Download Shearer et al Observations of Fermi Pulsars 2009-10

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.