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Comment: A few extra explanatory sentences.

Overview

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Overview

This page is for distribution of pulsar timing models made by the LAT team directly from LAT gamma-ray data, independent of any radio timing data that may exist. We use the methods documented in Ray, Kerr, Parent et al. (2011, ApJS, 194, 17, arXiv:1011.2468). The primary focus is on the blind search pulsars and other pulsars that are not easily timed in the radio or X-ray bands. If you would like a particular pulsar added to this page, please contact us. This work is being This work has been supported by the Fermi Cycle 3 Guest Observer program.

You are free to use these LAT timing solutions to fold your data. If you publish work based on these models, please reference Ray, Kerr, Parent et al. (2011) and this page in your publication. The primary intent is to support pulsar analyses requiring timing ephemerides, such as phase-resolved spectroscopy and analyses of sources close to bright pulsars through the use of pulsar `gating'.  If, on the other hand, you want to publish something based on the values of the timing model parameters (e.g. timing positions, glitch parameters, etc...) we ask that you contact us first because there may be important caveats or publication plans. Anchorparpar

Participants

Paul Ray, Aous Abdo, Matthew  Matthew Kerr, Pablo Saz Parkinson, Michael DormodyMax Razzano, and others... Anchorephemerisephemeris

Timing solutions

Latest models are available HERE

Models will be updated every 3-6 months, or sooner if requested.

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Thanks much to those who have moved on to other projects, including Damien Parent, Michael Dormody, and Aous Abdo.

Timing Solutions

New! Matthew Kerr has developed a sophisticated highly-automated timing pipeline that handles glitch detection and fitting in the presence of timing noise much better than our previous scripts. We run it on nearly all LAT-detected pulsars that are bright enough for a TOA to be formed in less than about 56 days of integration. The results are posted to a machine-generated web page accessible from the link below. Please pay attention to the following notes when accessing these models:

  • These methods used for this pipeline will be documented in Kerr et al. (2014, in prep).  Once this paper is available, please cite it for any uses of this work.
  • Each row of the table corresponds to one pulsar timed using the LAT data. Both the full par file and the TOAs are available via links in the first column.
  • The Whitened Residuals show the residuals for the full timing model.  Unlike previous timing solutions, whitening is achieved by estimating the time-domain realization of the timing noise, then subtracting this signal by linear interpolation (the "SIFUNC" terms in the ephemeris).
  • The Unwhitened Residuals show the residuals to a model without any red noise terms. For most pulsars, only the first frequency derivative is included in this model.  For the Crab, this includes up to F2.
  • Horizontal dashed lines on the plots indicate the epoch of glitches.
  • The Phaseogram shows a 2-D plot of the LAT photons vs pulse phase and time.
  • The Pulse Profile plot shows the full LAT profile along with the analytic template (solid blue, with the individual components in dashed blue lines). The residuals between the model and the data are in red.
  • The Position plot shows the timing position with uncertainty, along with the published multiwavelength location (e.g. X-ray counterpart), when available. The LAT timing position uncertainty includes the effects of timing noise.

Be very cautious about applying these models to data outside the START/FINISH range in the PAR file!  Many of them will not extrapolate well.  Also, beware that we don't typically follow any particular absolute phase convention in these models since they are gamma-ray only. In particular, you cannot assume that phase 0.0 is at the peak of the radio pulse (if there is one) or any other particular convention.  If you need to figure out phase ranges to blank, fold the data using the PAR file and make your selection based on that, not a phase range from a published paper or other source.

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List of Pulsars that have a LAT timing model

Note that not all of these pulsar will have up to date models depending on when we last ran them. If you have a need for one, just let us know.

Pulsars timed with the Fermi-LAT

Pulsar Name

Update Date

By

Start (MJD)

Finish (MJD)

Notes

Timing File

Rediduals

Phaseogram

J0007+7303

9-Feb-2012

Paul

54686.37

55421.29

Two overlapping timing models

PAR File

Timing Residuals

Phaseogram

J0007+7303

9-Feb-2012

Paul

55010.80

55961.10

Will try to merge into one later

PAR File

Timing Residuals

Phaseogram

J0106+4855

6-June-2012

Aous

54695.16

56071.43

Found Radio PSR (GBT 820 MHz)

PAR File

Timing Residuals

Phaseogram

J0205+6449

 

 

 

 

 

PAR File

Timing Residuals

Phaseogram

J0357+3205

5-June-2012

Paul

54695.86

56069.70

 

PAR File

Timing Residuals

Phaseogram

J0622+3749

6-June-2012

Aous

54697.88

56068.71

 

PAR File

Timing Residuals

Phaseogram

J0633+0632

5-June-2012

Aous

54697.88

56068.71

 

PAR File

Timing Residuals

Phaseogram

J0633+1746

6-June-2012

Aous

54684.15

56082.44

 

PAR File

Timing Residuals

Phaseogram

J0734-1559

23-Aug-2011

Damien

54693.79

55784.86

 

PAR File

Timing Residuals

Phaseogram

J1022-5746 / J1023-5746

29-Sep-2011

Damien

54691.24

55824.21

 

PAR File

Timing Residuals

Phaseogram

J1044-5737

30-Sep-2011

Max

54682.00

55794.04

 

