHT/ GASP Bright To be taken TNG/ Dolores Dark To be taken 2010 July 9th Preliminary Results The table shows a summary of the observations. Target PSR J1836+5925 J2021+4026 J2032+41 J0007+7303 J0205+6449 J0357+32 B0355+54 SGR0418+5729 J0613-0200 J0631+1036 Filte r Telescopes Observation Time (s) V INT/TNG 3960 R INT/TNG 3660 B INT 7320 V INT 10860 R INT 1250 B TNG 1500 V TNG 3960 R TNG 3660 V TNG 2760 R INT/TNG 11700 V TNG 3060 R INT/TNG 14820 B INT 6000 R INT 6000 I INT 6000 R INT 12100 Hα INT 6160 R TNG 2110 I TNG 3030 B INT 3000 I ING 1200 V INT 3300 R INT 3300 I INT 3300 Target PSR Filte r Telescopes Observation Time (s) B INT 6900 V INT 6610 R INT 3000 J0633+0632 I INT 3000 J0751+1807 B INT 3000 V INT 3000 I INT 3000 B INT 2400 V INT 6600 R INT 4200 I INT 2700 J0633+0632 J1231.5-1410 We are nearing the end of our initial analysis which gives a good starting point for actual identification using timing. Our limiting magnitudes, were in the range 23.5 (INT bright time) to 26.5 TNG Dark with the majority in excess of 25. The next stage will be to compare with existing X and gamma ray fluxes to determine FX/FOpt either for identification or in the case of upper limits to give limits to emission mechanism (thermal, beaming angle ...) for the particular pulsar. For two of our pulsar [PSR J0007+7303 and PSR J0205+6449] we already have candidate targets for follow on timing observations. Fermi targets have increasingly improved locations, through longer timing solutions. Consequently optical identification will be easier in the future based upon these improved position and then timing. Publications strategy Our initial upper limits, and tentative detections, will be published in four papers currently under preparation. PSR J0205+6449 - Possible Optical Counterpart PSR J0007+7303 - Upper Limits to the Optical Counterpart Survey of Optical Counterparts to Northern Hemisphere Fermi Pulsars Optical Upper Limits for the Gamma-Ray Pulsar PSR J0357+32 These will be submitted to MNRAS in late March. Two more papers will submitted to A&A in May 2010 Optical Observations of the Pulsar PSR B0355+54 and possible PWN Optical and X-ray observations of the Putative Gamma Ray Source 0FGL J2021.5+4026 Future publications will include an overall summary paper, specific results from the GASP observations and the final TNG observation in July. Future Observations We will be requesting more time under the International Time Programme primarily to use the time resolved camera systems UltraCam, Optima and GASP. We are particularly interested in polarisation measurements as these give a unique insight into the geometry of the emission region - these observations can be taken by Optima and GASP. Follow on observations, primarily of southern hemisphere objects will also be made by the same systems (UltraCam, GASP and Optima) and the Iqueye camera using ESO facilities (NTT and VLT). Benefits of the International Time Programme The ITP has enabled something unique in optical pulsar astrophysics - that is sufficient telescope time to carry out a survey. Without a proper survey optical pulsar studies have been limited to observations of a few favourite targets. Having a such a survey enables a proper characterisation of optical pulsar properties and statistics. A secondary benefit has been the ability, through ITP, to coordinate some of the observational programmes of three significant high-time resolution optical instruments.