PAR File

Timing Residuals

Phaseogram

J1124-5916

1-Nov-2011

Paul

54682.00

55191.00

 

PAR File

Timing Residuals

Phaseogram

J1124-5916

1-Nov-2011

Paul

55191.00

55800.00

 

PAR File

Timing Residuals

Phaseogram

J1135-6055

2-Oct-2011

Max

54726.05

55805.89

 

PAR File

Timing Residuals

Phaseogram

J1413-6205

5-June-2012

Aous

54695.15

56070.40

 

PAR File

Timing Residuals

Phaseogram

J1418-6058

29-Sep-2011

Damien

54690.22

55825.22

 

PAR File

Timing Residuals

Phaseogram

J1429-5911

29-Sep-2011

Damien

54693.30

55822.14

 

PAR File

Timing Residuals

Phaseogram

J1459-6053

4-Oct-2011

Damien

54694.21

55826.48

 

PAR File

Timing Residuals

Phaseogram

J1620-4927

29-Sep-2011

Damien

54695.73

55819.72

 

PAR File

Timing Residuals

Phaseogram

J1732-3131

29-Sep-2011

Damien

54694.89

55820.55

 

PAR File

Timing Residuals

Phaseogram

J1741-2054

29-Sep-2011

Damien

54693.30

55822.14

Found Radio PSR (Parkes Multibeam)

PAR File

Timing Residuals

Phaseogram

J1746-3239

4-Oct-2011

Damien

54700.10

55816.53

 

PAR File

Timing Residuals

Phaseogram

J1747-2958

4-Oct-2011

Damien

54693.30

55822.14

 

PAR File

Timing Residuals

Phaseogram

J1803-2148/J1803-2149

4-Oct-2011

Damien

54695.74

55820.89

 

PAR File

Timing Residuals

Phaseogram

J1809-2332

4-Oct-2011

Pablo

54682.00

55800.00

 

PAR File

Timing Residuals

Phaseogram

J1813-1246

4-Oct-2011

Damien

54692.79

55827.90

One or two glitches likely one glitch the GLF2_2 in the timing solution is probably a typo

PAR File

Timing Residuals

Phaseogram

J1826-1256

4-Oct-2011

Damien

54693.73

55822.91

 

PAR File

Timing Residuals

Phaseogram

J1833-1034

 

 

 

 

Paul requested from Fernando. He says 'next week' as of 2012 Feb 8.

PAR File

Timing Residuals

Phaseogram

J1836+5925

4-Oct-2011

Pablo

54682.00

55800.00

 

PAR File

Timing Residuals

Phaseogram

J1846+0919

4-Oct-2011

Damien

54697.42

55819.22

 

PAR File

Timing Residuals

Phaseogram

J1907+0602

24-Jan-2011

Aous

54682.66

55928.34

Found Radio PSR (AO L-band)

PAR File

Timing Residuals

Phaseogram

J1954+2836

4-Oct-2011

Pablo

54682.00

55800.00

 

PAR File

Timing Residuals

Phaseogram

J1957+5036/J1957+5033

4-Oct-2011

Pablo

54582.00

55800.00

 

PAR File

Timing Residuals

Phaseogram

J1958+2846

4-Oct-2011

Pablo

54582.00

55800.00

 

PAR File

Timing Residuals

Phaseogram

J2021+4026

6-Dec-2011

Max

54682.00

55777.00

 

PAR File

Timing Residuals

Phaseogram

J2028+3332

3-Oct-2011

Damien

54695.20

55824.27

 

PAR File

Timing Residuals

Phaseogram

J2030+4415

3-Oct-2011

Damien

54693.75

55825.72

 

PAR File

Timing Residuals

Phaseogram

J2032+4127

05-Jun-2012

Paul

54688.69

56076.87

Found Radio PSR (S-band GBT 1-hour)

PAR File

Timing Residuals

Phaseogram

J2055+2539

3-Oct-2011

Max

54742.90

55803.64

 

PAR File

Timing Residuals

Phaseogram

J2111+4606

7-Feb-2012

Paul

54689.59

55814.35

 

PAR File

Timing Residuals

Phaseogram

J2139+4716

29-Sep-2012

Max

54717.66

55783.01

 

PAR File

Timing Residuals

Phaseogram

J2229+6114

9-Feb-2012

Matthew

54589.66

55266.75

Solutions overlap

PAR File

Timing Residuals

Phaseogram

J2229+6114

9-Feb-2012

Matthew

55149.19

55808.57

Solutions overlap

PAR File

Timing Residuals

Phaseogram

J2238+5903

1-Oct-2011

Max

54682.00

55792.24

 

PAR File

Timing Residuals

Phaseogram

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Radio/X-ray Selected Pulsars that the LAT can do a better job on

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Pulsar Name

Comments

J0205+6449

in 3C 58

J0835-4510

Vela

J1124-5916

 

J2021+3651

Dragonfly

J2229+6114

in Boomerang

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Comments :

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The LAT solutions can be used with the Fermi plugin available in the TEMPO2 distribution.the TEMPO2 distribution. This is generally the preferred method as the Fermi ScienceTool gtpphase doesn't support the full complexity of many timing models.

Access Current Timing Models HERE